The Luminosity Function of Low‐Redshift Abell Galaxy Clusters

Barkhouse, W. A.; Yee, H. K. C.; López-Cruz, Omar

doi:10.1086/523257

Cited by 68 publications

(150 citation statements)

References 80 publications

(214 reference statements)

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“…Our best fit parameters are: N = 260 ± 45 gal/mag/deg 2 , M = −21.8 ± 0.2 and α = −0.8 ± 0.1, with a reduced χ 2 = 0.57. The value of M is rather close to the value found by Barkhouse et al (2007) (M * = −22.36, obtained with a fixed the faint end slope α = −1) and is typical for rich clusters. The faint end slope is found slightly larger than the canonical value α = −1 but it has a large uncertainty associated to the background corrections in our sample S3.…”

Section: The Luminosity Function Of a 1413supporting

confidence: 88%

Deep optical observations of the massive galaxy cluster Abell 1413

Castagne

Soucail

Pointecouteau

et al. 2012

A&A

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Aims. We investigate the morphology and dynamics of the massive nearby galaxy cluster Abell 1413. Methods. Using wide field imaging and spectroscopic data obtained from observations at the Canada-France-Hawaii Telescope and archival SDSS data, we build a sample of more than 250 galaxies covering a region centered on the cluster and extending to its outskirts on large scales. Results. We probe the cluster morphology analyzing the projected density distribution of galaxies and find a strong variation in the ellipticity of the distribution, from 0.8 at the center of the cluster down to ∼0.35 at the periphery. This may be the tracer of a prolate global mass distribution, slightly attenuated in the collisional distribution of the gas. We also study the large scale environment, identifying several structures associated to the cluster and organized along the major axis in the North-South direction. From spectroscopic data we derive the velocity dispersion and we investigate the overall dynamics of the cluster. The regular velocity dispersion supports the case for a prolate cluster aligned in the plane of the sky and embedded in a larger scale structure.

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Section: The Luminosity Function Of a 1413supporting

confidence: 88%

Deep optical observations of the massive galaxy cluster Abell 1413

Castagne

Soucail

Pointecouteau

et al. 2012

A&A

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“…Andreon 1998;Popesso et al 2006;Barkhouse, Yee, & López-Cruz 2007). This independence is likely a result of dynamical friction.…”

Section: The Bright End Of the Lfmentioning

confidence: 96%

“…It is a powerful observable to study the characteristics of galaxies and to compare environments of different densities (e.g., Trentham & Hodgkin 2002;Trentham, Sampson, & Banerji 2005;Tully et al 2002;Blanton et al 2003;Infante, Mieske, & Hilker 2003, and references therein). In particular, the faint end seems to be shaped by the environment (e.g., Popesso et al 2006;Barkhouse, Yee, & López-Cruz 2007), making deep spectroscopic study of dwarf galaxies and the comparison between those in field and clusters fundamental. The Schechter function (Schechter 1976) is commonly used to fit the LF of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Agulli¹,

Aguerri²,

Sánchéz-Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a new deep spectroscopic catalogue for Abell 85, within 3.0 × 2.6 Mpc 2 and down to M r ∼ M * r +6. Using the Visible Multi-Object Spectrograph at the Very Large Telescope and the AutoFiber 2 at the William Herschel Telescope, we obtained almost 1430 new redshifts for galaxies with m r ≤ 21 mag and µ e,r ≤ 24 mag arcsec −2 . These redshifts, together with SDSS-DR6 and NED spectroscopic information, result in 460 confirmed cluster members. This data set allows the study of the luminosity function (LF) of the cluster galaxies covering three orders of magnitudes in luminosities. The total and radial LFs are best modelled by a double Schechter function. The normalized LFs show that their bright (M r ≤ −21.5) and faint (M r ≥ −18.0) ends are independent of clustercentric distance and similar to the field LFs unlike the intermediate luminosity range (−21.5 ≤ M r ≤ −18.0). Similar results are found for the LFs of the dominant types of galaxies: red, passive, virialized and early-infall members. On the contrary, the LFs of blue, star-forming, non-virialized and recent-infall galaxies are well described by a single Schechter function. These populations contribute to a small fraction of the galaxy density in the innermost cluster region. However, in the outskirts of the cluster, they have similar densities to red, passive, virialized and early-infall members at the LF faint end. These results confirm a clear dependence of the colour and star formation of Abell 85 members in the cluster centric distance.

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“…The interpretation of this observational result, however, is not straightforward since the different environmental processes can modify in a complex way both the number of objects and the luminosity of the perturbed galaxies. As a first indication we would be tempted to exclude for Virgo the combined effect of dwarf tidal disruption in the core of the cluster and galaxy harassment invoked by Popesso et al (2006), Barkhouse et al (2007), and de Filippis et al (2011) to explain the observed flattening in the core and the steepening in the periphery in the optical luminosity function of nearby clusters. We do not observe in Virgo any radial variations of the luminosity function either in the NUV or in the r-band (Rines & Geller 2008).…”

Section: Figmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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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.

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The Luminosity Function of Low‐Redshift Abell Galaxy Clusters

Cited by 68 publications

References 80 publications

Deep optical observations of the massive galaxy cluster Abell 1413

Deep optical observations of the massive galaxy cluster Abell 1413

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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