U-, B- and r-band luminosity functions of galaxies in the Coma cluster

Beijersbergen, Marco W.; Hoekstra, Henk; Dokkum, Pieter van; Hulst, J. M. van der

doi:10.1046/j.1365-8711.2002.05004.x

Cited by 67 publications

(103 citation statements)

References 41 publications

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“…deg). A steepening of the faint end slope of the UV luminosity function in the outskirts of Virgo is expected since already observed in the optical bands in other clusters such as Coma (Beijersbergen et al 2002;Adami et al 2007Adami et al , 2008. The accurate morphological classification available for the VCC galaxies (from Binggeli et al 1985, those not catalogued in the VCC being classified as late-type dwarfs according to their optical morphology and blue colors) allows us to estimate the UV luminosity function separately for late-(Sa-Sm-Im-BCD) and early-type (E-S0a-dE-dS0) systems (see Fig.…”

Section: The Uv Luminosity Function Of the Central 12 Degmentioning

confidence: 52%

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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Section: The Uv Luminosity Function Of the Central 12 Degmentioning

confidence: 52%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Heinis

et al. 2011

A&A

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“…For example, this effect has been observed in several clusters such as Coma (Lobo et al 1997;Beijersbergen et al 2002;Adami et al 2007a) or Abell 496 (Boué et al 2008), and it was shown that the faint-end slope gives indications of the cluster formation history (see e.g. Adami et al 2007a, and references therein).…”

Section: Introductionmentioning

confidence: 88%

The cluster Abell 780: an optical view

Durret

Slezak

Adami

2009

A&A

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Context. The Abell 780 cluster, better known as the Hydra A cluster, has been thouroughly analyzed in X-rays. However, little is known about its optical properties. Aims. We propose to derive the galaxy luminosity function (GLF) in this apparently relaxed cluster and to search for possible environmental effects by comparing the GLFs in various regions and by looking at the galaxy distribution at large scale around Abell 780. Methods. Our study is based on optical images obtained with the ESO 2.2m telescope and WFI camera in the B and R bands, covering a total region of 67.22 × 32.94 arcmin 2 , or 4.235 × 2.075 Mpc 2 for a cluster redshift of 0.0539. Results. In a region of 500 kpc radius around the cluster center, the GLF in the R band shows a double structure, with a broad and flat bright part and a flat faint end that can be fit by a power law with an index α ∼ −0.85 ± 0.12 in the 20.25 ≤ R ≤ 21.75 interval. If we divide this 500 kpc radius region in north+south or east+west halves, we find no clear difference between the GLFs in these smaller regions. No obvious large-scale structure is apparent within 5 Mpc from the cluster, based on galaxy redshifts and magnitudes collected from the NED database in a much larger region than that covered by our data, suggesting that there is no major infall of material in any preferential direction. However, the Serna-Gerbal method reveals a gravitationally bound structure of 27 galaxies, which includes the cD, and of a more strongly gravitationally bound structure of 14 galaxies. Conclusions. These optical results agree with the overall relaxed structure of Abell 780 previously derived from X-ray analyses.

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“…A certain portion can also be attributed to the inclusion of galaxies in cluster outskirts that are projected onto the central region. Beijersbergen et al (2002) published a study of the LF of the Coma Cluster in which they corrected the LF for projection effects by subtracting the contribution of the outer Coma LF that is projected onto the central region. The resulting ''deprojected'' LF was measured to be marginally flatter than the projected two-dimensional LF.…”

Section: A2 Deprojecting the Luminosity Functionmentioning

confidence: 99%

“…Since different morphological types are characterized by different LFs (Binggeli et al 1988), the cluster LF (integrated over all galaxy types) should not be universal. Indeed, some studies have provided evidence that the cluster LF does vary with clustercentric radius (e.g., Beijersbergen et al 2002;Hansen et al 2005;Popesso et al 2006). The main goal of this paper is to investigate the change in the cluster R C band LF as a function of clustercentric radius.…”

Section: Introductionmentioning

confidence: 99%

The Luminosity Function of Low‐Redshift Abell Galaxy Clusters

Barkhouse¹,

Yee²,

López-Cruz³

2007

ApJ

128

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We present the results from a survey of 57 low-redshift Abell galaxy clusters to study the radial dependence of the luminosity function (LF). The dynamical radius of each cluster, r 200 , was estimated from the photometric measurement of cluster richness, B gc . The shape of the LFs is found to correlate with radius such that the faint-end slope, , is generally steeper on the cluster outskirts. The sum of two Schechter functions provides a more adequate fit to the composite LFs than a single Schechter function. LFs based on the selection of red and blue galaxies are bimodal in appearance. The red LFs are generally flat for À22 M R C À18, with a radius-dependent steepening of for M R C > À18. The blue LFs contain a larger contribution from faint galaxies than the red LFs. The blue LFs have a rising faint-end component ( $ À1:7) for M R C > À21, with a weaker dependence on radius than the red LFs. The dispersion of M Ã was determined to be 0.31 mag, which is comparable to the median measurement uncertainty of 0.38 mag. This suggests that the bright end of the LF is universal in shape at the 0.3 mag level. We find that M Ã is not correlated with cluster richness when using a common dynamical radius. Also, we find that M Ã is weakly correlated with BM type such that later BM-type clusters have a brighter M Ã . A correlation between M Ã and radius was found for the red and blue galaxies such that M Ã fades toward the cluster center.

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U-, B- and r-band luminosity functions of galaxies in the Coma cluster

Cited by 67 publications

References 41 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The cluster Abell 780: an optical view

The Luminosity Function of Low‐Redshift Abell Galaxy Clusters

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