The Ultraviolet Galaxy Luminosity Function in the Local Universe from
                    <i>GALEX</i>
                    Data

Wyder, Ted K.; Treyer, Marie; Milliard, B.; Schiminovich, David; Arnouts, S.; Budavàri, Tamás; Barlow, Tom A.; Bianchi, Luciana; Byun, Yong Ik; Donas, J.; Forster, Karl; Friedman, Peter G.; Heckman, Timothy M.; Jelinsky, Patrick; Lee, Young-Wook; Madore, Barry F.; Malina, Roger F.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Rich, R. Michael; Siegmund, Oswald H. W.; Small, Todd; Szalay, Alexander S.; Welsh, Barry Y.

doi:10.1086/424735

Cited by 235 publications

(313 citation statements)

References 36 publications

Supporting

Mentioning

277

Contrasting

Order By: Relevance

“…FUV, NUV, and K s band magnitudes are corrected for galactic extinction using the corrections from (Wyder et al 2005). For FUV, NUV, and K bands, the ratio of…”

Section: Galactic Extinction Correctionmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

View full text Add to dashboard Cite

We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

show abstract

“…FUV, NUV, and K s band magnitudes are corrected for galactic extinction using the corrections from (Wyder et al 2005). For FUV, NUV, and K bands, the ratio of…”

Section: Galactic Extinction Correctionmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

View full text Add to dashboard Cite

show abstract

“…The luminosity function is a statistical tool widely used to study the mean properties of large samples of galaxies. Often used in other wavelength domains, it has been derived at rest frame in the GALEX UV bands only for the general field (Wyder et al 2005) and for a few other nearby clusters (Coma, Cortese et al 2008;Hammer et al 2012;A1367, Cortese et al 2005; Shapley, Haines et al 2011). Compared to these previous works, the UV luminosity function derived from the GUViCS survey has the great advantage of including a significantly large number of objects with direct redshift measurements, of sampling a much wider range in galaxy density, from the core of the cluster out to the periphery (∼2 R vir ), and of including the dwarf galaxy population (NUV < ∼ −11.5 mag).…”

Section: Introductionmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

View full text Add to dashboard Cite

We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

show abstract

“…To further put Haro 11 into context, we compare it to the local Universe luminosity functions (LFs) of galaxies: Haro 11 has L FUV = 4.8 L FUV (compared to M FUV = −18.0 of Wyder et al 2005), the Hα luminosity is L Hα = 4.4 L Hα (L Hα = 6.6 × 10 41 erg/s/cm 2 , Gallego et al 1995), r-band L r = 0.9 L r (M r = −20.82, Blanton et al 2003), and L K = 0.36 L K (M K = −20.97, Kochanek et al 2001), where literature values were rescaled to the currently used H 0 and photometric system. Since the K-band luminosity of Haro 11 is still dominated by the bright central (r < 5 kpc) burst component (Micheva et al 2010), the underlying host galaxy (contributing ∼30% to the K-band luminosity) has a stellar mass of the order of 10% that of a typical quiescent L K galaxy.…”

Section: Introductionmentioning

confidence: 99%

Kinematics of Haro 11: The miniature Antennae

Östlin

Marquart

Cumming

et al. 2015

A&A

View full text Add to dashboard Cite

Luminous blue compact galaxies are among the most active galaxies in the local Universe in terms of their star formation rate per unit mass. They are rare at the current cosmic epoch, but were more abundant in the past and may be seen as the local analogues of higher red shift Lyman break galaxies. Studies of their kinematics is key to understanding what triggers their unusually active star formation. In this work, we investigate the kinematics of stars and ionised gas in Haro 11, one of the most luminous blue compact galaxies in the local Universe. Previous works have indicated that many of these galaxies may be triggered by galaxy mergers. We have employed Fabry-Perot interferometry, long-slit spectroscopy, and integral field unit (IFU) spectroscopy to explore the kinematics of Haro 11. We target the near-infrared calcium triplet, and use cross-correlation and penalised pixel fitting techniques to derive the stellar velocity field and velocity dispersion. We analyse ionised gas through emission lines from hydrogen, [O ], and [S ]. When spectral resolution and signal to noise allows, we investigate the line profile in detail and identify multiple velocity components when present. The spectra reveal a complex velocity field whose components, both stellar and gaseous, we attempt to disentangle. We find that to first order, the velocity field and velocity dispersions derived from stars and ionised gas agree. Hence the complexities reveal real dynamical disturbances providing further evidence for a merger in Haro 11. Through decomposition of emission lines, we find evidence for kinematically distinct components, for instance, a tidal arm. The ionised gas velocity field can be traced to large galactocentric radii, and shows significant velocity dispersion even far out in the halo. If interpreted as virial motions, this indicates that Haro 11 may have a mass of ∼10 11 M . Haro 11 shows many resemblances with the famous Antennae galaxies both morphologically and kinematically, but it is much denser, which is the likely explanation for the higher star formation efficiency in Haro 11.

show abstract

The Ultraviolet Galaxy Luminosity Function in the Local Universe from GALEX Data

Cited by 235 publications

References 36 publications

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Kinematics of Haro 11: The miniature Antennae

Contact Info

Product

Resources

About