The Luminosity Function of the Coma Cluster Core for -25&lt;M/R&lt;-9.4

Bernstein, G. M.; Nichol, R. C.; Tyson, J. A.; Ulmer, M. P.; Wittman, David

doi:10.1086/117624

Cited by 243 publications

(365 citation statements)

References 37 publications

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“…The results are essentially the same as those reported, for instance, for other groups [a \ [1.44 (^0.1), Ferguson & Sandage 1991], the Virgo cluster [a \ [1.25 (^0.05), , and the Coma cluster [a \ [1.42 (^0.05), Bernstein et al 1995]. Our result is also consistent with the previous Ðnding a \ [1.25 by Schmidt & Boller (1992b), which was based on the 10 Mpc galaxy catalog.…”

Section: Luminosity Functions Of Nearby Groupssupporting

confidence: 88%

Surface [ITAL]BR[/ITAL] Photometry of Newly Discovered Dwarf Elliptical Galaxies in the Nearby Sculptor and Centaurus A Groups

Jerjen

Binggeli

Freeman

2000

The Astronomical Journal

162

207

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Prompted by the recent Ðnding of a large number of gas-rich dwarf irregular galaxies in the nearby southern galaxy groups Sculptor (Scl) and Centaurus A (Cen A) we carried out a complementary survey to search for members of the gas-poor dwarf elliptical (dE) galaxy family. In total 18 dE candidates were identiÐed on SRC Sky Survey Ðlms covering the group regions. For Ðve dEÏs in the Scl group and Ðve in the Cen A group, membership information is available from surface brightness Ñuctuations distance measurements ; two dEs in each group also have independent redshift measurements. The remaining eight galaxies have been associated to the groups based on their morphology. We acquired deep B-and R-band CCD images for all galaxies and determined their photometric and structural parameters. According to the magnitude range covered, (not counting the bright dS0 NGC 59), [ 14 \ M B \ [9 these objects are local dwarf spheroidal (dSph) analogues. The surface brightness proÐles of most dwarfs are strongly nonexponential but are perfectly explained by the three-parametric law. The bestSersic Ðtting parameters are compared with corresponding data for Virgo dEÏs and dSphÏs. The present Sersic dEs follow the relations between the parameters and absolute B-band magnitude for Virgo dEÏs Sersic and local dwarfs, thus conÐrming the membership in the Scl and Cen A groups, respectively. Most of our dwarfs exhibit color gradients in in the sense of a reddening outward. We also show and (B[R) 0 , discuss the sky distributions and B-band luminosity functions of the Scl and Cen A groups. The completeness magnitude for both populations (from the present survey) is estimated to be We M B lim B [13. Ðnd that the composite luminosity function of four nearby galaxy groups is well Ðtted by a Schechter function down to with a faint end slope a \ [1.29(^0.10). In the appendices we present M B lim \ [14 best-Ðtting proÐle parameters for the dSph members of the Local Group and introduce two new Sersic dwarf irregulars found in the Cen A group.

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Section: Luminosity Functions Of Nearby Groupssupporting

confidence: 88%

Surface [ITAL]BR[/ITAL] Photometry of Newly Discovered Dwarf Elliptical Galaxies in the Nearby Sculptor and Centaurus A Groups

Jerjen

Binggeli

Freeman

2000

The Astronomical Journal

162

207

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“…Marzke et al (1994b) report an upturn in the luminosity function of late-type galaxies with M(B) > −16 + log 10 h, but LCRS, Autofib, and Cowie et al (1996) all derive a flat faint-end slope. There is, however, evidence for a steep faint-end slope in galaxy clusters (e.g., De Propris et al 1995, Bernstein et al 1995. Environmental influences on galaxy evolution may be reflected in variations of the LF for galaxies in different environments, and it is therefore important to measure the LF in a variety of environments.…”

Section: Introductionmentioning

confidence: 99%

The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

Small

Sargent

et al. 1998

ApJ

106

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We measure the field galaxy luminosity function (LF) as a function of color and redshift from z = 0 to z = 0.5 using galaxies from the Norris Survey of the Corona Borealis Supercluster. The data set consists of 603 field galaxies with 0 < z ≤ 0.5 and spans a wide range in apparent magnitude (14.0 m ∼ < r ∼ < 21.5 m ), although our field galaxy LF analysis is limited to 493 galaxies with r ≤ 20.0 m . We use the observed g − r colors of the galaxies to compute accurate corrections to the rest B AB and r bands. We find that our local r-band LF, when normalized to counts in high galactic latitude fields, agrees well with the local LF measured in the Las Campanas Redshift Survey. Our B AB -band local LF, however, does not match the b j -band LF from the Stromlo/APM survey, having a normalization 1.6 times higher. We see compelling evidence that the B AB -band field galaxy LF evolves with redshift. The evolution is strongest for the population of star-forming galaxies with [O II] λ3727 rest-frame equivalent widths greater than 10Å. The population of red, quiescent galaxies shows no sign of evolution to z = 0.5. The evolution of the LF which we observe is consistent with the findings of other faint galaxy redshift surveys. The fraction of galaxies with [O II] emission increases rapidly with redshift, but the fraction of galaxies with strong Hδ absorption, a signature of a burst of star-formation, does not. We thus conclude that the star formation in distant galaxies is primarily long-lived.We also compute the LFs of the Corona Borealis supercluster (z ≈ 0.07, 419 galaxies with 14.1 m ≤ r ≤ 20.0 m ) and the Abell 2069 supercluster (z ≈ 0.11, 1 present address: Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK -2 -318 galaxies with 15.1 m ≤ r ≤ 20.0 m ). The shapes of the two supercluster luminosity functions are broadly similar to the shape of the local luminosity function. However, there are important differences. Both supercluster LFs have an excess of very bright galaxies. In addition, the characteristic magnitude of the Corona Borealis supercluster LF is roughly half a magnitude brighter than that of the local field galaxy LF, and there is a suggestion of an upturn in the LF for galaxies fainter than M(B AB ) ∼ −17 m .

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“…Integrating its density distribution along the LOS, the slopes from our simulations are in agreement with those observed for the surface brightness profiles of the diffuse light in nearby clusters. In the Coma Cluster, Bernstein et al (1995) parameterize the surface brightness as and find that the difb r fuse light is best fitted by . In the Fornax b p Ϫ1.3 ‫ע‬ 0.1 Cluster, the surface brightness profile of the cD envelope of NGC 1399 follows a power law of the form proportional to with (Bicknell et al 1989).…”

mentioning

confidence: 99%

The Diffuse Light in Simulations of Galaxy Clusters

Murante

Arnaboldi

Gerhard³

et al. 2004

ApJ

179

244

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We study the properties of the diffuse light in galaxy clusters forming in a large hydrodynamical cosmological simulation of the L cold dark matter cosmology. The simulation includes a model for radiative cooling, star formation in dense cold gas, and feedback by Type II supernova explosions. We select clusters having mass 14 Ϫ1M 1 10 h M , and study the spatial distribution of their star particles. While most stellar light is concentrated in gravitationally bound galaxies orbiting in the cluster potential, we find evidence for a substantial diffuse component, which may account for the extended halos of light observed around central cD galaxies. We find that more massive simulated clusters have a larger fraction of stars in the diffuse light than the less massive ones. The intracluster light is more centrally concentrated than the galaxy light, and the stars in the diffuse component are on average older than the stars in cluster galaxies, supporting the view that the diffuse light is not a random sampling of the stellar population in the cluster galaxies. We thus expect that at least ∼10% of the stars in a cluster may be distributed as intracluster light, largely hidden thus far because of its very low surface brightness.

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The Luminosity Function of the Coma Cluster Core for -25<M/R<-9.4

Cited by 243 publications

References 37 publications

Surface [ITAL]BR[/ITAL] Photometry of Newly Discovered Dwarf Elliptical Galaxies in the Nearby Sculptor and Centaurus A Groups

Surface [ITAL]BR[/ITAL] Photometry of Newly Discovered Dwarf Elliptical Galaxies in the Nearby Sculptor and Centaurus A Groups

The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

The Diffuse Light in Simulations of Galaxy Clusters

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