H i in group interactions: HCG 44

Hess, Kelley M.; Cluver, Michelle; Yahya, Sahba; Serra, P.; Lucero, D. M.; Passmoor, S. S.; Carignan, C.

doi:10.1093/mnras/stw2338

Cited by 31 publications

(29 citation statements)

References 66 publications

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“…Since the first interferometric observations of the Magellanic Clouds (Kerr, Hindman, & Robinson 1954;Hindman, Kerr, & McGee 1963), and of pairs and group galaxies in our nearest neighborhoods (Roberts 1968;Rots 1975), it was clear that environment can directly remove HI and create striking trails and streams. As showcased in Figure 14, we currently have a plethora of examples of HI stripping in groups, with most of the evidence pointing towards gravitational interactions as primarily responsible for creating these features (e.g., Yun, Ho, & Lo 1994;Hibbard et al 2001;Williams, Yun, & Verdes-Montenegro 2002;Koribalski, Gordon, & Jones 2003;Kantharia et al 2005;English et al 2010;Michel-Dansac et al 2010;Serra et al 2013Serra et al , 2015Leisman et al 2016;Hess et al 2017;de Blok et al 2018;Lee-Waddell et al 2019). This is due to the fact that, in most cases, stellar tidal features and/or peculiar optical morphologies are also clearly visible in these systems, suggesting a prominent role of tidal forces in affecting both their gas and stellar distributions.…”

Section: Hi Stripping In Groupsmentioning

confidence: 99%

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Cortese

Catinella

Smith

2021

Publ. Astron. Soc. Aust.

133

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One of the key open questions in extragalactic astronomy is what stops star formation in galaxies. While it is clear that the cold gas reservoir, which fuels the formation of new stars, must be affected first, how this happens and what are the dominant physical mechanisms involved is still a matter of debate. At least for satellite galaxies, it is generally accepted that internal processes alone cannot be responsible for fully quenching their star formation, but that environment should play an important, if not dominant, role. In nearby clusters, we see examples of cold gas being removed from the star-forming discs of galaxies moving through the intracluster medium, but whether active stripping is widespread and/or necessary to halt star formation in satellites, or quenching is just a consequence of the inability of these galaxies to replenish their cold gas reservoirs, remains unclear. In this work, we review the current status of environmental studies of cold gas in star-forming satellites in the local Universe from an observational perspective, focusing on the evidence for a physical link between cold gas stripping and quenching of the star formation. We find that stripping of cold gas is ubiquitous in satellite galaxies in both group and cluster environments. While hydrodynamical mechanisms such as ram pressure are important, the emerging picture across the full range of dark matter halos and stellar masses is a complex one, where different physical mechanisms may act simultaneously and cannot always be easily separated. Most importantly, we show that stripping does not always lead to full quenching, as only a fraction of the cold gas reservoir might be affected at the first pericentre passage. We argue that this is a key point to reconcile apparent tensions between statistical and detailed analyses of satellite galaxies, as well as disagreements between various estimates of quenching timescales. We conclude by highlighting several outstanding questions where we expect to see substantial progress in the coming decades, thanks to the advent of the Square Kilometre Array and its precursors, as well as the next-generation optical and millimeter facilities.

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Section: Hi Stripping In Groupsmentioning

confidence: 99%

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Cortese

Catinella

Smith

2021

Publ. Astron. Soc. Aust.

133

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“…The dark matter halos of some of these galaxies may overlap and lead them to interact strongly. Such interactions can remove a substantial amount of gas from galaxies to form the intragroup medium (Thilker et al 2004;Chynoweth et al 2008;Mihos et al 2012;Hess et al 2017). In this section we explore the hypothesis that the absorbing gas originates from the tidal debris or from the gas left in between these galaxies.…”

Section: Gas Associated With An Overdensitymentioning

confidence: 99%

Observational signatures of a warped disk associated with cold-flow accretion

Rahmani

Péroux

Augustin

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present MUSE observations of the field of the quasar Q0152−020 whose spectrum shows a Lyman limit system (LLS) at redshift z abs = 0.38, with a metallicity Z 0.06 Z ⊙ . The low ionization metal lines associated with the LLS present two narrow distinct absorption components with a velocity separation of 26 km s −1 . We detect six galaxies within 600 km s −1 from the absorption redshift; their projected distances from the quasar sightline range from 60 to 200 kpc. The optical spectra of five of these galaxies exhibit prominent nebular emission lines, from which we deduce extinctioncorrected star formation rates in the range SFR = 0.06-1.3 M ⊙ yr −1 , and metallicities between 0.2 Z ⊙ and Z ⊙ . The sixth galaxy is only detected in the stellar continuum. By combining our data with archival Keck/HIRES spectroscopy of the quasar and HST/WFPC2 imaging of the field, we can relate absorption line and galaxy kinematics; we conclude that the LLS is most likely associated with the galaxy closest to the quasar sight-line (galaxy "a"). Our morphokinematic analysis of galaxy "a" combined with the absorption line kinematics supports the interpretation that one of the absorption components originates from an extension of the stellar disk of galaxy "a", while the other component may arise in accreting gas in a warped disk with specific angular momentum ∼ 3 times larger than the specific angular momentum of the galaxy halo. Such warped disks are common features in hydrodynamical simulations of cold-flow accretion onto galaxies; the data presented here provide observational evidence in favour of this scenario.

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“…While all forms of hydrogen are typically detected in the inner discs and spiral arms of galaxies in the Local Universe, most often it is the H I 21-cm line that reveals the outermost regions of galaxy discs (e.g., Warren et al 2004;Begum et al 2005;Sancisi et al 2008;Heald et al 2011;Koribalski et al 2018). Occasionally H I is found in filaments, plumes and/or bridges, tracing the gravitational interactions with neighbouring galaxies (e.g., Yun et al 1993Yun et al , 1994Koribalski et al 2003;Koribalski and Dickey 2004;Pearson et al 2016) and in groups/clusters (e.g., Verdes-Montenegro et al 2001;Oosterloo and van Gorkom 2005;Chung et al 2009;English et al 2010;Lee-Waddell et al 2012;Hess et al 2017;Scott et al 2018;Saponara et al 2018). Beyond the inner galaxy disk in which molecular hydrogen is typically the dominant gas component (Leroy et al 2008;Bigiel and Blitz 2012), H I is also an excellent tracer of star formation in the outer discs of galaxies (e.g., Battaglia et al 2006;Koribalski and López-Sánchez 2009;Koribalski 2017).…”

Section: Introductionmentioning

confidence: 99%

WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

Self Cite

201

125

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The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (H I) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 × 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radioquiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (−90 • < δ < +30 • ) to a redshift of z 0.26, and generate spectral line image cubes at ∼30 arcsec resolution and ∼1.6 mJy beam −1 per 4 km s −1 channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect around half a million galaxies with a mean redshift of z ∼ 0.05 (∼200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the H I properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of recent and planned large-scale H I surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. -First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA).

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H i in group interactions: HCG 44

Cited by 31 publications

References 66 publications

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Observational signatures of a warped disk associated with cold-flow accretion

WALLABY – an SKA Pathfinder H i survey

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