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SOFACelestialToObserved Method
ICRS RA,Dec to observed place using the SOFA Atco13 function.

Namespace: ASCOM.Astrometry.SOFA
Assembly: ASCOM.Astrometry (in ASCOM.Astrometry.dll) Version: 6.0.0.0 (6.2.0.2774)
Syntax
public int CelestialToObserved(
	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,
	ref double aob,
	ref double zob,
	ref double hob,
	ref double dob,
	ref double rob,
	ref double eo
)

Parameters

rc
Type: SystemDouble
ICRS RA (radians, note 1)
dc
Type: SystemDouble
ICRS Dec (radians, note 2)
pr
Type: SystemDouble
RA Proper motion (radians/year)
pd
Type: SystemDouble
Dec Proper motion (radians/year
px
Type: SystemDouble
Parallax (arcsec)
rv
Type: SystemDouble
Radial veolcity (Km/s, +ve if receding
utc1
Type: SystemDouble
UTC Julian date (part 1, notes 3,4)
utc2
Type: SystemDouble
UTC Julian date (part 2, notes 3,4)
dut1
Type: SystemDouble
UT1 - UTC (seonds, note 5)
elong
Type: SystemDouble
Site longitude (radians, note 6)
phi
Type: SystemDouble
Site Latitude (radians, note 6)
hm
Type: SystemDouble
Site Height (meters, notes 6,8)
xp
Type: SystemDouble
Polar motion co-ordinate (radians, note 7)
yp
Type: SystemDouble
Polar motion co-ordinate (radians,note 7)
phpa
Type: SystemDouble
Site Presure (hPa = mB, note 8)
tc
Type: SystemDouble
Site Temperature (C)
rh
Type: SystemDouble
Site relative humidity (fraction in the range: 0.0 to 1.0)
wl
Type: SystemDouble
Observation wavem=length (micrometres, note 9)
aob
Type: SystemDouble
Observed Azimuth (radians)
zob
Type: SystemDouble
Observed Zenith distance (radians)
hob
Type: SystemDouble
Observed Hour Angle (radians)
dob
Type: SystemDouble
Observed Declination (radians)
rob
Type: SystemDouble
Observed RA (radians)
eo
Type: SystemDouble
Equation of the origins (ERA-GST)

Return Value

Type: Int32
+1 = dubious year (Note 4), 0 = OK, -1 = unacceptable date
Remarks
Notes:
  1. Star data for an epoch other than J2000.0 (for example from the Hipparcos catalog, which has an epoch of J1991.25) will require a preliminary call to iauPmsafe before use.
  2. The proper motion in RA is dRA/dt rather than cos(Dec)*dRA/dt.
  3. utc1+utc2 is quasi Julian Date (see Note 2), apportioned in any convenient way between the two arguments, for example where utc1 is the Julian Day Number and utc2 is the fraction of a day.

    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.

  4. The warning status "dubious year" flags UTCs that predate the introduction of the time scale or that are too far in the future to be trusted. See iauDat for further details.
  5. UT1-UTC is tabulated in IERS bulletins. It increases by exactly one second at the end of each positive UTC leap second, introduced in order to keep UT1-UTC within +/- 0.9s. n.b. This practice is under review, and in the future UT1-UTC may grow essentially without limit.
  6. The geographical coordinates are with respect to the WGS84 reference ellipsoid. TAKE CARE WITH THE LONGITUDE SIGN: the longitude required by the present function is east-positive (i.e. right-handed), in accordance with geographical convention.
  7. The polar motion xp,yp can be obtained from IERS bulletins. The values are the coordinates (in radians) of the Celestial Intermediate Pole with respect to the International Terrestrial Reference System (see IERS Conventions 2003), measured along the meridians 0 and 90 deg west respectively. For many applications, xp and yp can be set to zero.
  8. If hm, the height above the ellipsoid of the observing station in meters, is not known but phpa, the pressure in hPa (=mB), is available, an adequate estimate of hm can be obtained from the expression:

    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.

  9. The argument wl specifies the observing wavelength in micrometers. The transition from optical to radio is assumed to occur at 100 micrometers (about 3000 GHz).
  10. The accuracy of the result is limited by the corrections for refraction, which use a simple A*tan(z) + B*tan^3(z) model. Providing the meteorological parameters are known accurately and there are no gross local effects, the predicted observed coordinates should be within 0.05 arcsec (optical) or 1 arcsec (radio) for a zenith distance of less than 70 degrees, better than 30 arcsec (optical or radio) at 85 degrees and better than 20 arcmin (optical) or 30 arcmin (radio) at the horizon.

    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.

  11. "Observed" Az,ZD means the position that would be seen by a perfect geodetically aligned theodolite. (Zenith distance is used rather than altitude in order to reflect the fact that no allowance is made for depression of the horizon.) This is related to the observed HA,Dec via the standard rotation, using the geodetic latitude (corrected for polar motion), while the observed HA and RA are related simply through the Earth rotation angle and the site longitude. "Observed" RA,Dec or HA,Dec thus means the position that would be seen by a perfect equatorial with its polar axis aligned to the Earth's axis of rotation.
  12. It is advisable to take great care with units, as even unlikely values of the input parameters are accepted and processed in accordance with the models used.
See Also