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

Agulli, I.; Aguerri, J. A. L.; Sánchéz-Janssen, R.; Vecchia, Claudio Dalla; Diaferio, Antonaldo; Barrena, R.; Palmero, L. Dominguez; Yu, Heng

doi:10.1093/mnras/stw422

Cited by 34 publications

(67 citation statements)

References 72 publications

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“…The large uncertainty in α results from the large observational errors in the LF. This slope is less steep than others from massive clusters (α ∼ −1.5; Agulli et al 2014;Agulli et al 2016) or the field (Blanton et al 2005). Nevertheless, the slope is similar within the uncertainties with the LF in groups of galaxies (α ∼ −1.16; Zandivarez & Martínez 2011) or some dynamically young massive clusters (α ∼ −1.13; Agulli et al 2017).…”

Section: The Spectroscopic Galaxy Luminosity Functionsupporting

confidence: 68%

“…A total of 129 spectroscopic targets were selected and located in two AF2 fiber configurations. We obtained low-resolution spectra (R = 280 and grism R158B) in three exposures of 1800s per pointing, with the spectra reaching S /N > 5 for a secure redshift determination (see e.g., Agulli et al 2016). We also selected targets with g−r < 1.1 and 19.5 < m r < 21.0 to be observed with the OSIRIS@GTC instrument.…”

Section: The Data For Rxj0752436+455653mentioning

confidence: 99%

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Fossil group origins

Aguerri

Longobardi

Zarattini

et al. 2018

A&A

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Context. It is thought that fossil systems are relics of structure formation in the primitive Universe. They are galaxy aggregations that have assembled their mass at high redshift with few or no subsequent accretion. Observationally these systems are selected by large magnitude gaps between their 1st and 2nd ranked galaxies (∆m 12 ). Nevertheless, there is still debate over whether or not this observational criterium selects dynamically evolved ancient systems. Aims. We have studied the properties of the nearby fossil group RXJ075243.6+455653 in order to understand the mass assembly of this system. Methods. Deep spectroscopic observations allow us to construct the galaxy luminosity function (LF) of RXJ075243.6+455653 down to M * r + 6. The analysis of the faint-end of the LF in groups and clusters provides valuable information about the mass assembly of the system. In addition, we have analyzed the nearby large-scale structure around this group. The LF of the group shows a flat faint-end slope (α = −1.08 ± 0.33). This low density of dwarf galaxies is confirmed by the low value of the dwarf-to-giant ratio (DGR = 0.99 ± 0.49) for this system. Both the lack of dwarf galaxies and the low luminosity of the BGG suggests that RXJ075243.6+455653 still has to accrete mass from its nearby environment. This mass accretion will be achieved because it is the dominant structure of a rich environment formed by several groups of galaxies (15) within ∼ 7 Mpc from the group center and with ±1000 km s −1 . Conclusions. RXJ075243.6+455653 is a group of galaxies that has not yet completed the process of its mass assembly. This new mass accretion will change the fossil state of the group. This group is an example of a galaxy aggregation selected by a large magnitude gap but still in the process of the accretion of its mass.

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Section: The Spectroscopic Galaxy Luminosity Functionsupporting

confidence: 68%

Section: The Data For Rxj0752436+455653mentioning

confidence: 99%

Fossil group origins

Aguerri

Longobardi

Zarattini

et al. 2018

A&A

Self Cite

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“…Ferrarese et al (2016) show that the Virgo LF (and also SMF) is significantly shallower than the expected distribution from ΛCDM (a~-1.9, e.g., Springel et al 2008). Other spectroscopic LFs including A85 (Agulli et al 2016) and A2199 (Rines & Geller 2008) are also less steep than the subhalo mass distributions derived from simulations. However, the complexity of the transformation from subhalo mass to luminosity is nontrivial and thus these comparisons are hard to interpret.…”

Section: Comparison Of the Smfs With Simulationsmentioning

confidence: 73%

“…Statistical studies of spectroscopically confirmed cluster members control for some observational biases. Nonetheless, there are few studies that explore the LF (Rines & Geller 2008;Agulli et al 2014Agulli et al , 2016 or the SMF (Ferrarese et al 2016) of spectroscopically identified members. In contrast, there are many studies based on photometrically determined membership (e.g., Barkhouse et al 2007;Moretti et al 2015;Lan et al 2016;Lee & Jang 2016).…”

Section: Introductionmentioning

confidence: 99%

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Sohn¹,

Geller²,

Zahid³

et al. 2017

ApJS

107

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Based on an extensive redshift survey for galaxy clusters Abell 2029 and Coma, we measure the luminosity functions (LFs) and stellar mass functions (SMFs) for the entire cluster member galaxies. Most importantly, we measure the velocity dispersion functions (VDFs) for quiescent members. The MMT/Hectospec redshift survey for galaxies in A2029 identifies 982 spectroscopic members; for 838 members, we derive the central velocity dispersion from the spectroscopy. Coma is the only other cluster surveyed as densely. The LFs, SMFs, and VDFs for A2029 and Coma are essentially identical. The SMFs of the clusters are consistent with simulations. The A2029 and Coma VDFs for quiescent galaxies have a significantly steeper slope than those of field galaxies for velocity dispersion  -100 km s 1 . The cluster VDFs also exceed the field at velocity dispersion  -250 km s 1 . The differences between cluster and field VDFs are potentially important tests of simulations and of the formation of structure in the universe.

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“…The dip magnitude of Abell 2744 is similar to the values in the previous studies, M r ≈ −18 ± 1 mag. It has been suggested that the presence of this gap can be explained by the efficiency of merging of intermediate luminosity galaxies depending on the galaxy density (Miles et al 2004;Mercurio et al 2006;Agulli et al 2016;Lee et al 2016). Low density regions like the galaxy groups, poor galaxy clusters, or outskirt of rich galaxy clusters have a higher efficiency of galaxy merging than that of the high density regions, because they have lower velocity dispersion.…”

Section: Discussion 41 Comparison Of the Galaxy Lfsmentioning

confidence: 99%

Globular Clusters, Ultracompact Dwarfs, and Dwarf Galaxies in Abell 2744 at a Redshift of 0.308

Lee

Jang

2016

ApJ

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We report a photometric study of globular clusters (GCs), ultracompact dwarfs (UCDs), and dwarf galaxies in the giant merging galaxy cluster Abell 2744 at z = 0.308. Color-magnitude diagrams of the point sources derived from deep F814W (restframe r ′ ) and F105W (restframe I) images of Abell 2744 in the Hubble Space Telescope Frontier Field show a rich population of point sources whose colors are similar to those of typical GCs. These sources are as bright as −14.9 < M r ′ ≤ −11.4 (26.0

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

Cited by 34 publications

References 72 publications

Fossil group origins

Fossil group origins

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Globular Clusters, Ultracompact Dwarfs, and Dwarf Galaxies in Abell 2744 at a Redshift of 0.308

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