scholarly journals Improving the dynamical reference frame through minor planet orbit correction using crossing point observations

1988 ◽  
Vol 128 ◽  
pp. 55-60
Author(s):  
Arthur L. Whipple ◽  
Raynor L. Duncombe ◽  
Paul D. Hemenway
Keyword(s):  
Computer Program ◽  
Reference Frame ◽  
Reference System ◽  
Hubble Space Telescope ◽  
Simulated Data ◽  
Minor Planet ◽  
Minor Planets ◽  
Space Telescope ◽  
Orbit Correction ◽  
Crossing Point

We have begun a program to establish a dynamical reference frame based on the motions of minor planets. The program will utilize observations from the Hubble Space Telescope, and will ultimately tie the HIPPARCOS reference system to a dynamical base. Thirty-four minor planets, 20 of which are suitable for observation with the Hubble Space Telescope, have been selected. Ground based observations, particularly crossing-point observations with long focus reflectors, have been initiated.A computer program to simultaneously solve for the corrections of the orbits of the 34 minor planets including the crossing-point observations, was successfully run. The observations are treated by the method of W. H. Jeffreys. Using simulated data, solutions with and without crossing point observations demonstrate the value of those observations to produce a homogeneous and coherent set of results.

scholarly journals The Reference Frame Determined From the Observation of Minor Planets by Hipparcos

1990 ◽  
Vol 141 ◽  
pp. 329-336
Author(s):  
B. Morando ◽  
A. Bec-Borsenberger
Keyword(s):  
Reference Frame ◽  
High Precision ◽  
Reference System ◽  
Initial Position ◽  
Minor Planet ◽  
Minor Planets ◽  
The Moon ◽  
Phase Effect ◽  
The Earth ◽  
A Minor

The observation of minor planets by Hipparcos offers the opportunity to obtain high precision positions for some minor planets. About fifty minor planets are on the programme. Their ephemerides had to be improved in order to reach a precision of 1 arsec and occultations by the Earth and the Moon had to be predicted.From the position of a minor planet on reference great circles at different times better values of the initial position and velocity will be deduced but the reduction of the observations of the minor planets have to take into account the displacement of the photocentre relative to the centre which is due to the shape, the phase effect and the scattering properties of the surface. For some very small planets considered as star like this diplacement will be small and the precise positions obtained will allow to position the dynamical reference system relative to the Hipparcos system. For the bigger minor planets the observations by Hipparcos may give informations on the shape and scattering properties of the surface.

scholarly journals A Note on the Astrometric Precision of Minor Planet Observations

1991 ◽  
Vol 127 ◽  
pp. 327-330
Author(s):  
D. Pascu
Keyword(s):  
Reference Frame ◽  
Lower Limit ◽  
Satellite Observations ◽  
Minor Planet ◽  
Minor Planets ◽  
Crossing Point

AbstractFor years, interest in precise positions of minor planets has centered on tying the dynamical reference frame with the stellar frame and determining catalog zone errors. Photographic methods are generally used in obtaining observed spherical equatorial coordinates (R.A., Dec.) or crossing-point observations. Estimates of the external precision of the equatorial coordinates are overly pessimistic, while those for crossing-point observations, too optimistic.It is estimated that equatorial positions for the brighter (m < 11) minor planets can be determined with an external precision not worse than +/−0.2 arcsec (m.e.), and perhaps as low as +/−0.1 arcsec (m.e.), depending on the reference catalog zonal errors.Intersatellite observations are a type of crossing-point observation in which the images of two different objects appear in the same exposure. This is the most precise type of crossing-point observation and gives an estimate for the lower limit to the external precision of this observation type. Recent studies of satellite observations indicate that this lower limit is in the +/−0.05 to +/−0.08 arcsec (m.e.) range.

scholarly journals Using the Hubble Space Telescope to Relate the HIPPARCOS and Extragalactic Reference Frames

1988 ◽  
Vol 129 ◽  
pp. 335-336
Author(s):  
P. D. Hemenway ◽  
R. L. Duncombe
Keyword(s):  
Reference Frame ◽  
Solid Body ◽  
Reference System ◽  
Reference Frames ◽  
Hubble Space Telescope ◽  
Inertial Reference Frame ◽  
Body Rotation ◽  
Space Telescope ◽  
Solid Body Rotation ◽  
Instrumental System

The HIPPARCOS satellite will produce positions, motions and parallaxes of celestial objects with previously unattained accuracy. This HIPPARCOS Instrumental System, however, will have an unknown solid body rotation with respect to an inertial reference frame. One aspect of our program of astrometric observations with the Hubble Space Telescope is to determine the rotation of the HIPPARCOS reference frame with respect to an extragalactic reference system.

The Program to Link the HIPPARCOS Reference Frame to an Extragalactic Reference System Using the Fine Guidance Sensors of the Hubble Space Telescope

1997 ◽  
Vol 114 ◽  
pp. 2796 ◽  
Author(s):  
P. D. Hemenway ◽  
R. L. Duncombe ◽  
E. P. Bozyan ◽  
A. M. Lalich ◽  
A. N. Argue ◽  
...  
Keyword(s):  
Reference Frame ◽  
Reference System ◽  
Hubble Space Telescope ◽  
Space Telescope

Initial refinement of minor planet orbits for pointing and observation with the Hubble Space Telescope

1991 ◽  
Vol 102 ◽  
pp. 816
Author(s):  
Arthur L. Whipple ◽  
Paul D. Hemenway ◽  
Doug Ingram
Keyword(s):  
Hubble Space Telescope ◽  
Minor Planet ◽  
Space Telescope

A Catalogue of QSOs and Link Stars for the HST link of the Hipparcos Reference Frame

1990 ◽  
Vol 8 (04) ◽  
pp. 368-371 ◽  
Author(s):  
Graeme L. White ◽  
David L. Jauncey ◽  
John E. Reynolds ◽  
David Malin ◽  
A. N. Argue ◽  
...  
Keyword(s):  
Data Base ◽  
Reference Frame ◽  
Hubble Space Telescope ◽  
Space Telescope

AbstractWe present a list of bright (&lt; 17 mag) southern QSOs and bright (&lt; 11 mag) stars that may be suitable for theHubble Space Telescopelink between theHipparcosastrometric reference frame and the VLBI extragalactic frame. The QSOs have been selected from various lists of radio objects and identifications. The stars have been selected from the Strasbourg (CDS) data base and from the Preliminary Second Cape Photographic Catalogue, and supplemented with stars measured from the SERC IIIa-J Schmidt survey. The list of QSOs and stars have been included in theHipparcosandHSTschedule of observations.

scholarly journals Hipparcos – Link with Extragalactic Reference Frames

1986 ◽  
Vol 7 ◽  
pp. 719-722
Author(s):  
A.N. Argue
Keyword(s):  
Time Scales ◽  
Data Reduction ◽  
Reference System ◽  
Reference Frames ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Hipparcos Catalogue ◽  
Radio Stars

AbstractThe link of the Hipparcos Catalogue to an extragalactic reference system will be carried out on two time-scales: the first, coinciding with the duration of the mission, to provide data for immediate use by the data reduction consortia, and the second over a longer term to provide for subsequent reappraisal of the final Hipparcos catalogue. The first will be based on radio stars and on an indirect link to extragalactic objects by means of observations with the Hubble Space Telescope; for the second we hope for longer term programmes with the Hubble Space Telescope, together with a variety of ground-based links.

scholarly journals Prospects for space Telescope in the search for other Planetary Systems

1985 ◽  
Vol 112 ◽  
pp. 75-84
Author(s):  
J. L. Russell
Keyword(s):  
High Speed ◽  
Hubble Space Telescope ◽  
Planetary Systems ◽  
Wide Field ◽  
Minor Planets ◽  
Scientific Instruments ◽  
The Moon ◽  
Space Telescope ◽  
Faint Object

The Hubble Space Telescope (ST) will be launched with five dedicated scientific instruments and a capability to do astrometric measurements with the fine guidance sensors. Four of these – the Faint Object Camera, the Wide Field Camera, the Fine Guidance Sensors and the High Speed Photometer – can be used in the search for extrasolar planetary systems. The Faint Object Camera will be able to directly detect planets around a few of the nearby bright stars. The Wide Field Camera and the Fine Guidance Sensors can be used astrometrically, both with an accuracy of about 2 mas per observation. The High Speed Photometer possibly can detect planets during occultation of stars by the moon and minor planets. The ST is expected to be launched in mid-1986 and these observations are the among the first planned with the instruments.

scholarly journals Extending Gaia  DR2 with HST  narrow-field astrometry – II. Refining the method on WISE J163940.83−684738.6★

2020 ◽  
Vol 494 (2) ◽  
pp. 2068-2075
Author(s):  
L R Bedin ◽  
C Fontanive
Keyword(s):  
High Precision ◽  
Reference System ◽  
Hubble Space Telescope ◽  
High Accuracy ◽  
Test Case ◽  
Wide Field ◽  
Brown Dwarf ◽  
Space Telescope ◽  
Infra Red ◽  
Gaia Dr2

ABSTRACT In the second paper of this series, we perfected our method of linking high-precision Hubble Space Telescope astrometry to the high-accuracy Gaia DR2 absolute reference system to overcome the limitations of relative astrometry with narrow-field cameras. Our test case here is the Y brown dwarf WISE  J163940.83−684738.6, observed at different epochs spread over a 6-yr time baseline with the Infra-Red channel of the Wide Field Camera 3. We derived significantly improved astrometric parameters compared to previous determinations, finding (μαcos δ, μδ, ϖ) = (577.21 ± 0.24 mas yr−1, −3108.39 ± 0.27 mas yr−1, 210.4 ± 1.8 mas). In particular, our derived absolute parallax (ϖ ) corresponds to a distance of 4.75 ± 0.05 pc for the faint ultracool dwarf.

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