Crossmatch RAVE DR5 and UCAC5 (ravedr5.rave_ucac5)

The table has 503739 rows, 25 columns.

Description

Cross-matching of RAVEDR5 against UCAC5:

RAVE fiber has a diameter of 6.7″. The fiber positioning uncertainty is 0.7″ (see DR1 paper). With this in mind the cross-matching radius was set to 4.05″ (6.7 / 2 + 0.7). Cross-matching was done using the J2000 coordinates from both catalogs.

For every RAVE star all UCAC5 stars within the matching radius were collected. If there were multiple stars withing the radius the brightest one (in Gaia g-band magnitude) was chosen as the primary. The fluxes of the rest of the stars were added together. The ratio of their fluxes with respect to the primary’s flux was expressed as the contamination ratio (gmag_cont). For example, the value of 0.2 implies that the rest of the stars within the fiber radius contribute 20% of the flux in g-band.

While g-band magnitude is available for all cross-matches, some of the stars also have measurements from other bands. r-band and j-band contamination ratios are also available (rmag_cont, jmag_cont). They are computed in the same was as the g-band contamination ratio except using the different bands. Please note that regardless of the band in which the contamination ratio is computed the brightest star (primary) is always defined as the one with the lowest g-band magnitude.

Contamination ratios are set to NULL if there is only one UCAC5 star present in the cross-matching radius. If there are more stars, but magnitudes in r- or j-band are not available the contamination ratio is set to -1. This means there is some flux contribution from the surrounding stars but the value is unknown.

The distance to the primary matching star is given in the Dist_UCAC5 column. Crossmatch RAVEDR5 and UCAC5 (zone catalog)

Attribution

Funding for Rave has been provided by:

• the Leibniz Institute for Astrophysics Potsdam (AIP);
• the Australian Astronomical Observatory;
• the Australian National University;
• the Australian Research Council;
• the French National Research Agency;
• the German Research Foundation (SPP 1177 and SFB 881);
• the European Research Council (ERC-StG 240271 Galactica);
• the Istituto Nazionale di Astrofisica at Padova;
• the Johns Hopkins University;
• the National Science Foundation of the USA (AST-0908326);
• the W. M. Keck foundation;
• the Macquarie University;
• the Netherlands Research School for Astronomy;
• the Natural Sciences and Engineering Research Council of Canada;
• the Slovenian Research Agency;
• the Swiss National Science Foundation;
• the Science & Technology FacilitiesCouncil of the UK;
• Opticon;
• Strasbourg Observatory;
• the Universities of Basel, Groningen, Heidelberg and Sydney.

This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the GaiaData Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

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