Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Schroetter, Ilane; Bouché, Nicolas; Wendt, Martin; Contini, T.; Finley, Hayley; Pelló, R.; Bacon, Roland; Cantalupo, Sebastiano; Marino, R. A.; Richard, Johan; Lilly, S. J.; Schaye, Joop; Soto, Kurt T.; Steinmetz, Matthias; Straka, Lorrie A.; Wisotzki, L.

doi:10.3847/1538-4357/833/1/39

Cited by 107 publications

(132 citation statements)

References 78 publications

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“…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). Finally, the metallicity distribution of LLS and pLLS appears bimodal, which also suggests that outflows and accretion are dominant phenomena within the CGM (Wotta et al 2016.…”

Section: Fig 5-same As Left Panel Ofmentioning

confidence: 96%

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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Section: Fig 5-same As Left Panel Ofmentioning

confidence: 96%

The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities

Kacprzak

Pointon

Nielsen

et al. 2019

ApJ

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“…Cuts in both impact parameter and velocity difference between absorber and galaxy differ between published MUSE absorber studies, making the comparison of results not straightforward. MusE GAs FLOw and WInd (MEGAFLOW), a MUSE survey of Mg ii absorbers, (Schroetter et al 2016) allows for a 1000 km s −1 velocity difference between the galaxy and the absorber, and in case of multiple detections, the lowest-impact-parameter object is selected. Quasar Sightline And Galaxy Evolution (QSAGE), an OVI absorption oriented MUSE program (Bielby et al 2019), supported by a larger impact parameter coverage with HST grisms, uses a tight limit of 400 km s −1 (expected outflow velocity).…”

Section: Absorbers Are Associated With Multiple Galaxiesmentioning

confidence: 99%

“…Integral-field spectroscopy with instruments like SIN-FONI (Eisenhauer et al 2003), MUSE (Bacon et al 2006) or OSIRIS (Larkin et al 2006), make it possible to obtain spectra of many sources in the field-of-view and efficiently classify galaxies associated with absorbers. Combined with highresolution UV spectroscopy of quasars, these studies have revealed relevant features interpreted as galactic outflows (Schroetter et al 2016;Rahmani et al 2018b;Schroetter et al 2019), warped accretion discs (Rahmani et al 2018a) and galactic fountains (Bouché et al 2016). Alongside the detection of kinematic traces of gas inflows and outflows, new studies detected multiple galaxies associated with one absorber (Bielby et al 2017;Péroux et al 2017;Klitsch et al 2018;Nielsen et al 2018;Péroux et al 2019;Muzahid et al 2019).…”

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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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“…In particular, thanks to its large 1 arcmin 2 field of view, its extended wavelength coverage in the optical, and its exquisite sensitivity, MUSE has become the ideal instrument for studies of the CGM of galaxies in quasar fields (e.g. Schroetter et al 2016;Fumagalli et al 2016Fumagalli et al , 2017bPéroux et al 2017;Bielby et al 2017;Klitsch et al 2018;Chen et al 2019).…”

mentioning

confidence: 99%

The MUSE Ultra Deep Field (MUDF). II. Survey design and the gaseous properties of galaxy groups at 0.5 < z < 1.5

Fossati

Fumagalli

Lofthouse

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the goals, design, and first results of the MUSE Ultra Deep Field (MUDF) survey, a large programme using the Multi Unit Spectroscopic Explorer (MUSE) instrument at the ESO Very Large Telescope. The MUDF survey is collecting ≈ 150 hours on-source of integral field optical spectroscopy in a 1.5 × 1.2 arcmin 2 region which hosts several astrophysical structures along the line of sight, including two bright z ≈ 3.2 quasars with close separation (≈ 500 kpc). Following the description of the data reduction procedures, we present the analysis of the galaxy environment and gaseous properties of seven groups detected at redshifts 0.5 < z < 1.5, spanning a large dynamic range in halo mass, log(M h /M ) ≈ 11 − 13.5. For four of the groups, we find associated Mg ii absorbers tracing cool gas in high-resolution spectroscopy of the two quasars, including one case of correlated absorption in both sightlines at distance ≈ 480 kpc. The absorption strength associated with the groups is higher than what has been reported for more isolated galaxies of comparable mass and impact parameters. We do not find evidence for widespread cool gas giving rise to strong absorption within these groups. Combining these results with the distribution of neutral and ionised gas seen in emission in lower-redshift groups, we conclude that gravitational interactions in the group environment strip gas from the galaxy haloes into the intragroup medium, boosting the cross section of cool gas and leading to the high fraction of strong Mg ii absorbers that we detect.

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Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Cited by 107 publications

References 78 publications

The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities

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

The MUSE Ultra Deep Field (MUDF). II. Survey design and the gaseous properties of galaxy groups at 0.5 < z < 1.5

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Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Cited by 107 publications

References 78 publications

The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities

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

The MUSE Ultra Deep Field (MUDF). II. Survey design and the gaseous properties of galaxy groups at 0.5 &lt; z &lt; 1.5

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The MUSE Ultra Deep Field (MUDF). II. Survey design and the gaseous properties of galaxy groups at 0.5 < z < 1.5