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

Rines, Kenneth J.; Geller, Margaret J.

doi:10.1088/0004-6256/135/5/1837

Cited by 92 publications

(163 citation statements)

References 77 publications

(196 reference statements)

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“…We can compare our results to those obtained by Rines & Geller (2008) in the r-band within 1 Mpc from M87 since their sampled region closely corresponds to the cluster A definition adopted in this work (<0.8 Mpc). Furthermore both works use membership criteria based on spectroscopic redshifts and are thus only marginally affected by statistical corrections.…”

Section: Figsupporting

confidence: 58%

“…This indicates that the determination of the NUV luminosity function is very robust against statistical uncertainties, making the Virgo cluster the ideal target for such studies in the nearby universe (e.g. Rines & Geller 2008).…”

Section: Applied Statistical Correctionmentioning

confidence: 99%

“…d) The determination of the slope of the UV luminosity function at the faint end strongly depends on poorly constrained statistical corrections in clusters other than Virgo (e.g. Rines & Geller 2008; see Fig. 2).…”

Section: Figmentioning

confidence: 99%

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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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Section: Figsupporting

confidence: 58%

Section: Applied Statistical Correctionmentioning

confidence: 99%

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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“…Moreover, the radial analysis of Rines & Geller (2008) does not present a significant dependence of the LF on clustercentric radius, but opposite trends in the radial variation of M * between Virgo and Abell 2199. Indeed, the characteristic luminosity seems to be fainter at small radii for Abell 2199, while Virgo shows a trend similar to A 85 (see Section 5.1).…”

Section: Environmental Influence On Dwarfsmentioning

confidence: 77%

“…g − r = 1.0 is the typical colour of a 12 Gyr old stellar population with [Fe/H] = +0.25 supersolar metallicity (Worthey 1994). The fraction of cluster members lost due to this colour selection is expected to be very small, and we match at the same time the colour distribution of the nearby Universe (see Hogg et al 2004;Rines & Geller 2008). The brightest cluster galaxy (BCG, α(J2000): 00 h 41 m 50.448 s δ(J2000): −9 • 18 ′ 11.45 ′′ ) is assumed to lie at the centre of the cluster.…”

Section: Target Selection and Spectroscopic Observationsmentioning

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 Impact of Surveys

Rampazzo¹,

D’Onofrio²,

Zaggia³

et al. 2016

From the Realm of the Nebulae to Populations of Galaxies

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International audienceSince the most ancient times astronomers felt the need to collect and list in atlases and catalogs all the visible objects in the sky. The first stellar catalog known in the western world being the one of Hipparchus (second century BC). We have to wait until Charles Messier at the end of the eighteenth century to have the first incidental catalog of nebulae, i.e. including a mixture of fuzzy objects, nebulæ, that telescopes of the epoch could detect. In Chap. 1 we have already discussed the atlases and catalogs that soon after the discovery of galaxies appeared in the literature describing the properties of the nearby galaxies, in particular their morphologies in Chap. 3 . The subject of extragalactic papers, during the photographic plate era, was one or few galaxies, whose properties were carefully scrutinized looking at all the details resolved by telescopes in the optical waveband. This happens also today, of course, basically at all wavelengths. However, the impact of new technologies permits in the last two decades to tackle survey programs addressed to the study of specific extragalactic problems considering millions of galaxies

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

Cited by 92 publications

References 77 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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

The Impact of Surveys

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