MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Schroetter, Ilane; Bouché, Nicolas; Zabl, Johannes; Contini, T.; Wendt, Martin; Schaye, Joop; Mitchell, Peter D.; Muzahid, Sowgat; Marino, R. A.; Bacon, Roland; Lilly, S. J.; Richard, Johan; Wisotzki, L.

doi:10.1093/mnras/stz2822

Cited by 131 publications

(164 citation statements)

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“…Bordoloi et al (2011) found a strong azimuthal dependence of Mg II absorption, implying the presence of a bipolar outflow aligned along the disc rotation axis. Concomitantly, Bouché et al (2012) and Kacprzak, Churchill & Nielsen (2012) found a bimodal distribution of azimuthal angles hosting strong Mg II absorption, suggestive of bipolar outflows contributing to the cold gas cross-section (Schroetter et al 2019;Martin et al 2019b). Such signatures are also found in hotter gas phases including ionized gas traced by OVI absorption (Kacprzak et al 2015b).…”

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confidence: 81%

“…Early efforts started with the AO-equipped near-infrared spectrograph VLT/SINFONI (Bouché et al 2007b;Péroux et al 2011;Péroux et al 2013Péroux et al , 2016Schroetter et al 2015). The potential of this technique for studying the CGM with the wide-field optical spectrograph VLT/MUSE has been further demonstrated (Bouché et al 2016;Schroetter et al 2016;Schroetter et al 2019;Zabl et al 2019;Muzahid et al 2020;Lofthouse et al 2020) as well as with the high spectral resolution optical spectrograph Keck/KCWI (Martin et al 2019a;Nielsen et al 2020). At z abs <1, the MUSE-ALMA Halos survey has measured the kinematics of the neutral, molecular, and ionized gas of the multiphase CGM (Péroux et al 2017;Klitsch et al 2018;Rahmani et al 2018a, b;Péroux et al 2019;Hamanowicz et al 2020).…”

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confidence: 99%

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Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Péroux

Nelson

Voort

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use cosmological hydrodynamical simulations to examine the physical properties of the gas in the circumgalactic media (CGM) of star-forming galaxies as a function of angular orientation. We utilise TNG50 of the IllustrisTNG project, as well as the EAGLE simulation to show that observable properties of CGM gas correlate with azimuthal angle, defined as the galiocentric angle with respect to the central galaxy. Both simulations are in remarkable agreement in predicting a strong modulation of flow rate direction with azimuthal angle: inflow is more substantial along the galaxy major axis, while outflow is strongest along the minor axis. The absolute rates are noticeably larger for higher ($\log {(M_\star / \rm {M}_\odot )} \sim 10.5$) stellar mass galaxies, up to an order of magnitude compared to $\dot{M} \lesssim 1$ M⊙ yr−1 sr−1 for $\log {(M_\star / \rm {M}_\odot )}\sim 9.5$ objects. Notwithstanding the different numerical and physical models, both TNG50 and EAGLE predict that the average metallicity of the CGM is higher along the minor versus major axes of galaxies. The angular signal is robust across a wide range of galaxy stellar mass $8.5 < \log {(M_\star / \rm {M}_\odot )} < 10.5$ at z < 1. This azimuthal dependence is particularly clear at larger impact parameters b ≥ 100 kpc. Our results present a global picture whereby, despite the numerous mixing processes, there is a clear angular dependence of the CGM metallicity. We make forecasts for future large survey programs that will be able to compare against these expectations. Indeed, characterising the kinematics, spatial distribution and metal content of CGM gas is key to a full understanding of the exchange of mass, metals, and energy between galaxies and their surrounding environments.

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confidence: 81%

mentioning

confidence: 99%

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Péroux

Nelson

Voort

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Several studies of Mg II-galaxy pairs have in fact reported that the distribution of Mg II absorption is not isotropic around galaxies (e.g. Bordoloi et al 2011;Bouché et al 2012;Kacprzak et al 2012;Lan & Mo 2018;Martin et al 2019;Schroetter et al 2019;Zabl et al 2019), with Mg II absorption clustering either in the direction of the major or minor axis. These observations are often interpreted with models in which the Mg II absorbing gas traces either biconical outflows perpendicular to the galaxy disc along the minor axis or co-rotating/accreting gas along the galaxy major axis.…”

Section: Azimuthal Distribution Of Mg II Absorbersmentioning

confidence: 99%

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

Dutta

Fumagalli

Fossati

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a study of the metal-enriched cool halo gas traced by Mg ii absorption around 228 galaxies at z ∼ 0.8 − 1.5 within 28 quasar fields from the MUSE Analysis of Gas around Galaxies (MAGG) survey. We observe no significant evolution in the Mg ii equivalent width versus impact parameter relation and in the Mg ii covering fraction compared to surveys at z ≲ 0.5. The stellar mass, along with distance from galaxy centre, appears to be the dominant factor influencing the Mg ii absorption around galaxies. With a sample that is 90% complete down to a star formation rate of ≈0.1 $\rm M_\odot yr^{-1}$PLXINSERT-, and up to impact parameters ≈250 − 350 kpc from quasars, we find that the majority ($67^{+12}_{-15}$% or 14/21) of the Mg ii absorption systems are associated with more than one galaxy. The complex distribution of metals in these richer environments adds substantial scatter to previously-reported correlations. Multiple galaxy associations show on average five times stronger absorption and three times higher covering fraction within twice the virial radius than isolated galaxies. The dependence of Mg ii absorption on galaxy properties disfavours the scenario in which a widespread intra-group medium dominates the observed absorption. This leaves instead gravitational interactions among group members or hydrodynamic interactions of the galaxy haloes with the intra-group medium as favoured mechanisms to explain the observed enhancement in the Mg ii absorption strength and cross section in rich environments.

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“…The major result from these studies is that the Mg ii absorbing gas is not isotropically distributed around the galaxies (e.g. Bordoloi et al 2011;Bouché et al 2012; Kacprzak et al 2012;Lan et al 2014;Lan & Mo 2018;Zabl et al 2019;Martin et al 2019;Schroetter et al 2019). Instead, the observations support a two-component geometry: a bi-conical outflow perpendicular to the galaxy disk and an extended gas disk approximately co-planar with the stellar disk.…”

Section: Introductionmentioning

confidence: 96%

“…This allows to split the Mg ii absorber sightlines into an outflow and a disk sub-sample, which can be used to study the kinematics of the outflows (e.g. Bouché et al 2012;Kacprzak et al 2014;Muzahid et al 2015;Schroetter et al 2015Schroetter et al , 2016Schroetter et al , 2019Rahmani et al 2018b;Martin et al 2019) and the extended gas accretion disks (e.g. Steidel et al 2002;Chen et al 2005;Kacprzak et al 2010Kacprzak et al , 2011bBouché et al 2013Bouché et al , 2016Ho et al 2017;Rahmani et al 2018a;Zabl et al 2019), respectively.…”

Section: Introductionmentioning

confidence: 99%

MusE GAs FLOw and Wind (MEGAFLOW) IV. A two sightline tomography of a galactic wind

Zabl

Bouché

Schroetter

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Galactic outflows are thought to eject baryons back out to the circum-galactic medium (CGM). Studies based on metal absorption lines (Mg ii in particular) in the spectra of background quasars indicate that the gas is ejected anisotropically, with galactic winds likely leaving the host in a bi-conical flow perpendicular to the galaxy disk. In this paper, we present a detailed analysis of an outflow from a z = 0.7 "green-valley" galaxy (log(M * /M ) = 9.9; SFR = 0.5 M yr −1 ) probed by two background sources part of the MUSE Gas Flow and Wind (MEGAFLOW) survey. Thanks to a fortuitous configuration with a background quasar (SDSSJ1358+1145) and a bright background galaxy at z = 1.4, both at impact parameters of ≈ 15 kpc, we can -for the first time -probe both the receding and approaching components of a putative galactic outflow around a distant galaxy. We measure a significant velocity shift between the Mg ii absorption from the two sightlines (84 ± 17 km s −1 ), which is consistent with the expectation from our simple fiducial wind model, possibly combined with an extended disk contribution.

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MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Cited by 131 publications

References 129 publications

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

MusE GAs FLOw and Wind (MEGAFLOW) IV. A two sightline tomography of a galactic wind

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