public class JSOFA extends Object
Modifier and Type | Class and Description |
---|---|
static class |
JSOFA.Astrom
Star-independent astrometry parameters.
|
static class |
JSOFA.Calendar
Representation of Gregorian Calendar with fractional day.
|
static class |
JSOFA.CalendarHMS
Representation of Gregorian Calendar with integer hours minutes and seconds.
|
static class |
JSOFA.CatalogCoords
Typical catalogue coordinates.
|
static class |
JSOFA.CelestialIntermediatePole
The components x,y are components of the Celestial Intermediate
Pole unit vector in the Geocentric Celestial Reference System.
|
static class |
JSOFA.EquatorialCoordinate
Position consisting of (ha, declination) pairs in radians.
|
static class |
JSOFA.EulerAngles
Euler Angles.
|
static class |
JSOFA.FrameBias
Frame bias components of IAU 2000 precession-nutation models.
|
static class |
JSOFA.FWPrecessionAngles
Precession angles, IAU 2006 (Fukushima-Williams 4-angle formulation).
|
static class |
JSOFA.GeodeticCoord
Geodetic coordinates.
|
static class |
JSOFA.HorizonCoordinate
Position consisting of (az, el) pairs in radians.
|
static class |
JSOFA.ICRFrame
The Celestial Intermediate Pole coordinates are the x,y
components of the unit vector in the Geocentric Celestial
Reference System.
|
static class |
JSOFA.JulianDate
Julian Date representation.
|
static class |
JSOFA.Ldbody
Body parameters for light deflection.
|
static class |
JSOFA.NormalizedVector
A normalized vector with r being the modulus and u[3] being the unit vector.
|
static class |
JSOFA.NutationTerms
Nutation Terms.
|
static class |
JSOFA.ObservedPosition
Observed Position.
|
static class |
JSOFA.ObservedPositionEO
Observed position with the equation of the origins.
|
static class |
JSOFA.PrecessionAngles
equinox based precession angles.
|
static class |
JSOFA.PrecessionDeltaTerms
Precession correction terms.
|
static class |
JSOFA.PrecessionNutation
Precession-nutation model.
|
static class |
JSOFA.PVModulus
Modulus of pv-vector.
|
static class |
JSOFA.RefCos
constants A and B in the atmospheric refraction model
dZ = A tan Z + B tan^3 Z.
|
static class |
JSOFA.ReferenceEllipsoid
Reference Ellipsoid of Earth.
|
static class |
JSOFA.SphericalCoordinate
Position consisting of (α, δ) pairs in radians.
|
static class |
JSOFA.SphericalCoordinateEO
Spherical coordinate with equation of origins .
|
static class |
JSOFA.SphericalPosition
A position expressed in spherical polar coordinates.
|
static class |
JSOFA.SphericalPositionVelocity
A position and velocity expressed in spherical polar coordinates.
|
static class |
JSOFA.TangentPlaneCoordinate
Tangent Plane Position consisting of (xi, eta) pairs in radians.
|
static class |
JSOFA.TangentPointDirectionCosines
Tangent point soutions as direction cosines.
|
static class |
JSOFA.TangentPointSolution
Tangent point soulutions.
|
Modifier and Type | Field and Description |
---|---|
static double |
AULT
Light time for 1 au (s) 499.00478383615643
|
static double |
CMPS
Speed of light (m/s) 2.99792458E8
|
static double |
D2PI
2Pi 6.283185307179586
|
static double |
DAS2R
Arcseconds to radians 4.84813681109536E-6
|
static double |
DAU
Astronomical unit (m) IAU 2012 1.495978707E11
|
static double |
DAYSEC
Seconds per day.
|
static double |
DC
Speed of light (au per day) 173.1446326742403
|
static double |
DD2R
Degrees to radians 0.017453292519943295
|
static double |
DJ00
Reference epoch (J2000.0), Julian Date 2451545.0
|
static double |
DJC
Days per Julian century 36525.0
|
static double |
DJM
Days per Julian millennium 365250.0
|
static double |
DJM0
Julian Date of Modified Julian Date zero 2400000.5
|
static double |
DJM00
Reference epoch (J2000.0), Modified Julian Date 51544.5
|
static double |
DJM77
1977 Jan 1.0 as MJD
|
static double |
DJY
Days per Julian year
|
static double |
DMAS2R
Milliarcseconds to radians 4.84813681109536E-9
|
static double |
DPI
Pi 3.141592653589793
|
static double |
DR2AS
Radians to arcseconds 206264.80624709636
|
static double |
DR2D
Radians to degrees 57.29577951308232
|
static double |
DS2R
Seconds of time to radians 7.27220521664304E-5
|
static double |
DTY
Length of tropical year B1900 (days) 365.242198781
|
static double |
ELB
L_B = 1 - d(TDB)/d(TCB) at TAI 1977/1/1.0
|
static double |
ELG
L_G = 1 - d(TT)/d(TCG)
|
static int |
IYV
Release year for this version of jauDat 2021
|
static String |
JSOFA_RELEASE
JSOFA release "20210512"
|
static JSOFA.JulianDate |
latestConfirmedNoLeapSecondChange
The latest confirmed omission of a leap second form IERS
|
static String |
SOFA_RELEASE
tracked IAU SOFA release "2021-05-12".
|
static String |
SOFA_REVISION
tracked IAU SOFA revision "18".
|
static double |
SRS
Schwarzschild radius of the Sun (au) 1.97412574336E-8
= 2 * 1.32712440041e20 / (2.99792458e8)^2 / 1.49597870700e11
|
static double |
TDB0
TDB (s) at TAI 1977/1/1.0
|
static double |
TTMTAI
TT minus TAI (s)
|
static double |
TURNAS
Arcseconds in a full circle 1296000.0
|
Constructor and Description |
---|
JSOFA() |
Modifier and Type | Method and Description |
---|---|
static char |
jauA2af(int ndp,
double angle,
int[] idmsf)
Decompose radians into degrees, arcminutes, arcseconds, fraction.
|
static char |
jauA2tf(int ndp,
double angle,
int[] ihmsf)
Decompose radians into hours, minutes, seconds, fraction.
|
static double[] |
jauAb(double[] pnat,
double[] v,
double s,
double bm1)
Apply aberration to transform natural direction into proper
direction.
|
static JSOFA.EquatorialCoordinate |
jauAe2hd(double az,
double el,
double phi)
Horizon to equatorial coordinates: transform azimuth and altitude
to hour angle and declination.
|
static double |
jauAnp(double a)
Normalize angle into the range
0 <= a < 2pi . |
static double |
jauAnpm(double a)
Normalize angle into the range
-pi <= a < +pi . |
static void |
jauApcg(double date1,
double date2,
double[][] ebpv,
double[] ehp,
JSOFA.Astrom astrom)
For a geocentric observer, prepare star-independent astrometry
parameters for transformations between ICRS and GCRS coordinates.
|
static void |
jauApcg13(double date1,
double date2,
JSOFA.Astrom astrom)
For a geocentric observer, prepare star-independent astrometry
parameters for transformations between ICRS and GCRS coordinates.
|
static void |
jauApci(double date1,
double date2,
double[][] ebpv,
double[] ehp,
double x,
double y,
double s,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between ICRS and geocentric CIRS
coordinates.
|
static double |
jauApci13(double date1,
double date2,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between ICRS and geocentric CIRS
coordinates.
|
static void |
jauApco(double date1,
double date2,
double[][] ebpv,
double[] ehp,
double x,
double y,
double s,
double theta,
double elong,
double phi,
double hm,
double xp,
double yp,
double sp,
double refa,
double refb,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between ICRS and observed
coordinates.
|
static double |
jauApco13(double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between ICRS and observed
coordinates.
|
static void |
jauApcs(double date1,
double date2,
double[][] pv,
double[][] ebpv,
double[] ehp,
JSOFA.Astrom astrom)
For an observer whose geocentric position and velocity are known,
prepare star-independent astrometry parameters for transformations
between ICRS and GCRS.
|
static void |
jauApcs13(double date1,
double date2,
double[][] pv,
JSOFA.Astrom astrom)
For an observer whose geocentric position and velocity are known,
prepare star-independent astrometry parameters for transformations
between ICRS and GCRS.
|
static void |
jauAper(double theta,
JSOFA.Astrom astrom)
In the star-independent astrometry parameters, update only the
Earth rotation angle, supplied by the caller explicitly.
|
static void |
jauAper13(double ut11,
double ut12,
JSOFA.Astrom astrom)
In the star-independent astrometry parameters, update only the
Earth rotation angle.
|
static void |
jauApio(double sp,
double theta,
double elong,
double phi,
double hm,
double xp,
double yp,
double refa,
double refb,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between CIRS and observed
coordinates.
|
static void |
jauApio13(double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl,
JSOFA.Astrom astrom)
For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between CIRS and observed
coordinates.
|
static JSOFA.SphericalCoordinate |
jauAtcc13(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
double date1,
double date2)
Transform a star's ICRS catalog entry (epoch J2000.0) into ICRS
astrometric place.
|
static JSOFA.SphericalCoordinate |
jauAtccq(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
JSOFA.Astrom astrom)
Quick transformation of a star's ICRS catalog entry (epoch J2000.0)
into ICRS astrometric place, given precomputed star-independent
astrometry parameters.
|
static JSOFA.SphericalCoordinateEO |
jauAtci13(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
double date1,
double date2)
Transform ICRS star data, epoch J2000.0, to CIRS.
|
static JSOFA.SphericalCoordinate |
jauAtciq(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
JSOFA.Astrom astrom)
Quick ICRS, epoch J2000.0, to CIRS transformation, given precomputed
star-independent astrometry parameters.
|
static JSOFA.SphericalCoordinate |
jauAtciqn(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
JSOFA.Astrom astrom,
int n,
JSOFA.Ldbody[] b)
Quick ICRS, epoch J2000.0, to CIRS transformation, given precomputed
star-independent astrometry parameters plus a list of light-
deflecting bodies.
|
static JSOFA.SphericalCoordinate |
jauAtciqz(double rc,
double dc,
JSOFA.Astrom astrom)
Quick ICRS to CIRS transformation, given precomputed star-
independent astrometry parameters, and assuming zero parallax and
proper motion.
|
static JSOFA.ObservedPositionEO |
jauAtco13(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl)
ICRS RA,Dec to observed place.
|
static JSOFA.SphericalCoordinateEO |
jauAtic13(double ri,
double di,
double date1,
double date2)
Transform star RA,Dec from geocentric CIRS to ICRS astrometric.
|
static JSOFA.SphericalCoordinate |
jauAticq(double ri,
double di,
JSOFA.Astrom astrom)
Quick CIRS RA,Dec to ICRS astrometric place, given the star-
independent astrometry parameters.
|
static JSOFA.SphericalCoordinate |
jauAticqn(double ri,
double di,
JSOFA.Astrom astrom,
int n,
JSOFA.Ldbody[] b)
Quick CIRS to ICRS astrometric place transformation, given the star-
independent astrometry parameters plus a list of light-deflecting
bodies.
|
static JSOFA.ObservedPosition |
jauAtio13(double ri,
double di,
double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl)
CIRS RA,Dec to observed place.
|
static JSOFA.ObservedPosition |
jauAtioq(double ri,
double di,
JSOFA.Astrom astrom)
Quick CIRS to observed place transformation.
|
static JSOFA.SphericalCoordinate |
jauAtoc13(String type,
double ob1,
double ob2,
double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl)
Observed place at a groundbased site to to ICRS astrometric RA,Dec.
|
static JSOFA.SphericalCoordinate |
jauAtoi13(String type,
double ob1,
double ob2,
double utc1,
double utc2,
double dut1,
double elong,
double phi,
double hm,
double xp,
double yp,
double phpa,
double tc,
double rh,
double wl)
Observed place to CIRS.
|
static JSOFA.SphericalCoordinate |
jauAtoiq(String type,
double ob1,
double ob2,
JSOFA.Astrom astrom)
Quick observed place to CIRS, given the star-independent astrometry
parameters.
|
static JSOFA.FrameBias |
jauBi00()
Frame bias components of IAU 2000 precession-nutation models part
of the Mathews-Herring-Buffett (MHB2000) nutation series, with additions.
|
static void |
jauBp00(double date1,
double date2,
double[][] rb,
double[][] rp,
double[][] rbp)
Frame bias and precession, IAU 2000.
|
static void |
jauBp06(double date1,
double date2,
double[][] rb,
double[][] rp,
double[][] rbp)
Frame bias and precession, IAU 2006.
|
static JSOFA.CelestialIntermediatePole |
jauBpn2xy(double[][] rbpn)
Extract from the bias-precession-nutation matrix the X,Y coordinates
of the Celestial Intermediate Pole.
|
static double[][] |
jauC2i00a(double date1,
double date2)
Form the celestial-to-intermediate matrix for a given date using the
IAU 2000A precession-nutation model.
|
static double[][] |
jauC2i00b(double date1,
double date2)
Form the celestial-to-intermediate matrix for a given date using the
IAU 2000B precession-nutation model.
|
static double[][] |
jauC2i06a(double date1,
double date2)
Form the celestial-to-intermediate matrix for a given date using the
IAU 2006 precession and IAU 2000A nutation models.
|
static double[][] |
jauC2ibpn(double date1,
double date2,
double[][] rbpn)
Form the celestial-to-intermediate matrix for a given date given
the bias-precession-nutation matrix.
|
static double[][] |
jauC2ixy(double date1,
double date2,
double x,
double y)
Form the celestial to intermediate-frame-of-date matrix for a given
date when the CIP X,Y coordinates are known.
|
static double[][] |
jauC2ixys(double x,
double y,
double s)
Form the celestial to intermediate-frame-of-date matrix given the CIP
X,Y and the CIO locator s.
|
static JSOFA.SphericalCoordinate |
jauC2s(double[] p)
P-vector to spherical coordinates.
|
static double[][] |
jauC2t00a(double tta,
double ttb,
double uta,
double utb,
double xp,
double yp)
Form the celestial to terrestrial matrix given the date, the UT1 and
the polar motion, using the IAU 2000A nutation model.
|
static double[][] |
jauC2t00b(double tta,
double ttb,
double uta,
double utb,
double xp,
double yp)
Form the celestial to terrestrial matrix given the date, the UT1 and
the polar motion, using the IAU 2000B precession-nutation model.
|
static double[][] |
jauC2t06a(double tta,
double ttb,
double uta,
double utb,
double xp,
double yp)
Form the celestial to terrestrial matrix given the date, the UT1 and
the polar motion, using the IAU 2006/2000A precession-nutation
nutation model.
|
static double[][] |
jauC2tcio(double[][] rc2i,
double era,
double[][] rpom)
Assemble the celestial to terrestrial matrix from CIO-based
components (the celestial-to-intermediate matrix, the Earth Rotation
Angle and the polar motion matrix).
|
static double[][] |
jauC2teqx(double[][] rbpn,
double gst,
double[][] rpom)
Assemble the celestial to terrestrial matrix from equinox-based
components (the celestial-to-true matrix, the Greenwich Apparent
Sidereal Time and the polar motion matrix).
|
static double[][] |
jauC2tpe(double tta,
double ttb,
double uta,
double utb,
double dpsi,
double deps,
double xp,
double yp)
Form the celestial to terrestrial matrix given the date, the UT1,
the nutation and the polar motion.
|
static double[][] |
jauC2txy(double tta,
double ttb,
double uta,
double utb,
double x,
double y,
double xp,
double yp)
Form the celestial to terrestrial matrix given the date, the UT1,
the CIP coordinates and the polar motion.
|
static JSOFA.JulianDate |
jauCal2jd(int iy,
int im,
int id)
Gregorian Calendar to Julian Date.
|
static double[] |
jauCp(double[] p,
double[] c)
Copy a p-vector.
|
static double[][] |
jauCpv(double[][] pv,
double[][] c)
Copy a position/velocity vector.
|
static void |
jauCr(double[][] r,
double[][] c)
Copy an r-matrix.
|
static JSOFA.CalendarHMS |
jauD2dtf(String scale,
int ndp,
double d1,
double d2)
Format for output a 2-part Julian Date (or in the case of UTC a
quasi-JD form that includes special provision for leap seconds).
|
static char |
jauD2tf(int ndp,
double days,
int[] ihmsf)
Decompose days to hours, minutes, seconds, fraction.
|
static double |
jauDat(int iy,
int im,
int id,
double fd)
For a given UTC date, calculate delta(AT) = TAI-UTC.
|
static double |
jauDtdb(double date1,
double date2,
double ut,
double elong,
double u,
double v)
An approximation to TDB-TT, the difference between barycentric
dynamical time and terrestrial time, for an observer on the Earth.
|
static JSOFA.JulianDate |
jauDtf2d(String scale,
int iy,
int im,
int id,
int ihr,
int imn,
double sec)
Encode date and time fields into 2-part Julian Date (or in the case
of UTC a quasi-JD form that includes special provision for leap
seconds).
|
static JSOFA.SphericalCoordinate |
jauEceq06(double date1,
double date2,
double dl,
double db)
Transformation from ecliptic coordinates (mean equinox and ecliptic
of date) to ICRS RA,Dec, using the IAU 2006 precession model.
|
static double[][] |
jauEcm06(double date1,
double date2)
ICRS equatorial to ecliptic rotation matrix, IAU 2006.
|
static double |
jauEe00(double date1,
double date2,
double epsa,
double dpsi)
The equation of the equinoxes, compatible with IAU 2000 resolutions,
given the nutation in longitude and the mean obliquity.
|
static double |
jauEe00a(double date1,
double date2)
Equation of the equinoxes, compatible with IAU 2000 resolutions.
|
static double |
jauEe00b(double date1,
double date2)
Equation of the equinoxes, compatible with IAU 2000 resolutions but
using the truncated nutation model IAU 2000B.
|
static double |
jauEe06a(double date1,
double date2)
Equation of the equinoxes, compatible with IAU 2000 resolutions and
IAU 2006/2000A precession-nutation.
|
static double |
jauEect00(double date1,
double date2)
Equation of the equinoxes complementary terms, consistent with
IAU 2000 resolutions.
|
static JSOFA.ReferenceEllipsoid |
jauEform(int n)
Earth reference ellipsoids.
|
static double |
jauEo06a(double date1,
double date2)
Equation of the origins, IAU 2006 precession and IAU 2000A nutation.
|
static double |
jauEors(double[][] rnpb,
double s)
Equation of the origins, given the classical NPB matrix and the
quantity s.
|
static double |
jauEpb(double dj1,
double dj2)
Julian Date to Besselian Epoch.
|
static JSOFA.JulianDate |
jauEpb2jd(double epb)
Besselian Epoch to Julian Date.
|
static double |
jauEpj(double dj1,
double dj2)
Julian Date to Julian Epoch.
|
static JSOFA.JulianDate |
jauEpj2jd(double epj)
Julian Epoch to Julian Date.
|
static int |
jauEpv00(double date1,
double date2,
double[][] pvh,
double[][] pvb)
Earth position and velocity, heliocentric and barycentric, with
respect to the Barycentric Celestial Reference System.
|
static JSOFA.SphericalCoordinate |
jauEqec06(double date1,
double date2,
double dr,
double dd)
Transformation from ICRS equatorial coordinates to ecliptic
coordinates (mean equinox and ecliptic of date) using IAU 2006
precession model.
|
static double |
jauEqeq94(double date1,
double date2)
Equation of the equinoxes, IAU 1994 model.
|
static double |
jauEra00(double dj1,
double dj2)
Earth rotation angle (IAU 2000 model).
|
static double |
jauFad03(double t)
Fundamental argument, IERS Conventions (2003):
mean elongation of the Moon from the Sun.
|
static double |
jauFae03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Earth.
|
static double |
jauFaf03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of the Moon minus mean longitude of the ascending
node.
|
static double |
jauFaju03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Jupiter.
|
static double |
jauFal03(double t)
Fundamental argument, IERS Conventions (2003):
mean anomaly of the Moon.
|
static double |
jauFalp03(double t)
Fundamental argument, IERS Conventions (2003):
mean anomaly of the Sun.
|
static double |
jauFama03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Mars.
|
static double |
jauFame03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Mercury.
|
static double |
jauFane03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Neptune.
|
static double |
jauFaom03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of the Moon's ascending node.
|
static double |
jauFapa03(double t)
Fundamental argument, IERS Conventions (2003):
general accumulated precession in longitude.
|
static double |
jauFasa03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Saturn.
|
static double |
jauFaur03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Uranus.
|
static double |
jauFave03(double t)
Fundamental argument, IERS Conventions (2003):
mean longitude of Venus.
|
static JSOFA.CatalogCoords |
jauFk425(double r1950,
double d1950,
double dr1950,
double dd1950,
double p1950,
double v1950)
Convert B1950.0 FK4 star catalog data to J2000.0 FK5.
|
static JSOFA.SphericalCoordinate |
jauFk45z(double r1950,
double d1950,
double bepoch)
Convert a B1950.0 FK4 star position to J2000.0 FK5, assuming zero
proper motion in the FK5 system.
|
static JSOFA.CatalogCoords |
jauFk524(double r2000,
double d2000,
double dr2000,
double dd2000,
double p2000,
double v2000)
Convert J2000.0 FK5 star catalog data to B1950.0 FK4.
|
static JSOFA.CatalogCoords |
jauFk52h(double r5,
double d5,
double dr5,
double dd5,
double px5,
double rv5)
Transform FK5 (J2000.0) star data into the Hipparcos system.
|
static JSOFA.CatalogCoords |
jauFk54z(double r2000,
double d2000,
double bepoch)
Convert a J2000.0 FK5 star position to B1950.0 FK4, assuming zero
proper motion in FK5 and parallax.
|
static void |
jauFk5hip(double[][] r5h,
double[] s5h)
FK5 to Hipparcos rotation and spin.
|
static JSOFA.SphericalCoordinate |
jauFk5hz(double r5,
double d5,
double date1,
double date2)
Transform an FK5 (J2000.0) star position into the system of the
Hipparcos catalogue, assuming zero Hipparcos proper motion.
|
static double[][] |
jauFw2m(double gamb,
double phib,
double psi,
double eps)
Form rotation matrix given the Fukushima-Williams angles.
|
static JSOFA.CelestialIntermediatePole |
jauFw2xy(double gamb,
double phib,
double psi,
double eps)
CIP X,Y given Fukushima-Williams bias-precession-nutation angles.
|
static JSOFA.SphericalCoordinate |
jauG2icrs(double dl,
double db)
Transformation from Galactic Coordinates to ICRS.
|
static JSOFA.GeodeticCoord |
jauGc2gd(int n,
double[] xyz)
Transform geocentric coordinates to geodetic using the specified
reference ellipsoid.
|
static JSOFA.GeodeticCoord |
jauGc2gde(double a,
double f,
double[] xyz)
Transform geocentric coordinates to geodetic for a reference
ellipsoid of specified form.
|
static double[] |
jauGd2gc(int n,
double elong,
double phi,
double height)
Transform geodetic coordinates to geocentric using the specified
reference ellipsoid.
|
static double[] |
jauGd2gce(double a,
double f,
double elong,
double phi,
double height)
Transform geodetic coordinates to geocentric for a reference
ellipsoid of specified form.
|
static double |
jauGmst00(double uta,
double utb,
double tta,
double ttb)
Greenwich mean sidereal time (model consistent with IAU 2000
resolutions).
|
static double |
jauGmst06(double uta,
double utb,
double tta,
double ttb)
Greenwich mean sidereal time (consistent with IAU 2006 precession).
|
static double |
jauGmst82(double dj1,
double dj2)
Universal Time to Greenwich mean sidereal time (IAU 1982 model).
|
static double |
jauGst00a(double uta,
double utb,
double tta,
double ttb)
Greenwich apparent sidereal time (consistent with IAU 2000
resolutions).
|
static double |
jauGst00b(double uta,
double utb)
Greenwich apparent sidereal time (consistent with IAU 2000
resolutions but using the truncated nutation model IAU 2000B).
|
static double |
jauGst06(double uta,
double utb,
double tta,
double ttb,
double[][] rnpb)
Greenwich apparent sidereal time, IAU 2006, given the NPB matrix.
|
static double |
jauGst06a(double uta,
double utb,
double tta,
double ttb)
Greenwich apparent sidereal time (consistent with IAU 2000 and 2006
resolutions).
|
static double |
jauGst94(double uta,
double utb)
Greenwich apparent sidereal time (consistent with IAU 1982/94
resolutions).
|
static JSOFA.CatalogCoords |
jauH2fk5(double rh,
double dh,
double drh,
double ddh,
double pxh,
double rvh)
Transform Hipparcos star data into the FK5 (J2000.0) system.
|
static JSOFA.HorizonCoordinate |
jauHd2ae(double ha,
double dec,
double phi)
Equatorial to horizon coordinates: transform hour angle and
declination to azimuth and altitude.
|
static double |
jauHd2pa(double ha,
double dec,
double phi)
Parallactic angle for a given hour angle and declination.
|
static JSOFA.CatalogCoords |
jauHfk5z(double rh,
double dh,
double date1,
double date2)
Transform a Hipparcos star position into FK5 J2000.0, assuming
zero Hipparcos proper motion.
|
static JSOFA.SphericalCoordinate |
jauIcrs2g(double dr,
double dd)
Transformation from ICRS to Galactic Coordinates.
|
static double[][] |
jauIr()
return a new r-matrix as the identity matrix.
|
static void |
jauIr(double[][] r)
Initialize an r-matrix to the identity matrix.
|
static JSOFA.Calendar |
jauJd2cal(double dj1,
double dj2)
Julian Date to Gregorian year, month, day, and fraction of a day.
|
static int |
jauJdcalf(int ndp,
double dj1,
double dj2,
int[] iymdf)
Julian Date to Gregorian Calendar, expressed in a form convenient
for formatting messages: rounded to a specified precision.
|
static double[] |
jauLd(double bm,
double[] p,
double[] q,
double[] e,
double em,
double dlim)
Apply light deflection by a solar-system body, as part of
transforming coordinate direction into natural direction.
|
static double[] |
jauLdn(int n,
JSOFA.Ldbody[] b,
double[] ob,
double[] sc) |
static double[] |
jauLdsun(double[] p,
double[] e,
double em)
Deflection of starlight by the Sun.
|
static JSOFA.SphericalCoordinate |
jauLteceq(double epj,
double dl,
double db)
Transformation from ecliptic coordinates (mean equinox and ecliptic
of date) to ICRS RA,Dec, using a long-term precession model.
|
static double[][] |
jauLtecm(double epj)
ICRS equatorial to ecliptic rotation matrix, long-term.
|
static JSOFA.SphericalCoordinate |
jauLteqec(double epj,
double dr,
double dd)
Transformation from ICRS equatorial coordinates to ecliptic
coordinates (mean equinox and ecliptic of date) using a long-term
precession model.
|
static double[][] |
jauLtp(double epj)
Long-term precession matrix.
|
static double[][] |
jauLtpb(double epj)
Long-term precession matrix, including ICRS frame bias.
|
static double[] |
jauLtpecl(double epj)
Long-term precession of the ecliptic.
|
static double[] |
jauLtpequ(double epj)
Long-term precession of the equator.
|
static double[][] |
jauMoon98(double date1,
double date2)
Approximate geocentric position and velocity of the Moon.
|
static double[][] |
jauNum00a(double date1,
double date2)
Form the matrix of nutation for a given date, IAU 2000A model.
|
static double[][] |
jauNum00b(double date1,
double date2)
Form the matrix of nutation for a given date, IAU 2000B model.
|
static double[][] |
jauNum06a(double date1,
double date2)
Form the matrix of nutation for a given date, IAU 2006/2000A model.
|
static double[][] |
jauNumat(double epsa,
double dpsi,
double deps)
Form the matrix of nutation.
|
static JSOFA.NutationTerms |
jauNut00a(double date1,
double date2)
Nutation, IAU 2000A model (MHB2000 luni-solar and planetary nutation
with free core nutation omitted).
|
static JSOFA.NutationTerms |
jauNut00b(double date1,
double date2)
Nutation, IAU 2000B model.
|
static JSOFA.NutationTerms |
jauNut06a(double date1,
double date2)
IAU 2000A nutation with adjustments to match the IAU 2006
precession.
|
static JSOFA.NutationTerms |
jauNut80(double date1,
double date2)
Nutation, IAU 1980 model.
|
static double[][] |
jauNutm80(double date1,
double date2)
Form the matrix of nutation for a given date, IAU 1980 model.
|
static double |
jauObl06(double date1,
double date2)
Mean obliquity of the ecliptic, IAU 2006 precession model.
|
static double |
jauObl80(double date1,
double date2)
Mean obliquity of the ecliptic, IAU 1980 model.
|
static JSOFA.PrecessionAngles |
jauP06e(double date1,
double date2)
Precession angles, IAU 2006, equinox based.
|
static double[][] |
jauP2pv(double[] p)
Extend a p-vector to a pv-vector by appending a zero velocity.
|
static JSOFA.SphericalPosition |
jauP2s(double[] p)
P-vector to spherical polar coordinates.
|
static double |
jauPap(double[] a,
double[] b)
Position-angle from two p-vectors.
|
static double |
jauPas(double al,
double ap,
double bl,
double bp)
Position-angle from spherical coordinates.
|
static JSOFA.EulerAngles |
jauPb06(double date1,
double date2)
This function forms three Euler angles which implement general
precession from epoch J2000.0, using the IAU 2006 model.
|
static double |
jauPdp(double[] a,
double[] b)
p-vector inner (=scalar=dot) product.
|
static JSOFA.FWPrecessionAngles |
jauPfw06(double date1,
double date2)
Precession angles, IAU 2006 (Fukushima-Williams 4-angle formulation).
|
static double[][] |
jauPlan94(double date1,
double date2,
int np)
Approximate heliocentric position and velocity of a nominated major
planet: Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus or
Neptune (but not the Earth itself).
|
static double |
jauPm(double[] p)
Modulus of p-vector.
|
static double[][] |
jauPmat00(double date1,
double date2)
Precession matrix (including frame bias) from GCRS to a specified
date, IAU 2000 model.
|
static double[][] |
jauPmat06(double date1,
double date2)
Precession matrix (including frame bias) from GCRS to a specified
date, IAU 2006 model.
|
static double[][] |
jauPmat76(double date1,
double date2)
Precession matrix from J2000.0 to a specified date, IAU 1976 model.
|
static double[] |
jauPmp(double[] a,
double[] b)
P-vector subtraction.
|
static double[] |
jauPmpx(double rc,
double dc,
double pr,
double pd,
double px,
double rv,
double pmt,
double[] pob)
Proper motion and parallax.
|
static JSOFA.CatalogCoords |
jauPmsafe(double ra1,
double dec1,
double pmr1,
double pmd1,
double px1,
double rv1,
double ep1a,
double ep1b,
double ep2a,
double ep2b)
Star proper motion: update star catalog data for space motion, with
special handling to handle the zero parallax case.
|
static JSOFA.NormalizedVector |
jauPn(double[] p)
Convert a p-vector into modulus and unit vector.
|
static JSOFA.PrecessionNutation |
jauPn00(double date1,
double date2,
double dpsi,
double deps)
Precession-nutation, IAU 2000 model: a multi-purpose function,
supporting classical (equinox-based) use directly and CIO-based
use indirectly.
|
static JSOFA.PrecessionNutation |
jauPn00a(double date1,
double date2)
Precession-nutation, IAU 2000A model: a multi-purpose function,
supporting classical (equinox-based) use directly and CIO-based
use indirectly.
|
static JSOFA.PrecessionNutation |
jauPn00b(double date1,
double date2)
Precession-nutation, IAU 2000B model: a multi-purpose function,
supporting classical (equinox-based) use directly and CIO-based
use indirectly.
|
static JSOFA.PrecessionNutation |
jauPn06(double date1,
double date2,
double dpsi,
double deps)
Precession-nutation, IAU 2006 model: a multi-purpose function,
supporting classical (equinox-based) use directly and CIO-based use
indirectly.
|
static JSOFA.PrecessionNutation |
jauPn06a(double date1,
double date2)
Precession-nutation, IAU 2006/2000A models: a multi-purpose function,
supporting classical (equinox-based) use directly and CIO-based use
indirectly.
|
static double[][] |
jauPnm00a(double date1,
double date2)
Form the matrix of precession-nutation for a given date (including
frame bias), equinox-based, IAU 2000A model.
|
static double[][] |
jauPnm00b(double date1,
double date2)
Form the matrix of precession-nutation for a given date (including
frame bias), equinox-based, IAU 2000B model.
|
static double[][] |
jauPnm06a(double date1,
double date2)
Form the matrix of precession-nutation for a given date (including
frame bias), equinox based, IAU 2006 precession and IAU 2000A nutation models.
|
static double[][] |
jauPnm80(double date1,
double date2)
Form the matrix of precession/nutation for a given date, IAU 1976
precession model, IAU 1980 nutation model.
|
static double[][] |
jauPom00(double xp,
double yp,
double sp)
Form the matrix of polar motion for a given date, IAU 2000.
|
static double[] |
jauPpp(double[] a,
double[] b)
P-vector addition.
|
static double[] |
jauPv2p(double[][] pv)
Discard velocity component of a pv-vector.
|
static JSOFA.SphericalPositionVelocity |
jauPv2s(double[][] pv)
Convert position/velocity from Cartesian to spherical coordinates.
|
static double[] |
jauPvdpv(double[][] a,
double[][] b)
Inner (=scalar=dot) product of two pv-vectors.
|
static JSOFA.PVModulus |
jauPvm(double[][] pv)
Modulus of pv-vector.
|
static double[][] |
jauPvmpv(double[][] a,
double[][] b)
Subtract one pv-vector from another.
|
static double[][] |
jauPvppv(double[][] a,
double[][] b)
Add one pv-vector to another.
|
static JSOFA.CatalogCoords |
jauPvstar(double[][] pv)
Convert star position+velocity vector to catalog coordinates.
|
static double[][] |
jauPvtob(double[] xyzm,
double xp,
double yp,
double sp,
double theta)
Alternative Position and velocity of a terrestrial observing station with observatory position already in cartesian.
|
static double[][] |
jauPvtob(double elong,
double phi,
double hm,
double xp,
double yp,
double sp,
double theta)
Position and velocity of a terrestrial observing station.
|
static double[][] |
jauPvu(double dt,
double[][] pv)
Update a pv-vector.
|
static double[] |
jauPvup(double dt,
double[][] pv)
Update a pv-vector, discarding the velocity component.
|
static double[][] |
jauPvxpv(double[][] a,
double[][] b)
Outer (=vector=cross) product of two pv-vectors.
|
static double[] |
jauPxp(double[] a,
double[] b)
p-vector outer (=vector=cross) product.
|
static JSOFA.RefCos |
jauRefco(double phpa,
double tc,
double rh,
double wl)
Determine the constants A and B in the atmospheric refraction model
dZ = A tan Z + B tan^3 Z.
|
static double[] |
jauRm2v(double[][] r)
Express an r-matrix as an r-vector.
|
static double[][] |
jauRv2m(double[] w)
Form the r-matrix corresponding to a given r-vector.
|
static void |
jauRx(double phi,
double[][] r)
Rotate an r-matrix about the x-axis.
|
static double[] |
jauRxp(double[][] r,
double[] p)
Multiply a p-vector by an r-matrix.
|
static double[][] |
jauRxpv(double[][] r,
double[][] pv)
Multiply a pv-vector by an r-matrix.
|
static double[][] |
jauRxr(double[][] a,
double[][] b)
Multiply two r-matrices.
|
static void |
jauRy(double theta,
double[][] r)
Rotate an r-matrix about the y-axis.
|
static void |
jauRz(double psi,
double[][] r)
Rotate an r-matrix about the z-axis.
|
static double |
jauS00(double date1,
double date2,
double x,
double y)
The CIO locator s, positioning the Celestial Intermediate Origin on
the equator of the Celestial Intermediate Pole, given the CIP's X,Y
coordinates.
|
static double |
jauS00a(double date1,
double date2)
The CIO locator s, positioning the Celestial Intermediate Origin on
the equator of the Celestial Intermediate Pole, using the IAU 2000A
precession-nutation model.
|
static double |
jauS00b(double date1,
double date2)
The CIO locator s, positioning the Celestial Intermediate Origin on
the equator of the Celestial Intermediate Pole, using the IAU 2000B
precession-nutation model.
|
static double |
jauS06(double date1,
double date2,
double x,
double y)
The CIO locator s, positioning the Celestial Intermediate Origin on
the equator of the Celestial Intermediate Pole, given the CIP's X,Y
coordinates.
|
static double |
jauS06a(double date1,
double date2)
The CIO locator s, positioning the Celestial Intermediate Origin on
the equator of the Celestial Intermediate Pole, using the IAU 2006
precession and IAU 2000A nutation models.
|
static double[] |
jauS2c(double theta,
double phi)
Convert spherical coordinates to Cartesian.
|
static double[] |
jauS2p(double theta,
double phi,
double r)
Convert spherical polar coordinates to p-vector.
|
static double[][] |
jauS2pv(double theta,
double phi,
double r,
double td,
double pd,
double rd)
Convert position/velocity from spherical to Cartesian coordinates.
|
static double[][] |
jauS2xpv(double s1,
double s2,
double[][] pv)
Multiply a pv-vector by two scalars.
|
static double |
jauSepp(double[] a,
double[] b)
Angular separation between two p-vectors.
|
static double |
jauSeps(double al,
double ap,
double bl,
double bp)
Angular separation between two sets of spherical coordinates.
|
static double |
jauSp00(double date1,
double date2)
The TIO locator s', positioning the Terrestrial Intermediate Origin
on the equator of the Celestial Intermediate Pole.
|
static JSOFA.CatalogCoords |
jauStarpm(double ra1,
double dec1,
double pmr1,
double pmd1,
double px1,
double rv1,
double ep1a,
double ep1b,
double ep2a,
double ep2b)
Star proper motion: update star catalog data for space motion.
|
static int |
jauStarpv(double ra,
double dec,
double pmr,
double pmd,
double px,
double rv,
double[][] pv)
Convert star catalog coordinates to position+velocity vector.
|
static double[] |
jauSxp(double s,
double[] p)
Multiply a p-vector by a scalar.
|
static double[][] |
jauSxpv(double s,
double[][] pv)
Multiply a pv-vector by a scalar.
|
static JSOFA.JulianDate |
jauTaitt(double tai1,
double tai2)
Time scale transformation: International Atomic Time, TAI, to
Terrestrial Time, TT.
|
static JSOFA.JulianDate |
jauTaiut1(double tai1,
double tai2,
double dta)
Time scale transformation: International Atomic Time, TAI, to
Universal Time, UT1.
|
static JSOFA.JulianDate |
jauTaiutc(double tai1,
double tai2)
Time scale transformation: International Atomic Time, TAI, to
Coordinated Universal Time, UTC.
|
static JSOFA.JulianDate |
jauTcbtdb(double tcb1,
double tcb2)
Time scale transformation: Barycentric Coordinate Time, TCB, to
Barycentric Dynamical Time, TDB.
|
static JSOFA.JulianDate |
jauTcgtt(double tcg1,
double tcg2)
Time scale transformation: Geocentric Coordinate Time, TCG, to
Terrestrial Time, TT.
|
static JSOFA.JulianDate |
jauTdbtcb(double tdb1,
double tdb2)
Time scale transformation: Barycentric Dynamical Time, TDB, to
Barycentric Coordinate Time, TCB.
|
static JSOFA.JulianDate |
jauTdbtt(double tdb1,
double tdb2,
double dtr)
Time scale transformation: Barycentric Dynamical Time, TDB, to
Terrestrial Time, TT.
|
static double |
jauTf2a(char s,
int ihour,
int imin,
double sec)
Convert hours, minutes, seconds to radians.
|
static double |
jauTf2d(char s,
int ihour,
int imin,
double sec)
Convert hours, minutes, seconds to days.
|
static JSOFA.TangentPointSolution |
jauTpors(double xi,
double eta,
double a,
double b)
In the tangent plane projection, given the rectangular coordinates
of a star and its spherical coordinates, determine the spherical
coordinates of the tangent point.
|
static JSOFA.TangentPointDirectionCosines |
jauTporv(double xi,
double eta,
double[] v)
In the tangent plane projection, given the rectangular coordinates
of a star and its direction cosines, determine the direction
cosines of the tangent point.
|
static JSOFA.SphericalCoordinate |
jauTpsts(double xi,
double eta,
double a0,
double b0)
In the tangent plane projection, given the star's rectangular
coordinates and the spherical coordinates of the tangent point,
solve for the spherical coordinates of the star.
|
static double[] |
jauTpstv(double xi,
double eta,
double[] v0)
In the tangent plane projection, given the star's rectangular
coordinates and the direction cosines of the tangent point, solve
for the direction cosines of the star.
|
static JSOFA.TangentPlaneCoordinate |
jauTpxes(double a,
double b,
double a0,
double b0)
In the tangent plane projection, given celestial spherical
coordinates for a star and the tangent point, solve for the star's
rectangular coordinates in the tangent plane.
|
static JSOFA.TangentPlaneCoordinate |
jauTpxev(double[] v,
double[] v0)
In the tangent plane projection, given celestial direction cosines
for a star and the tangent point, solve for the star's rectangular
coordinates in the tangent plane.
|
static double[][] |
jauTr(double[][] r)
Transpose an r-matrix.
|
static double[] |
jauTrxp(double[][] r,
double[] p)
Multiply a p-vector by the transpose of an r-matrix.
|
static double[][] |
jauTrxpv(double[][] r,
double[][] pv)
Multiply a pv-vector by the transpose of an r-matrix.
|
static JSOFA.JulianDate |
jauTttai(double tt1,
double tt2)
Time scale transformation: Terrestrial Time, TT, to International
Atomic Time, TAI.
|
static JSOFA.JulianDate |
jauTttcg(double tt1,
double tt2)
Time scale transformation: Terrestrial Time, TT, to Geocentric
Coordinate Time, TCG.
|
static JSOFA.JulianDate |
jauTttdb(double tt1,
double tt2,
double dtr)
Time scale transformation: Terrestrial Time, TT, to Barycentric
Dynamical Time, TDB.
|
static JSOFA.JulianDate |
jauTtut1(double tt1,
double tt2,
double dt)
Time scale transformation: Terrestrial Time, TT, to Universal Time,
UT1.
|
static JSOFA.JulianDate |
jauUt1tai(double ut11,
double ut12,
double dta)
Time scale transformation: Universal Time, UT1, to International
Atomic Time, TAI.
|
static JSOFA.JulianDate |
jauUt1tt(double ut11,
double ut12,
double dt)
Time scale transformation: Universal Time, UT1, to Terrestrial
Time, TT.
|
static JSOFA.JulianDate |
jauUt1utc(double ut11,
double ut12,
double dut1)
Time scale transformation: Universal Time, UT1, to Coordinated
Universal Time, UTC.
|
static JSOFA.JulianDate |
jauUtctai(double utc1,
double utc2)
Time scale transformation: Coordinated Universal Time, UTC, to
International Atomic Time, TAI.
|
static JSOFA.JulianDate |
jauUtcut1(double utc1,
double utc2,
double dut1)
Time scale transformation: Coordinated Universal Time, UTC, to
Universal Time, UT1.
|
static JSOFA.CelestialIntermediatePole |
jauXy06(double date1,
double date2) |
static JSOFA.ICRFrame |
jauXys00a(double date1,
double date2)
For a given TT date, compute the X,Y coordinates of the Celestial
Intermediate Pole and the CIO locator s, using the IAU 2000A
precession-nutation model.
|
static JSOFA.ICRFrame |
jauXys00b(double date1,
double date2)
For a given TT date, compute the X,Y coordinates of the Celestial
Intermediate Pole and the CIO locator s, using the IAU 2000B
precession-nutation model.
|
static JSOFA.ICRFrame |
jauXys06a(double date1,
double date2)
For a given TT date, compute the X,Y coordinates of the Celestial
Intermediate Pole and the CIO locator s, using the IAU 2006
precession and IAU 2000A nutation models.
|
static double[] |
jauZp()
Return Zero p-vector.
|
static void |
jauZp(double[] p)
Zero a p-vector.
|
static double[][] |
jauZpv()
A Zero pv-vector.
|
static void |
jauZpv(double[][] pv)
Zero a pv-vector.
|
static double[][] |
jauZr()
Initialize an r-matrix to the null matrix.
|
static void |
jauZr(double[][] r)
Initialize an r-matrix to the null matrix.
|
static JSOFA.JulianDate |
lastLeapSecondDate()
the date of the last leap second.
|
public static final String SOFA_RELEASE
public static final String JSOFA_RELEASE
public static final String SOFA_REVISION
public static final int IYV
public static final JSOFA.JulianDate latestConfirmedNoLeapSecondChange
public static final double DS2R
public static final double DPI
public static final double D2PI
public static final double DR2D
public static final double DD2R
public static final double DR2AS
public static final double DAS2R
public static final double TURNAS
public static final double DMAS2R
public static final double DTY
public static final double DJ00
public static final double DJM0
public static final double DJM00
public static final double DAYSEC
public static final double DJY
public static final double DJC
public static final double DJM
public static final double DJM77
public static final double TTMTAI
public static final double DAU
public static final double CMPS
public static final double AULT
public static final double DC
public static final double ELG
public static final double ELB
public static final double SRS
public static final double TDB0
public static char jauA2af(int ndp, double angle, int[] idmsf)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
Called:
jauD2tf(int, double, int[])
decompose days to hms
Notes:
ndp resolution : ...0000 00 00 -7 1000 00 00 -6 100 00 00 -5 10 00 00 -4 1 00 00 -3 0 10 00 -2 0 01 00 -1 0 00 10 0 0 00 01 1 0 00 00.1 2 0 00 00.01 3 0 00 00.001 : 0 00 00.000...
ndp
- int resolution (Note 1)angle
- double angle in radiansidmsf
- int[4] returned degrees, arcminutes, arcseconds, fraction
public static char jauA2tf(int ndp, double angle, int[] ihmsf)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
ndp
- int resolution (Note 1)angle
- double angle in radians
ihmsf
- int[4] returned hours, minutes, seconds, fractionCalled:
jauD2tf(int, double, int[])
decompose days to hms
Notes:
ndp resolution : ...0000 00 00 -7 1000 00 00 -6 100 00 00 -5 10 00 00 -4 1 00 00 -3 0 10 00 -2 0 01 00 -1 0 00 10 0 0 00 01 1 0 00 00.1 2 0 00 00.01 3 0 00 00.001 : 0 00 00.000...
public static double jauAnp(double a)
0 <= a < 2pi
.
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double angle (radians)
public static double jauAnpm(double a)
-pi <= a < +pi
.
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double angle (radians)
public static JSOFA.FrameBias jauBi00()
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
Notes:
References: Chapront, J., Chapront-Touze, M. &Francou, G., Astron. Astrophys., 387, 700, 2002.
Mathews, P.M., Herring, T.A., Buffet, B.A., "Modeling of nutation and precession New nutation series for nonrigid Earth and insights into the Earth's interior", J.Geophys.Res., 107, B4, 2002. The MHB2000 code itself was obtained on 9th September 2002 from ftp://maia.usno.navy.mil/conv2000/chapter5/IAU2000A.
public static void jauBp00(double date1, double date2, double[][] rb, double[][] rp, double[][] rbp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
rb
- double[3][3] returned frame bias matrix (Note 2)rp
- double[3][3] returned precession matrix (Note 3)rbp
- double[3][3] returned bias-precession matrix (Note 4)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauBi00()
frame bias components, IAU 2000
jauPr00(double, double)
IAU 2000 precession adjustments
jauIr(double[][])
initialize r-matrix to identity
jauRx(double, double[][])
rotate around X-axis
jauRy(double, double[][])
rotate around Y-axis
jauRz(double, double[][])
rotate around Z-axis
jauCr(double[][], double[][])
copy r-matrix
jauRxr(double[][], double[][])
product of two r-matrices
Reference: "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
public static void jauBp06(double date1, double date2, double[][] rb, double[][] rp, double[][] rbp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
rb
- double[3][3] returned frame bias matrix (Note 2)rp
- double[3][3] returned precession matrix (Note 3)rbp
- double[3][3] returned bias-precession matrix (Note 4)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauPfw06(double, double)
bias-precession F-W angles, IAU 2006
jauFw2m(double, double, double, double)
F-W angles to r-matrix
jauPmat06(double, double)
PB matrix, IAU 2006
jauTr(double[][])
transpose r-matrix
jauRxr(double[][], double[][])
product of two r-matrices
References:
Capitaine, N. &Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P.T. &Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static JSOFA.CelestialIntermediatePole jauBpn2xy(double[][] rbpn)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
rbpn
- double[3][3] celestial-to-true matrix (Note 1)
Notes:
Reference: "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
public static double[][] jauC2i00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauPnm00a(double, double)
classical NPB matrix, IAU 2000A
jauC2ibpn(double, double, double[][])
celestial-to-intermediate matrix, given NPB matrix
References:
public static double[][] jauC2i00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauPnm00b(double, double)
classical NPB matrix, IAU 2000B
jauC2ibpn(double, double, double[][])
celestial-to-intermediate matrix, given NPB matrix
References:
"Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2i06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, Given X,Y, IAU 2006
jauC2ixys(double, double, double)
celestial-to-intermediate matrix, Given X,Y and s
References:
McCarthy, D. D., Petit, G. (eds.), 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
public static double[][] jauC2ibpn(double date1, double date2, double[][] rbpn)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)rbpn
- double[3][3] celestial-to-true matrix (Note 2)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauC2ixy(double, double, double, double)
celestial-to-intermediate matrix, given X,Y
References:
"Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003)
n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2ixy(double date1, double date2, double x, double y)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)x
- double Celestial Intermediate Pole (Note 2)y
- double Celestial Intermediate Pole (Note 2)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date &time methods are both good compromises between resolution and convenience.
Called:
jauC2ixys(double, double, double)
celestial-to-intermediate matrix, given X,Y and s
jauS00(double, double, double, double)
the CIO locator s, given X,Y, IAU 2000A
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2ixys(double x, double y, double s)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
x
- double Celestial Intermediate Pole (Note 1)y
- double Celestial Intermediate Pole (Note 1)s
- double the CIO locator s (Note 2)
Notes:
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRz(double, double[][])
rotate around Z-axis
jauRy(double, double[][])
rotate around Y-axis
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.SphericalCoordinate jauC2s(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector
Notes:
public static double[][] jauC2t00a(double tta, double ttb, double uta, double utb, double xp, double yp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
tta
- double TT as a 2-part Julian Date (Note 1)ttb
- double TT as a 2-part Julian Date (Note 1)uta
- double UT1 as a 2-part Julian Date (Note 1)utb
- double UT1 as a 2-part Julian Date (Note 1)xp
- double CIP coordinates (radians, Note 2)yp
- double CIP coordinates (radians, Note 2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. In the case of uta,utb, the date &time method is best matched to the Earth rotation angle algorithm used: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauC2i00a(double, double)
celestial-to-intermediate matrix, IAU 2000A
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauSp00(double, double)
the TIO locator s', IERS 2000
jauPom00(double, double, double)
polar motion matrix
jauC2tcio(double[][], double, double[][])
form CIO-based celestial-to-terrestrial matrix
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2t00b(double tta, double ttb, double uta, double utb, double xp, double yp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
tta
- double TT as a 2-part Julian Date (Note 1)ttb
- double TT as a 2-part Julian Date (Note 1)uta
- double UT1 as a 2-part Julian Date (Note 1)utb
- double UT1 as a 2-part Julian Date (Note 1)xp
- double coordinates of the pole (radians, Note 2)yp
- double coordinates of the pole (radians, Note 2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. In the case of uta,utb, the date &time method is best matched to the Earth rotation angle algorithm used: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauC2i00b(double, double)
celestial-to-intermediate matrix, IAU 2000B
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauPom00(double, double, double)
polar motion matrix
jauC2tcio(double[][], double, double[][])
form CIO-based celestial-to-terrestrial matrix
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2t06a(double tta, double ttb, double uta, double utb, double xp, double yp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
tta
- double TT as a 2-part Julian Date (Note 1)ttb
- double TT as a 2-part Julian Date (Note 1)uta
- double UT1 as a 2-part Julian Date (Note 1)utb
- double UT1 as a 2-part Julian Date (Note 1)xp
- double coordinates of the pole (radians, Note 2)yp
- double coordinates of the pole (radians, Note 2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. In the case of uta,utb, the date &time method is best matched to the Earth rotation angle algorithm used: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauC2i06a(double, double)
celestial-to-intermediate matrix, IAU 2006/2000A
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauSp00(double, double)
the TIO locator s', IERS 2000
jauPom00(double, double, double)
polar motion matrix
jauC2tcio(double[][], double, double[][])
form CIO-based celestial-to-terrestrial matrix
Reference:
McCarthy, D. D., Petit, G. (eds.), 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
public static double[][] jauC2tcio(double[][] rc2i, double era, double[][] rpom)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
rc2i
- double[3][3] celestial-to-intermediate matrixera
- double Earth rotation angle (radians)rpom
- double[3][3] polar-motion matrix
Notes:
Called:
jauCr(double[][], double[][])
copy r-matrix
jauRz(double, double[][])
rotate around Z-axis
jauRxr(double[][], double[][])
product of two r-matrices
Reference:
McCarthy, D. D., Petit, G. (eds.), 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
public static double[][] jauC2teqx(double[][] rbpn, double gst, double[][] rpom)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
rbpn
- double[3][3] celestial-to-true matrixgst
- double Greenwich (apparent) Sidereal Time (radians)rpom
- double[3][3] polar-motion matrix
Notes:
Called:
jauCr(double[][], double[][])
copy r-matrix
jauRz(double, double[][])
rotate around Z-axis
jauRxr(double[][], double[][])
product of two r-matrices
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2tpe(double tta, double ttb, double uta, double utb, double dpsi, double deps, double xp, double yp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
tta
- double TT as a 2-part Julian Date (Note 1)ttb
- double TT as a 2-part Julian Date (Note 1)uta
- double UT1 as a 2-part Julian Date (Note 1)utb
- double UT1 as a 2-part Julian Date (Note 1)dpsi
- double nutation (Note 2)deps
- double nutation (Note 2)xp
- double coordinates of the pole (radians, Note 3)yp
- double coordinates of the pole (radians, Note 3)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. In the case of uta,utb, the date &time method is best matched to the Earth rotation angle algorithm used: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauPn00(double, double, double, double)
bias/precession/nutation results, IAU 2000
jauGmst00(double, double, double, double)
Greenwich mean sidereal time, IAU 2000
jauSp00(double, double)
the TIO locator s', IERS 2000
jauEe00(double, double, double, double)
equation of the equinoxes, IAU 2000
jauPom00(double, double, double)
polar motion matrix
jauC2teqx(double[][], double, double[][])
form equinox-based celestial-to-terrestrial matrix
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[][] jauC2txy(double tta, double ttb, double uta, double utb, double x, double y, double xp, double yp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
tta
- double TT as a 2-part Julian Date (Note 1)ttb
- double TT as a 2-part Julian Date (Note 1)uta
- double UT1 as a 2-part Julian Date (Note 1)utb
- double UT1 as a 2-part Julian Date (Note 1)x
- double Celestial Intermediate Pole (Note 2)y
- double Celestial Intermediate Pole (Note 2)xp
- double coordinates of the pole (radians, Note 3)yp
- double coordinates of the pole (radians, Note 3)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date &time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. In the case of uta,utb, the date &time method is best matched to the Earth rotation angle algorithm used: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauC2ixy(double, double, double, double)
celestial-to-intermediate matrix, given X,Y
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauSp00(double, double)
the TIO locator s', IERS 2000
jauPom00(double, double, double)
polar motion matrix
jauC2tcio(double[][], double, double[][])
form CIO-based celestial-to-terrestrial matrix
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.JulianDate jauCal2jd(int iy, int im, int id) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
iy
- int year in Gregorian calendar (Note 1)im
- int month in Gregorian calendar (Note 1)id
- int day in Gregorian calendar (Note 1)
JSOFAIllegalParameter
- status:
0 = OK
-1 = bad year (Note 3: JD not computed)
-2 = bad month (JD not computed)
-3 = bad day (JD computed)
Notes:
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 12.92 (p604).
public static double[] jauCp(double[] p, double[] c)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector to be copied
c
- double[3] given and returned copypublic static double[][] jauCpv(double[][] pv, double[][] c)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
pv
- double[2][3] position/velocity vector to be copiedc
- double[2][3] returned copy
Called:
jauCp(double[], double[])
copy p-vector
public static void jauCr(double[][] r, double[][] c)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrix to be copied.
c
- double[3][3] given and returned the elements of r are copied into this.
Called:
jauCp(double[], double[])
copy p-vector
public static char jauD2tf(int ndp, double days, int[] ihmsf)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
ndp
- int resolution (Note 1)days
- double interval in days
ihmsf
- int[4] returned hours, minutes, seconds, fractionNotes:
public static JSOFA.CalendarHMS jauD2dtf(String scale, int ndp, double d1, double d2) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
scale
- char[] time scale ID (Note 1)ndp
- int resolution (Note 2)d1
- double time as a 2-part Julian Date (Notes 3,4)d2
- double time as a 2-part Julian Date (Notes 3,4)
Notes:
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date (notes 5,6)public static JSOFA.JulianDate jauDtf2d(String scale, int iy, int im, int id, int ihr, int imn, double sec) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
scale
- char time scale ID (Note 1)iy
- int year in Gregorian calendar (Note 2)im
- int month in Gregorian calendar (Note 2)id
- int day in Gregorian calendar (Note 2)ihr
- int hourimn
- int minutesec
- double seconds
JSOFAIllegalParameter
- bad yearJSOFAInternalError
- status: +3 = both of next two
+2 = time is after end of day (Note 5)
+1 = dubious year (Note 6)
0 = OK
-1 = bad year
-2 = bad month
-3 = bad day
-4 = bad hour
-5 = bad minute
-6 = bad second (<0)
Notes:
public static JSOFA.JulianDate lastLeapSecondDate()
JSOFA.JulianDate
of the last leap second.public static double jauDat(int iy, int im, int id, double fd) throws JSOFAIllegalParameter, JSOFAInternalError
:------------------------------------------: : : : IMPORTANT : : : : A new version of this function must be : : produced whenever a new leap second is : : announced. There are four items to : : change on each such occasion: : : : : 1) A new line must be added to the set : : of statements that initialize the : : array "changes". : : : : 2) The parameter IYV must be set to : : the current year. : : : : 3) The "Latest leap second" comment : : below must be set to the new leap : : second date. : : : : 4) The "This revision" comment, later, : : must be set to the current date. : : : : Change (2) must also be carried out : : whenever the function is re-issued, : : even if no leap seconds have been : : added. : : : : Latest leap second: 2017 Jan 01 : : : :__________________________________________:
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
iy
- int UTC: year (Notes 1 and 2)im
- int month (Note 2)id
- int day (Notes 2 and 3)fd
- double fraction of day (Note 4)
JSOFAIllegalParameter
- status (Note 5):
1 = dubious year (Note 1)
0 = OK
-1 = bad year
-2 = bad month
-3 = bad day (Note 3)
-4 = bad fraction (Note 4)JSOFAInternalError
- Notes:
References:
Called:
jauCal2jd(int, int, int)
Gregorian calendar to Julian Day number
@version 20160729
public static double jauDtdb(double date1, double date2, double ut, double elong, double u, double v)
TAI <- physically realized
:
offset <- observed (nominally +32.184s)
:
TT <- terrestrial time
:
rate adjustment (L_G) <- definition of TT
:
TCG <- time scale for GCRS
:
"periodic" terms <- jauDtdb is an implementation
:
rate adjustment (L_C) <- function of solar-system ephemeris
:
TCB <- time scale for BCRS
:
rate adjustment (-L_B) <- definition of TDB
:
TDB <- TCB scaled to track TT
:
"periodic" terms <- -jau_DTDB is an approximation
:
TT <- terrestrial time
Adopted values for the various constants can be found in the IERS
Conventions (McCarthy & Petit 2003).
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double date, TDB (Notes 1-3)date2
- double date, TDB (Notes 1-3)ut
- double universal time (UT1, fraction of one day)elong
- double longitude (east positive, radians)u
- double distance from Earth spin axis (km)v
- double distance north of equatorial plane (km)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. Although the date is, formally, barycentric dynamical time (TDB), the terrestrial dynamical time (TT) can be used with no practical effect on the accuracy of the prediction.
References:
Fairhead, L., & Bretagnon, P., Astron.Astrophys., 229, 240-247 (1990).
IAU 2006 Resolution 3.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
Moyer, T.D., Cel.Mech., 23, 33 (1981).
Murray, C.A., Vectorial Astrometry, Adam Hilger (1983).
Seidelmann, P.K. et al., Explanatory Supplement to the Astronomical Almanac, Chapter 2, University Science Books (1992).
Simon, J.L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G. & Laskar, J., Astron.Astrophys., 282, 663-683 (1994).
public static double jauEe00(double date1, double date2, double epsa, double dpsi)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)epsa
- double mean obliquity (Note 2)dpsi
- double nutation in longitude (Note 3)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauEect00(double, double)
equation of the equinoxes complementary terms
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauEe00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPr00(double, double)
IAU 2000 precession adjustments
jauObl80(double, double)
mean obliquity, IAU 1980
jauNut00a(double, double)
nutation, IAU 2000A
jauEe00(double, double, double, double)
equation of the equinoxes, IAU 2000
References:
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003).
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004).
public static double jauEe00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPr00(double, double)
IAU 2000 precession adjustments
jauObl80(double, double)
mean obliquity, IAU 1980
jauNut00b(double, double)
nutation, IAU 2000B
jauEe00(double, double, double, double)
equation of the equinoxes, IAU 2000
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
McCarthy, D.D. & Luzum, B.J., "An abridged model of the precession-nutation of the celestial pole", Celestial Mechanics & Dynamical Astronomy, 85, 37-49 (2003)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauEe06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauAnpm(double)
normalize angle into range +/- pi
jauGst06a(double, double, double, double)
Greenwich apparent sidereal time, IAU 2006/2000A
jauGmst06(double, double, double, double)
Greenwich mean sidereal time, IAU 2006
Reference:
McCarthy, D. D., Petit, G. (eds.), 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
public static double jauEect00(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauFal03(double)
mean anomaly of the Moon
jauFalp03(double)
mean anomaly of the Sun
jauFaf03(double)
mean argument of the latitude of the Moon
jauFad03(double)
mean elongation of the Moon from the Sun
jauFaom03(double)
mean longitude of the Moon's ascending node
jauFave03(double)
mean longitude of Venus
jauFae03(double)
mean longitude of Earth
jauFapa03(double)
general accumulated precession in longitude
References:
Capitaine, N. & Gontier, A.-M., Astron. Astrophys., 275, 645-650 (1993)
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
IAU Resolution C7, Recommendation 3 (1994)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.ReferenceEllipsoid jauEform(int n) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's JSOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
n
- int ellipsoid identifier (Note 1)
JSOFAIllegalParameter
- int status:
0 = OK
-1 = illegal identifier (Note 3)
Notes:
References:
Department of Defense World Geodetic System 1984, National Imagery and Mapping Agency Technical Report 8350.2, Third Edition, p3-2.
Moritz, H., Bull. Geodesique 66-2, 187 (1992).
The Department of Defense World Geodetic System 1972, World Geodetic System Committee, May 1974.
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), p220.
public static double jauEo06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
jauEors(double[][], double)
equation of the origins, Given NPB matrix and s
References:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static double jauEors(double[][] rnpb, double s)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
rnpb
- double[3][3] classical nutation x precession x bias matrixs
- double the quantity s (the CIO locator) in radians
Notes:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static double jauEpb(double dj1, double dj2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
dj1
- double Julian Date (see note)dj2
- double Julian Date (see note)
Reference: Lieske,J.H., 1979. Astron.Astrophys.,73,282.
public static JSOFA.JulianDate jauEpb2jd(double epb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
epb
- double Besselian Epoch (e.g. 1957.3D0)
Reference:
Lieske, J.H., 1979, Astron.Astrophys. 73, 282.
public static double jauEpj(double dj1, double dj2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
dj1
- double Julian Date (see note)dj2
- double Julian Date (see note)
Reference:
Lieske, J.H., 1979, Astron.Astrophys. 73, 282.
public static JSOFA.JulianDate jauEpj2jd(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian Epoch (e.g. 1996.8D0)
Reference:
Lieske, J.H., 1979, Astron.Astrophys. 73, 282.
public static int jauEpv00(double date1, double date2, double[][] pvh, double[][] pvb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB date (Note 1)date2
- double TDB date (Note 1)
pvh
- double[2][3] returned heliocentric Earth position/velocity (au, au/d)pvb
- double[2][3] returned barycentric Earth position/velocity (au, au/d)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. However, the accuracy of the result is more likely to be limited by the algorithm itself than the way the date has been expressed. n.b. TT can be used instead of TDB in most applications.
public static double jauEqeq94(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TDB date (Note 1)date2
- double TDB date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut80(double, double)
nutation, IAU 1980
jauObl80(double, double)
mean obliquity, IAU 1980
References:
IAU Resolution C7, Recommendation 3 (1994).
Capitaine, N. & Gontier, A.-M., 1993, Astron. Astrophys., 275, 645-650.
public static double jauEra00(double dj1, double dj2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
dj1
- double UT1 as a 2-part Julian Date (see note)dj2
- double UT1 as a 2-part Julian Date (see note)
Notes:
dj1 dj2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. The date & time method is best matched to the algorithm used: maximum precision is delivered when the dj1 argument is for 0hrs UT1 on the day in question and the dj2 argument lies in the range 0 to 1, or vice versa.
Called:
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Capitaine N., Guinot B. and McCarthy D.D, 2000, Astron. Astrophys., 355, 398-405.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauFad03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFae03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static double jauFaf03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFaju03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static double jauFal03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFalp03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFama03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683 Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static double jauFame03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683 Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static double jauFane03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFaom03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFapa03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References: Kinoshita, H. and Souchay J. 1990, Celest.Mech. and Dyn.Astron. 48, 187
Lieske, J.H., Lederle, T., Fricke, W. & Morando, B. 1977, Astron.Astrophys. 58, 1-16
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauFasa03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683 Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static double jauFaur03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
public static double jauFave03(double t)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
t
- double TDB, Julian centuries since J2000.0 (Note 1)
Notes:
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683 Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
public static JSOFA.CatalogCoords jauFk52h(double r5, double d5, double dr5, double dd5, double px5, double rv5)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function. Given (all FK5, equinox J2000.0, epoch J2000.0):
r5
- double RA (radians)d5
- double Dec (radians)dr5
- double proper motion in RA (dRA/dt, rad/Jyear)dd5
- double proper motion in Dec (dDec/dt, rad/Jyear)px5
- double parallax (arcsec)rv5
- double radial velocity (km/s, positive = receding)
Returned (all Hipparcos, epoch J2000.0):Notes:
jauH2fk5(double, double, double, double, double, double)
, jauFk5hz(double, double, double, double)
, jauHfk5z(double, double, double, double)
.
Called:
jauStarpv(double, double, double, double, double, double, double[][])
star catalog data to space motion pv-vector
jauFk5hip(double[][], double[])
FK5 to Hipparcos rotation and spin
jauRxp(double[][], double[])
product of r-matrix and p-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauPpp(double[], double[])
p-vector plus p-vector
jauPvstar(double[][])
space motion pv-vector to star catalog data
Reference:
F.Mignard & M.Froeschle, Astron. Astrophys. 354, 732-739 (2000).
public static void jauFk5hip(double[][] r5h, double[] s5h)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
r5h
- double[3][3] returned r-matrix: FK5 rotation wrt Hipparcos (Note 2)s5h
- double[3] returned r-vector: FK5 spin wrt Hipparcos (Note 3)
Notes:
Called:
jauRv2m(double[])
r-vector to r-matrix
Reference:
F.Mignard & M.Froeschle, Astron. Astrophys. 354, 732-739 (2000).
public static JSOFA.SphericalCoordinate jauFk5hz(double r5, double d5, double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
r5
- double FK5 RA (radians), equinox J2000.0, at dated5
- double FK5 Dec (radians), equinox J2000.0, at datedate1
- double TDB date (Notes 1,2)date2
- double TDB date (Notes 1,2)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauS2c(double, double)
spherical coordinates to unit vector
jauFk5hip(double[][], double[])
FK5 to Hipparcos rotation and spin
jauSxp(double, double[])
multiply p-vector by scalar
jauRv2m(double[])
r-vector to r-matrix
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
Reference:
F.Mignard & M.Froeschle, 2000, Astron.Astrophys. 354, 732-739.
public static double[][] jauFw2m(double gamb, double phib, double psi, double eps)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
gamb
- double F-W angle gamma_bar (radians)phib
- double F-W angle phi_bar (radians)psi
- double F-W angle psi (radians)eps
- double F-W angle epsilon (radians)
Notes:
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRz(double, double[][])
rotate around Z-axis
jauRx(double, double[][])
rotate around X-axis
References: Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855 Hilton, J. et al., 2006, Celest.Mech.Dyn.Astron. 94, 351
public static JSOFA.CelestialIntermediatePole jauFw2xy(double gamb, double phib, double psi, double eps)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
gamb
- double F-W angle gamma_bar (radians)phib
- double F-W angle phi_bar (radians)psi
- double F-W angle psi (radians)eps
- double F-W angle epsilon (radians)
Notes:
Called:
jauFw2m(double, double, double, double)
F-W angles to r-matrix
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
Reference: Hilton, J. et al., 2006, Celest.Mech.Dyn.Astron. 94, 351
public static JSOFA.GeodeticCoord jauGc2gd(int n, double[] xyz) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's JSOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical transformation.
n
- int ellipsoid identifier (Note 1)xyz
- double[3] geocentric vector (Note 2)
JSOFAIllegalParameter
- 0 = OK
-1 = illegal identifier (Note 3)
-2 = internal error (Note 3)
Notes:
Called:
jauEform(int)
Earth reference ellipsoids
jauGc2gde(double, double, double[])
geocentric to geodetic transformation, general
public static JSOFA.GeodeticCoord jauGc2gde(double a, double f, double[] xyz) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's JSOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
a
- double equatorial radius (Notes 2,4)f
- double flattening (Note 3)xyz
- double[3] geocentric vector (Note 4)
JSOFAIllegalParameter
- int status:
-1 = illegal a
-2 = illegal f
Notes:
Reference: Fukushima, T., "Transformation from Cartesian to geodetic coordinates accelerated by Halley's method", J.Geodesy (2006) 79: 689-693
public static double[] jauGd2gc(int n, double elong, double phi, double height) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's JSOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical transformation.
n
- int ellipsoid identifier (Note 1)elong
- double longitude (radians, east +ve)phi
- double latitude (geodetic, radians, Note 3)height
- double height above ellipsoid (geodetic, Notes 2,3)
JSOFAIllegalParameter
- -1 = illegal identifier (Note 3)
-2 = illegal case (Note 3)
Notes:
Called:
jauEform(int)
Earth reference ellipsoids
jauGd2gce(double, double, double, double, double)
geodetic to geocentric transformation, general
jauZp(double[])
zero p-vector
JSOFAInternalError
public static double[] jauGd2gce(double a, double f, double elong, double phi, double height) throws JSOFAInternalError
This function is derived from the International Astronomical Union's JSOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
a
- double equatorial radius (Notes 1,4)f
- double flattening (Notes 2,4)elong
- double longitude (radians, east +ve)phi
- double latitude (geodetic, radians, Note 4)height
- double height above ellipsoid (geodetic, Notes 3,4)
JSOFAInternalError
- 0 = OK
-1 = illegal case (Note 4)
Notes:
References:
Green, R.M., Spherical Astronomy, Cambridge University Press, (1985) Section 4.5, p96.
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 4.22, p202.
public static double jauGmst00(double uta, double utb, double tta, double ttb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)tta
- double TT as a 2-part Julian Date (Notes 1,2)ttb
- double TT as a 2-part Julian Date (Notes 1,2)
Notes:
Part A Part B 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable (in the case of UT; the TT is not at all critical in this respect). The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth Rotation Angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauGmst06(double uta, double utb, double tta, double ttb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)tta
- double TT as a 2-part Julian Date (Notes 1,2)ttb
- double TT as a 2-part Julian Date (Notes 1,2)
Notes:
u1a utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable (in the case of UT; the TT is not at all critical in this respect). The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth rotation angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauAnp(double)
normalize angle into range 0 to 2pi
Reference:
Capitaine, N., Wallace, P.T. & Chapront, J., 2005, Astron.Astrophys. 432, 355
public static double jauGmst82(double dj1, double dj2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
dj1
- double UT1 Julian Date (see note)dj2
- double UT1 Julian Date (see note)
Notes:
dj1 dj2 2450123.7D0 0D0 (JD method) 2451545D0 -1421.3D0 (J2000 method) 2400000.5D0 50123.2D0 (MJD method) 2450123.5D0 0.2D0 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. The date & time method is best matched to the algorithm used: maximum accuracy (or, at least, minimum noise) is delivered when the dj1 argument is for 0hrs UT1 on the day in question and the dj2 argument lies in the range 0 to 1, or vice versa.
Called:
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Transactions of the International Astronomical Union, XVIII B, 67 (1983).
Aoki et al., Astron. Astrophys. 105, 359-361 (1982).
public static double jauGst00a(double uta, double utb, double tta, double ttb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)tta
- double TT as a 2-part Julian Date (Notes 1,2)ttb
- double TT as a 2-part Julian Date (Notes 1,2)
Notes:
Part A Part B 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable (in the case of UT; the TT is not at all critical in this respect). The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth Rotation Angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauGmst00(double, double, double, double)
Greenwich mean sidereal time, IAU 2000
jauEe00a(double, double)
equation of the equinoxes, IAU 2000A
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauGst00b(double uta, double utb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth Rotation Angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauGmst00(double, double, double, double)
Greenwich mean sidereal time, IAU 2000
jauEe00b(double, double)
equation of the equinoxes, IAU 2000B
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Capitaine, N., Wallace, P.T. and McCarthy, D.D., "Expressions to implement the IAU 2000 definition of UT1", Astronomy & Astrophysics, 406, 1135-1149 (2003)
McCarthy, D.D. & Luzum, B.J., "An abridged model of the precession-nutation of the celestial pole", Celestial Mechanics & Dynamical Astronomy, 85, 37-49 (2003)
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauGst06(double uta, double utb, double tta, double ttb, double[][] rnpb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)tta
- double TT as a 2-part Julian Date (Notes 1,2)ttb
- double TT as a 2-part Julian Date (Notes 1,2)rnpb
- double[3][3] nutation x precession x bias matrix
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable (in the case of UT; the TT is not at all critical in this respect). The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth rotation angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
jauAnp(double)
normalize angle into range 0 to 2pi
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauEors(double[][], double)
equation of the origins, given NPB matrix and s
Reference:
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static double jauGst06a(double uta, double utb, double tta, double ttb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)tta
- double TT as a 2-part Julian Date (Notes 1,2)ttb
- double TT as a 2-part Julian Date (Notes 1,2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable (in the case of UT; the TT is not at all critical in this respect). The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth rotation angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauGst06(double, double, double, double, double[][])
Greenwich apparent ST, IAU 2006, given NPB matrix
Reference:
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static double jauGst94(double uta, double utb)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
uta
- double UT1 as a 2-part Julian Date (Notes 1,2)utb
- double UT1 as a 2-part Julian Date (Notes 1,2)
Notes:
uta utb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. For UT, the date & time method is best matched to the algorithm that is used by the Earth Rotation Angle function, called internally: maximum precision is delivered when the uta argument is for 0hrs UT1 on the day in question and the utb argument lies in the range 0 to 1, or vice versa.
Called:
jauGmst82(double, double)
Greenwich mean sidereal time, IAU 1982
jauEqeq94(double, double)
equation of the equinoxes, IAU 1994
jauAnp(double)
normalize angle into range 0 to 2pi
References:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992) IAU Resolution C7, Recommendation 3 (1994)
public static JSOFA.CatalogCoords jauH2fk5(double rh, double dh, double drh, double ddh, double pxh, double rvh)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function. Given (all Hipparcos, epoch J2000.0):
rh
- double RA (radians)dh
- double Dec (radians)drh
- double proper motion in RA (dRA/dt, rad/Jyear)ddh
- double proper motion in Dec (dDec/dt, rad/Jyear)pxh
- double parallax (arcsec)rvh
- double radial velocity (km/s, positive = receding)Notes:
Called:
jauStarpv(double, double, double, double, double, double, double[][])
star catalog data to space motion pv-vector
jauFk5hip(double[][], double[])
FK5 to Hipparcos rotation and spin
jauRv2m(double[])
r-vector to r-matrix
jauRxp(double[][], double[])
product of r-matrix and p-vector
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauPmp(double[], double[])
p-vector minus p-vector
jauPvstar(double[][])
space motion pv-vector to star catalog data
Reference:
F.Mignard & M.Froeschle, Astron. Astrophys. 354, 732-739 (2000).
public static JSOFA.CatalogCoords jauHfk5z(double rh, double dh, double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
rh
- double Hipparcos RA (radians)dh
- double Hipparcos Dec (radians)date1
- double TDB date (Note 1)date2
- double TDB date (Note 1)
FIXME original did not return the parallax and radial velocity of the CatalogCoords type.Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauS2c(double, double)
spherical coordinates to unit vector
jauFk5hip(double[][], double[])
FK5 to Hipparcos rotation and spin
jauRxp(double[][], double[])
product of r-matrix and p-vector
jauSxp(double, double[])
multiply p-vector by scalar
jauRxr(double[][], double[][])
product of two r-matrices
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauPv2s(double[][])
pv-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
Reference:
F.Mignard & M.Froeschle, 2000, Astron.Astrophys. 354, 732-739.
public static void jauIr(double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] returned r-matrix
Called:
jauZr(double[][])
zero r-matrix
public static double[][] jauIr()
jauIr(double[][])
that does not require
the vector to be passed in.public static JSOFA.Calendar jauJd2cal(double dj1, double dj2) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
dj1
- double Julian Date (Notes 1, 2)dj2
- double Julian Date (Notes 1, 2)
Returned (arguments):
iy int year
im int month
id int day
fd double fraction of day
JSOFAIllegalParameter
- unacceptable date (Note 3)
Notes:
dj1 dj2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)Separating integer and fraction uses the "compensated summation" algorithm of Kahan-Neumaier to preserve as much precision as possible irrespective of the jd1+jd2 apportionment.
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 12.92 (p604).
Klein, A., A Generalized Kahan-Babuska-Summation-Algorithm. Computing 76, 279-293 (2006), Section 3.
public static int jauJdcalf(int ndp, double dj1, double dj2, int[] iymdf)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
ndp
- int number of decimal places of days in fractiondj1
- double dj1+dj2 = Julian Date (Note 1)dj2
- double dj1+dj2 = Julian Date (Note 1)
iymdf
- int[4] returned year, month, day, fraction in Gregorian calendar
Notes:
dj1 dj2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
Called:
jauJd2cal(double, double)
JD to Gregorian calendar
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 12.92 (p604).
public static double[][] jauNum00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPn00a(double, double)
bias/precession/nutation, IAU 2000A
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.222-3 (p114).
public static double[][] jauNum00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPn00b(double, double)
bias/precession/nutation, IAU 2000B
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.222-3 (p114).
public static double[][] jauNum06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauObl06(double, double)
mean obliquity, IAU 2006
jauNut06a(double, double)
nutation, IAU 2006/2000A
jauNumat(double, double, double)
form nutation matrix
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.222-3 (p114).
public static double[][] jauNumat(double epsa, double dpsi, double deps)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
epsa
- double mean obliquity of date (Note 1)dpsi
- double nutation (Note 2)deps
- double nutation (Note 2)
Notes:
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRx(double, double[][])
rotate around X-axis
jauRz(double, double[][])
rotate around Z-axis
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.222-3 (p114).
public static JSOFA.NutationTerms jauNut00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauFal03(double)
mean anomaly of the Moon
jauFaf03(double)
mean argument of the latitude of the Moon
jauFaom03(double)
mean longitude of the Moon's ascending node
jauFame03(double)
mean longitude of Mercury
jauFave03(double)
mean longitude of Venus
jauFae03(double)
mean longitude of Earth
jauFama03(double)
mean longitude of Mars
jauFaju03(double)
mean longitude of Jupiter
jauFasa03(double)
mean longitude of Saturn
jauFaur03(double)
mean longitude of Uranus
jauFapa03(double)
general accumulated precession in longitude
References:
Chapront, J., Chapront-Touze, M. & Francou, G. 2002, Astron.Astrophys. 387, 700
Lieske, J.H., Lederle, T., Fricke, W. & Morando, B. 1977, Astron.Astrophys. 58, 1-16
Mathews, P.M., Herring, T.A., Buffet, B.A. 2002, J.Geophys.Res. 107, B4. The MHB_2000 code itself was obtained on 9th September 2002 from ftp//maia.usno.navy.mil/conv2000/chapter5/IAU2000A.
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
Wallace, P.T., "Software for Implementing the IAU 2000 Resolutions", in IERS Workshop 5.1 (2002)
public static JSOFA.NutationTerms jauNut00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
References:
Lieske, J.H., Lederle, T., Fricke, W., Morando, B., "Expressions for the precession quantities based upon the IAU /1976/ system of astronomical constants", Astron.Astrophys. 58, 1-2, 1-16. (1977)
Luzum, B., private communication, 2001 (Fortran code MHB_2000_SHORT)
McCarthy, D.D. & Luzum, B.J., "An abridged model of the precession-nutation of the celestial pole", Cel.Mech.Dyn.Astron. 85, 37-49 (2003)
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J., Astron.Astrophys. 282, 663-683 (1994)
public static JSOFA.NutationTerms jauNut06a(double date1, double date2)
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Status: canonical model.
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut00a(double, double)
nutation, IAU 2000A
References:
Chapront, J., Chapront-Touze, M. & Francou, G. 2002, Astron.Astrophys. 387, 700
Lieske, J.H., Lederle, T., Fricke, W. & Morando, B. 1977, Astron.Astrophys. 58, 1-16
Mathews, P.M., Herring, T.A., Buffet, B.A. 2002, J.Geophys.Res. 107, B4. The MHB_2000 code itself was obtained on 9th September 2002 from ftp//maia.usno.navy.mil/conv2000/chapter5/IAU2000A.
Simon, J.-L., Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., Laskar, J. 1994, Astron.Astrophys. 282, 663-683
Souchay, J., Loysel, B., Kinoshita, H., Folgueira, M. 1999, Astron.Astrophys.Supp.Ser. 135, 111
Wallace, P.T., "Software for Implementing the IAU 2000 Resolutions", in IERS Workshop 5.1 (2002)
public static JSOFA.NutationTerms jauNut80(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauAnpm(double)
normalize angle into range +/- pi
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.222 (p111).
public static double[][] jauNutm80(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB date (Note 1)date2
- double TDB date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut80(double, double)
nutation, IAU 1980
jauObl80(double, double)
mean obliquity, IAU 1980
jauNumat(double, double, double)
form nutation matrix
public static double jauObl06(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Reference: Hilton, J. et al., 2006, Celest.Mech.Dyn.Astron. 94, 351
public static double jauObl80(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Expression 3.222-1 (p114).
public static JSOFA.PrecessionAngles jauP06e(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical models.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
References:
Called:
jauObl06(double, double)
mean obliquity, IAU 2006
public static double[][] jauP2pv(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector
Called:
jauCp(double[], double[])
copy p-vector
jauZp(double[])
zero p-vector
public static JSOFA.SphericalPosition jauP2s(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector
Notes:
Called:
jauC2s(double[])
p-vector to spherical
jauPm(double[])
modulus of p-vector
public static double jauPap(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] direction of reference pointb
- double[3] direction of point whose PA is required
Notes:
Called:
jauPn(double[])
decompose p-vector into modulus and direction
jauPm(double[])
modulus of p-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauPmp(double[], double[])
p-vector minus p-vector
jauPdp(double[], double[])
scalar product of two p-vectors
public static double jauPas(double al, double ap, double bl, double bp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
al
- double longitude of point A (e.g. RA) in radiansap
- double latitude of point A (e.g. Dec) in radiansbl
- double longitude of point Bbp
- double latitude of point B
Notes:
public static JSOFA.EulerAngles jauPb06(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPmat06(double, double)
PB matrix, IAU 2006
jauRz(double, double[][])
rotate around Z-axis
public static double jauPdp(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] first p-vectorb
- double[3] second p-vector
public static JSOFA.FWPrecessionAngles jauPfw06(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Reference: Hilton, J. et al., 2006, Celest.Mech.Dyn.Astron. 94, 351
Called:
jauObl06(double, double)
mean obliquity, IAU 2006
public static double[][] jauPlan94(double date1, double date2, int np) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB date part A (Note 1)date2
- double TDB date part B (Note 1)np
- int planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars,
5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune)
Returned (argument):Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. The limited accuracy of the present algorithm is such that any of the methods is satisfactory.
pv[0][0] x } pv[0][1] y } heliocentric position, au pv[0][2] z } pv[1][0] xdot } pv[1][1] ydot } heliocentric velocity, au/d pv[1][2] zdot }The reference frame is equatorial and is with respect to the mean equator and equinox of epoch J2000.0.
L (arcsec) B (arcsec) R (km) Mercury 4 1 300 Venus 5 1 800 EMB 6 1 1000 Mars 17 1 7700 Jupiter 71 5 76000 Saturn 81 13 267000 Uranus 86 7 712000 Neptune 11 1 253000Over the interval 1000-3000, they report that the accuracy is no worse than 1.5 times that over 1800-2050. Outside 1000-3000 the accuracy declines. Comparisons of the present function with the JPL DE200 ephemeris give the following RMS errors over the interval 1960-2025:
position (km) velocity (m/s) Mercury 334 0.437 Venus 1060 0.855 EMB 2010 0.815 Mars 7690 1.98 Jupiter 71700 7.70 Saturn 199000 19.4 Uranus 564000 16.4 Neptune 158000 14.4Comparisons against DE200 over the interval 1800-2100 gave the following maximum absolute differences. (The results using DE406 were essentially the same.)
L (arcsec) B (arcsec) R (km) Rdot (m/s) Mercury 7 1 500 0.7 Venus 7 1 1100 0.9 EMB 9 1 1300 1.0 Mars 26 1 9000 2.5 Jupiter 78 6 82000 8.2 Saturn 87 14 263000 24.6 Uranus 86 7 661000 27.4 Neptune 11 2 248000 21.4
Called:
jauAnp(double)
normalize angle into range 0 to 2pi
Reference: Simon, J.L, Bretagnon, P., Chapront, J., Chapront-Touze, M., Francou, G., and Laskar, J., Astron. Astrophys. 282, 663 (1994).
JSOFAIllegalParameter
- for a bad np (planet number)public static double jauPm(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector
public static double[][] jauPmat00(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauBp00(double, double, double[][], double[][], double[][])
frame bias and precession matrices, IAU 2000
Reference: IAU: Trans. International Astronomical Union, Vol. XXIVB; Proc. 24th General Assembly, Manchester, UK. Resolutions B1.3, B1.6. (2000)
public static double[][] jauPmat06(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPfw06(double, double)
bias-precession F-W angles, IAU 2006
jauFw2m(double, double, double, double)
F-W angles to r-matrix
References:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
IAU: Trans. International Astronomical Union, Vol. XXIVB; Proc. 24th General Assembly, Manchester, UK. Resolutions B1.3, B1.6.(2000)
public static double[][] jauPmat76(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double ending date, TT (Note 1)date2
- double ending date, TT (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPrec76(double, double, double, double)
accumulated precession angles, IAU 1976
jauIr(double[][])
initialize r-matrix to identity
jauRz(double, double[][])
rotate around Z-axis
jauRy(double, double[][])
rotate around Y-axis
jauCr(double[][], double[][])
copy r-matrix
References:
Lieske, J.H., 1979, Astron.Astrophys. 73, 282. equations (6) & (7), p283. Kaplan,G.H., 1981. USNO circular no. 163, pA2.
public static double[] jauPmp(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] first p-vectorb
- double[3] second p-vector
public static JSOFA.NormalizedVector jauPn(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] p-vector
Notes:
Called:
jauPm(double[])
modulus of p-vector
jauZp(double[])
zero p-vector
jauSxp(double, double[])
multiply p-vector by scalar
public static JSOFA.PrecessionNutation jauPn00(double date1, double date2, double dpsi, double deps)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)dpsi
- double nutation (Note 2)deps
- double nutation (Note 2)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPr00(double, double)
IAU 2000 precession adjustments
jauObl80(double, double)
mean obliquity, IAU 1980
jauBp00(double, double, double[][], double[][], double[][])
frame bias and precession matrices, IAU 2000
jauCr(double[][], double[][])
copy r-matrix
jauNumat(double, double, double)
form nutation matrix
jauRxr(double[][], double[][])
product of two r-matrices
Reference:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
public static JSOFA.PrecessionNutation jauPn00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut00a(double, double)
nutation, IAU 2000A
jauPn00(double, double, double, double)
bias/precession/nutation results, IAU 2000
Reference:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
public static JSOFA.PrecessionNutation jauPn00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut00b(double, double)
nutation, IAU 2000B
jauPn00(double, double, double, double)
bias/precession/nutation results, IAU 2000
Reference:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003). n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
public static JSOFA.PrecessionNutation jauPn06(double date1, double date2, double dpsi, double deps)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)dpsi
- double nutation (Note 2)deps
- double nutation (Note 2)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPfw06(double, double)
bias-precession F-W angles, IAU 2006
jauFw2m(double, double, double, double)
F-W angles to r-matrix
jauCr(double[][], double[][])
copy r-matrix
jauTr(double[][])
transpose r-matrix
jauRxr(double[][], double[][])
product of two r-matrices
References:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static JSOFA.PrecessionNutation jauPn06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauNut06a(double, double)
nutation, IAU 2006/2000A
jauPn06(double, double, double, double)
bias/precession/nutation results, IAU 2006
Reference:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
public static double[][] jauPnm00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPn00a(double, double)
bias/precession/nutation, IAU 2000A
Reference: IAU: Trans. International Astronomical Union, Vol. XXIVB; Proc. 24th General Assembly, Manchester, UK. Resolutions B1.3, B1.6. (2000)
public static double[][] jauPnm00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPn00b(double, double)
bias/precession/nutation, IAU 2000B
Reference: IAU: Trans. International Astronomical Union, Vol. XXIVB; Proc. 24th General Assembly, Manchester, UK. Resolutions B1.3, B1.6. (2000)
public static double[][] jauPnm06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPfw06(double, double)
bias-precession F-W angles, IAU 2006
jauNut06a(double, double)
nutation, IAU 2006/2000A
jauFw2m(double, double, double, double)
F-W angles to r-matrix
Reference:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855.
public static double[][] jauPnm80(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB date (Note 1)date2
- double TDB date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPmat76(double, double)
precession matrix, IAU 1976
jauNutm80(double, double)
nutation matrix, IAU 1980
jauRxr(double[][], double[][])
product of two r-matrices
Reference:
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992), Section 3.3 (p145).
public static double[][] jauPom00(double xp, double yp, double sp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
xp
- double coordinates of the pole (radians, Note 1)yp
- double coordinates of the pole (radians, Note 1)sp
- double the TIO locator s' (radians, Note 2)
Notes:
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRz(double, double[][])
rotate around Z-axis
jauRy(double, double[][])
rotate around Y-axis
jauRx(double, double[][])
rotate around X-axis
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double[] jauPpp(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] first p-vectorb
- double[3] second p-vector
public static double[] jauPv2p(double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
pv
- double[2][3] pv-vector
Called:
jauCp(double[], double[])
copy p-vector
public static JSOFA.SphericalPositionVelocity jauPv2s(double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
pv
- double[2][3] pv-vector
Notes:
public static double[] jauPvdpv(double[][] a, double[][] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[2][3] first pv-vectorb
- double[2][3] second pv-vector
Called:
jauPdp(double[], double[])
scalar product of two p-vectors
public static JSOFA.PVModulus jauPvm(double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
pv
- double[2][3] pv-vector
Called:
jauPm(double[])
modulus of p-vector
public static double[][] jauPvmpv(double[][] a, double[][] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[2][3] first pv-vectorb
- double[2][3] second pv-vector
Called:
jauPmp(double[], double[])
p-vector minus p-vector
public static double[][] jauPvppv(double[][] a, double[][] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[2][3] first pv-vectorb
- double[2][3] second pv-vector
Called:
jauPpp(double[], double[])
p-vector plus p-vector
public static JSOFA.CatalogCoords jauPvstar(double[][] pv) throws JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function. Given (Note 1):
pv
- double[2][3] pv-vector (au, au/day)
JSOFAInternalError
- superluminal speed (Note 5), or null position vector
Notes:
Called:
jauPn(double[])
decompose p-vector into modulus and direction
jauPdp(double[], double[])
scalar product of two p-vectors
jauSxp(double, double[])
multiply p-vector by scalar
jauPmp(double[], double[])
p-vector minus p-vector
jauPm(double[])
modulus of p-vector
jauPpp(double[], double[])
p-vector plus p-vector
jauPv2s(double[][])
pv-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
Reference: Stumpff, P., 1985, Astron.Astrophys. 144, 232-240.
public static double[][] jauPvu(double dt, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
dt
- double time intervalpv
- double[2][3] pv-vector
Notes:
Called:
jauPpsp(double[], double, double[])
p-vector plus scaled p-vector
jauCp(double[], double[])
copy p-vector
public static double[] jauPvup(double dt, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
dt
- double time intervalpv
- double[2][3] pv-vector
Notes:
public static double[][] jauPvxpv(double[][] a, double[][] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[2][3] first pv-vectorb
- double[2][3] second pv-vector
Notes:
Called:
jauCpv(double[][], double[][])
copy pv-vector
jauPxp(double[], double[])
vector product of two p-vectors
jauPpp(double[], double[])
p-vector plus p-vector
public static double[] jauPxp(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] first p-vectorb
- double[3] second p-vector
public static double[] jauRm2v(double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] rotation matrix
Notes:
public static double[][] jauRv2m(double[] w)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
w
- double[3] rotation vector (Note 1)
Notes:
public static void jauRx(double phi, double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
phi
- double angle (radians)
Given and returned:r
- double[3][3] r-matrix given and returned
Sign convention: The matrix can be used to rotate the reference
frame of a vector. Calling this function with positive phi
incorporates in the matrix an additional rotation, about the x-axis,
anticlockwise as seen looking towards the origin from positive x.
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRxr(double[][], double[][])
product of two r-matrices
jauCr(double[][], double[][])
copy r-matrix
public static double[] jauRxp(double[][] r, double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrixp
- double[3] p-vector
Called:
jauCp(double[], double[])
copy p-vector
public static double[][] jauRxpv(double[][] r, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrixpv
- double[2][3] pv-vector
Called:
jauRxp(double[][], double[])
product of r-matrix and p-vector
public static double[][] jauRxr(double[][] a, double[][] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3][3] first r-matrixb
- double[3][3] second r-matrix
Called:
jauCr(double[][], double[][])
copy r-matrix
public static void jauRy(double theta, double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
theta
- double angle (radians)
Given and returned:r
- double[3][3] given & returned r-matrix
Sign convention: The matrix can be used to rotate the reference
frame of a vector. Calling This function with positive theta
incorporates in the matrix an additional rotation, about the y-axis,
anticlockwise as seen looking towards the origin from positive y.
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRxr(double[][], double[][])
product of two r-matrices
jauCr(double[][], double[][])
copy r-matrix
public static void jauRz(double psi, double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
psi
- double angle (radians)
Given and returned:r
- double[3][3] given & retunedr-matrix, rotated
Sign convention: The matrix can be used to rotate the reference
frame of a vector. Calling This function with positive psi
incorporates in the matrix an additional rotation, about the z-axis,
anticlockwise as seen looking towards the origin from positive z.
Called:
jauIr(double[][])
initialize r-matrix to identity
jauRxr(double[][], double[][])
product of two r-matrices
jauCr(double[][], double[][])
copy r-matrix
public static double jauS00(double date1, double date2, double x, double y)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)x
- double CIP coordinates (Note 3)y
- double CIP coordinates (Note 3)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauFal03(double)
mean anomaly of the Moon
jauFalp03(double)
mean anomaly of the Sun
jauFaf03(double)
mean argument of the latitude of the Moon
jauFad03(double)
mean elongation of the Moon from the Sun
jauFaom03(double)
mean longitude of the Moon's ascending node
jauFave03(double)
mean longitude of Venus
jauFae03(double)
mean longitude of Earth
jauFapa03(double)
general accumulated precession in longitude
References:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauS00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm00a(double, double)
classical NPB matrix, IAU 2000A
jauBpn2xy(double[][])
extract CIP X,Y from the BPN matrix
jauS00(double, double, double, double)
the CIO locator s, given X,Y, IAU 2000A
References:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauS00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm00b(double, double)
classical NPB matrix, IAU 2000B
jauBpn2xy(double[][])
extract CIP X,Y from the BPN matrix
jauS00(double, double, double, double)
the CIO locator s, given X,Y, IAU 2000A
References:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static double jauS06(double date1, double date2, double x, double y)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)x
- double CIP coordinates (Note 3)y
- double CIP coordinates (Note 3)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauFal03(double)
mean anomaly of the Moon
jauFalp03(double)
mean anomaly of the Sun
jauFaf03(double)
mean argument of the latitude of the Moon
jauFad03(double)
mean elongation of the Moon from the Sun
jauFaom03(double)
mean longitude of the Moon's ascending node
jauFave03(double)
mean longitude of Venus
jauFae03(double)
mean longitude of Earth
jauFapa03(double)
general accumulated precession in longitude
References:
Capitaine, N., Wallace, P.T. & Chapront, J., 2003, Astron. Astrophys. 432, 355
McCarthy, D.D., Petit, G. (eds.) 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
public static double jauS06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
References:
Capitaine, N., Chapront, J., Lambert, S. and Wallace, P., "Expressions for the Celestial Intermediate Pole and Celestial Ephemeris Origin consistent with the IAU 2000A precession- nutation model", Astron.Astrophys. 400, 1145-1154 (2003) n.b. The celestial ephemeris origin (CEO) was renamed "celestial intermediate origin" (CIO) by IAU 2006 Resolution 2.
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
McCarthy, D. D., Petit, G. (eds.), 2004, IERS Conventions (2003), IERS Technical Note No. 32, BKG
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static double[] jauS2c(double theta, double phi)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
theta
- double longitude angle (radians)phi
- double latitude angle (radians)
public static double[] jauS2p(double theta, double phi, double r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
theta
- double longitude angle (radians)phi
- double latitude angle (radians)r
- double radial distance
Called:
jauS2c(double, double)
spherical coordinates to unit vector
jauSxp(double, double[])
multiply p-vector by scalar
public static double[][] jauS2pv(double theta, double phi, double r, double td, double pd, double rd)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
theta
- double longitude angle (radians)phi
- double latitude angle (radians)r
- double radial distancetd
- double rate of change of thetapd
- double rate of change of phird
- double rate of change of r
public static double[][] jauS2xpv(double s1, double s2, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
s1
- double scalar to multiply position component bys2
- double scalar to multiply velocity component bypv
- double[2][3] pv-vector
Called:
jauSxp(double, double[])
multiply p-vector by scalar
public static double jauSepp(double[] a, double[] b)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
a
- double[3] first p-vector (not necessarily unit length)b
- double[3] second p-vector (not necessarily unit length)
Notes:
Called:
jauPxp(double[], double[])
vector product of two p-vectors
jauPm(double[])
modulus of p-vector
jauPdp(double[], double[])
scalar product of two p-vectors
public static double jauSeps(double al, double ap, double bl, double bp)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
al
- double first longitude (radians)ap
- double first latitude (radians)bl
- double second longitude (radians)bp
- double second latitude (radians)
Called:
jauS2c(double, double)
spherical coordinates to unit vector
jauSepp(double[], double[])
angular separation between two p-vectors
public static double jauSp00(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: canonical model.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.CatalogCoords jauStarpm(double ra1, double dec1, double pmr1, double pmd1, double px1, double rv1, double ep1a, double ep1b, double ep2a, double ep2b) throws JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
ra1
- double right ascension (radians), beforedec1
- double declination (radians), beforepmr1
- double RA proper motion (radians/year), beforepmd1
- double Dec proper motion (radians/year), beforepx1
- double parallax (arcseconds), beforerv1
- double radial velocity (km/s, +ve = receding), beforeep1a
- double "before" epoch, part A (Note 1)ep1b
- double "before" epoch, part B (Note 1)ep2a
- double "after" epoch, part A (Note 1)ep2b
- double "after" epoch, part B (Note 1)
JSOFAInternalError
public static int jauStarpv(double ra, double dec, double pmr, double pmd, double px, double rv, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function. Given (Note 1):
ra
- double right ascension (radians)dec
- double declination (radians)pmr
- double RA proper motion (radians/year)pmd
- double Dec proper motion (radians/year)px
- double parallax (arcseconds)rv
- double radial velocity (km/s, positive = receding)
Returned (Note 2):pv
- double[2][3] pv-vector (au, au/day)
Notes:
Called:
jauS2pv(double, double, double, double, double, double)
spherical coordinates to pv-vector
jauPm(double[])
modulus of p-vector
jauZp(double[])
zero p-vector
jauPn(double[])
decompose p-vector into modulus and direction
jauPdp(double[], double[])
scalar product of two p-vectors
jauSxp(double, double[])
multiply p-vector by scalar
jauPmp(double[], double[])
p-vector minus p-vector
jauPpp(double[], double[])
p-vector plus p-vector
Reference: Stumpff, P., 1985, Astron.Astrophys. 144, 232-240.
public static double[] jauSxp(double s, double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
s
- double scalarp
- double[3] p-vector
public static double[][] jauSxpv(double s, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
s
- double scalarpv
- double[2][3] pv-vector
Called:
jauS2xpv(double, double, double[][])
multiply pv-vector by two scalars
public static JSOFA.JulianDate jauTaitt(double tai1, double tai2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tai1
- double TAI as a 2-part Julian Datetai2
- double TAI as a 2-part Julian Date
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
public static JSOFA.JulianDate jauTaiut1(double tai1, double tai2, double dta)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tai1
- double TAI as a 2-part Julian Datetai2
- double TAI as a 2-part Julian Datedta
- double UT1-TAI in seconds
Notes:
public static JSOFA.JulianDate jauTaiutc(double tai1, double tai2) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tai1
- TAI as a 2-part Julian Date (Note 1)tai2
- TAI as a 2-part Julian Date (Note 1)
Notes:
jauJd2cal(double, double)
JD to Gregorian calendar
jauDat(int, int, int, double)
delta(AT) = TAI-UTC
jauCal2jd(int, int, int)
Gregorian calendar to JD
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
JSOFAIllegalParameter
JSOFAInternalError
- an internal error has occuredpublic static JSOFA.JulianDate jauTcbtdb(double tcb1, double tcb2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tcb1
- double TCB as a 2-part Julian Datetcb2
- double TCB as a 2-part Julian Date
Notes:
public static JSOFA.JulianDate jauTcgtt(double tcg1, double tcg2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tcg1
- double TCG as a 2-part Julian Datetcg2
- double TCG as a 2-part Julian Date
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003),. IERS Technical Note No. 32, BKG (2004) IAU 2000 Resolution B1.9
public static JSOFA.JulianDate jauTdbtcb(double tdb1, double tdb2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tdb1
- TDB as a 2-part Julian Datetdb2
- TDB as a 2-part Julian Date
Notes:
public static JSOFA.JulianDate jauTdbtt(double tdb1, double tdb2, double dtr)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tdb1
- double TDB as a 2-part Julian Datetdb2
- double TDB as a 2-part Julian Datedtr
- double TDB-TT in seconds
Notes:
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) IAU 2006 Resolution 3
public static double jauTf2a(char s, int ihour, int imin, double sec) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
s
- char sign: '-' = negative, otherwise positiveihour
- int hoursimin
- int minutessec
- double seconds
JSOFAIllegalParameter
- illegal parameter of some form
1 = ihour outside range 0-23
2 = imin outside range 0-59
3 = sec outside range 0-59.999...
Notes:
public static double jauTf2d(char s, int ihour, int imin, double sec) throws JSOFAIllegalParameter
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
s
- char sign: '-' = negative, otherwise positiveihour
- int hoursimin
- int minutessec
- double seconds
Notes:
JSOFAIllegalParameter
- whne the inputs outside range - hour outside range 0-23, imin outside range 0-59, sec outside range 0-59.999...public static double[][] jauTr(double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrix
Called:
jauCr(double[][], double[][])
copy r-matrix
public static double[] jauTrxp(double[][] r, double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrixp
- double[3] p-vector
Called:
jauTr(double[][])
transpose r-matrix
jauRxp(double[][], double[])
product of r-matrix and p-vector
public static double[][] jauTrxpv(double[][] r, double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] r-matrixpv
- double[2][3] pv-vector
Called:
jauTr(double[][])
transpose r-matrix
jauRxpv(double[][], double[][])
product of r-matrix and pv-vector
public static JSOFA.JulianDate jauTttai(double tt1, double tt2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tt1
- double TT as a 2-part Julian Datett2
- double TT as a 2-part Julian Date
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
public static JSOFA.JulianDate jauTttcg(double tt1, double tt2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tt1
- double TT as a 2-part Julian Datett2
- double TT as a 2-part Julian Date
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) IAU 2000 Resolution B1.9
public static JSOFA.JulianDate jauTttdb(double tt1, double tt2, double dtr)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tt1
- double TT as a 2-part Julian Datett2
- double TT as a 2-part Julian Datedtr
- double TDB-TT in seconds
Notes: 1 tt1+tt2 is Julian Date, apportioned in any convenient way between the two arguments, for example where tt1 is the Julian Day Number and tt2 is the fraction of a day. The returned tdb1,tdb2 follow suit. 2 The argument dtr represents the quasi-periodic component of the GR transformation between TT and TCB. It is dependent upon the adopted solar-system ephemeris, and can be obtained by numerical integration, by interrogating a precomputed time ephemeris or by evaluating a model such as that implemented in the SOFA function jauDtdb. The quantity is dominated by an annual term of 1.7 ms amplitude. 3 TDB is essentially the same as Teph, the time argument for the JPL solar system ephemerides.
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) IAU 2006 Resolution 3
public static JSOFA.JulianDate jauTtut1(double tt1, double tt2, double dt)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
tt1
- double TT as a 2-part Julian Datett2
- double TT as a 2-part Julian Datedt
- double TT-UT1 in seconds
Notes: 1 tt1+tt2 is Julian Date, apportioned in any convenient way between the two arguments, for example where tt1 is the Julian Day Number and tt2 is the fraction of a day. The returned ut11,ut12 follow suit. 2 The argument dt is classical Delta T. Reference: Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
public static JSOFA.JulianDate jauUt1tai(double ut11, double ut12, double dta)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
ut11
- double UT1 as a 2-part Julian Dateut12
- double UT1 as a 2-part Julian Datedta
- double UT1-TAI in seconds
Notes: 1 ut11+ut12 is Julian Date, apportioned in any convenient way between the two arguments, for example where ut11 is the Julian Day Number and ut12 is the fraction of a day. The returned TAI1,TAI2 follow suit. 2 The argument dta, i.e. UT1-TAI, is an observed quantity, and is available from IERS tabulations. Reference: Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
public static JSOFA.JulianDate jauUt1tt(double ut11, double ut12, double dt)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
ut11
- double UT1 as a 2-part Julian Dateut12
- double UT1 as a 2-part Julian Datedt
- double TT-UT1 in seconds
Notes: 1 ut11+ut12 is Julian Date, apportioned in any convenient way between the two arguments, for example where ut11 is the Julian Day Number and ut12 is the fraction of a day. The returned tt1,tt2 follow suit. 2 The argument dt is classical Delta T. Reference: Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
public static JSOFA.JulianDate jauUt1utc(double ut11, double ut12, double dut1) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
ut11
- double UT1 as a 2-part Julian Date (Note 1)ut12
- double UT1 as a 2-part Julian Date (Note 1)dut1
- double Delta UT1: UT1-UTC in seconds (Note 2)
Notes:
jauJd2cal(double, double)
JD to Gregorian calendar
jauDat(int, int, int, double)
delta(AT) = TAI-UTC
jauCal2jd(int, int, int)
Gregorian calendar to JD
References:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
JSOFAIllegalParameter
- unacceptable dateJSOFAInternalError
- an internal error has occuredpublic static JSOFA.JulianDate jauUtctai(double utc1, double utc2) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
utc1
- double UTC as a 2-part quasi Julian Date (Notes 1-4)utc2
- double UTC as a 2-part quasi Julian Date (Notes 1-4)
Notes:
jauJd2cal(double, double)
JD to Gregorian calendar
jauDat(int, int, int, double)
delta(AT) = TAI-UTC
jauCal2jd(int, int, int)
Gregorian calendar to JD
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992)
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unaccaptable datepublic static JSOFA.JulianDate jauUtcut1(double utc1, double utc2, double dut1) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: canonical.
utc1
- double UTC as a 2-part quasi Julian Date (Notes 1-4)utc2
- double UTC as a 2-part quasi Julian Date (Notes 1-4)dut1
- double Delta UT1 = UT1-UTC in seconds (Note 5)
Notes:
References: McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004) Explanatory Supplement to the Astronomical Almanac, P. Kenneth Seidelmann (ed), University Science Books (1992) Called:
jauJd2cal(double, double)
JD to Gregorian calendar
jauDat(int, int, int, double)
delta(AT) = TAI-UTC
jauUtctai(double, double)
UTC to TAI
jauTaiut1(double, double, double)
TAI to UT1
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unaccepatble datepublic static JSOFA.CelestialIntermediatePole jauXy06(double date1, double date2)
public static JSOFA.ICRFrame jauXys00a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm00a(double, double)
classical NPB matrix, IAU 2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS00(double, double, double, double)
the CIO locator s, given X,Y, IAU 2000A
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.ICRFrame jauXys00b(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm00b(double, double)
classical NPB matrix, IAU 2000B
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS00(double, double, double, double)
the CIO locator s, given X,Y, IAU 2000A
Reference:
McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), IERS Technical Note No. 32, BKG (2004)
public static JSOFA.ICRFrame jauXys06a(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian Date (Note 1)date2
- double TT as a 2-part Julian Date (Note 1)
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
Called:
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
References:
Capitaine, N. & Wallace, P.T., 2006, Astron.Astrophys. 450, 855
Wallace, P.T. & Capitaine, N., 2006, Astron.Astrophys. 459, 981
public static void jauZp(double[] p)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
p
- double[3] returned p-vectorpublic static double[] jauZp()
jauZp(double[])
that does not require
the vector to be passed in.public static void jauZpv(double[][] pv)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
pv
- double[2][3] returned pv-vector
Called:
jauZp(double[])
zero p-vector
public static double[][] jauZpv()
jauZpv(double[][])
that does not require
the vector to be passed in.public static void jauZr(double[][] r)
This function is derived from the International Astronomical Union's SOFA (Standards Of Fundamental Astronomy) software collection.
Status: vector/matrix support function.
r
- double[3][3] returned r-matrixpublic static double[][] jauZr()
jauZr(double[][])
that does not require
the vector to be passed in.public static double[] jauAb(double[] pnat, double[] v, double s, double bm1)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
pnat
- double[3] natural direction to the source (unit vector)v
- double[3] observer barycentric velocity in units of cs
- double distance between the Sun and the observer (au)bm1
- double sqrt(1-|v|^2): reciprocal of Lorenz factor
Notes:
o Rigorous rather than approximate normalization is applied.
o The gravitational potential term from Expr. (7) in Klioner (2003) is added, taking into account only the Sun's contribution. This has a maximum effect of about 0.4 microarcsecond.
References:
jauPdp(double[], double[])
scalar product of two p-vectors
public static void jauApcg(double date1, double date2, double[][] ebpv, double[] ehp, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)ebpv
- double[2][3] Earth barycentric pos/vel (au, au/day)ehp
- double[3] Earth heliocentric position (au)
astrom
- jauASTROM Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed
.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauApcs(double, double, double[][], double[][], double[], org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-GCRS, space observer
public static void jauApcg13(double date1, double date2, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)
astrom
- Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed
.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauEpv00(double, double, double[][], double[][])
Earth position and velocity
jauApcg(double, double, double[][], double[], org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-GCRS, geocenter
public static void jauApci(double date1, double date2, double[][] ebpv, double[] ehp, double x, double y, double s, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)ebpv
- double[2][3] Earth barycentric position/velocity (au, au/day)ehp
- double[3] Earth heliocentric position (au)x
- double CIP X,Y (components of unit vector)y
- double CIP X,Y (components of unit vector)s
- double the CIO locator s (radians)
astrom
- Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauApcg(double, double, double[][], double[], org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-GCRS, geocenter
jauC2ixys(double, double, double)
celestial-to-intermediate matrix, given X,Y and s
public static double jauApci13(double date1, double date2, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)
astrom
- jauASTROM Returned star-independent astrometry parameters:
pmt double Returned PM time interval (SSB, Julian years)
eb double[3] Returned SSB to observer (vector, au)
eh double[3] Returned Sun to observer (unit vector)
em double Returned distance from Sun to observer (au)
v double[3] Returned barycentric observer velocity (vector, c)
bm1 double Returned sqrt(1-|v|^2): reciprocal of Lorenz factor
bpn double[3][3] Returned bias-precession-nutation matrix
along double Returned unchanged
xpl double Returned unchanged
ypl double Returned unchanged
sphi double Returned unchanged
cphi double Returned unchanged
diurab double Returned unchanged
eral double Returned unchanged
refa double Returned unchanged
refb double Returned unchangedNotes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauEpv00(double, double, double[][], double[][])
Earth position and velocity
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
jauApci(double, double, double[][], double[], double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-CIRS
jauEors(double[][], double)
equation of the origins, given NPB matrix and s
public static void jauApco(double date1, double date2, double[][] ebpv, double[] ehp, double x, double y, double s, double theta, double elong, double phi, double hm, double xp, double yp, double sp, double refa, double refb, JSOFA.Astrom astrom) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)ebpv
- double[2][3] Earth barycentric PV (au, au/day, Note 2)ehp
- double[3] Earth heliocentric P (au, Note 2)x
- double CIP X,Y (components of unit vector)y
- double CIP X,Y (components of unit vector)s
- double the CIO locator s (radians)theta
- double Earth rotation angle (radians)elong
- double longitude (radians, east +ve, Note 3)phi
- double latitude (geodetic, radians, Note 3)hm
- double height above ellipsoid (m, geodetic, Note 3)xp
- double polar motion coordinates (radians, Note 4)yp
- double polar motion coordinates (radians, Note 4)sp
- double the TIO locator s' (radians, Note 4)refa
- double refraction constant A (radians, Note 5)refb
- double refraction constant B (radians, Note 5)
astrom
- Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
Internally, the polar motion is stored in a form rotated onto the local meridian.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauAper(double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters: update ERA
jauC2ixys(double, double, double)
celestial-to-intermediate matrix, given X,Y and s
jauPvtob(double, double, double, double, double, double, double)
position/velocity of terrestrial station
jauTrxpv(double[][], double[][])
product of transpose of r-matrix and pv-vector
jauApcs(double, double, double[][], double[][], double[], org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-GCRS, space observer
jauCr(double[][], double[][])
copy r-matrix
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable datepublic static double jauApco13(double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl, JSOFA.Astrom astrom) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 1,2)dut1
- double UT1-UTC (seconds, Note 3)elong
- double longitude (radians, east +ve, Note 4)phi
- double latitude (geodetic, radians, Note 4)hm
- double height above ellipsoid (m, geodetic, Notes 4,6)xp
- double polar motion coordinates (radians, Note 5)yp
- double polar motion coordinates (radians, Note 5)phpa
- double pressure at the observer (hPa = mB, Note 6)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 7)
astrom
- Returned star-independent astrometry parameters:JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 2)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
Internally, the polar motion is stored in a form rotated onto the local meridian.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauUtctai(double, double)
UTC to TAI
jauTaitt(double, double)
TAI to TT
jauUtcut1(double, double, double)
UTC to UT1
jauEpv00(double, double, double[][], double[][])
Earth position and velocity
jauPnm06a(double, double)
classical NPB matrix, IAU 2006/2000A
jauBpn2xy(double[][])
extract CIP X,Y coordinates from NPB matrix
jauS06(double, double, double, double)
the CIO locator s, given X,Y, IAU 2006
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauSp00(double, double)
the TIO locator s', IERS 2000
jauRefco(double, double, double, double)
refraction constants for given ambient conditions
jauApco(double, double, double[][], double[], double, double, double, double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-observed
jauEors(double[][], double)
equation of the origins, given NPB matrix and s
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static void jauApcs(double date1, double date2, double[][] pv, double[][] ebpv, double[] ehp, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)pv
- double[2][3] observer's geocentric pos/vel (m, m/s)ebpv
- double[2][3] Earth barycentric PV (au, au/day)ehp
- double[3] Earth heliocentric P (au)
astrom
- Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauCp(double[], double[])
copy p-vector
jauPm(double[])
modulus of p-vector
jauPn(double[])
decompose p-vector into modulus and direction
jauIr(double[][])
initialize r-matrix to identity
public static void jauApcs13(double date1, double date2, double[][] pv, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)pv
- double[2][3] observer's geocentric pos/vel (Note 3)
astrom
- Returned star-independent astrometry parameters:
Notes:
date1 date2 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauEpv00(double, double, double[][], double[][])
Earth position and velocity
jauApcs(double, double, double[][], double[][], double[], org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-GCRS, space observer
public static void jauAper(double theta, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
theta
- double Earth rotation angle (radians, Note 2)astrom
- Astrom star-independent astrometry parameters:pmt double not used
eb double[3] not used
eh double[3] not used
em double not used
v double[3] not used
bm1 double not used
bpn double[3][3] not used
along double longitude + s' (radians)
xpl double not used
ypl double not used
sphi double not used
cphi double not used
diurab double not used
eral double not used
refa double not used
refb double not used
astrom Returned star-independent astrometry parameters:
Notes:
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
public static void jauAper13(double ut11, double ut12, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ut11
- double UT1 as a 2-part...ut12
- double ...Julian Date (Note 1)astrom
- star-independent astrometry parameters:
pmt double not used
eb double[3] not used
eh double[3] not used
em double not used
v double[3] not used
bm1 double not used
bpn double[3][3] not used
along double longitude + s' (radians)
xpl double not used
ypl double not used
sphi double not used
cphi double not used
diurab double not used
eral double not used
refa double not used
refb double not used
astrom
- Returned star-independent astrometry parameters:
Notes:
ut11 ut12 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 and MJD methods are good compromises between resolution and convenience. The date & time method is best matched to the algorithm used: maximum precision is delivered when the ut11 argument is for 0hrs UT1 on the day in question and the ut12 argument lies in the range 0 to 1, or vice versa.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
<p>iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauAper(double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters: update ERA
jauEra00(double, double)
Earth rotation angle, IAU 2000
public static void jauApio(double sp, double theta, double elong, double phi, double hm, double xp, double yp, double refa, double refb, JSOFA.Astrom astrom) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
sp
- double the TIO locator s' (radians, Note 1)theta
- double Earth rotation angle (radians)elong
- double longitude (radians, east +ve, Note 2)phi
- double geodetic latitude (radians, Note 2)hm
- double height above ellipsoid (m, geodetic Note 2)xp
- double polar motion coordinates (radians, Note 3)yp
- double polar motion coordinates (radians, Note 3)refa
- double refraction constant A (radians, Note 4)refb
- double refraction constant B (radians, Note 4)
astrom
- JSOFA.Astrom
Returned star-independent astrometry parameters:
Notes:
Internally, the polar motion is stored in a form rotated onto the local meridian.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauPvtob(double, double, double, double, double, double, double)
position/velocity of terrestrial station
jauAper(double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters: update ERA
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static void jauApio13(double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl, JSOFA.Astrom astrom) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 1,2)dut1
- double UT1-UTC (seconds)elong
- double longitude (radians, east +ve, Note 3)phi
- double geodetic latitude (radians, Note 3)hm
- double height above ellipsoid (m, geodetic Notes 4,6)xp
- double polar motion coordinates (radians, Note 5)yp
- double polar motion coordinates (radians, Note 5)phpa
- double pressure at the observer (hPa = mB, Note 6)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 7)
astrom
- Returned star-independent astrometry parameters:JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 2)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
Internally, the polar motion is stored in a form rotated onto the local meridian.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
ICRS <-> GCRS <-> CIRS <-> observed.
The various functions support different classes of observer and portions of the transformation chain:
functions observer transformation
iauApcg iauApcg13 geocentric ICRS <-> GCRS
iauApci iauApci13 terrestrial ICRS <-> CIRS
iauApco iauApco13 terrestrial ICRS <-> observed
iauApcs iauApcs13 space ICRS <-> GCRS
iauAper iauAper13 terrestrial update Earth rotation
iauApio iauApio13 terrestrial CIRS <-> observed
Those with names ending in "13" use contemporary SOFA models to compute the various ephemerides. The others accept ephemerides supplied by the caller.
The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration. From GCRS to CIRS
comprises frame bias and precession-nutation. From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.
jauUtctai(double, double)
UTC to TAI
jauTaitt(double, double)
TAI to TT
jauUtcut1(double, double, double)
UTC to UT1
jauSp00(double, double)
the TIO locator s', IERS 2000
jauEra00(double, double)
Earth rotation angle, IAU 2000
jauRefco(double, double, double, double)
refraction constants for given ambient conditions
jauApio(double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, CIRS-observed
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static JSOFA.SphericalCoordinateEO jauAtci13(double rc, double dc, double pr, double pd, double px, double rv, double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS right ascension at J2000.0 (radians, Note 1)dc
- double ICRS declination at J2000.0 (radians, Note 1)pr
- double RA proper motion (radians/year; Note 2)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 3)
Notes:
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
jauApci13(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-CIRS, 2013
jauAtciq(double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick ICRS to CIRS
public static JSOFA.SphericalCoordinate jauAtciq(double rc, double dc, double pr, double pd, double px, double rv, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS RA,Dec at J2000.0 (radians)dc
- double ICRS RA,Dec at J2000.0 (radians)pr
- double RA proper motion (radians/year; Note 3)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)astrom
- star-independent astrometry parameters:
Notes:
jauPmpx(double, double, double, double, double, double, double, double[])
proper motion and parallax
jauLdsun(double[], double[], double)
light deflection by the Sun
jauAb(double[], double[], double, double)
stellar aberration
jauRxp(double[][], double[])
product of r-matrix and pv-vector
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
public static JSOFA.SphericalCoordinate jauAtciqn(double rc, double dc, double pr, double pd, double px, double rv, JSOFA.Astrom astrom, int n, JSOFA.Ldbody[] b)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS RA,Dec at J2000.0 (radians)dc
- double ICRS RA,Dec at J2000.0 (radians)pr
- double RA proper motion (radians/year; Note 3)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)astrom
- star-independent astrometry parameters:n
- int number of bodies (Note 3)b
- jauLDBODY[n] data for each of the n bodies (Notes 3,4):
Notes:
body i b[i].bm b[i].dl Sun 1.0 6e-6 Jupiter 0.00095435 3e-9 Saturn 0.00028574 3e-10
jauPmpx(double, double, double, double, double, double, double, double[])
proper motion and parallax
jauLdn(int, org.jastronomy.jsofa.JSOFA.Ldbody[], double[], double[])
light deflection by n bodies
jauAb(double[], double[], double, double)
stellar aberration
jauRxp(double[][], double[])
product of r-matrix and pv-vector
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
public static JSOFA.SphericalCoordinate jauAtciqz(double rc, double dc, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS astrometric RA,Dec (radians)dc
- double ICRS astrometric RA,Dec (radians)astrom
- star-independent astrometry parameters:
public static JSOFA.ObservedPositionEO jauAtco13(double rc, double dc, double pr, double pd, double px, double rv, double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS right ascension at J2000.0 (radians, Note 1)dc
- double ICRS right ascension at J2000.0 (radians, Note 1)pr
- double RA proper motion (radians/year; Note 2)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 3-4)dut1
- double UT1-UTC (seconds, Note 5)elong
- double longitude (radians, east +ve, Note 6)phi
- double latitude (geodetic, radians, Note 6)hm
- double height above ellipsoid (m, geodetic, Notes 6,8)xp
- double polar motion coordinates (radians, Note 7)yp
- double polar motion coordinates (radians, Note 7)phpa
- double pressure at the observer (hPa = mB, Note 8)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 9)
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 4)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
Without refraction, the complementary functions iauAtco13 and iauAtoc13 are self-consistent to better than 1 microarcsecond all over the celestial sphere. With refraction included, consistency falls off at high zenith distances, but is still better than 0.05 arcsec at 85 degrees.
jauApco13(double, double, double, double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-observed, 2013
jauAtciq(double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick ICRS to CIRS
jauAtioq(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick ICRS to observed
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static JSOFA.SphericalCoordinateEO jauAtic13(double ri, double di, double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ri
- double CIRS geocentric RA,Dec (radians)di
- double CIRS geocentric RA,Dec (radians)date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 1)
Notes:
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience. For most applications of this function the choice will not be at all critical.
TT can be used instead of TDB without any significant impact on accuracy.
jauApci13(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-CIRS, 2013
jauAticq(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick CIRS to ICRS astrometric
public static JSOFA.SphericalCoordinate jauAticq(double ri, double di, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ri
- double CIRS RA,Dec (radians)di
- double CIRS RA,Dec (radians)astrom
- star-independent astrometry parameters:
Notes:
jauS2c(double, double)
spherical coordinates to unit vector
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauZp(double[])
zero p-vector
jauAb(double[], double[], double, double)
stellar aberration
jauLdsun(double[], double[], double)
light deflection by the Sun
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range +/- pi
public static JSOFA.SphericalCoordinate jauAticqn(double ri, double di, JSOFA.Astrom astrom, int n, JSOFA.Ldbody[] b)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ri
- double CIRS RA,Dec (radians)di
- double CIRS RA,Dec (radians)astrom
- star-independent astrometry parameters:n
- number of bodies.b[]
- data for each of the n bodies.
Notes:
body i b[i].bm b[i].dl
Sun 1.0 6e-6 Jupiter 0.00095435 3e-9 Saturn 0.00028574 3e-10
jauS2c(double, double)
spherical coordinates to unit vector
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauZp(double[])
zero p-vector
jauAb(double[], double[], double, double)
stellar aberration
jauLdn(int, org.jastronomy.jsofa.JSOFA.Ldbody[], double[], double[])
light deflection by n bodies
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range +/- pi
public static JSOFA.ObservedPosition jauAtio13(double ri, double di, double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ri
- double CIRS right ascension (CIO-based, radians)di
- double CIRS declination (radians)utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 1,2)dut1
- double UT1-UTC (seconds, Note 3)elong
- double longitude (radians, east +ve, Note 4)phi
- double geodetic latitude (radians, Note 4)hm
- double height above ellipsoid (m, geodetic Notes 4,6)xp
- double polar motion coordinates (radians, Note 5)yp
- double polar motion coordinates (radians, Note 5)phpa
- double pressure at the observer (hPa = mB, Note 6)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 7)
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 2)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
jauApio13(double, double, double, double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, CIRS-observed, 2013
jauAtioq(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick CIRS to observed
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static JSOFA.ObservedPosition jauAtioq(double ri, double di, JSOFA.Astrom astrom)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ri
- double CIRS right ascensiondi
- double CIRS declinationastrom
- star-independent astrometry parameters:
Notes:
Without refraction, the complementary functions iauAtioq and iauAtoiq are self-consistent to better than 1 microarcsecond all over the celestial sphere. With refraction included, consistency falls off at high zenith distances, but is still better than 0.05 arcsec at 85 degrees.
jauS2c(double, double)
spherical coordinates to unit vector
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
public static JSOFA.SphericalCoordinate jauAtoc13(String type, double ob1, double ob2, double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
type
- char[] type of coordinates - "R", "H" or "A" (Notes 1,2)ob1
- double observed Az, HA or RA (radians; Az is N=0,E=90)ob2
- double observed ZD or Dec (radians)utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 3,4)dut1
- double UT1-UTC (seconds, Note 5)elong
- double longitude (radians, east +ve, Note 6)phi
- double geodetic latitude (radians, Note 6)hm
- double height above ellipsoid (m, geodetic Notes 6,8)xp
- double polar motion coordinates (radians, Note 7)yp
- double polar motion coordinates (radians, Note 7)phpa
- double pressure at the observer (hPa = mB, Note 8)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 9)
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 4)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
Without refraction, the complementary functions iauAtco13 and iauAtoc13 are self-consistent to better than 1 microarcsecond all over the celestial sphere. With refraction included, consistency falls off at high zenith distances, but is still better than 0.05 arcsec at 85 degrees.
jauApco13(double, double, double, double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, ICRS-observed
jauAtoiq(java.lang.String, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick observed to CIRS
jauAticq(double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick CIRS to ICRS
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static JSOFA.SphericalCoordinate jauAtoi13(String type, double ob1, double ob2, double utc1, double utc2, double dut1, double elong, double phi, double hm, double xp, double yp, double phpa, double tc, double rh, double wl) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
type
- char[] type of coordinates - "R", "H" or "A" (Notes 1,2)ob1
- double observed Az, HA or RA (radians; Az is N=0,E=90)ob2
- double observed ZD or Dec (radians)utc1
- double UTC as a 2-part...utc2
- double ...quasi Julian Date (Notes 3,4)dut1
- double UT1-UTC (seconds, Note 5)elong
- double longitude (radians, east +ve, Note 6)phi
- double geodetic latitude (radians, Note 6)hm
- double height above the ellipsoid (meters, Notes 6,8)xp
- double polar motion coordinates (radians, Note 7)yp
- double polar motion coordinates (radians, Note 7)phpa
- double pressure at the observer (hPa = mB, Note 8)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers, Note 9)
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- int status: Returned +1 = dubious year (Note 2)
0 = Returned OK
-1 = Returned unacceptable date
Notes:
However, JD cannot unambiguously represent UTC during a leap second unless special measures are taken. The convention in the present function is that the JD day represents UTC days whether the length is 86399, 86400 or 86401 SI seconds.
Applications should use the function iauDtf2d to convert from calendar date and time of day into 2-part quasi Julian Date, as it implements the leap-second-ambiguity convention just described.
hm = -29.3 * tsl * log ( phpa / 1013.25 );
where tsl is the approximate sea-level air temperature in K (See Astrophysical Quantities, C.W.Allen, 3rd edition, section 52). Similarly, if the pressure phpa is not known, it can be estimated from the height of the observing station, hm, as follows:
phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );
Note, however, that the refraction is nearly proportional to the pressure and that an accurate phpa value is important for precise work.
Without refraction, the complementary functions iauAtio13 and iauAtoi13 are self-consistent to better than 1 microarcsecond all over the celestial sphere. With refraction included, consistency falls off at high zenith distances, but is still better than 0.05 arcsec at 85 degrees.
jauApio13(double, double, double, double, double, double, double, double, double, double, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
astrometry parameters, CIRS-observed, 2013
jauAtoiq(java.lang.String, double, double, org.jastronomy.jsofa.JSOFA.Astrom)
quick observed to CIRS
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static JSOFA.SphericalCoordinate jauAtoiq(String type, double ob1, double ob2, JSOFA.Astrom astrom)
Status: support function.
type
- char[] type of coordinates: "R", "H" or "A" (Note 1)ob1
- double observed Az, HA or RA (radians; Az is N=0,E=90)ob2
- double observed ZD or Dec (radians)astrom
- star-independent astrometry parameters:
Notes:
Without refraction, the complementary functions iauAtioq and iauAtoiq are self-consistent to better than 1 microarcsecond all over the celestial sphere. With refraction included, consistency falls off at high zenith distances, but is still better than 0.05 arcsec at 85 degrees.
jauS2c(double, double)
spherical coordinates to unit vector
jauC2s(double[])
p-vector to spherical
jauAnp(double)
normalize angle into range 0 to 2pi
public static double[] jauLd(double bm, double[] p, double[] q, double[] e, double em, double dlim)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
bm
- double mass of the gravitating body (solar masses)p
- double[3] direction from observer to source (unit vector)q
- double[3] direction from body to source (unit vector)e
- double[3] direction from body to observer (unit vector)em
- double distance from body to observer (au)dlim
- double deflection limiter (Note 4)
Notes:
References:
jauPdp(double[], double[])
scalar product of two p-vectors
jauPxp(double[], double[])
vector product of two p-vectors
public static double[] jauLdn(int n, JSOFA.Ldbody[] b, double[] ob, double[] sc)
public static double[] jauLdsun(double[] p, double[] e, double em)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
p
- double[3] direction from observer to star (unit vector)e
- double[3] direction from Sun to observer (unit vector)em
- double distance from Sun to observer (au)
Notes:
jauLd(double, double[], double[], double[], double, double)
light deflection by a solar-system body
public static double[] jauPmpx(double rc, double dc, double pr, double pd, double px, double rv, double pmt, double[] pob)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
rc
- double ICRS RA,Dec at catalog epoch (radians)dc
- double ICRS RA,Dec at catalog epoch (radians)pr
- double RA proper motion (radians/year; Note 1)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)pmt
- double proper motion time interval (SSB, Julian years)pob
- double[3] SSB to observer vector (au)
Notes:
References:
jauPdp(double[], double[])
scalar product of two p-vectors
jauPn(double[])
decompose p-vector into modulus and direction
public static JSOFA.CatalogCoords jauPmsafe(double ra1, double dec1, double pmr1, double pmd1, double px1, double rv1, double ep1a, double ep1b, double ep2a, double ep2b) throws JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ra1
- double right ascension (radians), beforedec1
- double declination (radians), beforepmr1
- double RA proper motion (radians/year), beforepmd1
- double Dec proper motion (radians/year), beforepx1
- double parallax (arcseconds), beforerv1
- double radial velocity (km/s, +ve = receding), beforeep1a
- double "before" epoch, part A (Note 1)ep1b
- double "before" epoch, part B (Note 1)ep2a
- double "after" epoch, part A (Note 1)ep2b
- double "after" epoch, part B (Note 1)
JSOFAInternalError
- int status:
-1 = Returned system error (should not occur)
0 = Returned no warnings or errors
1 = Returned distance overridden (Note 6)
2 = Returned excessive velocity (Note 7)
4 = Returned solution didn't converge (Note 8)
else = Returned binary logical OR of the above warnings
Notes:
epNa epNb 2450123.7 0.0 (JD method) 2451545.0 -1421.3 (J2000 method) 2400000.5 50123.2 (MJD method) 2450123.5 0.2 (date & time method)
The JD method is the most natural and convenient to use in cases where the loss of several decimal digits of resolution is acceptable. The J2000 method is best matched to the way the argument is handled internally and will deliver the optimum resolution. The MJD method and the date & time methods are both good compromises between resolution and convenience.
The proper motions are the rate of change of the right ascension and declination at the catalog epoch and are in radians per TDB Julian year.
The parallax and radial velocity are in the same frame.
jauSeps(double, double, double, double)
angle between two points
jauStarpm(double, double, double, double, double, double, double, double, double, double)
update star catalog data for space motion
JSOFAInternalError
- an internal error has occuredpublic static double[][] jauPvtob(double elong, double phi, double hm, double xp, double yp, double sp, double theta) throws JSOFAIllegalParameter, JSOFAInternalError
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
elong
- double longitude (radians, east +ve, Note 1)phi
- double latitude (geodetic, radians, Note 1)hm
- double height above ref. ellipsoid (geodetic, m)xp
- double coordinates of the pole (radians, Note 2)yp
- double coordinates of the pole (radians, Note 2)sp
- double the TIO locator s' (radians, Note 2)theta
- double Earth rotation angle (radians, Note 3)
Notes:
References:
jauGd2gc(int, double, double, double)
geodetic to geocentric transformation
jauPom00(double, double, double)
polar motion matrix
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
JSOFAInternalError
- an internal error has occuredJSOFAIllegalParameter
- unacceptable date.public static double[][] jauPvtob(double[] xyzm, double xp, double yp, double sp, double theta) throws JSOFAIllegalParameter, JSOFAInternalError
xyzm
- observatory geocentric position in metres.xp
- double coordinates of the pole (radians, Note 2)yp
- double coordinates of the pole (radians, Note 2)sp
- double the TIO locator s' (radians, Note 2)theta
- double Earth rotation angle (radians, Note 3)JSOFAIllegalParameter
- unacceptable date.JSOFAInternalError
- an internal error has occuredfor more detail.
public static JSOFA.RefCos jauRefco(double phpa, double tc, double rh, double wl)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
phpa
- double pressure at the observer (hPa = millibar)tc
- double ambient temperature at the observer (deg C)rh
- double relative humidity at the observer (range 0-1)wl
- double wavelength (micrometers)
Notes:
The model was tested using the following range of conditions:
lapse rates 0.0055, 0.0065, 0.0075 deg/meter latitudes 0, 25, 50, 75 degrees heights 0, 2500, 5000 meters ASL pressures mean for height -10% to +5% in steps of 5% temperatures -10 deg to +20 deg with respect to 280 deg at SL relative humidity 0, 0.5, 1 wavelengths 0.4, 0.6, ... 2 micron, + radio zenith distances 15, 45, 75 degrees
The accuracy with respect to raytracing through a model atmosphere was as follows:
worst RMS
optical/IR 62 mas 8 mas radio 319 mas 49 mas
For this particular set of conditions:
lapse rate 0.0065 K/meter latitude 50 degrees sea level pressure 1005 mb temperature 280.15 K humidity 80% wavelength 5740 Angstroms
the results were as follows:
ZD raytrace iauRefco Saastamoinen 10 10.27 10.27 10.27 20 21.19 21.20 21.19 30 33.61 33.61 33.60 40 48.82 48.83 48.81 45 58.16 58.18 58.16 50 69.28 69.30 69.27 55 82.97 82.99 82.95 60 100.51 100.54 100.50 65 124.23 124.26 124.20 70 158.63 158.68 158.61 72 177.32 177.37 177.31 74 200.35 200.38 200.32 76 229.45 229.43 229.42 78 267.44 267.29 267.41 80 319.13 318.55 319.10
deg arcsec arcsec arcsec
The values for Saastamoinen's formula (which includes terms up to tan^5) are taken from Hohenkerk and Sinclair (1985).
a) The formula for the saturation vapour pressure of water as a function of temperature and temperature is taken from Equations (A4.5-A4.7) of Gill (1982).
b) The formula for the water vapour pressure, given the saturation pressure and the relative humidity, is from Crane (1976), Equation (2.5.5).
c) The refractivity of air is a function of temperature, total pressure, water-vapour pressure and, in the case of optical/IR, wavelength. The formulae for the two cases are developed from Hohenkerk & Sinclair (1985) and Rueger (2002). The IAG (1999) optical refractivity for dry air is used.
d) The formula for beta, the ratio of the scale height of the atmosphere to the geocentric distance of the observer, is an adaption of Equation (9) from Stone (1996). The adaptations, arrived at empirically, consist of (i) a small adjustment to the coefficient and (ii) a humidity term for the radio case only.
e) The formulae for the refraction constants as a function of n-1 and beta are from Green (1987), Equation (4.31).
References:
public static JSOFA.SphericalCoordinate jauG2icrs(double dl, double db)
Status: support routine.
dl
- double galactic longitude (radians)db
- double galactic latitude (radians)Notes:
public static JSOFA.SphericalCoordinate jauIcrs2g(double dr, double dd)
Status: support routine.
dr
- double ICRS right ascension (radians)dd
- double ICRS declination (radians)Notes:
public static JSOFA.SphericalCoordinate jauEceq06(double date1, double date2, double dl, double db)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian date (Note 1)date2
- double TT as a 2-part Julian date (Note 1)dl
- double ecliptic longitude and latitude (radians)db
- double ecliptic longitude and latitude (radians)
jauS2c(double, double)
spherical coordinates to unit vector
jauEcm06(double, double)
J2000.0 to ecliptic rotation matrix, IAU 2006
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauC2s(double[])
unit vector to spherical coordinates
jauAnp(double)
normalize angle into range 0 to 2pi
jauAnpm(double)
normalize angle into range +/- pi
public static double[][] jauEcm06(double date1, double date2)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian date (Note 1)date2
- double TT as a 2-part Julian date (Note 1)
Notes:
jauObl06(double, double)
mean obliquity, IAU 2006
jauPmat06(double, double)
PB matrix, IAU 2006
jauIr(double[][])
initialize r-matrix to identity
jauRx(double, double[][])
rotate around X-axis
jauRxr(double[][], double[][])
product of two r-matrices
public static JSOFA.SphericalCoordinate jauEqec06(double date1, double date2, double dr, double dd)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
date1
- double TT as a 2-part Julian date (Note 1)date2
- double TT as a 2-part Julian date (Note 1)dr
- double ICRS right ascension and declination (radians)dd
- double ICRS right ascension and declination (radians)
jauS2c(double, double)
spherical coordinates to unit vector
jauEcm06(double, double)
J2000.0 to ecliptic rotation matrix, IAU 2006
jauRxp(double[][], double[])
product of r-matrix and p-vector
jauC2s(double[])
unit vector to spherical coordinates
jauAnp(double)
normalize angle into range 0 to 2pi
jauAnpm(double)
normalize angle into range +/- pi
public static JSOFA.SphericalCoordinate jauLteceq(double epj, double dl, double db)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)dl
- double ecliptic longitude and latitude (radians)db
- double ecliptic longitude and latitude (radians)
jauS2c(double, double)
spherical coordinates to unit vector
jauLtecm(double)
J2000.0 to ecliptic rotation matrix, long term
jauTrxp(double[][], double[])
product of transpose of r-matrix and p-vector
jauC2s(double[])
unit vector to spherical coordinates
jauAnp(double)
normalize angle into range 0 to 2pi
jauAnpm(double)
normalize angle into range +/- pi
public static double[][] jauLtecm(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)
Notes:
jauLtpequ(double)
equator pole, long term
jauLtpecl(double)
ecliptic pole, long term
jauPxp(double[], double[])
vector product
jauPn(double[])
normalize vector
public static JSOFA.SphericalCoordinate jauLteqec(double epj, double dr, double dd)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)dr
- double ICRS right ascension and declination (radians)dd
- double ICRS right ascension and declination (radians)
jauS2c(double, double)
spherical coordinates to unit vector
jauLtecm(double)
J2000.0 to ecliptic rotation matrix, long term
jauRxp(double[][], double[])
product of r-matrix and p-vector
jauC2s(double[])
unit vector to spherical coordinates
jauAnp(double)
normalize angle into range 0 to 2pi
jauAnpm(double)
normalize angle into range +/- pi
public static double[][] jauLtp(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)
Notes:
jauLtpequ(double)
equator pole, long term
jauLtpecl(double)
ecliptic pole, long term
jauPxp(double[], double[])
vector product
jauPn(double[])
normalize vector
Vondrak, J., Capitaine, N. and Wallace, P., 2011, New precession expressions, valid for long time intervals, Astron.Astrophys. 534, A22
Vondrak, J., Capitaine, N. and Wallace, P., 2012, New precession expressions, valid for long time intervals (Corrigendum), Astron.Astrophys. 541, C1
public static double[][] jauLtpb(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)
Notes:
public static double[] jauLtpecl(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)
Notes:
public static double[] jauLtpequ(double epj)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
epj
- double Julian epoch (TT)
Notes:
public static JSOFA.EquatorialCoordinate jauAe2hd(double az, double el, double phi)
az
- double azimuthel
- double altitude (informally, elevation)phi
- double site latitude
Notes:
public static JSOFA.HorizonCoordinate jauHd2ae(double ha, double dec, double phi)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ha
- double hour angle (local)dec
- double declinationphi
- double site latitude
Notes:
public static double jauHd2pa(double ha, double dec, double phi)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
ha
- double hour angledec
- double declinationphi
- double site latitudeNotes:
public static JSOFA.TangentPointSolution jauTpors(double xi, double eta, double a, double b)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
xi
- double rectangular coordinates of star image (Note 2)eta
- double rectangular coordinates of star image (Note 2)a
- double star's spherical coordinates (Note 3)b
- double star's spherical coordinates (Note 3)
Notes:
spherical vector solve for
iauTpxes iauTpxev xi,eta
iauTpsts iauTpstv star
> iauTpors < iauTporv origin
public static JSOFA.TangentPointDirectionCosines jauTporv(double xi, double eta, double[] v)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
xi
- double rectangular coordinates of star image (Note 2)eta
- double rectangular coordinates of star image (Note 2)v
- double[3] star's direction cosines (Note 3)
Notes:
spherical vector solve for
iauTpxes iauTpxev xi,eta
iauTpsts iauTpstv star
iauTpors > iauTporv < origin
public static JSOFA.SphericalCoordinate jauTpsts(double xi, double eta, double a0, double b0)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
xi
- double rectangular coordinates of star image (Note 2)eta
- double rectangular coordinates of star image (Note 2)a0
- double tangent point's spherical coordinatesb0
- double tangent point's spherical coordinates
spherical vector solve for
iauTpxes iauTpxev xi,eta
> iauTpsts < iauTpstv star
iauTpors iauTporv origin
public static double[] jauTpstv(double xi, double eta, double[] v0)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
xi
- double rectangular coordinates of star image (Note 2)eta
- double rectangular coordinates of star image (Note 2)v0
- double[3] tangent point's direction cosines
spherical vector solve for
iauTpxes iauTpxev xi,eta
iauTpsts > iauTpstv < star
iauTpors iauTporv origin
public static JSOFA.TangentPlaneCoordinate jauTpxes(double a, double b, double a0, double b0)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
a
- double star's spherical coordinatesb
- double star's spherical coordinatesa0
- double tangent point's spherical coordinatesb0
- double tangent point's spherical coordinates
Notes:
spherical vector solve for
> iauTpxes < iauTpxev xi,eta
iauTpsts iauTpstv star
iauTpors iauTporv origin
public static JSOFA.TangentPlaneCoordinate jauTpxev(double[] v, double[] v0)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection.
Status: support function.
v
- double[3] direction cosines of star (Note 4)v0
- double[3] direction cosines of tangent point (Note 4)
Notes:
spherical vector solve for
iauTpxes > iauTpxev < xi,eta
iauTpsts iauTpstv star
iauTpors iauTporv origin
public static JSOFA.CatalogCoords jauFk425(double r1950, double d1950, double dr1950, double dd1950, double p1950, double v1950)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection. Status: support function. (all B1950.0, FK4)
r1950
- double B1950.0 RA (rad)d1950
- double B1950.0 Dec (rad)dr1950
- double B1950.0 proper motions (rad/trop.yr)dd1950
- double B1950.0 proper motions (rad/trop.yr)p1950
- double parallax (arcsec)v1950
- double radial velocity (km/s, +ve = moving away)
Returned:Notes:
References:
public static JSOFA.SphericalCoordinate jauFk45z(double r1950, double d1950, double bepoch)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection. Status: support function. This function converts a star's catalog data from the old FK4 (Bessel-Newcomb) system to the later IAU 1976 FK5 (Fricke) system, in such a way that the FK5 proper motion is zero. Because such a star has, in general, a non-zero proper motion in the FK4 system, the routine requires the epoch at which the position in the FK4 system was determined.
r1950
- double B1950.0 FK4 RA at epoch (rad)d1950
- double B1950.0 FK4 Dec at epoch (rad)bepoch
- double Besselian epoch (e.g. 1979.3)
Notes:
References:
public static JSOFA.CatalogCoords jauFk524(double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection. Status: support function.
r2000
- double J2000.0 RA (rad)d2000
- double J2000.0 Dec (rad)dr2000
- double J2000.0 proper motions (rad/Jul.yr)dd2000
- double J2000.0 proper motions (rad/Jul.yr)p2000
- double parallax (arcsec)v2000
- double radial velocity (km/s, +ve = moving away)Notes:
References:
public static JSOFA.CatalogCoords jauFk54z(double r2000, double d2000, double bepoch)
This function is derived from the International Astronomical Union's SOFA (Standards of Fundamental Astronomy) software collection. Status: support function.
r2000
- double J2000.0 FK5 RA (rad)d2000
- double J2000.0 FK5 Dec (rad)bepoch
- double Besselian epoch (e.g. 1950.0)Notes:
public static double[][] jauMoon98(double date1, double date2)
Status: support function.
n.b. Not IAU-endorsed and without canonical status.
date1
- double TT date part A (Notes 1,4)date2
- double TT date part B (Notes 1,4)
Notes:
References:
public static JSOFA.SphericalCoordinate jauAtcc13(double rc, double dc, double pr, double pd, double px, double rv, double date1, double date2)
rc
- double ICRS right ascension at J2000.0 (radians, Note 1)dc
- double ICRS declination at J2000.0 (radians, Note 1)pr
- double RA proper motion (radians/year, Note 2)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)date1
- double TDB as a 2-part...date2
- double ...Julian Date (Note 3)
Notes:
public static JSOFA.SphericalCoordinate jauAtccq(double rc, double dc, double pr, double pd, double px, double rv, JSOFA.Astrom astrom)
rc
- double ICRS RA at J2000.0 (radians)dc
- double ICRS Dec at J2000.0 (radians)pr
- double RA proper motion (radians/year, Note 3)pd
- double Dec proper motion (radians/year)px
- double parallax (arcsec)rv
- double radial velocity (km/s, +ve if receding)astrom
- Astrom star-independent astrometry parameters:
Notes:
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