Evidence for galaxy-galaxy interactions as an active agent of the 'Butcher-Oemler' effect at a redshift of 0.2

Lavery, R. J.; Henry, J. P.

doi:10.1086/166496

Cited by 144 publications

(132 citation statements)

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“…In group environments with relatively low velocity dispersion, it has been known that interactions between member galaxies are more frequent (Toomre & Toomre 1972;Lavery & Henry 1988;Byrd & Valtonen 1990;Mamon 1990). This is supported by HI surveys of galaxies in the Ursa Major cluster in which a large fraction of galaxies show evidence of tidal interactions (see Verheijen & Sancisi 2001;Verheijen & Zwaan 2001;Verheijen 2004;Wolfinger et al 2013).…”

Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using SDSS-DR7 and NASA/IPAC Extragalactic Database spectroscopic data, we identify 166 galaxies as members of the Ursa Major cluster with M r < −13.5 mag. We morphological classify all galaxies by means of carefully inspecting g−, r−, i−band colour and monochromatic images. We show that the Ursa Major cluster is dominated by late-type galaxies, but also contains a significant number of earlytype galaxies, particularly in the dwarf regime. We present further evidence for the existence of several subgroups in the cluster, consistent with previous findings. The early-type fraction is found to correlate with the mass of the subgroup. We also investigate environmental effects by comparing the properties of the Ursa Major early-type dwarf galaxies to those of the Virgo cluster. In contrast to the Virgo, the red sequence of the Ursa Major cluster is only sparsely populated in the optical and ultraviolet colour-magnitude relations. It also shows a statistically significant gap between −18 < M r < −17 mag, i.e. the Ursa Major cluster lacks early-type dwarf galaxies at the bright end of their luminosity function. We discover that the majority of early-type dwarf galaxies in the Ursa Major cluster have blue cores with hints of recent or ongoing star formation. We suggest that gravitational tidal interactions can trigger central blue star forming regions in early-type dwarfs. After that, star formation would only fade completely when the galaxies experience ram pressure stripping or harassment, both of which are nearly absent in the Ursa Major cluster.

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Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Processes that are expected to operate best in lower-σ environments, where the lower relative velocities between galaxies allow them to interact more effectively, include mergers and galaxy-galaxy interactions (Toomre & Toomre 1972;Icke 1985;Lavery & Henry 1988;Byrd & Valtonen 1990;Mihos 2004). Those expected to work best in higher-σ environments, either directly because of the high velocities, the deeper potential * Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution; and based on data collected at the Magellan Telescope, which is operated by the Carnegie Observatories.…”

Section: Introductionmentioning

confidence: 99%

The Environmental Dependence of the Evolving S0 Fraction

Just

Zaritsky

Sand

et al. 2010

ApJ

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We re-investigate the dramatic rise in the S0 fraction, f S0 , within clusters since z ∼ 0.5. In particular, we focus on the role of the global galaxy environment on f S0 by compiling, either from our own observations or the literature, robust line-of-sight velocity dispersions, σ s, for a sample of galaxy groups and clusters at 0.1 < z < 0.8 that have uniformly determined, published morphological fractions. We find that the trend of f S0 with redshift is twice as strong for σ < 750 km s −1 groups/poor clusters than for higher-σ , rich clusters. From this result, we infer that over this redshift range galaxy-galaxy interactions, which are more effective in lower-σ environments, are more responsible for transforming spiral galaxies into S0's than galaxy-environment processes, which are more effective in higher-σ environments. The rapid, recent growth of the S0 population in groups and poor clusters implies that large numbers of progenitors exist in low-σ systems at modest redshifts (∼0.5), where morphologies and internal kinematics are within the measurement range of current technology.

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“…(Dressler & Gunn 1982, 1992Lavery & Henry 1986, 1988Fabricant et al 1991;Poggianti et al 1999Poggianti et al , 2006Ellingson et al 2001), has been extended to groups (Allington-Smith et al 1993;Wilman et al 2005a;Gerke et al 2007;Cucciati et al 2009b), and critically discussed in the context of selection biases (Andreon & Ettori 1999;Andreon et al 2004Andreon et al , 2006.…”

Section: Introductionmentioning

confidence: 99%

The zCOSMOS redshift survey: how group environment alters global downsizing trends

Iovino¹,

Cucciati

Scodeggio

et al. 2009

A&A

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Context. Groups of galaxies are a common environment, bridging the gap between starforming field galaxies and quiescent cluster galaxies. Within groups secular processes could be at play, contributing to the observed strong decrease of star formation with cosmic time in the global galaxy population. Aims. We took advantage of the wealth of information provided by the first ∼10 000 galaxies of the zCOSMOS-bright survey and its group catalogue to study in detail the complex interplay between group environment and galaxy properties. Methods. The classical indicator F blue , i.e., the fraction of blue galaxies, proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples, divided as to define groups/field/isolated galaxy subsamples. Results. Using rest-frame evolving B-band volume-limited samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a systematic difference (a lower F blue ) with respect to the global galaxy population, and an even larger difference with respect to the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By carefully focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored, i.e., log(M * /M ) ≤ 10.6, does a significant residual difference in color remain as a function of environment, while this difference becomes negligible toward higher masses. Conclusions. Our results indicate that red galaxies of mass log(M * /M ) ≥ 10.8 are already in place at z ∼ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called nature or internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ∼ 1, we observe the emergence in groups of a population of nurture red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution. Our analysis implies that these mechanisms begin to significantly influence galaxy evolution after z ∼ 1, a redshift corresponding to the emergence of structures in which these mechanisms take place.

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Evidence for galaxy-galaxy interactions as an active agent of the 'Butcher-Oemler' effect at a redshift of 0.2

Cited by 144 publications

References 0 publications

The properties of early-type galaxies in the Ursa Major cluster

The properties of early-type galaxies in the Ursa Major cluster

The Environmental Dependence of the Evolving S0 Fraction

The zCOSMOS redshift survey: how group environment alters global downsizing trends

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