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

Fossati, M.; Fumagalli, Michele; Lofthouse, Emma K.; D’Odorico, V.; Lusso, Elisabeta; Cantalupo, Sebastiano; Cooke, Ryan; Cristiani, S.; Haardt, Francesco; Morris, Simon L.; Péroux, Céline; Prichard, Laura; Rafelski, Marc; Smail, Ian; Theuns, Tom

doi:10.1093/mnras/stz2693

Cited by 61 publications

(99 citation statements)

References 126 publications

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“…Wide-field optical integral field unit (IFU) spectrographs like the Multi Unit Spectroscopic Explorer (MUSE; Bacon et al 2010) at the Very Large Telescope (VLT) have revolutionized the study of CGM by enabling efficient and sensitive spectroscopic surveys complete down to a given flux limit around quasar sightlines (e.g. Fumagalli et al 2016Fumagalli et al , 2017Schroetter et al 2016;Mackenzie et al 2019;Zabl et al 2019;Fossati et al 2019b;Lofthouse et al 2020;Muzahid et al 2020). Such type of surveys allows a more complete characterization of the smallscale galaxy environment, a complete (flux limited) analysis of the CGM-galaxy connection up to 250 kpc from the quasar sightlines, and enables studies of CGM to lower mass galaxies (M * <10 10 M ) at z ≥ 1.…”

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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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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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“…All of them used the MUSE pipeline to process the raw data, or directly used datacubes made available by ESO through their Phase 3 process 37 . While most publications used the pipeline as described above (Krajnović et al 2015;Guérou et al 2016;Husser et al 2016;Roth et al 2018), others tried to improve sky subtraction or background uniformity in different ways (e.g., Borisova et al 2016;Urrutia et al 2019;Fossati et al 2019), often using the external ZAP-tool (Zurich Atmosphere Purge, Soto et al 2016) to improve sky residuals. This tool was integrated into the ESO MUSE Reflex workflow to improve accessibility for users.…”

Section: Discussionmentioning

confidence: 99%

The data processing pipeline for the MUSE instrument

Weilbacher

Palsa

Streicher

et al. 2020

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The processing of raw data from modern astronomical instruments is often carried out nowadays using dedicated software, known as pipelines, largely run in automated operation. In this paper we describe the data reduction pipeline of the Multi Unit Spectroscopic Explorer (MUSE) integral field spectrograph operated at the ESO Paranal Observatory. This spectrograph is a complex machine: it records data of 1152 separate spatial elements on detectors in its 24 integral field units. Efficiently handling such data requires sophisticated software with a high degree of automation and parallelization. We describe the algorithms of all processing steps that operate on calibrations and science data in detail, and explain how the raw science data is transformed into calibrated datacubes. We finally check the quality of selected procedures and output data products, and demonstrate that the pipeline provides datacubes ready for scientific analysis.

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“…As in previous analyses of MUSE data (e.g. Fumagalli et al 2017b;Mackenzie et al 2019;Lofthouse et al 2019;Fossati et al 2019), we conduct a redshift survey of galaxies detected in the continuum together with a search for line emitters in the cube. 18 19 20 21 22 23 24 25 26 27 28 29 30 31 33 34 36 37 38 39 41 42 43 44 45 46 47 48 49 50 52 53 54 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 80 81 82 84 86 87 89 90 91 92 93 95 96 97 98 99 100 101 103 104 105 106 107 108 110 111 112113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 129 130 131 132 133 ...…”

Section: Search For Associated Galaxiesmentioning

confidence: 99%

“…Evidence of inhomogeneous enrichment is indeed building up at lower redshifts (e.g. Fumagalli et al 2011a;Mackenzie et al 2019;Lofthouse et al 2019;Fossati et al 2019), and it is thus not surprising to find hints of similar inhomogeneity at these higher redshifts, where the time available for enriched pockets to grow is limited. When compared to the eagle simulated data, we find in our observations a significant fraction of upper limits at impact parameters of > 100 kpc, consistent with the predictions from simulation.…”

Section: Metal Absorption Around Z ∼ 4 − 5 Laesmentioning

confidence: 99%

“…Bergeron & Boisse 1986;Møller & Warren 1998;Kacprzak et al 2010), dedicated MUSE surveys are beginning to uncover greater numbers of associations with galaxy groups at low redshifts (e.g. Péroux et al 2017;Bielby et al 2017aBielby et al , 2019Fossati et al 2019) as well as similarly complex environments traced by Lyα emitters (LAEs) at 3 z 4 (e.g. Fumagalli et al 2016bFumagalli et al , 2017bMackenzie et al 2019;Lofthouse et al 2019).…”

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confidence: 99%

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Into the Ly α jungle: exploring the circumgalactic medium of galaxies at z ∼ 4−5 with MUSE

Bielby

Fumagalli

Fossati

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a study of the galaxy environment of 9 strong H i+C iv absorption line systems (16.2 < log(N(HI)) < 21.2) spanning a wide range in metallicity at z ∼ 4 − 5, using MUSE integral field and X-Shooter spectroscopic data collected in a z ≈ 5.26 quasar field. We identify galaxies within a 250 kpc and ±1000 km s −1 window for 6 out of the 9 absorption systems, with 2 of the absorption line systems showing multiple associated galaxies within the MUSE field of view. The space density of Lyα emitting galaxies (LAEs) around the H i and C iv systems is ≈ 10 − 20 times the average sky density of LAEs given the flux limit of our survey, showing a clear correlation between the absorption and galaxy populations. Further, we find that the strongest C iv systems in our sample are those that are most closely aligned with galaxies in velocity space, i.e. within velocities of ±500 km s −1 . The two most metal poor systems lie in the most dense galaxy environments, implying we are potentially tracing gas that is infalling for the first time into star-forming groups at high redshift. Finally, we detect an extended Lyα nebula around the z ≈ 5.26 quasar, which extends up to ≈ 50 kpc at the surface brightness limit of 3.8 × 10 −18 erg s −1 cm −2 arcsec −2 . After scaling for surface brightness dimming, we find that this nebula is centrally brighter, having a steeper radial profile than the average for nebulae studied at z ∼ 3 and is consistent with the mild redshift evolution seen from z ≈ 2.

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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

Cited by 61 publications

References 126 publications

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

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

The data processing pipeline for the MUSE instrument

Into the Ly α jungle: exploring the circumgalactic medium of galaxies at z ∼ 4−5 with MUSE

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