Witnessing galaxy preprocessing in the local Universe: the case of a star-bursting group falling into Abell 1367

Cortese, Luca; Gavazzi, G.; Boselli, A.; Franzetti, P.; Kennicutt, R. C.; O'Neil, K.; Sakai, Shoko

doi:10.1051/0004-6361:20064873

Cited by 170 publications

(175 citation statements)

References 90 publications

(150 reference statements)

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“…Indeed, dynamical friction and viscous processes at z 2 proceed on a timescale of <1 Gyr, which is at least one order of magnitude faster than in z ∼ 0 disc galaxies. In overdense environments, such as clusters, ram pressure may also play a role, demolishing the star-forming disc (Cortese et al 2006). Recently, Bundy et al (2010) demonstrated that the colour and morphological transformations should proceed through several separate stages and explored the strengths and weaknesses of several more sophisticated explanations, including environmental effects, internal stabilization, and disc regrowth by means of gas-rich mergers.…”

Section: Timescales For the Quenching Of The Star Formation And Morphmentioning

confidence: 99%

zCOSMOS – 10k-bright spectroscopic sample

Pozzetti

Bolzonella

Zucca

et al. 2010

A&A

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425

309

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We present the galaxy stellar mass function (GSMF) to redshift z 1, based on the analysis of about 8500 galaxies with I < 22.5 (AB mag) over 1.4 deg 2 , which are part of the zCOSMOS-bright 10k spectroscopic sample. We investigate the total GSMF, as well as the contributions of early-and late-type galaxies (ETGs and LTGs, respectively), defined by different criteria (broad-band spectral energy distribution, morphology, spectral properties, or star formation activities). We unveil a galaxy bimodality in the global GSMF, whose shape is more accurately represented by 2 Schechter functions, one linked to the ETG and the other to the LTG populations. For the global population, we confirm a mass-dependent evolution ("mass-assembly downsizing"), i.e., galaxy number density increases with cosmic time by a factor of two between z = 1 and z = 0 for intermediate-to-low mass (log(M/M ) ∼ 10.5) galaxies but less than 15% for log(M/M ) > 11. We find that the GSMF evolution at intermediateto-low values of M (log(M/M ) < 10.6) is mostly explained by the growth in stellar mass driven by smoothly decreasing star formation activities, despite the redder colours predicted in particular at low redshift. The low residual evolution is consistent, on average, with ∼0.16 merger per galaxy per Gyr (of which fewer than 0.1 are major), with a hint of a decrease with cosmic time but not a clear dependence on the mass. From the analysis of different galaxy types, we find that ETGs, regardless of the classification method, increase in number density with cosmic time more rapidly with decreasing M, i.e., follow a top-down building history, with a median "building redshift" increasing with mass (z > 1 for log(M/M ) > 11), in contrast to hierarchical model predictions. For LTGs, we find that the number density of blue or spiral galaxies with log(M/M ) > 10 remains almost constant with cosmic time from z ∼ 1. Instead, the most extreme population of star-forming galaxies (with high specific star formation), at intermediate/high-mass, rapidly decreases in number density with cosmic time. Our data can be interpreted as a combination of different effects. Firstly, we suggest a transformation, driven mainly by SFH, from blue, active, spiral galaxies of intermediate mass to blue quiescent and subsequently (1−2 Gyr after) red, passive types of low specific star formation. We find an indication that the complete morphological transformation, probably driven by dynamical processes, into red spheroidal galaxies, occurred on longer timescales or followed after 1−2 Gyr. A continuous replacement of blue galaxies is expected to be accomplished by low-mass active spirals increasing their stellar mass. We estimate the growth rate in number and mass density of the red galaxies at different redshifts and masses. The corresponding fraction of blue galaxies that, at any given time, is transforming into red galaxies per Gyr, due to the quenching of their SFR, is on average ∼25% for log(M/M ) < 11. We conclude that the build-up of galaxies and in particular of...

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Section: Timescales For the Quenching Of The Star Formation And Morphmentioning

confidence: 99%

zCOSMOS – 10k-bright spectroscopic sample

Pozzetti

Bolzonella

Zucca

et al. 2010

A&A

Self Cite

425

309

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“…McGee et al 2009;Berrier et al 2009). Observational evidence has been found from the identification of groups embedded in the large-scale structure of clusters (Cortese et al 2006;Tanaka et al 2007;Ziparo et al 2012;Eckert et al 2014). This would explain, as already suggested by , the decreasing light contribution of the central brightest galaxies in clusters: BCGs would form in low-mass systems and then become bright galaxies in clusters as part of the hierarchical structure formation (Merritt 1985;Edge 1991;De Lucia & Blaizot 2007;De Lucia et al 2012).…”

Section: Richness and Bcg Contributionmentioning

confidence: 99%

The XXL Survey

Ziparo

Smith

Mulroy

et al. 2016

A&A

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Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, L K,500 − M 500,WL , for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M 500,WL = 3.5 × 10 13 M . This allows us to investigate whether the slope of the L K − M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M 500,WL = 0.35−12.10 × 10 14 M , at 0 < z < 0.6. The K-band luminosity scales as log 10 (L K,500 /10 12 L ) ∝ β log 10 (M 500,WL /10 14 M ) with β = 0.85 +0.35 −0.27 and an intrinsic scatter of σ ln L K |M = 0.37 +0.19 −0.17 . Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05 +0.16 −0.14 and an intrinsic scatter of 0.14 +0.09 −0.07 . The flattening in the L K − M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies.

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“…In addition to atomic gas pulled from the parent galaxies, these collisional debris actually contain surprisingly large amounts of molecular gas formed in-situ (Braine et al 2000(Braine et al , 2001Lisenfeld et al 2002Lisenfeld et al , 2004Petitpas & Taylor 2005;Duc et al 2007). As the gas subsequently collapses, starforming regions are created with masses ranging from a few hundred solar masses, creating OB associations, the "emission line dots" (Gerhard et al 2002;Yoshida et al 2002;Sakai et al 2002;Weilbacher et al 2003;Ryan-Weber et al 2004;Mendes de Oliveira et al 2004;Cortese et al 2006;Werk et al 2008Werk et al , 2010 to objects as massive as dwarf galaxies named tidal dwarf galaxies (TDGs, Duc 1995;Duc & Mirabel 1998;Duc et al 2000Duc et al , 2007Hancock et al 2007Hancock et al , 2009). These objects, A&A 533, A19 (2011) even though formed from material once pertaining to their parent galaxies, have a radically different and simpler environment.…”

Section: Introductionmentioning

confidence: 99%

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Boquien¹,

Lisenfeld²,

Duc³

et al. 2011

A&A

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Context. Recent studies have shown that star formation in mergers does not seem to follow the same Schmidt-Kennicutt relation as in spiral disks, presenting a higher star formation rate (SFR) for a given gas column density. Aims. In this paper we study why and how different models of star formation arise. To do so we examine the process of star formation in the interacting system Arp 158 and its tidal debris. Methods. We perform an analysis of the properties of specific regions of interest in Arp 158 using observations tracing the atomic and the molecular gas, star formation, the stellar populations as well as optical spectroscopy to determine their exact nature and their metallicity. We also fit their spectral energy distribution with an evolutionary synthesis code. Finally, we compare star formation in these objects to star formation in the disks of spiral galaxies and mergers. Results. Abundant molecular gas is found throughout the system and the tidal tails appear to have many young stars compared to their old stellar content. One of the nuclei is dominated by a starburst whereas the other is an active nucleus. We estimate the SFR throughout the systems using various tracers and find that most regions follow closely the Schmidt-Kennicutt relation seen in spiral galaxies with the exception of the nuclear starburst and the tip of one of the tails. We examine whether this diversity is due to uncertainties in the manner the SFR is determined or whether the conditions in the nuclear starburst region are such that it does not follow the same Schmidt-Kennicutt law as other regions. Conclusions. Observations of the interacting system Arp 158 provide the first evidence in a resolved fashion that different star-forming regions in a merger may be following different Schmidt-Kennicutt laws. This suggests that the physics of the interstellar medium at a scale no larger than 1 kpc, the size of the largest gravitational instabilities and the injection scale of turbulence, determines the origin of these laws.

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Witnessing galaxy preprocessing in the local Universe: the case of a star-bursting group falling into Abell 1367

Cited by 170 publications

References 90 publications

zCOSMOS – 10k-bright spectroscopic sample

zCOSMOS – 10k-bright spectroscopic sample

The XXL Survey

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

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