Empirical color transformations between SDSS photometry and Other photometric systems.

By K. Jordi, E. Grebel, K. Ammon. 2005

477 citations recorded by the source corpus.

Aims. We present empirical color transformations between the Sloan Digital Sky Survey (SDSS) ugriz photometry and the Johnson-Cousins UBVRI system and Becker's RGU system, respectively. Owing to the magnitude of data that is becoming available in the SDSS photometric system it is particularly important to be able to convert between this new system and traditional photometric systems. Unlike earlier published transformations we based our calculations on stars actually measured by the SDSS with the SDSS 2.5-m telescope. The photometric database of the SDSS provides in a sense a single-epoch set of “tertiary standards” covering more than one quarter of the sky. Our transformations should facilitate their use to easily and reliably derive the corresponding approximate Johnson-Cousins or RGU magnitudes. Methods. The SDSS survey covers a number of areas that were previously established as standard fields in the Johnson-Cousins system, in particular, fields established by Landolt and by Stetson. We used these overlapping fields to create well-photometered star samples on which our calculated transformations are based. For the RGU photometry we used fields observed in the framework of the new Basel high-latitude field star survey. Results. We calculated empirical color transformations between SDSS photometry and Johnson-Cousins UBVRI and Becker's RGU system. For all transformations we found linear relations to be sufficient. Furthermore we showed that the transformations between the Johnson-Cousins and the SDSS system have a slight dependence on metallicity.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/2fee7a7cba6bc85e50ea0415c88f17b130ce5903

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In Astronomy and Astrophysics

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Citations in the corpus

• CALCIUM-RICH GAP TRANSIENTS IN THE REMOTE OUTSKIRTS OF GALAXIES (2011, background): “Conversion from ugriz to the B band was done following Jordi et al. (2006).”
• THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, methodology): “29 and 35), converting the zero-point to the Cousins I−band using the SDSS (r − i) color and two equations from Jordi et al. (2006).”
• Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes (2017, unknown): “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…”
• Interstellar Interloper 1I/2017 U1: Observations from the NOT and WIYN Telescopes (2017, methodology): “Subsequent transformation from the Sloan filters to BVR filters employed at the NOT was made according to Jordi et al. (2006).”
• The EFIGI catalogue of 4458 nearby galaxies with detailed morphology (2011, methodology): “Colour conversion terms between the Johnson-Cousins system and SDSS system are extracted from Jordi et al. (2006).”
• A MegaCam Survey of Outer Halo Satellites. III. Photometric and Structural Parameters (2018, methodology): “To obtain the V −band values we used the transformation V = g−0.569× (g−r)−0.021 derived by Jordi et al. (2006) which is generally useful for metal-poor Population II stars.”
• The search for failed supernovae with the Large Binocular Telescope: first candidates (2014, methodology): “The SDSS photometry was transformed from the SDSS ugriz filter system to the UBV Rc system using the prescription described by Jordi et al. (2006).”
• THE QUENCHING OF THE ULTRA-FAINT DWARF GALAXIES IN THE REIONIZATION ERA (2014, methodology): “For CVn II, the Sand et al. (2012) photometry is inV and I, so we transformed the SDSS magnitudes to those bands with the relations derived by Jordi et al. (2006) for metal-poor stars and compared to a theoretical isochrone (Dotter et al. 2008) for an age of 12 Gyr and [Fe/H]=−2.21, which matches…”
• THE HOST GALAXIES OF SWIFT DARK GAMMA-RAY BURSTS: OBSERVATIONAL CONSTRAINTS ON HIGHLY OBSCURED AND VERY HIGH REDSHIFT GRBs (2009, methodology): “One field (GRB 060210) was calibrated to USNO directly (B2, R2, and I magnitudes), using an average color of B − g ∼ 0.4 ± 0.3 (Jordi et al. 2006) to convert B to g.”
• THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, methodology): “When necessary, we translate between the Sloan and Johnson-Cousins filters using the transformations for Population I stars provided by Jordi et al. (2006).”
• CALIFA : a diameter-selected sample for an integral field spectroscopy galaxy survey (2014, methodology): “13 shows a comparison between the g-band growth curve magnitudes and an estimate of the g band magnitude determined from the RC3 using their B-band total magnitude and B − V colour as well as the following equation from Jordi et al. (2006): g − B = −0.370 ∗ (B − V) − 0.124.”
• AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS (2010, methodology): “Using the SDSS observations of this field and the filter transformations of Jordi et al. (2006), we find an R-band magnitude for this source of R = 17.31mag (compared to an assumed value of 17.15mag from Kann et al. 2009b).”
• PLANETARY CANDIDATES FROM THE FIRST YEAR OF THE K2 MISSION (2015, methodology): “…outside the Boyajian et al. (2013) calibrated range, we converted the g and r SDSS colors to Johnson V and Cousins R using the transformations from Jordi et al. (2006), and for stars with only infrared colors, we interpolated the Mamajek H−K colors instead of J − K, because in M-dwarfs, J − K is…”
• MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES (2010, methodology): “Then, we transformed SDSS gri magnitudes to Johnson-Cousins BV RI magnitudes (Jordi et al. 2006).”
• Analytical approximations of K-corrections in optical and near-infrared bands (2010, methodology): “We used the photometric transformations defined in Jordi et al. (2006) for stars and those provided on the web-pages of SDSS in order to convert available SDSS ugriz magnitudes into Johnson-Cousins UBV RcIc, and UKIDSS Y JHK to 2MASS JHKs transformations presented in Hewett et al. (2006).”