CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITH HST/COS AND HST/STIS ABSORPTION-LINE SPECTROSCOPY

By J. Stocke, B. Keeney, C. Danforth, J. Michael Shull, C. Froning, James C. Green, S. Penton, B. Savage. 2012

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The circumgalactic medium (CGM) of late-type galaxies is characterized using UV spectroscopy of 11 targeted QSO/galaxy pairs at z ⩽ 0.02 with the Hubble Space Telescope Cosmic Origins Spectrograph (COS) and ∼60 serendipitous absorber/galaxy pairs at z ⩽ 0.2 with the Space Telescope Imaging Spectrograph. CGM warm cloud properties are derived, including volume filling factors of 3%–5%, cloud sizes of 0.1–30 kpc, masses of 10–108 M☉, and metallicities of ∼0.1–1 Z☉. Almost all warm CGM clouds within 0.5 Rvir are metal-bearing and many have velocities consistent with being bound, “galactic fountain” clouds. For galaxies with L ≳ 0.1 L*, the total mass in these warm CGM clouds approaches 1010 M☉, ∼10%–15% of the total baryons in massive spirals and comparable to the baryons in their parent galaxy disks. This leaves ≳ 50% of massive spiral-galaxy baryons “missing.” Dwarfs (<0.1 L*) have smaller area covering factors and warm CGM masses (⩽5% baryon fraction), suggesting that many of their warm clouds escape. Constant warm cloud internal pressures as a function of impact parameter (P/k ∼ 10 cm−3 K) support the inference that previous COS detections of broad, shallow O vi and Lyα absorptions are of an extensive (∼400–600 kpc), hot (T ≈ 106 K), intra-cloud gas which is very massive (⩾1011 M☉). While the warm CGM clouds cannot account for all the “missing baryons” in spirals, the hot intra-group gas can, and could account for ∼20% of the cosmic baryon census at z ∼ 0 if this hot gas is ubiquitous among spiral groups.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4ad6f914c7f10bc24b2492cef270341642406982

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Citations in the corpus

The Circumgalactic Medium (2017, methodology): “Both L∗ and super-L∗ galaxies have provided the most reliable constraints, mainly due to their relative ease of detection in photometric and spectroscopic surveys at z < 0.5 (Chen & Mulchaey 2009; Prochaska et al. 2011b; Werk et al. 2012; Stocke et al. 2013).”
THE BIMODAL METALLICITY DISTRIBUTION OF THE COOL CIRCUMGALACTIC MEDIUM AT z ≲ 1 (2013, result): “The present work and other recent results (e.g., Stocke et al. 2010, 2013; Thom et al. 2011; Tripp et al. 2011; Tumlinson et al. 2011a; Kacprzak et al. 2012b; Churchill et al. 2012; Werk et al. 2013) signal a shift in our ability to characterize the properties of the CGM and have already provided…”
Cool outflows in galaxies and their implications (2020, background): “2014; Lan and Mo 2018; Lan 2019), while the rate of incidence of H I absorption in general, and that of strong Mg II absorption on scales greater than ∼100 kpc, are virtually the same for both galaxy populations (Thom et al. 2012; Lan et al. 2014; Keeney et al. 2017; Lan and Mo 2018).”
A characteristic scale for cold gas (2016, background): “…(2002) Fe II/Mg II, C IV/Mg II (systems 7, 13, & 18) g Rauch, Sargent & Barlow (1999) H I, O I/C II, Si II/Si IV; gravitationally lensed quasar h Stocke et al. (2013) absorption (PKS 1302-102) i Crighton, Hennawi & Prochaska (2013) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .”
Figuring Out Gas & Galaxies in Enzo (FOGGIE). I. Resolving Simulated Circumgalactic Absorption at 2 ≤ z ≤ 2.5 (2018, background): “In the galactic ecosystem, the majority of baryons and heavy elements are in the diffuse gas outside of galaxies rather than in the relatively dense gas and stars composing the disks and central spheroids (Pagel 2008; Stocke et al. 2013; Peeples et al. 2014; Werk et al. 2014; Prochaska et al. 2017).”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “As metals (e.g., O VI) are observed at impact parameters beyond 150 kpc (Prochaska et al. 2011; Stocke et al. 2013), we do not expect that even in the most optimistic scenario for our current accounting to have found all of the metals.”
Probing Galactic Halos with Fast Radio Bursts (2019, methodology): “Assuming this cool CGM is photoionized by the EUVB (or local sources), researchers have crudely estimated the cool gas mass McoolCGM ∼ 10 10 − 1011M implying a significant baryon fraction from cool gas alone, e.g. fb,halo > 0.1Ωb/Ωm (Stocke et al. 2013; Werk et al. 2014; Keeney et al. 2017).”
THE COS-DWARFS SURVEY: THE CARBON RESERVOIR AROUND SUB-L* GALAXIES (2014, background): “…to systematically map the CGM and to correlate its properties with the host galaxy properties and the large scale environment (Tumlinson et al. 2013; Stocke et al. 2013; Bordoloi et al. 2011; Chen et al. 2010; Prochaska et al. 2011a; Zhu & Ménard 2013; Werk et al. 2013; Stocke et al. 2014).”
THE COS-HALOS SURVEY: RATIONALE, DESIGN, AND A CENSUS OF CIRCUMGALACTIC NEUTRAL HYDROGEN (2013, background): “…ionized medium surrounding galaxies, with an extent weakly depending on galaxy properties, was well established before the advent of COS. Recently, Stocke et al. (2013) have revisited this issue with a new sample of targeted galaxies and serendipitous QSO-galaxy pairs drawn from earlier studies.”
THE COS-HALOS SURVEY: ORIGINS OF THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM OF STAR-FORMING GALAXIES (2016, background): “Another is the systematically broader line widths of Ovi absorption (e.g. Tumlinson et al. 2005; Lehner et al. 2009; Narayanan et al. 2010; Savage et al. 2011; Muzahid et al. 2012; Stocke et al. 2013).”
The impact of star formation feedback on the circumgalactic medium (2016, methodology): “Here we briefly present additional analysis of our simulations for comparison to quasar absorption observations of the z ∼ 0 CGM (e.g., Tumlinson et al. 2013; Stocke et al. 2013).”
The Evolution of the Intergalactic Medium (2015, background): “The bottom three rows in Figure 3 illustrate how the absorption in the forest changes in the concordance 12 Matthew McQuinn cosmology relative to cosmologies with a low Ωm and a high σ8.”
Bimodality of low-redshift circumgalactic O VI in non-equilibrium EAGLE zoom simulations (2016, background): “…CGM relative to samples of galaxies, including Chen et al. (2010); Bordoloi et al. (2011); Kacprzak et al. (2011); Borthakur et al. (2013); Churchill et al. (2013); Nielsen et al. (2013); Stocke et al. (2013); Liang & Chen (2014); Kacprzak et al. (2015) at lowz and Turner et al. (2014) at high-z.”
THE COS-HALOS SURVEY: PHYSICAL CONDITIONS AND BARYONIC MASS IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2014, methodology): “In order to determine a volume filling factor, we must estimate a shadowing factor, S (see Stocke et al. 2013 for a full explanation of this factor), which is approximately equal to an average number of discrete absorption components at separate velocities along each line of sight.”
A Global Model for Circumgalactic and Cluster-core Precipitation (2016, background): “It should also apply to ambient circumgalactic gas near the virial temperature in lower-mass systems, in which the conditions can be probed by Hubble-COS observations (e.g., Stocke et al. 2013; Werk et al. 2014).”
The COS-Halos Survey: Metallicities in the Low-redshift Circumgalactic Medium (2017, methodology): “Independent of the debate on MhotCGM, estimates of the cool (T ∼ 104 K) gas mass in the halo M coolCGM derived from CGM experiments indicate masses exceeding 1010M (Prochaska et al. 2011; Stocke et al. 2013, W14).”