Eugenia Díaz-Giménez

Consejo Nacional de Investigaciones Científicas y Técnicas

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Ariel Zandivarez

Consejo Nacional de Investigaciones Científicas y Técnicas

Antonela Taverna

Instituto de Astronomía Teórica y Experimental

G. A. Mamon

Institut d'Astrophysique de Paris

H. Muriel

Universidad Nacional de Córdoba

C. Mendes de Oliveira

Universidade de São Paulo

L. Raul Abramo

Universidade de São Paulo

María José Kanagusuku

Consejo Nacional de Investigaciones Científicas y Técnicas

Héctor J. Martínez

Universidad Nacional de Córdoba

M. V. Alonso

Universidad Nacional de Córdoba

Andrés N. Ruiz

Consejo Nacional de Investigaciones Científicas y Técnicas

Cooperative Institutions

Valongo Observatory

Universidade de São Paulo

Consejo Nacional de Investigaciones Científicas y Técnicas

Instituto de Astronomía Teórica y Experimental

National Observatory

Consejo Superior de Investigaciones Científicas

Universidad Nacional de Córdoba

Argentine National Observatory

Centre National de la Recherche Scientifique

Museu de Astronomia e Ciências Afins

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Fossil groups in the Millennium Simulation - Evolution of the brightest galaxies

Astronomy and Astrophysics (2008)

Eugenia Díaz-Giménez H. Muriel C. Mendes de Oliveira

Aims. We create a catalogue of simulated fossil groups and study their properties, in particular the merging histories of their first-ranked galaxies. We compare the simulated fossil group properties with those of both simulated non-fossil and observed fossil groups. Methods. Using simulations and a mock galaxy catalogue, we searched for massive (>5 $\times$ 10$^{13}~h^{-1}~{\cal M}_\odot$) fossil groups in the Millennium Simulation Galaxy Catalogue. In addition, we attempted to identify observed fossil groups in the Sloan Digital Sky Survey Data Release 6 using identical selection criteria. Results. Our predictions on the basis of the simulation data are: (a) fossil groups comprise about 5.5% of the total population of groups/clusters with masses larger than 5 $\times$ 10$^{13}~h^{-1}~{\cal M}_\odot$. This fraction is consistent with the fraction of fossil groups identified in the SDSS, after all observational biases have been taken into account; (b) about 88% of the dominant central objects in fossil groups are elliptical galaxies that have a median R -band absolute magnitude of ~$-23.5{-}5~\log~h$, which is typical of the observed fossil groups known in the literature; (c) first-ranked galaxies of systems with $ {\cal M} >$ 5 $\times$ 10$^{13}~h^{-1}~{\cal M}_\odot$, regardless of whether they are either fossil or non-fossil, are mainly formed by gas-poor mergers; (d) although fossil groups, in general, assembled most of their virial masses at higher redshifts in comparison with non-fossil groups, first-ranked galaxies in fossil groups merged later, i.e. at lower redshifts , compared with their non-fossil-group counterparts. Conclusions. We therefore expect to observe a number of luminous galaxies in the centres of fossil groups that show signs of a recent major merger.

Virial mass

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Fossil groups in the Millennium simulation. From the brightest to the faintest galaxies during the past 8 Gyr

LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) (2015)

María José Kanagusuku Eugenia Díaz-Giménez Ariel Zandivarez

We investigate the evolution of bright and faint galaxies in fossil and non-fossil groups. We used mock galaxies constructed based on the Millennium run simulation II. We identified fossil groups at redshift zero according to two different selection criteria, and then built reliable control samples of non-fossil groups that reproduce the fossil virial mass and assembly time distributions. The faint galaxies were defined as having r-band absolute magnitudes in the range [-16,-11]. We analysed the properties of the bright and faint galaxies in fossil and non-fossil groups during the past 8 Gyr. We observed that the brightest galaxy in fossil groups is typically brighter and more massive than their counterparts in control groups. Fossil groups developed their large magnitude gap between the brightest galaxies around 3.5 Gyr ago. The brightest galaxy stellar masses of all groups show a notorious increment at that time. By analysing the behaviour of the magnitude gap between the first and the second, third, and fourth ranked galaxies, we found that at earlier times, fossil groups comprised two large brightest galaxies with similar magnitudes surrounded by much fainter galaxies, while in control groups these magnitude gaps were never as large as in fossils. At early times, fossil groups in the faint population were denser than non-fossil groups, then this trend reversed, and finally they became similar at the present day. The mean number of faint galaxies in non-fossil systems increases in an almost constant rate towards later times, while this number in fossil groups reaches a plateau at $z\sim0.6$ that lasts $\sim 2$ Gyr, and then starts growing again more rapidly. The formation of fossil groups is defined at the very beginning of the groups according to their galaxy luminosity sampling, which could be determined by their merging rate at early times.

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Compact Groups in the SDSS

Revista Mexicana de Astronomia y Astrofisica Conference Series (2006)

Eugenia Díaz-Giménez C. J. Ragone H. Muriel Ariel Zandivarez

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Cubing system for individual Quercus spp. trees in forests under management in Puebla, Mexico.

Revista mexicana de ciencias forestales (2017)

Juan Carlos Tamarit Urías Eugenia Díaz-Giménez Gerónimo Quiñonez-Barraza Casimiro Ordóñez-Prado J. C. Monárrez González

Arboriculture

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CATÁLOGOS SINTÉTICOS de Galaxias Y CÚMULOS de Galaxias

Revista Mexicana de Astronomia y Astrofisica Conference Series (2002)

Eugenia Díaz-Giménez M. Merchan H. Muriel D. G. Lambas

Galaxias

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The Nature of Compact Groups of Galaxies from Cosmological Simulations

G. A. Mamon Eugenia Díaz-Giménez

The nature of compact groups (CGs) of galaxies, apparently so dense that the galaxies often overlap, is still a subject of debate: Are CGs roughly as dense in 3D as they appear in projection? Or are they caused by chance alignments of galaxies along the line-of-sight, within larger virialized groups or even longer filamentary structures? The nature of CGs is re-appraised using the z=0 outputs of three galaxy formation models, applied to the dissipationless Millennium Simulation. The same selection criteria are applied to mock galaxy catalogs from these models as have been applied by Hickson and co-workers in redshift space. We find 20 times as many mock CGs as the `HCGs' found by Hickson within a distance corresponding to 9000 km/s. This very low (5%) HCG completeness is caused by Hickson missing groups that were either faint, near the surface brightness threshold, of small angular size, or with a dominant brightest galaxy. We find that most velocity-filtered CGs are physically dense, regardless of the precise threshold used in 3D group size and line-of-sight elongation, and of the galaxy formation model used. This result also holds for mock CGs with the same selection biases as was found for the HCGs.

Line-of-sight

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Compact groups from the Millennium Simulations: I. Nature and properties

arXiv (Cornell University) (2008)

Eugenia Díaz-Giménez Cinthia Ragone-Figueroa H. Muriel G. A. Mamon

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Compact groups from semi-analytical models of galaxy formation -- V: their assembly channels as a function of the environment

arXiv (Cornell University) (2023)

Antonela Taverna Eugenia Díaz-Giménez Ariel Zandivarez Héctor J. Martínez Andrés N. Ruiz

We delved into the assembly pathways and environments of compact groups (CGs) of galaxies using mock catalogues generated from semi-analytical models (SAMs) on the Millennium simulation. We investigate the ability of SAMs to replicate the observed CG environments and whether CGs with different assembly histories tend to inhabit specific cosmic environments. We also analyse whether the environment or the assembly history is more important in tailoring CG properties. We find that about half of the CGs in SAMs are non-embedded systems, 40% are inhabiting loose groups or nodes of filaments, while the rest distribute evenly in filaments and voids, in agreement with observations. We observe that early-assembled CGs preferentially inhabit large galaxy systems (~ 60%), while around 30% remain non-embedded. Conversely, lately-formed CGs exhibit the opposite trend. We also obtain that lately-formed CGs have lower velocity dispersions and larger crossing times than early-formed CGs, but mainly because they are preferentially non-embedded. Those lately-formed CGs that inhabit large systems do not show the same features. Therefore, the environment plays a strong role in these properties for lately-formed CGs. Early-formed CGs are more evolved, displaying larger velocity dispersions, shorter crossing times, and more dominant first-ranked galaxies, regardless of the environment. Finally, the difference in brightness between the two brightest members of CGs is dependent only on the assembly history and not on the environment. CGs residing in diverse environments have undergone varied assembly processes, making them suitable for studying their evolution and the interplay of nature and nurture on their traits.

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Cosmic time

10.48550/arxiv.2311.06721

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Are compact groups hostile towards faint galaxies?

Astronomy and Astrophysics (2014)

Ariel Zandivarez Eugenia Díaz-Giménez C. Mendes de Oliveira Henrique Gubolin

Aims. The goal of this work is to understand whether the extreme environment of compact groups (CGs) can affect the distribution and abundance of faint galaxies around them.

Peculiar galaxy

10.1051/0004-6361/201424677

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Compact groups of galaxies selected by stellar mass: the 2MASS compact group catalogue

Monthly Notices of the Royal Astronomical Society (2012)

Eugenia Díaz-Giménez G. A. Mamon Marcela Pacheco C. Mendes de Oliveira M. V. Alonso

We present a photometric catalogue of compact groups of galaxies (p2MCGs) automatically extracted from the Two-Micron All Sky Survey (2MASS) extended source catalogue. A total of 262 p2MCGs are identified, following the criteria defined by Hickson, of which 230 survive visual inspection (given occasional galaxy fragmentation and blends in the 2MASS parent catalogue). Only one quarter of these 230 groups were previously known compact groups (CGs). Among the 144 p2MCGs that have all their galaxies with known redshifts, 85 (59 per cent) have four or more accordant galaxies. This v2MCG sample of velocity-filtered p2MCGs constitutes the largest sample of CGs (with N ≥ 4) catalogued to date, with both well-defined selection criteria and velocity filtering, and is the first CG sample selected by stellar mass. It is fairly complete up to Kgroup ∼ 9 and radial velocity of ∼6000 km s−1.

Local Group

Stellar mass

10.1111/j.1365-2966.2012.21705.x

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Citations (41)