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

Бобылев, В. В.; Fedorov, P. N.; Bajkova, A. T.; Akhmetov, V. S.

doi:10.1134/s1063773710070066

Cited by 3 publications

(3 citation statements)

References 11 publications

(15 reference statements)

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“…The component ω 2 (and Ω z in the equatorial system) has the most significant value among the components of the rigid body rotation vector of the UCAC3 galaxies system. This does not contradict the results of the various investigations of the inertiality of the HCRF (Bobylev et al 2010). The value of ω 2 =−1.09 ± 0.02 mas yr −1 obtained as average from stars is in a good agreement with the corresponding component derived from the present analysis of the UCAC3 galactic ‘proper motions’.…”

Section: Resultssupporting

confidence: 82%

Rotational effects in the system of proper motions of the UCAC3 catalogue

Бобылев¹,

Khovritchev

2011

Monthly Notices of the Royal Astronomical Society

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A set of ≈8 million single stars of the UCAC3 catalogue has been analysed. It contains stars with reliable proper motions with not less than three epochs of observations used to compute the proper motion. Our main goal is to investigate the inertiality of the reference system defined by ‘good’ stars of the UCAC3 catalogue. The formalism of vectorial spherical harmonics has been applied to analyse the system of proper motions of the selected UCAC3 stars. A comparison between the results of solutions for several subsets of UCAC3 stars shows that the key parameters significantly change with stellar magnitudes, colours and average distances. The values of the components of the rigid‐body rotation vector of the Hipparcos Celestial Reference Frame (HCRF) with respect to extragalactic sources were determined using ‘proper motions’ of more than 8000 galaxies of the UCAC3 catalogue. The values are ω1= 0.58 ± 0.15, ω2=−1.02 ± 0.15, ω3=−0.59 ± 0.17 mas yr−1 in galactic coordinates. Traces of the considerable magnitude equation are seen in the ‘proper motions’ of the UCAC3 galaxies. The most significant component derived from the analysis of the UCAC3 galaxies is ω2. It does not contradict the results of the analysis of the proper motions of selected stars (ω2=−1.09 ± 0.02 mas yr−1).

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Section: Resultssupporting

confidence: 82%

Rotational effects in the system of proper motions of the UCAC3 catalogue

Бобылев¹,

Khovritchev

2011

Monthly Notices of the Royal Astronomical Society

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“…This result makes us conclude that either the dynamic theories DE403 and DE405 need to be improved, or the Hipparcos system requires correction. The parameters of mutual rotation were also determined by Bobylev et al (2010) from a comparison between the faint stars from the first version of XPM and UCAC2. The estimates of the rotation vector components are ω x , ω y , ω z = (0.06 ± 0.15, +0.17 ± 0.14, −0.84 ± 0.14) mas yr −1 .…”

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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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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“…The "EOP" solution was obtained as a result of the analysis of the Earth Orientation Parameters (EOPs) byVondrák et al (1997). Only two orientation parameters, ω x and ω y , are determined in this method (7). The "HST" solution was obtained by using the Hubble Space Telescope (HST).…”

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confidence: 99%

Residual HCRF rotation relative to the inertial coordinate system

Бобылев

2015

Astron. Lett.

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VLBI measurements of the absolute proper motions of 23 radio stars have been collected from published data. These are stars with maser emission, or very young stars, or asymptotic-giant-branch stars. By comparing these measurements with the stellar proper motions from the optical catalogs of the Hipparcos Celestial Reference Frame (HCRF), we have found the components of the residual rotation vector of this frame relative to the inertial coordinate system: (ω x , ω y , ω z ) = (−0.39, −0.51, −1.25) ± (0.58, 0.57, 0.56) mas yr −1 . Based on all the available data, we have determined new values of the components of the residual rotation vector for the optical realization of the HCRF relative to the inertial coordinate system: (ω x , ω y , ω z ) = (−0.15, +0.24, −0.53) ± (0.11, 0.10, 0.13) mas yr −1 .

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

Cited by 3 publications

References 11 publications

Rotational effects in the system of proper motions of the UCAC3 catalogue

Rotational effects in the system of proper motions of the UCAC3 catalogue

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

Residual HCRF rotation relative to the inertial coordinate system

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