The Galaxy Luminosity Functions down to<i>M</i>~ -10 in the Hydra I Cluster

Yamanoi, Hitomi; Tanaka, Masayuki; Hamabe, M.; Yagi, Masafumi; Okamura, S.; Iye, Masanori; Shimasaku, Kazuhiro; Doi, Mamoru; Komiyama, Yutaka; Furusawa, Hisanori

doi:10.1086/518475

Cited by 13 publications

(17 citation statements)

References 55 publications

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“…Sabatini et al 2003;Milne et al 2007, and references therein). The LF of the Hydra I cluster has previously been determined by Yamanoi et al (2007) who find α ∼ −1.6 in the magnitude range −20 < M B,R < −10. This is a steeper slope than reported by Yagi et al (2002) who give α = −1.31 for the faint end slope of the composite LF of 10 nearby clusters (including Hydra I) at −23 < M R < −16.…”

Section: The Galaxy Luminosity Functionmentioning

confidence: 83%

“…Recently, Yamanoi et al (2007) found α ∼ −1.6 for the cluster LF. Our observed fields overlap with their central observed region and we reach a similar limiting magnitude.…”

Section: The Hydra I Lfmentioning

confidence: 98%

“…The dwarf galaxy candidates in Yamanoi et al (2007) were selected only by setting lower limits in FWHM to the SExtractor detections. Contaminating background galaxies were statistically subtracted.…”

Section: The Hydra I Lfmentioning

confidence: 99%

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The early-type dwarf galaxy population of the Hydra I cluster

Misgeld

Mieske

Hilker

2008

A&A

114

199

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Aims. We analyse the properties of the early-type dwarf galaxy population (M V > −17 mag) in the Hydra I cluster. We investigate the galaxy luminosity function (LF), the colour-magnitude relation (CMR), and the magnitude-surface brightness relation down to M V ∼ −10 mag. Another goal of this study is to find candidates for ultra-compact dwarf galaxies (UCDs) in Hydra I. Methods. Two spectroscopic surveys performed with Magellan I/LDSS2 at Las Campanas Observatory and VLT/VIMOS, as well as deep VLT/FORS1 images in V and I bands, covering the central parts of the cluster, were examined. We identify cluster members by radial velocity measurements and select other cluster galaxy candidates by their morphology and low surface brightness. The candidates' total magnitudes and central surface brightnesses were derived from the analysis of their surface brightness profiles. To determine the faint-end slope of the LF, the galaxy number counts are completeness corrected. Results. We obtain radial velocities for 126 objects and identify 32 cluster members, of which 5 are previously uncatalogued dwarf galaxies. One possible UCD candidate with M V = −13.26 mag is found. Our sample of 100 morphologically selected dwarf galaxies with M V > −17 mag defines a CMR that extends the CMR of the giant cluster galaxies to the magnitude limit of our survey (M V ∼ −10 mag). It matches the relations found for the Local Group (LG) and the Fornax cluster dwarf galaxies almost perfectly. The Hydra I dwarf galaxies also follow a magnitude-surface brightness relation that is very similar to that of the LG dwarf galaxies. Moreover, we observe a continuous relation for dwarf galaxies and giant early-type galaxies when plotting the central surface brightness μ 0 of a Sérsic model vs. the galaxy magnitude. The effective radius is found to be largely independent of the luminosity for M V > −18 mag. It is consistent with a constant value of R e ∼ 0.8 kpc. We present the photometric parameters of the galaxies as the Hydra I Cluster Catalogue (HCC). By fitting a Schechter function to the luminosity distribution, we derive a very flat faint-end slope of the LF (α = −1.13 ± 0.04), whereas fitting a power law for M V > −14 mag gives α = −1.40 ± 0.18. Conclusions. Our findings of a continuous CMR and μ 0 − M V relation for dwarf and giant early-type galaxies suggests that they are the same class of objects. The similarity of those relations to other environments like the LG implies that internal processes could be more important for their global photometric properties than external influences.

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Section: The Galaxy Luminosity Functionmentioning

confidence: 83%

“…Recently, Yamanoi et al (2007) found α ∼ −1.6 for the cluster LF. Our observed fields overlap with their central observed region and we reach a similar limiting magnitude.…”

Section: The Hydra I Lfmentioning

confidence: 98%

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The early-type dwarf galaxy population of the Hydra I cluster

Misgeld

Mieske

Hilker

2008

A&A

114

199

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“…As most SNe Ia occur in massive galaxies, it is difficult to assess whether they might also have an enhanced rate in dwarf galaxies because of the large statistical uncertainty on the rate due to the relatively low number of SNe Ia in lowmass hosts (e.g., Quimby et al 2012). SN surveys of rich galaxy clusters are an efficient way to search many low-mass galaxies at once, owing to both a higher sky density of galaxies and the (putative) upturn in the faint-end slope of the cluster luminosity function (e.g., Milne et al 2007;Yamanoi et al 2007). In this work we find that one IC SN Ia may be hosted by a dwarf cluster galaxy, and we discuss the implications of this for SN Ia rates in faint hosts.…”

Section: Sn Ia Rates In Faint Hostsmentioning

confidence: 99%

CONFIRMATION OF HOSTLESS TYPE Ia SUPERNOVAE USINGHUBBLE SPACE TELESCOPEIMAGING

Graham

Sand

Zaritsky

2015

ApJ

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We present deep Hubble Space Telescope imaging at the locations of four, potentially hostless, long-faded Type Ia supernovae (SNe Ia) in low-redshift, rich galaxy clusters that were identified in the Multi-Epoch Nearby Cluster Survey. Assuming a steep faint-end slope for the galaxy cluster luminosity function (a = -1.5 d ), our data includeall but 0.2%of the stellar mass in cluster galaxies (0.005% with a = -1. ) may be either a globular cluster (GC) or a faint dwarf galaxy. We estimate the local surface densities of GCs and dwarfs to show that a GC is more likely, due to the proximity of an elliptical galaxy, but neither can be ruled out. This faint host implies that the SN Ia rate in dwarfs or GCs may be enhanced, but remains within previous observational constraints. We demonstrate that our results do not preclude the use of SNe Ia as bright tracers of IC light at higher redshifts, but that it will be necessary to first refine the constraints on their rate in dwarfs and GCs with deep imaging for a larger sample of low-redshift, apparently hostless SNe Ia.

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“…Because few deep spectroscopic surveys of clusters extend into the dwarf galaxy regime (M r −18; for exceptions, see Mobasher et al 2003;Christlein & Zabludoff 2003;Mahdavi et al 2005, and references therein), cluster membership is usually determined via statistical subtraction of background galaxies (e.g., Popesso et al 2006;Jenkins et al 2007;Milne et al 2007;Adami et al 2007;Yamanoi et al 2007; Barkhouse et al 2007, and references therein). Because galaxy number counts increase much more steeply than cluster member counts (even for very steep faint-end slopes), small systematic uncertainties in background subtraction can produce large uncertainties in the abundance of faint cluster galaxies.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic Determination of the Luminosity Function in the Galaxy Clusters A2199 and Virgo

Rines

Geller

2008

The Astronomical Journal

139

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We report a new determination of the faint end of the galaxy luminosity function (LF) in the nearby clusters Abell 2199 and Virgo using data from the Sloan Digital Sky Survey (SDSS) and the Hectospec multifiber spectrograph on the MMT. The luminosity function of A2199 is consistent with a single Schechter function to M r = −15.6 + 5 log h 70 with a faint-end slope of α = −1.13 ± 0.07 (statistical). The LF in Virgo extends to M r ≈ −13.5 ≈ M * + 8 and has a slope of α = −1.28 ± 0.06 (statistical). The red sequence of cluster members is prominent in both clusters, and almost no cluster galaxies are redder than this sequence. A large fraction of photometric red-sequence galaxies lies behind the cluster. We compare our results to previous estimates and find poor agreement with estimates based on statistical background subtraction but good agreement with estimates based on photometric membership classifications (e.g., colors, morphology, surface brightness). We conclude that spectroscopic data are critical for estimating the faint end of the LF in clusters. The faint-end slope we find is consistent with values found for field galaxies, weakening any argument for environmental evolution in the relative abundance of dwarf galaxies. However, dwarf galaxies in clusters are significantly redder than field galaxies of similar luminosity or mass, indicating that star-formation processes in dwarfs do depend on environment.

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The Galaxy Luminosity Functions down toM~ -10 in the Hydra I Cluster

Cited by 13 publications

References 55 publications

The early-type dwarf galaxy population of the Hydra I cluster

The early-type dwarf galaxy population of the Hydra I cluster

CONFIRMATION OF HOSTLESS TYPE Ia SUPERNOVAE USINGHUBBLE SPACE TELESCOPEIMAGING

Spectroscopic Determination of the Luminosity Function in the Galaxy Clusters A2199 and Virgo

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