CHILES VI: H <scp>i</scp> and H α observations for <i>z</i> &amp;lt; 0.1 galaxies; probing H <scp>i</scp> spin alignment with filaments in the cosmic web

Bird, J. Blue; Davis, Julie; Luber, Nicholas; Gorkom, J. H. van; Wilcots, Eric M.; Pisano, D. J.; Gim, Hansung B.; Momjian, Emmanuel; Fernández, Ximena; Hess, Kelley M.; Lucero, D. M.; Dodson, Richard; Vinsen, Kevin; Popping, Attila; Chung, Aeree; Kreckel, Kathryn; Hulst, J. M. van der; Yun, Min S.

doi:10.1093/mnras/stz3357

Cited by 42 publications

(21 citation statements)

References 80 publications

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“…Only a handful of studies have investigated the correlation between HI mass and distance from the spine of large-scale structure filaments, and samples are still relatively small and generally biased towards gas-rich systems. While there seems to be common agreement that gas richness may vary with distance from the filaments (Kleiner et al 2017;Crone Odekon et al 2018;Blue Bird et al 2020), additional work is needed to properly quantify these differences and their dependence on galaxy properties. For example, while Crone Odekon et al (2018) find an increase of HI content with increasing distance from the spine of the large-scale structure, Kleiner et al (2017) report the opposite trend for galaxies with stellar masses greater than 10 11 M .…”

Section: Large-scale Structure Filamentsmentioning

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: Large-scale Structure Filamentsmentioning

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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“…There have also been extensions of such studies beyond the local universe (e.g. Catinella et al 2008;Catinella & Cortese 2015;Verheijen et al 2007;Hess et al 2019;Bera et al 2019;Blue Bird et al 2020;Gogate et al 2020). How-ever, even with very deep integrations, direct detections of H i in emission have so far been from gas-rich, star-forming galaxies (≥2 × 10 9 M ; e.g.…”

Section: Introductionmentioning

confidence: 99%

Disc galaxy resolved in H I absorption against the radio lobe of 3C 433: Case study for future surveys

Murthy

Morganti

Emonts

et al. 2020

A&A

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The neutral atomic gas content of galaxies is usually studied in the H I 21 cm emission line of hydrogen. However, as we go to higher redshifts, owing to the weak strength of the transition, we need very deep integrations to detect H I emission. The H I absorption does not suffer from this dependence on distance as long as there is a sufficiently bright radio source to provide the background continuum. However, resolved H I absorption studies of galaxies are rare. We report one such rare study of resolved H I absorption against the radio galaxy 3C 433 at z = 0.101, detected with the Very Large Array. The absorption was known from single-dish observations, but owing to the higher spatial resolution of our data, we find that the absorber is located against the southern lobe of the radio galaxy. The resolved kinematics shows that the absorber has regular kinematics with an H I mass ≲3.4 × 108 M⊙ for Tspin = 100 K. We also present deep optical continuum observations and Hα observations from the Gran Telescopio CANARIAS (GTC), which reveal that the absorber is likely to be a faint disc galaxy in the same environment as 3C 433, with a stellar mass of ∼1010 M⊙ and a star-formation rate of 0.15 M⊙ yr−1 or less. Considering its H I mass, H I column density, stellar mass, and star-formation rate, this galaxy lies well below the main sequence of star forming galaxies. Its H I mass is lower than the galaxies studied in H I emission at z ∼ 0.1. Our GTC imaging has revealed, furthermore, interesting alignments between Hα and radio synchrotron emission in the H I companion and in the host galaxy of the active galactic nucleus as well as in the circumgalactic medium in between. This suggests that the shock ionization of gas by the propagating radio source may happen across a scale spanning many tens of kpc. Overall, our work supports the potential of studying the H I content in galaxies via absorption in the case of a fortuitous alignment with an extended radio continuum source. This approach may allow us to trace galaxies with low H I masses which would otherwise be missed by deep H I emission surveys. In conjunction with the deep all-sky optical surveys, the current and forthcoming blind H I surveys with the Square Kilometre Array (SKA) pathfinder facilities will be able to detect many such systems, though they may not be able to resolve the H I absorption spatially. Phase 1 of the SKA, with its sub-arcsecond resolution and high sensitivity, will be all the more able to resolve the absorption in such systems.

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“…The first robust observational evidence was provided by the Tempel, Stoica & Saar (2013) and Tempel & Libeskind (2013), who have shown that the spins of spiral galaxies are preferentially aligned with the filament axis while the minor axis of elliptical galaxies, which are typically of higher mass, is preferentially perpendicular to the filaments axis (see also Hirv et al 2017). The same trend, although at a lower statistical significance due to the smaller sample, is seen when inferring the spin from the stellar or gaseous velocity maps, such as those obtained using SAMI or MaNGA (Krolewski et al 2019;Blue Bird et al 2020;Welker et al 2020).…”

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confidence: 80%

Cosmic Ballet III: Halo spin evolution in the cosmic web

Veena

Cautun

Weygaert

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We explore the evolution of halo spins in the cosmic web using a very large sample of dark matter haloes in the ΛCDM Planck-Millennium N-body simulation. We use the nexus+ multiscale formalism to identify the hierarchy of filaments and sheets of the cosmic web at several redshifts. We find that at all times the magnitude of halo spins correlates with the web environment, being largest in filaments, and, for the first time, we show that it also correlates with filament thickness as well as the angle between spin-orientation and the spine of the host filament. For example, massive haloes in thick filaments spin faster than their counterparts in thin filaments, while for low-mass haloes the reverse is true. We also have studied the evolution of alignment between halo spin orientations and the preferential axes of filaments and sheets. The alignment varies with halo mass, with the spins of low-mass haloes being predominantly along the filament spine, while those of high-mass haloes being predominantly perpendicular to the filament spine. On average, for all halo masses, halo spins become more perpendicular to the filament spine at later times. At all redshifts, the spin alignment shows a considerable variation with filament thickness, with the halo mass corresponding to the transition from parallel to perpendicular alignment varying by more than one order of magnitude. The cosmic web environmental dependence of halo spin magnitude shows little evolution for z ≤ 2 and is likely a consequence of the correlations in the initial conditions or high redshift effects.

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CHILES VI: H i and H α observations for z < 0.1 galaxies; probing H i spin alignment with filaments in the cosmic web

Cited by 42 publications

References 80 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

Disc galaxy resolved in H I absorption against the radio lobe of 3C 433: Case study for future surveys

Cosmic Ballet III: Halo spin evolution in the cosmic web

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CHILES VI: H i and H α observations for z &lt; 0.1 galaxies; probing H i spin alignment with filaments in the cosmic web

Cited by 42 publications

References 80 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

Disc galaxy resolved in H I absorption against the radio lobe of 3C 433: Case study for future surveys

Cosmic Ballet III: Halo spin evolution in the cosmic web

Contact Info

Product

Resources

About

CHILES VI: H i and H α observations for z < 0.1 galaxies; probing H i spin alignment with filaments in the cosmic web

Disc galaxy resolved in H I absorption against the radio lobe of 3C 433: Case study for future surveys