Subject: proper-motions - STScI NAVO Directory Search Results

ID:: ivo://edu.gavo.org/hd/gavo_addpms
Title:: Adding catalog data to object lists using the VO
Date:: 02 Feb 2023 09:07:52
Publisher:: The GAVO DC team
Description:: This brief tutorial shows you how to quickly add proper motions and photometry from Gaia to (almost) any object list using the Virtual Observatory. The VO protocol most suited to this kind of this is TAP ("table access protocol") and lets you transfer data and queries to database servers. In the example, we will be using TOPCAT as a client. There is no lock-in to it: There are libraries and other tools allowing an integration of TAP operations into arbitrary workflows – that's what standards are about. Tutorial supplements apply the techniques to Simbad, show how to use TAP from Python, and introduce UCDs.

ID:: ivo://org.gavo.dc/arihip/q/cone
Title:: ARIHIP astrometric catalogue
Short Name:: arihip cone
Date:: 23 Mar 2022 13:13:11
Publisher:: The GAVO DC team
Description:: The catalogue ARIHIP has been constructed by selecting the 'best data' for a given star from combinations of HIPPARCOS data with Boss' GC and/or the Tycho-2 catalogue as well as the FK6. It provides 'best data' for 90 842 stars with a typical mean error of 0.89 mas/year (about a factor of 1.3 better than Hipparcos for this sample of stars).

ID:: ivo://org.gavo.dc/ucac3/q/corr
Title:: Corrections between UCAC3 and PPMXL
Short Name:: UCAC3 ICRS corr
Date:: 23 Mar 2022 13:13:19
Publisher:: The GAVO DC team
Description:: Differences between UCAC3 and PPMXL in positions and proper motions, on an all-sky one-degree grid. At each gridpoint we give the differences X(PPMXL)- X(UCAC3) averaged over all stars in a sqrt(2)/2-degrees environment around the gridpoint given. The corrections given here should bring UCAC3 based astrometry to the ICRS.

ID:: ivo://org.gavo.dc/ppmxl/q/corr
Title:: Corrections between USNO-B and PPMXL
Short Name:: PPMXL USNO corr
Date:: 23 Mar 2022 13:13:09
Publisher:: The GAVO DC team
Description:: Differences between USNO-B and PPMXL in positions and proper motions, on an all-sky one-degree grid. At each gridpoint we give the differences X(PPMXL)- X(USNO-B1.0) averaged over all stars in a sqrt(2)/2-degrees environment around the gridpoint given. The corrections given here should bring USNO-B based astrometry to the ICRS.

ID:: ivo://org.gavo.dc/dmubin/q/cone
Title:: Delta-mu Binaries
Short Name:: dmubin cone
Date:: 23 Mar 2022 13:13:09
Publisher:: The GAVO DC team
Description:: A collection of binary stars with a difference in instantaneous proper motion as measured by HIPPARCOS and the long-term proper motion.

ID:: ivo://org.gavo.dc/gaia/q/dr1
Title:: Gaia Data Release 1 (DR1) gaia_source
Date:: 17 Sep 2020 08:07:06
Publisher:: The GAVO DC team
Description:: This table, corresponding to gaia_source of the full DR1, contains the 1.15 billion objects reliably detected in the first 14 months of Gaia observations. It essentially consists of high-precision positions and magnitudes. The TGAS subset (about 2 million objects observed by both Gaia and Hipparcos) has proper motions and parallaxes. Users are advised to beware strong correlations between the astrometric parameters present for some of the less densely observed objects and the inhomogeneous coverage in this first data release (solution id: 1635378410781933568).

ID:: ivo://org.gavo.dc/gaia/q2/dr2epochflux
Title:: Gaia DR2 epoch fluxes
Short Name:: gaia.dr2epochflu
Date:: 23 Mar 2022 13:13:05
Publisher:: The GAVO DC team
Description:: A table of the light curves released with Gaia DR2 (about half a million in total). In each Gaia band (G, BP, RP), we give epochs, fluxes and their errors in arrays. We do not include the quality flags (DR2: “may be safely ignored for many general purpose applications”). You can access them through the associated datalink service if you select source_id. You will usually join this table with gaia.dr2light. We have also removed all entries with NaN observation times; hence, the array lengths in the different bands can be significantly different, and the indices in transit_ids do not always correspond to the indices in the time series. Furthermore, we only give fluxes and their errors here rather than magnitudes. Fluxes can be turned into magnitude using:: mag = -2.5 log10(flux)+zero point, where the zero points assumed for Gaia DR2 are 25.6884±0.0018 in G, 25.3514±0.0014 in BP, and 24.7619±0.0019 in RP (VEGAMAG).

ID:: ivo://org.gavo.dc/gaia/q2/dr2lcone
Title:: Gaia DR2-light Cone Search
Short Name:: GDR2light SCS
Date:: 23 Mar 2022 13:13:05
Publisher:: The GAVO DC team
Description:: This schema contains data re-published from the official Gaia mirrors (such as ivo://uni-heidelberg.de/gaia/tap) either to support combining its data with local tables (the various Xlite tables) or to make the data more accessible to VO clients (e.g., epoch fluxes). Other Gaia-related data is found in, among others, the gdr2dist, gdr3mock, gdr3spec, gedr3auto, gedr3dist, gedr3mock, and gedr3spur schemas.

ID:: ivo://org.gavo.dc/gaia/q2/ssa
Title:: Gaia DR2 light curves SSA
Short Name:: GDR2 TS SSAP
Date:: 23 Mar 2022 13:13:05
Publisher:: The GAVO DC team
Description:: This service exposes about 0.5 million light curves of stars classified as variable by the Gaia analysis system through the VO SSAP protocol. The lightcurves are published per-band and are also available through obscore.

ID:: ivo://xaovo/gaia/q3/cone
Title:: Gaia DR3 Lite Cone Search
Short Name:: DR3 lite Cone
Date:: 14 Jun 2023 08:15:26
Publisher:: Xinjiang Astronomical Observatory,CAS
Description:: This schema contains data re-published from the official Gaia mirrors (such as ivo://uni-heidelberg.de/gaia/tap) either to support combining its data with local tables (the various Xlite tables) or to make the data more accessible to VO clients (e.g., epoch fluxes).

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