The galaxy population of Abell 1367: the stellar mass-metallicity relation★

Mouhcine, M.; Kriwattanawong, Wichean; James, P. A.

doi:10.1111/j.1365-2966.2010.17993.x

Cited by 6 publications

(4 citation statements)

References 89 publications

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“…These differences are in agreement with previous findings on the color-magnitude diagrams of these clusters (e.g. Mouhcine et al 2011;Terlevich et al 2001). We note that in all clusters there are some SF galaxies with red colors and that the SF dwarfs at R ≤ R 200 span the whole color range.…”

Section: The Galaxy Samplesupporting

confidence: 93%

“…We have found that this galaxy mass estimate is consistent with the mass we derived using the k-correct algorithm (Blanton & Roweis 2007). We also have found a good agreement between the MPA-JHU mass estimates and Mouhcine et al (2011) galaxy masses, derived by K band imaging, for 7 galaxies of our sample that belong also to the sample of Mouhcine et al (2011).…”

Section: Spectroscopic Propertiessupporting

confidence: 87%

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Environmental Effects on the Metal Enrichment of Low Mass Galaxies in Nearby Clusters

Petropoulou,

Vilchez,

Iglesias-Paramo

2012

Preprint

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In this paper we study the chemical history of low-mass star-forming (SF) galaxies in the local Universe clusters Coma, A1367, A779, and A634. The aim of this work is to search for the imprint of the environment on the chemical evolution of these galaxies. Galaxy chemical evolution is linked to the star formation history (SFH), as well as to the gas interchange with the environment, and low-mass galaxies are well known to be vulnerable systems to environmental processes affecting both these parameters. For our study we have used spectra from the SDSS-III DR8. We have examined the spectroscopic properties of SF galaxies of stellar masses 10 8 − 10 10 M ⊙ , located from the core to the cluster's outskirts. The gas-phase O/H and N/O chemical abundances have been derived using the latest empirical calibrations. We have examined the mass-metallicity relation of cluster galaxies finding well defined sequences. The slope of these sequences, for galaxies in low-mass clusters and galaxies at large cluster-centric distances, follows the predictions of recent hydrodynamic models. A flattening of this slope has been observed for galaxies located in the core of the two more massive clusters of the sample, principally in Coma, suggesting that the imprint of the cluster environment on the chemical evolution of SF galaxies should be sensitive to both the galaxy mass and the host cluster mass. The HI gas content of Coma and A1367 galaxies indicate that low-mass SF galaxies, located at the core of these clusters, have been severely affected by ram-pressure stripping. The observed mass-dependent enhancement of the metal content of low-mass galaxies in dense environments seems plausible, according to hydrodynamic simulations. This enhanced metal enrichment could be produced by the combination of effects such as wind reaccretion, due to pressure cofinement by the intracluster medium (ICM), and the truncation of gas infall, as a result of the ram-pressure stripping. Thus, the properties of the ICM should play an important role in the chemical evolution of low-mass galaxies in clusters.

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Section: The Galaxy Samplesupporting

confidence: 93%

Section: Spectroscopic Propertiessupporting

confidence: 87%

Environmental Effects on the Metal Enrichment of Low Mass Galaxies in Nearby Clusters

Petropoulou,

Vilchez,

Iglesias-Paramo

2012

Preprint

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“…But as Boselli et al (2004) note MIR dust re-emission is more intense in massive quiescent galaxies than in star forming metal poor ones. CGCG 97-079 is both a dwarf and metal poor (F e/H = -0.62 Mouhcine et al 2011). However, while contamination by dust re-emission is significant at mid infrared (MIR) wavelengths (including the 6.75 µm and 15 µm) it is minimal in the Spitzer 3.6µm and 4.5µm (Fazio 2005;Utomo et al 2014;Meidt et al 2014).…”

Section: The Old Stellar Componentmentioning

confidence: 99%

Highly perturbed molecular gas in infalling cluster galaxies: the case of CGCG97-079

Scott

Usero

Brinks

et al. 2015

Mon. Not. R. Astron. Soc.

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We report on CO (J = 2 → 1) mapping with the IRAM 30-m HERA receiver array of CGCG 97-079, an irregular galaxy in the merging galaxy cluster Abell 1367 (z = 0.022). We find that ∼ 80% of the detected CO (J = 2 → 1) is projected within a 16 arcsec 2 (6.5 kpc 2 ) region to the north and west of the optical/NIR centre, with the intensity maximum offset ∼ 10 arcsec (4 kpc) NW of the optical/NIR centre and ∼ 7 arcsec (3 kpc) south-east of the H i intensity maximum. Evolutionary synthesis models indicate CGCG 97-079 experienced a burst of star formation ∼ 10 8 yr ago, most likely triggered by a tidal interaction with CGCG 97-073. For CGCG 97-079 we deduce an infall velocity to the cluster of ∼ 1000 km s −1 and moderate ram pressure (P ram ≈ 10 −11 dyn cm −2 ). The observed offset in CGCG 97-079 of the highest density H i and CO (J = 2 → 1) from the stellar components has not previously been observed in galaxies currently undergoing ram pressure stripping, although previous detailed studies of gas morphology and kinematics during ram pressure stripping were restricted to significantly more massive galaxies with deeper gravitational potential wells. We conclude the observed cold gas density maxima offsets are most likely the result of ram pressure and/or the high-speed tidal interaction with CGCG 97-073. However ram pressure stripping is likely to be playing a major role in the perturbation of lower density gas.

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“…In addition to the mass of a galaxy, its environment is one of the main independent factors when it comes to galaxy evolution, and as such has been studied extensively in the context of the MZR (Trager et al 2000;Kuntschner et al 2001;Thomas et al 2005Thomas et al , 2010Sheth et al 2006;Sánchez-Blázquez et al 2006;Pasquali et al 2010;Zhang et al 2018). It has been found that while the environment has a significant influence on the morphology, age, and star formation activity of a galaxy, its direct contribution to the shape of the MZR is small (Thomas et al 2010;Mouhcine et al 2011;Fitzpatrick & Graves 2015;Sybilska et al 2017). Peng et al (2015) and Trussler et al (2020), however, find that dwarf satellite galaxies in high-density environments are more metal rich compared to dwarfs residing in lower density environments.…”

Section: Introductionmentioning

confidence: 99%

Radial velocities and stellar population properties of 56 MATLAS dwarf galaxies observed with MUSE

Heesters

Müller

Marleau

et al. 2023

A&A

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Dwarf galaxies have been extensively studied in the Local Group, in nearby groups, and selected clusters, giving us a robust picture of their global stellar and dynamical properties, such as their circular velocity, stellar mass, surface brightness, age, and metallicity in particular locations in the Universe. Intense study of these properties has revealed correlations between them, called the scaling relations, including the well-known universal stellar mass-metallicity relation. However, since dwarfs play a role in a vast range of different environments, much can be learned about galaxy formation and evolution through extending the study of these objects to various locations. We present MUSE spectroscopy of a sample of 56 dwarf galaxies as a follow-up to the MATLAS survey in low- to moderate-density environments beyond the Local Volume. The dwarfs have stellar masses in the range of M*/M⊙ = 106.1–109.4 and show a distance range of D = 14–148 Mpc, the majority of which (75%) are located in the range targeted by the MATLAS survey (10–45 Mpc). We thus report a 75% success rate for the semi-automatic identification of dwarf galaxies (79% for dwarf ellipticals) in the MATLAS survey on the subsample presented here. Using pPXF full spectrum fitting, we determine their line-of-sight velocity and can match the majority of them with their massive host galaxy. Due to the observational setup of the MATLAS survey, the dwarfs are located in the vicinity of massive galaxies. Therefore, we are able to confirm their association through recessional velocity measurements. Close inspection of their spectra reveals that ∼30% show clear emission lines, and thus star formation activity. We estimate their stellar population properties (age and metallicity) and compare our results with other works investigating Local Volume and cluster dwarf galaxies. We find that the dwarf galaxies presented in this work show a systematic offset from the universal stellar mass-metallicity relation toward lower metallicities at the same stellar mass. A similar deviation is present in other works in the stellar mass range probed in this work and might be attributed to the use of different methodologies for deriving the metallicity.

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The galaxy population of Abell 1367: the stellar mass-metallicity relation★

Cited by 6 publications

References 89 publications

Environmental Effects on the Metal Enrichment of Low Mass Galaxies in Nearby Clusters

Environmental Effects on the Metal Enrichment of Low Mass Galaxies in Nearby Clusters

Highly perturbed molecular gas in infalling cluster galaxies: the case of CGCG97-079

Radial velocities and stellar population properties of 56 MATLAS dwarf galaxies observed with MUSE

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