The XPM Catalogue: absolute proper motions of 280 million stars

Fedorov, P. N.; Myznikov, A. A.; Akhmetov, V. S.

doi:10.1111/j.1365-2966.2008.14168.x

Cited by 42 publications

(25 citation statements)

References 20 publications

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“…Most of the systematic zonal errors inherent in the USNO‐A2.0 catalogue were eliminated before the calculation of proper motions. The mean formal error of absolute calibration is less than 1 mas yr −1 (Fedorov et al 2009).…”

Section: The Datamentioning

confidence: 89%

Candidate subdwarfs and white dwarfs from the 2MASS, Tycho-2, XPM and UCAC3 catalogues

Gontcharov

Bajkova

Fedorov³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Photometry from the Two‐Micron All‐Sky Survey (2MASS), United States Naval Observatory CCD Astrograph Catalog (UCAC3) and SuperCosmos catalogues, together with proper motions from the Tycho‐2, Kharkiv Proper Motions (XPM) and UCAC3 catalogues, is used to select all‐sky samples of 28 candidate white dwarfs, 1826 evolved and 7641 unevolved subdwarfs for R from 9–17 mag. The samples are separated from main‐sequence stars with an admixture of less than 10 per cent, owing to an analysis of the distribution of the stars in colour index versus reduced proper‐motion diagrams for various latitudes using related Monte Carlo simulations. It is shown that the XPM and UCAC3 catalogues have the same level of proper‐motion accuracy. Most of the selected stars have at least six‐band photometry. This allows us to eliminate some admixtures and reveal some binaries. Empirical calibrations of absolute magnitude versus colour index and reduced proper motion for Hipparcos stars give us distances and a three‐dimensional (3D) distribution for all the selected stars. It is shown that the subdwarf samples are almost complete for the Tycho‐2 stars, i.e. to 11 mag or 150 pc from the Sun. For fainter stars from the XPM and UCAC3 catalogues, the subdwarf samples are complete only to 20–60 per cent because of the selection method and incompleteness of the catalogues. Some conclusions can be made, however, especially for Tycho‐2 stars with known radial velocities and metallicities. The subdwarfs show some concentration in the Galactic Centre hemisphere, with voids due to extinction in the Gould belt and the Galactic plane. Some as yet unexplained overdensities of evolved subdwarfs are seen in several parts of the sky. For 176 stars with radial velocities, the 3D motion and Galactic orbits are calculated. For 57 stars with Fe/H we find relations of the metallicity with colour index, asymmetric drift velocity and orbital eccentricity. All the data are consistent with the suggestion that most unevolved subdwarfs belong to the low‐metallicity halo with large asymmetric drift, whereas evolved subdwarfs have various metallicities and velocities and include both disc and halo stars. The lower limit of the local mass density of unevolved subdwarfs, estimated as 2 × 10−5 M⊙ pc−3, appears twice as high as traditional estimates. The selected stars are listed in the new catalogue of candidate subdwarfs and white dwarfs from the 2MASS, Tycho‐2, XPM and UCAC3 catalogues (hereafter SDWD catalogue) for future spectroscopic confirmation of the subluminous status of these stars, because the majority of them are now classified for the first time.

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Section: The Datamentioning

confidence: 89%

Candidate subdwarfs and white dwarfs from the 2MASS, Tycho-2, XPM and UCAC3 catalogues

Gontcharov

Bajkova

Fedorov³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…The AWS of UkrVO provide automated search and selection of required data in accordance with the SCS standard [3] for three astronomical catalogues compiled in Ukraine, namely ASCC [4], FONAC [5], XPM [6]. The structure of AWS web address consists of path to script and search options after the question mark (Table 1).…”

Section: Aws For Astronomical Cataloguesmentioning

confidence: 99%

UkrVO Astronomical WEB Services

Mazhaev¹

2017

Sci. innov.

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“…This article is devoted to deriving and analysing the systematic differences of the coordinates and proper motions of the XPM (Fedorov, Akhmetov, Bobylev, & Bajkova, ; Fedorov, Myznikov, & Akhmetov, ) and UCAC4 (Zacharias et al, ) catalogues in the galactic coordinate system. It is a continuation of the work of Vityazev and Tsvetkov (), which describes these catalogues and the results of their comparison in the equatorial coordinate system.…”

Section: Introductionmentioning

confidence: 99%

Comparison of XPM and UCAC4 catalogues in the galactic coordinate system

et al. 2017

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This paper presents the results of the comparison of the galactic reference frames realized by the catalogues XPM and UCAC4. Based on about 40 million stars common to both catalogues, the systematic differences of the galactic coordinates and proper motions have been derived for 12 magnitudes in 0.5 m width bins with the mean J-values from 10 m .25 to 15 m .75. The systematic differences were represented by vector spherical harmonics, with the magnitude equation taken into consideration. The mutual orientation of the frames was found to be at the level of 10 mas. It is concluded that these differences are negligible in comparison with the accuracy of the implementation of the standard galactic coordinate system MAS 1958. We investigated two features of the XPM catalogue. First, unlike the HCRF and UCAC4 catalogues, whose proper motions are tied to the quasars and galaxies, the XPM catalogue implements a reference system based only on galaxies. Second, the XPM catalogue has two systems of proper motions-XPM x and XPM p , referred to the two galaxy sub-catalogues of the project 2MASS-PSC and XSC. The study of the differences XPM x −XPM p showed that they are free of the magnitude equation. The speed of relative rotation of XPM x over XPM p was found to be = 0.453 ± 0.003 mas/year, which exceeds the residual rotation of the HCRF (0.25 mas/year). Analysis of systematic differences XPM x −UCAC4 and XPM p −UCAC4 showed that both frames XPM x and XPM p have an appreciable rotation speed relative to the UCAC4 (hence the ICRF), especially large (up to 2 mas/year) for the brightest stars in our range. This shows that a relatively high speed of rotation of the two frames XPM x and XPM p with respect to the UCAC4 is a consequence of the transition from a combined "quasar-galaxy" to a purely "galactic" reference system. It is shown that the systematic difference between the proper motions of stars can be interpreted within the Ogorodnikov-Milne kinematic model of the velocity field. 489 t 1,0,1,0 −26.75 ± 0.65 t 3,3,0,1 −3.44 ± 0.76 t 5,5,0,0 12.97 ± 0.65 t 1,1,0,0 −22.86 ± 0.69 t 3,3,0,2 1.71 ± 0.75 t 5,5,0,1 −4.83 ± 0.76 t 1,1,0,1 −1.30 ± 0.76 t 3,3,1,0 8.79 ± 0.66 t 6,3,0,0 5.41 ± 0.72 t 1,1,0,2 2.81 ± 0.75 t 4,3,1,0 6.86 ± 0.65 t 6,3,0,1 −1.93 ± 0.79 t 1,1,1,0 18.71 ± 0.66 t 4,3,1,1 −4.10 ± 0.76 t 6,3,0,2 2.24 ± 0.78 t 2,0,1,0 −11.05 ± 0.65 t 5,0,1,0 −9.27 ± 0.69 t 6,5,0,0 3.71 ± 0.65 t 2,1,0,0 27.92 ± 0.69 t 5,0,1,1 6.08 ± 0.76 t 6,5,0,1 −4.97 ± 0.76 t 2,1,0,1 2.18 ± 0.90 t 5,0,1,2 −1.82 ± 0.75 t 6,6,0,0 −5.66 ± 0.69 t 2,1,0,2 −4.63 ± 0.75 t 5,1,0,0 13.97 ± 0.71 t 6,6,0,1 5.46 ± 0.76 t 2,1,0,3 −2.67 ± 0.79 t 5,1,0,1 −5.58 ± 0.82 t 6,6,0,2 −2.40 ± 0.75 t 2,1,1,0 −18.42 ± 0.65 t 5,1,1,0 −6.21 ± 0.76 t 8,4,1,0 4.69 ± 0.65 t 2,1,1,1 −2.36 ± 0.76 t 5,2,0,0 −10.70 ± 0.74 t 8,6,1,0 7.46 ± 0.65 t 2,2,0,0 −35.89 ± 0.69 t 5,2,0,1 6.19 ± 0.86 t 8,6,1,1 −4.14 ± 0.76 t 2,2,0,2 2.15 ± 0.75 t 5,2,1,0 −7.66 ± 0.69 t 8,7,1,0 −6.30 ± 0.65 t 2,2,1,0 −16.97 ± 0.66 t 5,2,1,1 4.66 ± 0.76 t 8,7,1,1 2.15 ± 0.76 t 2,2,1,1 2.42 ± 0.76 t 5,2,1,2 −...

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The XPM Catalogue: absolute proper motions of 280 million stars

Cited by 42 publications

References 20 publications

Candidate subdwarfs and white dwarfs from the 2MASS, Tycho-2, XPM and UCAC3 catalogues

Candidate subdwarfs and white dwarfs from the 2MASS, Tycho-2, XPM and UCAC3 catalogues

UkrVO Astronomical WEB Services

Comparison of XPM and UCAC4 catalogues in the galactic coordinate system

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