<i>GALEX</i>-SDSS CATALOGS FOR STATISTICAL STUDIES

Budavàri, Tamás; Heinis, S.; Szalay, Alexander S.; Nieto-Santisteban, María; Gupchup, Jayant; Shiao, Bernie; Smith, M. A.; Chang, Ruixiang; Kauffmann, Guinevere; Morrissey, Patrick; Schiminovich, David; Milliard, B.; Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Seibert, Mark; Forster, Karl; Bianchi, Luciana; Donas, J.; Friedman, Peter G.; Heckman, Timothy M.; Lee, Young-Wook; Madore, Barry F.; Neff, Susan G.; Rich, R. Michael; Welsh, Barry Y.

doi:10.1088/0004-637x/694/2/1281

Cited by 56 publications

(43 citation statements)

References 23 publications

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“…(a) Budavári et al (2009) reported slightly different values for the central wavelengths of both FUV and NUV, but the difference is so small as to be negligible.…”

Section: Data Selection and Galaxy Model Fittingmentioning

confidence: 93%

Far-UV to mid-IR properties of nearby radio galaxies

Ruiter

Parma

Fanti

et al. 2015

A&A

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Aims. We investigate whether the far-UV continuum of nearby radio galaxies is due solely to the parent galaxy that passively evolves, or if it reveals evidence for the presence of other star-forming or non-stellar components. If the UV excess is due to an additional radiation component, we compare this with other properties such as radio power, optical spectral type (e.g. high-and low-excitation galaxies), and the strength of the emission lines. We also discuss the possible correlation between the ultraviolet flux, IR properties, and the central black hole mass. Methods. We used a sample of low-luminosity B2 radio galaxies and a small sample of higher luminosity 3C radio galaxies at comparable redshift (z < 0.2). Spectral energy distributions (SEDs) were constructed using a number of on-line databases that are freely available now: GALEX, SDSS, 2MASS, and WISE. These were compared with model SEDs of early-type galaxies with passively evolving stellar populations at various ages (typically 0.5−1.3×10 9 years). We established whether a second component was needed to obtain a satisfactory fit with the observed overall SED. We introduce the parameter XUV , which measures the excess slope of the UV continuum between 4500 and 2000 Å with respect to the UV radiation produced by the underlying old galaxy component. Results. We find that the UV excess as measured by XUV is usually small or absent in low-luminosity (FR I) sources, but sets in abruptly at the transition radio power, above which we find mostly FRII sources. XUV behaves very similarly to the strength of the optical emission lines (in particular Hα). Below P 1.4 GHz < 10 24 WHz −1 XUV is close to zero. XUV correlates strongly with the Hα line strength, but only in sources with strong Hα emission. We discuss whether the line emission might be due to photoionization by radiation from the parent galaxy, possibly with additional star formation, or if it requires the presence of a non-stellar active galactic nucleus component. XUV and the slope of the mid-IR are strongly correlated, as measured by the WISE bands in the interval 3.4 to 22 μm, in the sense that sources with a strong UV excess also have stronger IR emission. There is an inverse correlation between XUV and central black hole mass: the M BH of objects with strong UV excess is on average two to three times less massive than that of objects without UV excess. Low-luminosity radio galaxies tend to be more massive and contain more massive black holes.

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“…(a) Budavári et al (2009) reported slightly different values for the central wavelengths of both FUV and NUV, but the difference is so small as to be negligible.…”

Section: Data Selection and Galaxy Model Fittingmentioning

confidence: 93%

Far-UV to mid-IR properties of nearby radio galaxies

Ruiter

Parma

Fanti

et al. 2015

A&A

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“…The uncertainty in the coordinates of each point source is about 20″-30″, making the identification of optical counterparts challenging. The match to the optical counterpart is performed in two steps: (1) the WISE counterparts are found using a Bayesian method based on that of Budavari et al (2009), taking into account priors in color-magnitude space; (2) counterparts in the SDSS DR9 imaging data are determined with a simple positional match to the WISE coordinates. XMMSL covers about 50% of the eBOSS area and provides an additional 0.2 deg −2 new point sources on average.…”

Section: Spiders Target Selectionmentioning

confidence: 99%

Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

et al. 2017

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“…We removed duplicates in GALEX overlapping fields by choosing the detections in the field with the largest exposure time. The cross correlation between GALEX and SDSS was performed following Budavari et al (2009), using a positional match radius of 7 arcsec. We only considered here GALEX objects with one and only one SDSS counterpart.…”

Section: Galaxy-star Identificationmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Heinis

et al. 2011

A&A

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering ∼40 sq. deg in the far UV (FUV, λ eff = 1539 Å, Δλ = 442 Å) and ∼120 sq. deg in the near UV (NUV, λ eff = 2316 Å, Δλ = 1060 Å). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared -submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early-and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (α ∼ −1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference.

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GALEX-SDSS CATALOGS FOR STATISTICAL STUDIES

Cited by 56 publications

References 23 publications

Far-UV to mid-IR properties of nearby radio galaxies

Far-UV to mid-IR properties of nearby radio galaxies

Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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