Mid-Infrared Evidence for Accelerated Evolution in Compact Group Galaxies

Walker, Lisa May; Johnson, K. E.; Gallagher, S. C.; Hibbard, J. E.; Hornschemeier, A. E.; Tzanavaris, P.; Charlton, Jane C.; Jarrett, T. H.

doi:10.1088/0004-6256/140/5/1254

Cited by 50 publications

(81 citation statements)

References 34 publications

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“…Our results are also consistent with previous studies of the galaxy SFR in compact groups, such as Walker et al (2010) and Tzanavaris et al (2010). The differences between the luminosity function of galaxies in CGs and LGs also support a scenario where low luminosity galaxies merge efficiently leading to both a smaller Fig.…”

Section: Conclusion and Discussionsupporting

confidence: 94%

“…Deng et al (2008) compared the properties of CGs, isolated, and field galaxies and found that, in dense regions, galaxies have A&A 543, A119 (2012) preferentially greater concentration indexes and early-type morphologies. There have been numerous studies of the star formation in CGs: Walker et al (2010) suggested that the compact group environment accelerates the evolution of galaxies from star-forming to quiescent; Bitsakis et al (2010) found a connection between dynamical state and the star formation rate (SFR) in the sense that old CGs host late-type galaxies with slightly lower specific star formation rates than in dynamically young groups; Johnson et al (2007) also found a connection between the star formation and the global properties of groups. Tzanavaris et al (2010) estimated the SFR using both ultraviolet and infrared information and found that the compact group environment accelerates the galaxy evolution by enhancing the star formation processes and favouring a fast transition to quiescence.…”

Section: Introductionmentioning

confidence: 99%

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Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2012

A&A

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Aims. We compare the properties of galaxies in compact groups, loose groups, and the field to deepen our understanding of the physical mechanisms acting upon galaxy evolution in different environments. Methods. We select samples of galaxies in compact groups, loose groups, and field galaxies from the Sloan Digital Sky Survey. We compare the properties of the galaxy populations in these different environments: absolute magnitude, colour, size, surface brightness, stellar mass, and concentration. We also study the fraction of red and early-type galaxies, the luminosity function, the colourluminosity, and luminosity-size relations.Results. The population of galaxies in compact groups differ from that of loose groups and the field. The fraction of red and early-type galaxies is larger in compact groups. Galaxies in compact groups are, on average, systematically smaller in size, more concentrated, and have higher surface brightnesses than galaxies in the field and in loose groups. At a fixed absolute magnitude, or fixed surface brightness, galaxies in compact groups are smaller in size. Conclusions. The physical mechanisms that transform galaxies into earlier types could be more effective within compact groups, owing to the typically high densities and small velocity dispersions of these environments, which could explain the large fraction of red and early-type galaxies we found in compact groups. Galaxies inhabiting compact groups have undergone a major transformation compared to galaxies that inhabit loose groups.

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Section: Conclusion and Discussionsupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2012

A&A

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“…However, our test indicates that this is not the main mechanism. Recent studies, based on UV and IR data, have also found a bimodality (gap) in the distribution of SSFR in HCG galaxies and suggested that the high-density environment of CGs has accelerated the evolution of galaxies, transforming star-forming galaxies into quiescent galaxies (Johnson et al 2007;Tzanavaris et al 2010;Walker et al 2010;Bitsakis et al 2010Bitsakis et al , 2011. According to our analysis, galaxies in the HCG have shorter SFTS than in the CIG because they have experienced higher astration rates.…”

Section: Discussionsupporting

confidence: 62%

The star formation histories of Hickson compact group galaxies

Plauchu-Frayn

Olmo

Coziol

et al. 2012

A&A

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Aims. We study the star formation fistory (SFH) of 210 galaxy members of 55 Hickson compact groups (HCG) and 309 galaxies from the Catalog of Isolated Galaxies (CIG). The SFH traces the variation of star formation over the lifetime of a galaxy, and consequently yields a snapshot picture of its formation. Comparing the SFHs in these extremes in galaxy density allows us to determine the main effects of compact groups (CG) on the formation of galaxies. Methods. We fit our spectra using the spectral synthesis code STARLIGHT and obtained the stellar population contents and mean stellar ages of HCG and CIG galaxies in three different morphological classes: early-type galaxies (EtG), early-type spirals (EtS), and late-type spirals (LtS). Results. We find that EtG and EtS galaxies in HCG show higher contents of old and intermediate stellar populations as well as an important deficit of the young stellar population, which clearly implies an older average stellar age in early galaxies in HCG. For LtS galaxies we find similar mean values for the stellar content and age in the two samples. However, we note that LtS can be split into two subclasses, namely old and young LtS. In HCG we find a higher fraction of young LtS than in the CIG sample, in addition, most of these galaxies belong to groups in which most of the galaxies are also young and actively forming stars. The specific star formation rate (SSFR) of spiral galaxies in the two samples differ. The EtS in HCG show lower SSFR values, while LtS peak at higher values compared with their counterparts in isolation. We also measured the shorter star formation time scale (SFTS) in HCG galaxies, which indicates that they have a shorter star formation activity than CIG galaxies. We take these observations as evidence that galaxies in CG have evolved more rapidly than galaxies in isolation, regardless of their morphology. Our observations are consistent with the hierarchical galaxy formation model, which states that CGs are structures that formed recently from primordial small-mass density fluctuations. From the systematic difference in SFTS we deduce that the HCG have most probably formed ∼3 Gyr in the past. The galaxies in the HCG are not in equilibrium state, but merging without gas (i.e., under dissipationless conditions), which may explain their relatively long lifetime.

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“…This in turn likely leads to fast consumption of the available gas and abrupt quenching. The observational signatures of this are "gaps" both in mid-infrared colors (Johnson et al 2007;Walker et al 2010Walker et al , 2012 as well as massnormalized star formation rates (specific SFRs, sSFRs, Tzanavaris et al 2010;L. Lenkic et al 2015, in preparation).…”

Section: Introductionmentioning

confidence: 99%

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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We obtain total galaxy X-ray luminosities, L X , originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of our galaxies, we find that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, we find that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the ±1σ scatter of the Mineo et al. L X -star formation rate (SFR) correlation or have higher L X than predicted by this correlation for their SFR. We discuss how these "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies are consistent with the Boroson et al. L X -stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low-or high-mass XRBs, we use appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L X values. We find that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L X values can be observed due to strong XRB variability.

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Mid-Infrared Evidence for Accelerated Evolution in Compact Group Galaxies

Cited by 50 publications

References 34 publications

Comparing galaxy populations in compact and loose groups of galaxies

Comparing galaxy populations in compact and loose groups of galaxies

The star formation histories of Hickson compact group galaxies

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

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