Gaia broad band photometry

By C. Jordi, M. Gebran, J. Carrasco, J. Bruijne, H. Voss, C. Fabricius, J. Knude, Antonella Vallenari, R. Kohley, A. Mora. 2010

353 citations recorded by the source corpus.

Aims. The scientific community needs to be prepared to analyse the data from Gaia, one of the most ambitious ESA space missions, which is to be launched in 2012. The purpose of this paper is to provide data and tools to predict how Gaia photometry is expected to be. To do so, we provide relationships among colours involving Gaia magnitudes (white light G, blue GBP, red GRP and GRVS bands) and colours from other commonly used photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, Hipparcos and Tycho). Methods. The most up-to-date information from industrial partners has been used to define the nominal passbands, and based on the BaSeL3.1 stellar spectral energy distribution library, relationships were obtained for stars with different reddening values, ranges of temperatures, surface gravities and metallicities. Results. The transformations involving Gaia and Johnson-Cousins V − IC and Sloan DSS g − z colours have the lowest residuals. A polynomial expression for the relation between the effective temperature and the colour GBP−GRP was derived for stars with Teff ≥ 4500 K. For stars with Teff < 4500 K, dispersions exist in gravity and metallicity for each absorption value in g − r and r − i. Transformations involving two Johnson or two Sloan DSS colours yield lower residuals than using only one colour. We also computed several ratios of total-to-selective absorption including absorption AG in the G band and colour excess E(GBP–GRP) for our sample stars. A relationship involving AG/AV and the intrinsic (V − IC) colour is provided. The derived Gaia passbands have been used to compute tracks and isochrones using the Padova and BASTI models. Finally, the performances of the predicted Gaia magnitudes have been estimated according to the magnitude and the celestial coordinates of the star. Conclusions. The provided dependencies among colours can be used for planning scientific exploitation of Gaia data, performing simulations of the Gaia-like sky, planning ground-based complementary observations and for building catalogues with auxiliary data for the Gaia data processing and validation.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fb6d2d031411f44e198b856f78390e09dc320c09

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In Astronomy and Astrophysics

1. Hans-Walter Rix
2. Jo Bovy
3. I. Minchev
4. D. Huber
5. S. Majewski
6. Timothy C. Beers
7. C. Chiappini
8. D. Schneider

In Atmospheric Science

1. A. Serenelli
2. S. Basu
3. M. Pinsonneault
4. C. Chiappini
5. G. Zasowski
6. P.-E. Tremblay
7. C. Soubiran
8. A. Mann

In Instrumentation

1. I. Minchev
2. Hans-Walter Rix
3. Jo Bovy
4. D. Huber
5. C. Chiappini
6. S. Majewski
7. D. Stello
8. Timothy C. Beers

Citations in the corpus

• HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “We also calculated Gaia G, GBP, and GRP magnitudes (Jordi et al. 2010).”
• Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 (2019, background): “For the Gaia passbands, however, this is not the case any more (Jordi et al. 2010).”
• Gaia Universe model snapshot - A statistical analysis of the expected contents of the Gaia catalogue (2012, methodology): “The G band can be related to JohnsonCousins V and IC passband by the following approximation (Jordi et al. 2010) for unreddened stars : G =V −0.0257−0.0924 (V − IC)−0.1623 (V − IC)2+ +0.0090 (V − IC)3 (1.1) for −0.4 < V − I .”
• A-type stars in the Canada–France Imaging Survey – II. Tracing the height of the disc at large distances with Blue Stragglers (2018, methodology): “The 1We have used the colour equations of Jordi et al. (2010) to transform from the SDSS g,r to Gaia G. 2Here θ is the elevation angle and φ is the azimuthal angle.”
• Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes (2017, positive): “The Gaia G-band magnitude and Johnson-Cousins V−I color were calculated from KIC gri photometry (Table 1) using the following relations (Jordi et al. 2006, 2010): = - - - - - + - + ( ( ) ( ) ( ) ) ( ) G g r g r g r g 0.0662 0.7854 0.2859 0.0145 , 8 2 3 and - = - + - < - - ⎧⎨⎩ ( ) ( ) ( )V I g r g r…”
• Painting a portrait of the Galactic disc with its stellar clusters (2020, background): “However, Jordi et al. (2010) remark that varying the extinction law within the range reported by Fitzpatrick & Massa (2007) has a negligible effect on the Gaia photometry.”
• THE APOGEE RED-CLUMP CATALOG: PRECISE DISTANCES, VELOCITIES, AND HIGH-RESOLUTION ELEMENTAL ABUNDANCES OVER A LARGE AREA OF THE MILKY WAY'S DISK (2014, methodology): “We estimate the Gaia G-band magnitudes of stars in the APOGEE-RC sample by using the PARSEC isochrones in the SDSS and 2MASS passbands in the RC region defined in § 2 and using the transformation between g, g − z and G of Table 5 of Jordi et al. (2010).”
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, methodology): “To compute our predicted G magnitudes, we utilized the g, r, and i color-color polynomial fits in Table 7 of Jordi et al. (2010).”
• The Optical to Mid-infrared Extinction Law Based on the APOGEE, Gaia DR2, Pan-STARRS1, SDSS, APASS, 2MASS, and WISE Surveys (2019, background): “The central wavelengths of G, GBP, and GRP bands are 673, 532, and 797 nm, respectively (Jordi et al. 2010).”
• AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, background): “For the Gaia passbands Vega has a magnitude of +0.03 (Jordi et al. 2010), and the zero points defined with this reference are given in Table 3 along with nominal wavelengths.”