Orientation of the hipparcos frame with respect to the reference frames of the DE403/LE403 and DE405/LE405 ephemerides based on asteroid observations

Chernetenko, Yu. A.

doi:10.1134/s1063773708040063

Cited by 7 publications

(8 citation statements)

References 6 publications

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“…For example, the KZS programme (Kislyuk et al 1997) obtained the estimate ω z =−1.07 ± 0.80 mas yr −1 while the Pulkovo programme (Bobylev, Bronnikova & Shakht 2004) provided ω z =−1.66 ± 0.42 mas yr −1 . The parameters of rotation obtained in this work do not contradict the above‐mentioned results of analysis of the long‐term observations of asteroids (Chernetenko 2008). We regard the discovered rotation to be real and connected with the residual rotation of the HCRF with respect to extragalactic sources, including the ICRF sources.…”

Section: Discussionsupporting

confidence: 79%

“…As a whole, it does not contradict the results of Boboltz et al (2007) as well, where an analysis of positions and proper motions of 46 radio stars has been carried out. Also, the estimate of the angular velocity of the Hipparcos system with respect to the coordinate systems defined by the DE403 and DE405 ephemeris should be noted, which was obtained by Chernetenko (2008) from the analysis of observations of asteroids – ∣ω∣ = 0.94 ± 0.20 mas yr −1 , while the components of this vector are ω x =+0.12 ± 0.08 mas yr −1 , ω y =+0.66 ± 0.09 mas yr −1 , ω z =−0.56 ± 0.16 mas yr −1 . This result makes us conclude that either the dynamic theories DE403 and DE405 need to be improved, or the Hipparcos system requires correction.…”

Section: Determining Residual Rotation Of the Hipparcos/tycho‐2 Systemmentioning

confidence: 99%

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Residual rotation of the Hipparcos/Tycho-2 system as determined from the data of the XPM catalogue

Fedorov¹,

Akhmetov²,

Бобылев

2011

Monthly Notices of the Royal Astronomical Society

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From a comparison of absolute proper motions of stars from the XPM catalogue with those of the same stars from the PPMXL, UCAC3, Tycho‐2 and XC1 catalogues, the equatorial components of the rotation vector of these coordinate systems are determined with respect to the coordinate system specified by positions and proper motions of XPM. These parameters are calculated with the use of about 90 million stars from the UCAC3 catalogue and about 300 million stars from the PPMXL catalogue. It is shown that the Hipparcos Celestial Reference Frame represented by the Tycho‐2, PPMXL, UCAC3 and XC1 catalogues has a significant rotation component ωz= (−1.8 ± 0.16) mas yr−1 about the equatorial axis directed to the celestial pole. The result is confirmed by an analysis of the formal proper motions of the extragalactic sources contained in the considered catalogues.

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Section: Discussionsupporting

confidence: 79%

Section: Determining Residual Rotation Of the Hipparcos/tycho‐2 Systemmentioning

confidence: 99%

Residual rotation of the Hipparcos/Tycho-2 system as determined from the data of the XPM catalogue

Fedorov¹,

Akhmetov²,

Бобылев

2011

Monthly Notices of the Royal Astronomical Society

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“…Boboltz et al (2007) reached the right conclusion that there are no significant rotations within the error limits. Note also the estimate of the angular velocity of rotation of the HIPPARCOS system relative the DE403 and DE405 systems of ephemerides obtained by Chernetenko (2008) by analyzing the observations of asteroids: |ω| = 0.940.20 mas yr −1 , where the components of the vector found are ω x = 0.12 ± 0.08 mas yr −1 , ω y = 0.66 ± 0.09 mas yr −1 , and ω z = −0.56 ± 0.16 mas yr −1 . This result suggests that either the dynamical DE403 and DE405 models need to be improved or the HIPPARCOS system needs to be corrected.…”

Section: Introductionmentioning

confidence: 99%

Determining the orientation parameters of the ICRS/UCAC2 system using the Kharkov catalog of absolute stellar proper motions

et al. 2010

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The absolute proper motions of about 275 million stars from the Kharkov XPM catalog have been obtained by comparing their positions in the 2MASS and USNO-A2.0 catalogs with an epoch difference of about 45 yr for northern-hemisphere stars and about 17 yr for southern-hemisphere stars. The zero point of the system of absolute proper motions has been determined using 1.45 million galaxies. The equatorial components of the residual rotation vector of the ICRS/UCAC2 coordinate system relative to the system of extragalactic sources have been determined by comparing the XPM and UCAC2 stellar proper motions: ω x,y,z = (−0.06, 0.17, −0.84) ±(0.15, 0.14, 0.14) mas yr −1 . These parameters have been calculated using about 1 million faintest UCAC2 stars with magnitudes R U CAC2 > 16 m and J > 14 m .7,for which the color and magnitude equation effects are negligible.

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“…Putting this expression in the equations of motion (22), one has a system of four unknowns (r, ρ, dρ/dt, d 2 ρ/dt 2 ), the quantities for the Earth being given by the ephemerides 22 . One again will write the additional Eq.…”

Section: The Methods Of Laplace -Brieflymentioning

confidence: 99%

“…-High accuracy astrometry of asteroids enabled to improve their ephemerides [50], and also to detect small systematic effects due to the photocentre offset [44]. -High accuracy astrometry of asteroids enables to link the dynamical inertial frame to the catalogue [101,5,22]. -The stellar astrometric catalogue, mostly Tycho2, has an indirect consequence on science for the Solar System.…”

Section: Before Gaia -The Hipparcos Legacymentioning

confidence: 99%

The Gaia Mission and the Asteroids

Hestroffer

Dell’Oro

Cellino

et al. 2009

Lecture Notes in Physics

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Summary. The Gaia space mission to be operated in early 2012 by the European Space Agency (ESA), will make a huge step in our knowledge of the Sun's neighborhood, up to the Magellanic clouds. Somewhat closer, Gaia will also provide major improvements in the science of asteroids, and more generally to our Solar System, either directly or indirectly. Gaia is a scanning survey telescope aimed to perform high accuracy astrometry and photometry. More specifically it will provide physical and dynamical characterization of asteroids, a better knowledge of the solar system composition, formation and evolution, local test of the general relativity, and linking the dynamical reference frame to the kinematical ICRS. We develop here the general aspects of asteroid observations and the scientific harvest in perspective of what was achieved in the pre-Gaia era. In this lecture we focus on the determination of size of asteroids, shape and rotation, taxonomy, orbits and their improvements with historical highlight, and also the dynamical model in general.

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Orientation of the hipparcos frame with respect to the reference frames of the DE403/LE403 and DE405/LE405 ephemerides based on asteroid observations

Cited by 7 publications

References 6 publications

Residual rotation of the Hipparcos/Tycho-2 system as determined from the data of the XPM catalogue

Residual rotation of the Hipparcos/Tycho-2 system as determined from the data of the XPM catalogue

Determining the orientation parameters of the ICRS/UCAC2 system using the Kharkov catalog of absolute stellar proper motions

The Gaia Mission and the Asteroids

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