The GALEX Ultraviolet Atlas of Nearby Galaxies

By A. G. D. Paz, S. Boissier, B. Madore, M. Seibert, Y. Joe, A. Boselli, T. Wyder, D. Thilker, L. Bianchi, S. Rey and 16 more. 2006

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We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; λeff = 1516 Å) and near-ultraviolet (NUV; λeff = 2267 Å) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1′ in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe. From the surface brightness profiles obtained we have computed asymptotic magnitudes, colors, and luminosities, along with the concentration indices C31 and C42. We have also morphologically classified the UV surface brightness profiles according to their shape. This data set has been complemented with archival optical, near-infrared, and far-infrared fluxes and colors. We find that the integrated (FUV − K) color provides robust discrimination between elliptical and spiral/irregular galaxies and also among spiral galaxies of different subtypes. Elliptical galaxies with brighter K-band luminosities (i.e., more massive) are redder in (NUV − K) color but bluer in (FUV − NUV) (a color sensitive to the presence of a strong UV upturn) than less massive ellipticals. In the case of the spiral/irregular galaxies our analysis shows the presence of a relatively tight correlation between the (FUV − NUV) color (or, equivalently, the slope of the UV spectrum, β) and the total infrared-to-UV ratio. The correlation found between (FUV − NUV) color and K-band luminosity (with lower luminosity objects being bluer than more luminous ones) can be explained as due to an increase in the dust content with galaxy luminosity. The images in this Atlas along with the profiles and integrated properties are publicly available through a dedicated Web page.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8ce998ce808e1f0a85b1719552cc376066191210

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Citations in the corpus

DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS (2011, methodology): “It should be noted that the large absolute calibration uncertainties (0.15 mag) in Gil de Paz et al. are included in the quoted errors in FUV and NUV for SINGS sample.”
THE STAR FORMATION EFFICIENCY IN NEARBY GALAXIES: MEASURING WHERE GAS FORMS STARS EFFECTIVELY (2008, neutral): “The FUV data come from the GALEX Nearby Galaxies Survey (Gil de Paz et al. 2007) and the 24µm maps are part of SINGS.”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…of nearby galaxies such as the Spitzer Infrared Nearby Galaxies Survey (SINGS) (Kennicutt et al. 2003), the GALEX Nearby Galaxies Survey (Gil de Paz et al. 2007), the Spitzer/GALEX Local Volume Legacy survey (LVL; Dale et al. 2009; Lee et al. 2011), and the Herschel KINGFISH Survey (Kennicutt…”
Implementing molecular hydrogen in hydrodynamic simulations of galaxy formation (2012, result): “The connection betweenH2 and star formation in other galaxies has been further supported by data from THINGS (Walter et al. 2008), HERACLES (Leroy et al. 2009), NGS (Gil de Paz et al. 2007), and SINGS (Kennicutt et al. 2003).”
A MOLECULAR STAR FORMATION LAW IN THE ATOMIC-GAS-DOMINATED REGIME IN NEARBY GALAXIES (2011, background): “This is mainly the overlap of several surveys: HERACLES (IRAM 30m CO, Leroy et al. 2009), THINGS (VLA H i, Walter et al. 2008), SINGS or LVL (Spitzer IR, Kennicutt et al. 2003a; Dale et al. 2009), and the GALEX NGS (GALEX FUV, Gil de Paz et al. 2007).”
DIRECT OXYGEN ABUNDANCES FOR LOW-LUMINOSITY LVL GALAXIES (2012, methodology): “The LVL is leveraged by ancillary data including Hα (Kennicutt et al. 2008) and UV (Lee et al. 2011) imaging from the 11 Mpc Hα and Ultraviolet Galaxy Survey (11HUGS; Lee et al. 2011) and the Nearby Galaxy Survey (NGS; Gil de Paz et al. 2007).”
On the impact of empirical and theoretical star formation laws on galaxy formation (2010, background): “…more reliable C© 2011 The Authors Monthly Notices of the Royal Astronomical Society C© 2011 RAS estimates of unobscured SF in the UV (e.g. Gil de Paz et al. 2007) and of dust-obscured SF in the IR (e.g. Calzetti et al. 2007) have allowed better determinations of the SFR, both globally and…”
UV Star Formation Rates in the Local Universe (2007, positive): “IRX-β relationship fornormalgalaxies, such as those in our sample, has been previously studied withGALEXdata by Seibert et al. (2005); Cortese et al. (2006); Gil de Paz et al. (2007); Boissier et al. (2007); Panuzzo et al. (2007).”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, methodology): “Abundance is low (though not primordial) in the outer disk, as measured in a population of faint H II regions (Gil de Paz et al. 2007b).”
EXTREMELY INEFFICIENT STAR FORMATION IN THE OUTER DISKS OF NEARBY GALAXIES (2010, methodology): “GALEX UV To trace recent star formation in the outer disks, we use far UV data from the ‘GALEX Nearby Galaxy Survey’ (NGS, Gil de Paz et al. 2007a).”
COMPARISON OF Hα AND UV STAR FORMATION RATES IN THE LOCAL VOLUME: SYSTEMATIC DISCREPANCIES FOR DWARF GALAXIES (2009, methodology): “Calibrations and scaling relationships which better describe the correlation for such systems have been published (e.g., Kong et al. 2004; Seibert et al. 2005; Cortese et al. 2006; Boisser et al. 2007; Gil de Paz et al. 2007).”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, methodology): “We obtained UV magnitudes from GALEX (using the values quoted in Gil de Paz et al. 2007 for NGC 2146), and converted them to fluxes using the calibration in Morrissey et al. (2007).”
EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE: FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS (2012, background): “The integrated flux of M 83 in these two bands is 9.56 [AB mag] and 10.12 [AB mag], respectively for NUV and FUV, where the magnitudes have been corrected for the foreground extinction toward M 83 (AV = 0.22 mag); see Gil de Paz et al. (2007) for the extinction coefficients.”