Dissecting Galaxy Colors with
                    <i>GALEX</i>
                    , SDSS, and
                    <i>Spitzer</i>

Johnson, Bradley D.; Schiminovich, David; Seibert, Mark; Treyer, Marie; Charlot, S.; Heckman, Timothy M.; Martin, D. Christopher; Salim, Samir; Kauffmann, Guinevere; Bianchi, Luciana; Donas, J.; Friedman, Peter G.; Lee, Y.-W.; Madore, Barry F.; Milliard, B.; Morrissey, Patrick; Neff, Susan G.; Rich, R. Michael; Szalay, Alexander S.; Forster, Karl; Barlow, Tom A.; Conrow, T.; Small, Todd; Wyder, Ted K.

doi:10.1086/505741

Cited by 22 publications

(88 citation statements)

References 19 publications

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“…Thus, we are forced to use more indirect methods. We have estimated the effects of dust on the colors of galaxies in our sample using two methods: the first using the Balmer lines, and the second using the empirical dust-SFH-color relation derived by Johnson et al (2006).…”

Section: Correcting For Dustmentioning

confidence: 99%

“…The data are plotted as contours where the density of galaxies is high and as individual points where it is low. The dashed curves indicate lines of constant NUV extinction ranging from 0.2 to 3 mag, as derived from the fits in Johnson et al (2006). been weighted by 1/V max .…”

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

“…The relation in equation (10) is an empirical description of the correlations observed in the joint SDSS-GALEX-Spitzer sample analyzed by Johnson et al (2006). As such, it is difficult to interpret directly in terms of physical variables.…”

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

“…The sample used by Johnson et al (2006) was selected by requiring galaxies to be detected both in the UV by GALEX and at 24 m by Spitzer. Thus, their sample will not include quiescent early-type galaxies with no recent star formation.…”

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

“…Despite this caveat for non-star-forming galaxies, we prefer the relations computed by Johnson et al (2006) as the best measure of the UVattenuation for our sample, because this method is based on the total FIR/UV ratio, which is the most direct measure of the UV light absorbed (e.g., Gordon et al 2000). Deriving an UV attenuation from the Balmer lines requires assuming an attenuation law to convert from the extinction in the Balmer lines to that in the UV in addition to the uncertainty associated with only having measurements in the central 3 00 of each galaxy.…”

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

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The UV‐Optical Galaxy Color‐Magnitude Diagram. I. Basic Properties

Wyder

Martin

Schiminovich

et al. 2007

ASTROPHYS J SUPPL S

392

287

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We have analyzed the bivariate distribution of galaxies as a function of ultraviolet-optical colors and absolute magnitudes in the local universe. The sample consists of galaxies with redshifts and optical photometry from the Sloan Digital Sky Survey (SDSS) main galaxy sample matched with detections in the near-ultraviolet (NUV) and far-ultraviolet (FUV ) bands in the Medium Imaging Survey being carried out by the Galaxy Evolution Explorer (GALEX ) satellite. In the (NUV À r) 0:1 versus M r;0:1 galaxy color-magnitude diagram, the galaxies separate into two well-defined blue and red sequences. The (NUV À r) 0:1 color distribution at each M r;0:1 is not well fit by the sum of two Gaussians due to an excess of galaxies in between the two sequences. The peaks of both sequences become redder with increasing luminosity, with a distinct blue peak visible up to M r;0:1 $ À23. The r 0:1 -band luminosity functions vary systematically with color, with the faint-end slope and characteristic luminosity gradually increasing with color. After correcting for attenuation due to dust, we find that approximately one-quarter of the color variation along the blue sequence is due to dust, with the remainder due to star formation history and metallicity. Finally, we present the distribution of galaxies as a function of specific star formation rate and stellar mass. The specific star formation rates imply that galaxies along the blue sequence progress from low-mass galaxies with star formation rates that increase somewhat with time to more massive galaxies with a more or less constant star formation rate. Above a stellar mass of $10 10.5 M , galaxies with low ratios of current to past averaged star formation rate begin to dominate.

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Section: Correcting For Dustmentioning

confidence: 99%

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

Section: The Dust-sfh-color Relationmentioning

confidence: 99%

See 3 more Smart Citations

The UV‐Optical Galaxy Color‐Magnitude Diagram. I. Basic Properties

Wyder

Martin

Schiminovich

et al. 2007

ASTROPHYS J SUPPL S

392

287

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Fitting the integrated spectral energy distributions of galaxies

Walcher

Groves

Budavàri

et al. 2010

Astrophys Space Sci

369

318

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Fitting the spectral energy distributions (SEDs) of galaxies is an almost universally used technique that has matured significantly in the last decade. Model predictions and fitting procedures have improved significantly over this time, attempting to keep up with the vastly increased volume and quality of available data. We review here the field of SED fitting, describing the modelling of ultraviolet to infrared galaxy SEDs, the creation of multiwavelength data sets, and the methods used to fit model SEDs to observed galaxy data sets. We touch upon the achievements and challenges in the major ingredients of SED fitting, with a special emphasis on describing the interplay between the quality of the available data, the quality of the available models, and the best fitting technique to use in order to obtain a realistic measurement as well as realistic uncertainties. We conclude that SED fitting can be used effectively to derive a range of physical properties of galaxies, such as redshift, stellar masses, star formation rates, dust masses, and metallicities, with care taken not to over-interpret the available data. Yet there still exist many issues such as estimating the age of the oldest stars in a galaxy, finer details of dust properties and dust-star geometry, and the influences of poorly understood, luminous stellar types and phases. The challenge for the coming years will be to improve both the models and the observational data sets to resolve these uncertainties. The present review will be made available on an interactive, moderated web page (sedfitting.org), where the community can access and change the text. The intention is to expand the text and keep it up to date over the coming years.

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The GALEX Extended Mission: Surveying UV Tracers of the Hidden Side of Galaxy Evolution

Martin¹

2010

AIP Conference Proceedings

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The Galaxy Evolution Explorer (GALEX) continues its surveys of the ultraviolet sky. GALEX surveys have supported the following galaxy evolution investigations: calibrating UV as a star formation rate tracer, using wide and deep surveys to measure star formation history, studying the evolution of dust extinction and metallicity, selecting and analyzing galaxies in transitory states, finding local analogs to Lyman Break Galaxies, probing and time-dating star formation in a wide variety of physical regimes. Our continuing mission is focussed on relating star formation history and galaxy evolution paths to the properties of dark matter halos and their assembly history, and on beginning to relate the evolution of galaxies to that of black holes and the intergalactic medium. GALEX has proven that the UV is an ideal band to find and map star formation in low mass, low density objects, and potentially in primordial gas. With future UV missions it may be possible to map emission from the intergalactic and circum-galactic medium, and make a definitive connection between galaxy evolution and the cooling, accretion, heating, and enrichment of gas in the cosmic web.

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Dissecting Galaxy Colors with GALEX , SDSS, and Spitzer

Cited by 22 publications

References 19 publications

The UV‐Optical Galaxy Color‐Magnitude Diagram. I. Basic Properties

The UV‐Optical Galaxy Color‐Magnitude Diagram. I. Basic Properties

Fitting the integrated spectral energy distributions of galaxies

The GALEX Extended Mission: Surveying UV Tracers of the Hidden Side of Galaxy Evolution

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