The Influence of Environment on Galaxy Evolution

Vollmer, B.

doi:10.1007/978-94-007-5609-0_5

Cited by 8 publications

(2 citation statements)

References 252 publications

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“…Even more powerful are IFU studies, that are able to reveal the gas that is stripped and ionized and also provide the kinematical and physical properties of the ionized gas as well as the stars (Merluzzi et al 2013, Fumagalli et al 2014. Hydrodynamical simulations of ram pressure stripping describe the formation of these gas tails and their evolution (Abadi et al 1999, Quilis et al 2000, Roediger & Brüggen 2007, Kapferer et al 2008, Tonnesen & Bryan 2012, Tonnesen & Stone 2014, Roediger et al 2014, see reviews by Roediger 2009 andVollmer 2013).…”

Section: Introductionmentioning

confidence: 99%

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

Poggianti

Moretti

Gullieuszik

et al. 2017

ApJ

334

406

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GASP (GAs Stripping Phenomena in galaxies with MUSE) is a new integral-field spectroscopic survey with MUSE at the VLT aiming at studying gas removal processes in galaxies. We present an overview of the survey and show a first example of a galaxy undergoing strong gas stripping. GASP is obtaining deep MUSE data for 114 galaxies at z=0.04-0.07 with stellar masses in the range 10 9.2 -10 11.5 M in different environments (galaxy clusters and groups, over more than four orders of magnitude in halo mass). GASP targets galaxies with optical signatures of unilateral debris or tails reminiscent of gas stripping processes ("jellyfish galaxies"), as well as a control sample of disk galaxies with no morphological anomalies. GASP is the only existing Integral Field Unit (IFU) survey covering both the main galaxy body and the outskirts and surroundings, where the IFU data can reveal the presence and the origin of the outer gas. To demonstrate GASP's ability to probe the physics of gas and stars, we show the complete analysis of a textbook case of a "jellyfish" galaxy, JO206. This is a massive galaxy (9 × 10 10 M ) in a low-mass cluster (σ ∼ 500 km s −1 ), at a small projected clustercentric radius and a high relative velocity, with ≥90kpc-long tentacles of ionized gas stripped away by ram pressure. We present the spatially resolved kinematics and physical properties of gas and stars, and depict the evolutionary history of this galaxy.

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Section: Introductionmentioning

confidence: 99%

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

Poggianti

Moretti

Gullieuszik

et al. 2017

ApJ

334

406

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“…The disruption could be due to halo mass quenching (e.g., Cattaneo et al 2006), the end of cold streams and the development of a hot halo due to shocks (Dekel & Birnboim 2006;Dekel et al 2009), or simply the continued expansion of the virial radius to a point where cooling from the halo to the disk becomes inefficient (i.e., too slow). While other environmental processes may also play a role -for example, ram pressure, stripping, or harassment (see Tonnesen 2011 andVollmer 2013 for recent reviews) -these local considerations cannot explain the global behavior of late-type galaxies as a class.…”

Section: The Evolution Of Late-type Galaxiesmentioning

confidence: 99%

The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies★

Schawinski

Urry

Simmons

et al. 2014

Monthly Notices of the Royal Astronomical Society

649

782

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We use SDSS+GALEX+Galaxy Zoo data to study the quenching of star formation in lowredshift galaxies. We show that the green valley between the blue cloud of star-forming galaxies and the red sequence of quiescent galaxies in the colour-mass diagram is not a single transitional state through which most blue galaxies evolve into red galaxies. Rather, an analysis that takes morphology into account makes clear that only a small population of blue earlytype galaxies move rapidly across the green valley after the morphologies are transformed from disk to spheroid and star formation is quenched rapidly. In contrast, the majority of blue star-forming galaxies have significant disks, and they retain their late-type morphologies as their star formation rates decline very slowly. We summarize a range of observations that lead to these conclusions, including UV-optical colours and halo masses, which both show a striking dependence on morphological type. We interpret these results in terms of the evolution of cosmic gas supply and gas reservoirs. We conclude that late-type galaxies are consistent with a scenario where the cosmic supply of gas is shut off, perhaps at a critical halo mass, followed by a slow exhaustion of the remaining gas over several Gyr, driven by secular and/or environmental processes. In contrast, early-type galaxies require a scenario where the gas supply and gas reservoir are destroyed virtually instantaneously, with rapid quenching accompanied by a morphological transformation from disk to spheroid. This gas reservoir destruction could be the consequence of a major merger, which in most cases transforms galaxies from disk to elliptical morphology, and mergers could play a role in inducing black hole accretion and possibly AGN feedback.

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HUBBLE SPACE TELESCOPEAND HI IMAGING OF STRONG RAM PRESSURE STRIPPING IN THE COMA SPIRAL NGC 4921: DENSE CLOUD DECOUPLING AND EVIDENCE FOR MAGNETIC BINDING IN THE ISM

Kenney

Abramson

Bravo-Alfaro

2015

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Remarkable dust extinction features in the deep HST V and I images of the face-on Coma cluster spiral galaxy NGC 4921 show in unprecedented ways how ram pressure strips the ISM from the disk of a spiral galaxy. New VLA HI maps show a truncated and highly asymmetric HI disk with a compressed HI distribution in the NW, providing evidence for ram pressure acting from the NW. Where the HI distribution is truncated in the NW region, HST images show a well-defined, continuous front of dust that extends over 90 degrees and 20 kpc. This dust front separates the dusty from dust-free regions of the galaxy, and we interpret it as galaxy ISM swept up near the leading side of the ICM-ISM interaction. We identify and characterize 100 pc-1 kpc scale substructure within this dust front caused by ram pressure, including head-tail filaments, C-shaped filaments, and long smooth dust fronts. The morphology of these features strongly suggests that dense gas clouds partially decouple from surrounding lower density gas during stripping, but decoupling is inhibited, possibly by magnetic fields which link and bind distant parts of the ISM.

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The Influence of Environment on Galaxy Evolution

Cited by 8 publications

References 252 publications

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies★

HUBBLE SPACE TELESCOPEAND HI IMAGING OF STRONG RAM PRESSURE STRIPPING IN THE COMA SPIRAL NGC 4921: DENSE CLOUD DECOUPLING AND EVIDENCE FOR MAGNETIC BINDING IN THE ISM

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