MusE GAs FLOw and Wind (MEGAFLOW) II. A study of gas accretion around <i>z</i> ≈ 1 star-forming galaxies with background quasars

Zabl, Johannes; Bouché, Nicolas; Schroetter, Ilane; Wendt, Martin; Finley, Hayley; Schaye, Joop; Conseil, Simon; Contini, T.; Marino, R. A.; Mitchell, Peter D.; Muzahid, Sowgat; Pezzulli, Gabriele; Wisotzki, L.

doi:10.1093/mnras/stz392

Cited by 131 publications

(157 citation statements)

References 161 publications

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“…Stewart 2017, and references therein). The kinematics of extended disc-like structures traced by cold gas around galaxies at z ≈ 1 is consistent with a cold accretion model (Zabl et al 2019). There is meagre direct observational evidence for accretion in massive galaxies at low redshifts (see, e.g.…”

Section: Introductionsupporting

confidence: 77%

UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

Saburova

Chilingarian

Kasparova

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The dominant physical processes responsible for the formation and longevity of giant gaseous and stellar discs in galaxies remain controversial. Although they are rare (less than 10 confirmed as of now), giant low-surface brightness (gLSB) discy galaxies provide interesting insights given their extreme nature. We describe observations of UGC 1378 including deep spectroscopy with the Russian 6m telescope and multi-band imaging with Binospec at the MMT. Galaxy UGC 1378 has both high surface brightness and an extended low surface brightness discs. Our stellar velocity dispersion data for the high-surface brightness, Milky Way-sized, disc appears inconsistent with a recent major merger, a widely discussed formation scenario for the very extended low surface brightness disc. We estimate the star formation rates (SFR) from archival Wide-Field Infrared Survey Explorer data. The SFR surface density in the LSB disc is low relative to its gas density, consistent with recent gas accretion. We argue that the unusually large size of UGC 1378's disc may be the product of a rich gas reservoir (e.g. a cosmic filament) and an isolated environment that has preserved the giant disc.

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Section: Introductionsupporting

confidence: 77%

UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

Saburova

Chilingarian

Kasparova

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Even the internal dispersion of the CGM absorption for low ions points to accretion and outflow scenarios . Furthermore, relative gas and galaxy kinematics show that low ions are kinematically connected to their host galaxy by aligning with their rotation curves and being modelled well by accreting+corotating gas (Steidel et al 2002;Kacprzak et al 2010Kacprzak et al , 2011aHo et al 2017;Martin et al 2019;Zabl et al 2019). On the other hand, minor axis gas also seems to be well modelled by outflowing gas (Bouché et al 2012;Gauthier & Chen 2012;Schroetter et al 2016).…”

Section: Fig 5-same As Left Panel Ofmentioning

confidence: 96%

“…Low ionization level ions within the CGM show strong kinematic signatures that are consistent with large-scale outflows (Bouché et al 2006;Tremonti et al 2007;Martin & Bouché 2009;Weiner et al 2009;Nestor et al 2011;Noterdaeme et al 2010;Coil et al 2011;Kacprzak et al 2010;Kacprzak et al 2014;Rubin et al 2010;Ménard & Fukugita 2012;Martin et al 2012;Noterdaeme et al 2012;Krogager et al 2013;Péroux et al 2013;Rubin et al 2014;Crighton et al 2015;Nielsen et al 2015Nielsen et al , 2016Lan & Mo 2018). Furthermore, low angular momentum and co-rotating gas around galaxies and orientation dependant absorption velocity widths point to signatures of gas accretion (Steidel et al 2002;Kacprzak et al 2010;Ho et al 2017;Kacprzak 2017;Martin et al 2019;Zabl et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities

Kacprzak

Pointon

Nielsen

et al. 2019

ApJ

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We present ISM and CGM metallicities for 25 absorption systems associated with isolated star-forming galaxies ( z = 0.28) with 9.4≤log(M * /M ⊙ )≤10.9 and with absorption detected within 200 kpc. Galaxy ISM metallicities were measured using Hα/[N II] emission lines from Keck/ESI spectra. CGM single-phase lowionization metallicities were modeled using MCMC and Cloudy analysis of absorption from HST/COS and Keck/HIRES or VLT/UVES quasar spectra. We find that the star-forming galaxy ISM metallicities follow the observed stellar mass metallicity relation (1σ scatter 0.19 dex). CGM metallicity shows no dependence with stellar mass and exhibits a scatter of ∼2 dex. All CGM metallicities are lower than the galaxy ISM metallicities and are offset by log(dZ) = −1.17 ± 0.11. There is no obvious metallicity gradient as a function of impact parameter or virial radius (< 2.3σ significance). There is no relationship between the relative CGM-galaxy metallicity and azimuthal angle. We find the mean metallicity differences along the major and minor axes are −1.13±0.18 and −1.23±0.11, respectively. Regardless of whether we examine our sample by low/high inclination or low/high impact parameter, or low/high N(H I), we do not find any significant relationship with relative CGM-galaxy metallicity and azimuthal angle. We find that 10/15 low column density systems (logN(H I)< 17.2) reside along the galaxy major axis while high column density systems (logN(H I)≥ 17.2) reside along the minor axis. This suggest N(H I) could be a useful indicator of accretion/outflows. We conclude that CGM is not well mixed, given the range of galaxy-CGM metallicities, and that metallicity at low redshift might not be a good tracer of CGM processes. On the-other-hand, we should replace integrated line-of-sight, single phase, metallicities with multi-phase, cloud-cloud metallicities, which could be more indicative of the physical processes within the CGM.

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“…Mg iiλ2796 absorption line equivalent width versus the impact parameter. The filled blue circles are the galaxies identified in MUSE-ALMA Halos (groups linked with a line, absorbers selected based on their H i feature are marked with orange squares), empty blue circles mark systems from the literature (Schroetter et al 2016;Bielby et al 2017;Klitsch et al 2018;Zabl et al 2019), groups are linked with lines. The blue, horizontal arrow marks the limits of the Q1211z105 with no detected associated galaxy.…”

Section: Absorbers Are Associated With Multiple Galaxiesmentioning

confidence: 99%

MUSE-ALMA haloes V: physical properties and environment of z ≤ 1.4 H i quasar absorbers

Hamanowicz

Péroux

Zwaan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present results of the MUSE-ALMA Halos, an ongoing study of the Circum-Galactic Medium (CGM) of low redshift galaxies (z ≤ 1.4), currently comprising 14 strong H i absorbers in five quasar fields. We detect 43 galaxies associated with absorbers down to star formation rate (SFR) limits of 0.01-0.1 M yr −1 , found within impact parameters (b) of 250 kpc from the quasar sightline. Excluding the targeted absorbers, we report a high detection rate of 89 per cent and find that most absorption systems are associated with pairs or groups of galaxies (three to eleven members). We note that galaxies with the smallest impact parameters are not necessarily the closest to the absorbing gas in velocity space. Using a multi-wavelength dataset (UVES/HIRES, HST, MUSE), we combine metal and H i column densities, allowing for derivation of the lower limits of neutral gas metallicity as well as emission line diagnostics (SFR, metallicities) of the ionised gas in the galaxies. We find that groups of associated galaxies follow the canonical relations of N(H i)b and W r (2796)b, defining a region in parameter space below which no absorbers are detected. The metallicity of the ISM of associated galaxies, when measured, is higher than the metallicity limits of the absorber. In summary, our findings suggest that the physical properties of the CGM of complex group environments would benefit from associating the kinematics of individual absorbing components with each galaxy member.

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MusE GAs FLOw and Wind (MEGAFLOW) II. A study of gas accretion around z ≈ 1 star-forming galaxies with background quasars

Cited by 131 publications

References 161 publications

UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities

MUSE-ALMA haloes V: physical properties and environment of z ≤ 1.4 H i quasar absorbers

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