Gaseous Galaxy Halos

By M. Putman, Joshua E. G. Peek, M. R. Joung. 2012

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Galactic halo gas traces inflowing star-formation fuel and feedback from a galaxy's disk and is therefore crucial to our understanding of galaxy evolution. In this review, we summarize the multiwavelength observational properties and origin models of Galactic and low-redshift spiral galaxy halo gas. Galactic halos contain multiphase gas flows that are dominated in mass by the ionized component and extend to large radii. The densest, coldest halo gas observed in neutral hydrogen (Hi) is generally closest to the disk (<20 kpc), and absorption line results indicate warm and warm-hot diffuse halo gas is present throughout a galaxy's halo. The hot halo gas detected is not a significant fraction of a galaxy's baryons. The disk-halo interface is where the multiphase flows are integrated into the star-forming disk, and there is evidence for both feedback and fueling at this interface from its temperature and kinematic gradients, and Hi structures. The origin and fate of halo gas are considered in the context of c...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7febb4aa2416dd25777b2f5d269a62ebbed50d18

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Citations in the corpus

The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations (2016, background): “Smooth accretion of fresh gas from the IGM, albeit difficult to detect, is required to sustain the observed star formation rate (SFR) in galaxies across cosmic time (Erb 2008; Tacconi et al. 2010; Putman et al. 2012; Sánchez Almeida et al. 2014).”
CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITH HST/COS AND HST/STIS ABSORPTION-LINE SPECTROSCOPY (2012, methodology): “There is little support for this conjecture however (Putman et al. 2012).”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “…on their H I column density, Sembach et al. 2000; Lockman et al. 2002; Shull et al. 2009; Lehner & Howk 2011; Shull et al. 2011; Lehner et al. 2012; Putman et al. 2012), their total mass is only Mhvc ∼ 10 8M⊙ (Shull et al. 2009; Putman et al. 2012, though see also Lehner & Howk 2011 for a…”
A Global Model for Circumgalactic and Cluster-core Precipitation (2016, background): “Observations of the circumgalactic medium at other wavelengths likewise show rich multiphase structure (e.g., Putman et al. 2012), which has been challenging for simulations to reproduce (e.g., Hummels et al. 2013; Ford et al. 2016).”
Figuring Out Gas & Galaxies in Enzo (FOGGIE). I. Resolving Simulated Circumgalactic Absorption at 2 ≤ z ≤ 2.5 (2018, background): “Milky Way high-velocity clouds (HVCs) with well-constrained distances show H I masses of ∼105–5×106 M (e.g., Wakker et al. 2008; Putman et al. 2012) and sizes in the few to ∼15 kpc range.”
The COS-Halos Survey: Metallicities in the Low-redshift Circumgalactic Medium (2017, background): “A number of metal transport mechanisms have been proposed, including galactic winds, AGN feedback, accretion, tidal stripping, and ram pressure (e.g. Veilleux et al. 2005; Putman et al. 2012; Oppenheimer & Schaye 2013).”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS): ENVIRONMENTAL DEPENDENCE OF GIANT MOLECULAR CLOUD PROPERTIES IN M51 (2014, background): “…dynamically hot component of the molecular gas in M51 (described by Pety et al. 2013) that spatially correlates with locations of star formation, and could be the result of galactic fountains or chimneys that have transported some of the molecular gas away from the disk (e.g., Putman et al. 2012).”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “Powerful galactic winds may force metals out of galaxies, while less powerful outflows may act as “fountains”, redistributing metals from the nuclear regions to larger radii (see Putman et al. 2012, for a review).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “In particular, what fraction of baryons are condensed into stars as opposed to spreading out in the form of gas and dust in and outside of galaxies (Cen & Ostriker 1999; McGaugh et al. 2010; Putman et al. 2012; Shull et al. 2012)?”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “Massive star feedback may also terminate star formation locally, blowing giant bubbles (Cox 2005) and leaking hot processed gas into the Galactic Halo (Putman et al. 2012).”
HI4PI: a full-sky H i survey based on EBHIS and GASS (2016, background): “High-velocity clouds cover a significant fraction of the H i sky (see Putman et al. 2012, their Fig.”