The<i>r'</i>-band luminosity function of Abell 1367: A comparison with Coma

Iglésias-Páramo, J.; Boselli, A.; Gavazzi, G.; Cortese, Luca; Vı́lchez, J. M.

doi:10.1051/0004-6361:20021553

Cited by 30 publications

(34 citation statements)

References 43 publications

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“…Wolf 1901; see Biviano 1998 and reference therein; and for recent studies, see e.g. Andreon & Cuillandre 2002;Beijersbergen et al 2002;Iglesias-Páramo et al 2003;Jenkins et al 2007;Lobo et al 1997;Milne et al 2007;Smith et al 2008;Terlevich et al 2001;Trentham 1998). Using CFH12K and Megacam data we now have a good statistical view of the faintest galaxies existing in the Coma cluster (M R ∼ −9.5).…”

Section: Introductionmentioning

confidence: 76%

Very deep spectroscopy of the Coma cluster line of sight: exploring new territories

Adami¹,

Brun²,

Biviano

et al. 2009

A&A

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Context. Environmental effects are known to have an important influence on cluster galaxies, but studies at very faint magnitudes (R > 21) are almost exclusively based on imaging. We present here a very deep spectroscopic survey of galaxies on the line of sight to the Coma cluster. Aims. After a series of papers based on deep multi-band imaging of the Coma cluster, we explore spectroscopically part of the central regions of Coma, in order to confirm and generalize previous results, concerning in particular the galaxy luminosity function, red sequence, stellar populations and the most likely formation scenario for the Coma cluster. Methods. We have obtained reliable VIMOS redshifts for 715 galaxies in the direction of the Coma cluster centre in the unprecedented magnitude range 21 ≤ R ≤ 23, corresponding to the absolute magnitude range −14 ≤ M R ≤ −12. Results. We confirm the substructures previously identified in Coma, and identify three new substructures. We detect a large number of groups behind Coma, in particular a large structure at z ∼ 0.5, the SDSS Great Wall, and a large and very young previously unknown structure at z ∼ 0.054, which we named the background massive group (BMG). These structures account for the mass maps derived from a recent weak lensing analysis. The orbits of dwarf galaxies are probably anisotropic and radial, and could originate from field galaxies radially falling into the cluster along the numerous cosmological filaments surrounding Coma. Spectral characteristics of Coma dwarf galaxies show that red or absorption line galaxies have larger stellar masses and are older than blue or emission line galaxies. R ≤ 22 galaxies show less prominent absorption lines than R ≥ 22 galaxies. This trend is less clear for field galaxies, which are similar to R ≥ 22 Coma galaxies. This suggests that part of the faint Coma galaxies could have been recently injected from the field following the NGC 4911 group infall. We present a list of five ultra compact dwarf galaxy candidates which need to be confirmed with high spatial resolution imaging with the HST. We also globally spectroscopically confirm our previous results concerning the galaxy luminosity functions based on imaging down to R = 23 (M R = −12) and find that dwarf galaxies follow a red sequence similar to that drawn by bright Coma galaxies. Conclusions. Spectroscopy of faint galaxies in Coma confirms that dwarf galaxies are very abundant in this cluster, and that they are partly field galaxies that have fallen onto the cluster along cosmological filaments.

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Section: Introductionmentioning

confidence: 76%

Very deep spectroscopy of the Coma cluster line of sight: exploring new territories

Adami¹,

Brun²,

Biviano

et al. 2009

A&A

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“…In fact, Iglesias-Páramo et al (2003) studied two clusters (Coma and Abell 1367) with similar X-ray luminosities and redshifts and found significant differences in their faint-end slopes. The authors suggest that these differences could be explained by differences in the evolutionary state of the two clusters.…”

Section: Comparison With the Literaturementioning

confidence: 99%

Fossil group origins

Zarattini

Aguerri

Sánchéz-Janssen

et al. 2015

A&A

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Context. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm 12 ). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found among the so-called fossil systems. The observed distribution of magnitude gaps is thought to be a consequence of the orbital decay of M * galaxies in massive halos and the associated growth of the central object. As a result, to first order the amplitude of this gap is a good statistical proxy for the dynamical age of a system of galaxies. Fossil and non-fossil systems could therefore have different galaxy populations that should be reflected in their luminosity functions. Aims. In this work we study, for the first time, the dependence of the luminosity function parameters on Δm 12 using data obtained by the fossil group origins (FOGO) project. Methods. We constructed a hybrid luminosity function for 102 groups and clusters at z ≤ 0.25 using both photometric data from the SDSS-DR7 and redshifts from the DR7 and the FOGO surveys. The latter consists of ∼1200 new redshifts in 34 fossil system candidates. We stacked all the individual luminosity functions, dividing them into bins of Δm 12 , and studied their best-fit Schechter parameters. We additionally computed a "relative" luminosity function, expressed as a function of the central galaxy luminosity, which boosts our capacity to detect differences -especially at the bright end. Results. We find trends as a function of Δm 12 at both the bright and faint ends of the luminosity function. In particular, at the bright end, the larger the magnitude gap, the fainter the characteristic magnitude M * . The characteristic luminosity in systems with negligible gaps is more than a factor three brighter than in fossil-like ones. Remarkably, we also find differences at the faint end. In this region, the larger the gap, the flatter the faint-end slope α. Conclusions. The differences found at the bright end support a dissipationless, dynamical friction-driven merging model for the growth of the central galaxy in group-and cluster-sized halos. The differences in the faint end cannot be explained by this mechanism. Other processes -such as enhanced tidal disruption due to early infall and/or prevalence of eccentric orbits -may play a role. However, a larger sample of systems with Δm 12 > 1.5 is needed to establish the differences at the faint end.

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“…r imaging material was used to extract a catalogue of galaxy candidates in Abell 1367 complete to r ∼ 20.5 mag, and to select the targets of the present spectroscopic survey. The majority of the photometric catalogue, covering the northern and western part of Abell 1367, was published by Iglesias-Páramo et al (2003); conversely the southeast catalogue extension will be given in a forthcoming paper. Spectroscopy of Abell 1367 was obtained with the AF2-WYFFOS multi fiber spectrograph at the 4.2 m William Herschel Telescope (WHT) on La Palma (Spain) during 2003, March 27−29.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Multiple merging in the Abell cluster 1367

Cortese

Gavazzi

Boselli

et al. 2004

A&A

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Abstract. We present a dynamical analysis of the central ∼1.3 square degrees of the cluster of galaxies Abell 1367, based on 273 redshift measurements (of which 119 are news). From the analysis of the 146 confirmed cluster members we derive a significantly non-Gaussian velocity distribution, with a mean location C BI = 6484 ± 81 km s −1 and a scale S BI = 891 ± 58 km s −1 . The cluster appears elongated from the North-West to the South-East with two main density peaks associated with two substructures. The North-West subcluster is probably in the early phase of merging into the South-East substructure (∼0.2 Gyr before core crossing). A dynamical study of the two subclouds points out the existence of a group of star-forming galaxies infalling into the core of the South-East subcloud and suggests that two other groups are infalling into the NW and SE subclusters respectively. These three subgroups contain a higher fraction of star-forming galaxies than the cluster core, as expected during merging events. Abell 1367 appears as a young cluster currently forming at the intersection of two filaments.

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Ther'-band luminosity function of Abell 1367: A comparison with Coma

Cited by 30 publications

References 43 publications

Very deep spectroscopy of the Coma cluster line of sight: exploring new territories

Very deep spectroscopy of the Coma cluster line of sight: exploring new territories

Fossil group origins

Multiple merging in the Abell cluster 1367

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