The CGM at Cosmic Noon with KCWI: Outflows from a Star-forming Galaxy at z = 2.071

Nielsen, Nikole M.; Kacprzak, Glenn G.; Pointon, Stephanie K.; Murphy, Michael T.; Churchill, Christopher W.; Davé, Romeel

doi:10.3847/1538-4357/abc561

Cited by 20 publications

(17 citation statements)

References 192 publications

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“…This complex environment is multiphase and has been observed in numerous surveys (e.g., Tumlinson et al 2013;Bordoloi et al 2014;Peek et al 2015;Borthakur et al 2015) at low redshift. A prominent feature of the CGM around active galaxies is the Lyα (Lymanα) emission line, which is also ubiquitously observed at high redshift (e.g., Haiman & Rees 2001;Reuland et al 2003;van Breugel et al 2006;Villar-Martín 2007;Humphrey et al 2013;Cantalupo et al 2014;Wisotzki et al 2016Wisotzki et al , 2018Arrigoni Battaia et al 2018, 2019Nielsen et al 2020). Lyα is the transition of the hydrogen electron from the 2p orbit to its ground state.…”

Section: Introductionmentioning

confidence: 99%

Mapping the “invisible” circumgalactic medium around a z ∼ 4.5 radio galaxy with MUSE

Wang

Wylezalek

Breuck

et al. 2021

A&A

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In this paper we present Multi Unit Spectroscopic Explorer integral field unit spectroscopic observations of the ∼70 × 30 kpc2 Lyα halo around the radio galaxy 4C04.11 at z = 4.5077. High-redshift radio galaxies are hosted by some of the most massive galaxies known at any redshift and are unique markers of concomitant powerful active galactic nucleus (AGN) activity and star formation episodes. We map the emission and kinematics of the Lyα across the halo as well as the kinematics and column densities of eight H I absorbing systems at −3500 < Δv < 0 km s−1. We find that the strong absorber at Δv ∼ 0 km s−1 has a high areal coverage (30 × 30 kpc2), being detected across a large extent of the Lyα halo, a significant column density gradient along the southwest to northeast direction, and a velocity gradient along the radio jet axis. We propose that the absorbing structure, which is also seen in C IV and N V absorption, represents an outflowing metal-enriched shell driven by a previous AGN or star formation episode within the galaxy and is now caught up by the radio jet, leading to jet-gas interactions. These observations provide evidence that feedback from AGN in some of the most massive galaxies in the early Universe may play an important role in redistributing material and metals in their environments.

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Section: Introductionmentioning

confidence: 99%

Mapping the “invisible” circumgalactic medium around a z ∼ 4.5 radio galaxy with MUSE

Wang

Wylezalek

Breuck

et al. 2021

A&A

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“…In particular, star formation-driven outflows could be a major pathway to populating the inner regions of DM halos with W r ≥ 0.6 Å C IV absorbers. And in fact, there is some observational evidence connecting strong C IV absorbers to galactic winds (Fox et al 2007;Steidel et al 2010;Nielsen et al 2020).…”

Section: Baryon Cycle and The Cgmmentioning

confidence: 99%

“…In the last few years, Multi-Object and Integral Field Spectroscopy-based programs like MEGAFLOW (e.g., Schroetter et al 2021), KBSS (e.g., Rudie et al 2019), CGM at Cosmic Noon with KCWI (e.g., Nielsen et al 2020), MUDF (e.g., Fossati et al 2019), andMAGG (e.g., Dutta et al 2020) have lead the way in mapping the CGM of galaxies across the vast majority of cosmic time and providing detailed information on the spatial distribution of gas halos relative to galaxies. In addition, measurements of galactic outflows at high redshifts, which will be enabled by the soon-to-be-launched James Webb Space Telescope, will be a direct empirical test of the scenario of early enrichment by low-mass halos we proposed.…”

Section: Improving Our Understanding Of C Ivmentioning

confidence: 99%

Evolution of CIV Absorbers. II. Where does CIV live?

Hasan,

Churchill,

Stemock

et al. 2021

Preprint

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We use the observed cumulative statistics of C IV absorbers and dark matter halos to infer the distribution of C IV-absorbing gas relative to galaxies at redshifts 0 ≤ z ≤ 5. We compare the cosmic incidence dN/dX of C IV absorber populations and galaxy halos, finding that massive L ≥ L halos alone cannot account for all the observed W r ≥ 0.05 Å absorbers. However, the dN/dX of lower mass halos exceeds that of W r ≥ 0.05 Å absorbers. We also estimate the characteristic gas radius of absorbing structures required for the observed C IV dN/dX, assuming each absorber is associated with a single galaxy halo. The W r ≥ 0.3 Å and W r ≥ 0.6 Å C IV gas radii are ∼30-70% (∼20-40%) of the virial radius of L (0.1L ) galaxies, and the W r ≥ 0.05 Å gas radius is ∼100-150% (∼60-100%) of the virial radius of L (0.1L ) galaxies. For stronger absorbers, the gas radius relative to virial radius rises across Cosmic Noon and falls afterwards, while for weaker absorbers, the relative gas radius declines across Cosmic Noon and then dramatically rises at z < 1. A strong luminosity-dependence of gas radius implies highly extended C IV envelopes around massive galaxies before Cosmic Noon, while a luminosity-independent gas radius implies highly extended envelopes around dwarf galaxies after Cosmic Noon. From available absorber-galaxy and C IV evolution data, we favor a scenario in which low-mass galaxies enrich the volume around massive galaxies at early epochs and propose that the outer halo gas (> 0.5R v ) was produced primarily in ancient satellite dwarf galaxy outflows, while the inner halo gas (< 0.5R v ) originated from the central galaxy and persists as recycled accreting gas.

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“…This suggests that either the DLA host galaxy is not strongly starforming, or the host is beyond an impact parameter of ∼ 12.5 kpc. We re-observed this DLA, which also has ultra-strong Mg , with the Keck Cosmic Web Imager (KCWI; Morrissey et al 2018) as part of our program to identify host galaxies of known 𝑧 = 2 − 3 Mg and C absorbers (Nielsen et al 2020). With our deeper and wider survey of the field, we identified four galaxies in a compact group at the redshift of the DLA beyond the search radius of the previous survey.…”

Section: Introductionmentioning

confidence: 99%

A Complex Multiphase DLA Associated with a Compact Group at z=2.431 Traces Accretion, Outflows, and Tidal Streams

Nielsen,

Kacprzak,

Murphy

et al. 2022

Preprint

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As part of our program to identify host galaxies of known 𝑧 = 2 − 3 Mg absorbers with the Keck Cosmic Web Imager (KCWI), we discovered a compact group giving rise to a 𝑧 = 2.431 DLA with ultra-strong Mg absorption in quasar field J234628+124859. The group consists of four star-forming galaxies within 8 − 28 kpc and 𝑣 ∼ 40 − 340 km s −1 of each other, where tidal streams are weakly visible in deep HST imaging. The group geometric centre is 𝐷 = 25 kpc from the quasar (𝐷 = 20 − 40 kpc for each galaxy). Galaxy G1 dominates the group (1.66𝐿 * , SFR FUV = 11.6 M yr −1 ) while G2, G3, and G4 are less massive (0.1 − 0.3𝐿 * , SFR FUV = 1.4 − 2.0 M yr −1 ). Using a VLT/UVES quasar spectrum covering the H Lyman series and metal lines such as Mg , Si , and C , we characterised the kinematic structure and physical conditions along the line-of-sight with cloud-by-cloud multiphase Bayesian modelling. The absorption system has a total log(𝑁 (H )/cm −2 ) = 20.53 and an 𝑁 (H )-weighted mean metallicity of log(𝑍/𝑍 ) = −0.68, with a very large Mg linewidth of Δ𝑣 ∼ 700 km s −1 . The highly kinematically complex profile is well-modelled with 30 clouds across low and intermediate ionisation phases with values 13 log(𝑁 (H )/cm −2 ) 20 and −3 log(𝑍/𝑍 ) 1. Comparing these properties to the galaxy properties, we infer a wide range of gaseous environments, including metal-rich outflows, metal-poor IGM accretion, and tidal streams from galaxy-galaxy interactions. This diversity of structures forms the intragroup medium around a complex compact group environment at the epoch of peak star formation activity. Surveys of low redshift compact groups would benefit from obtaining a more complete census of this medium for characterising evolutionary pathways.

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The CGM at Cosmic Noon with KCWI: Outflows from a Star-forming Galaxy at z = 2.071

Cited by 20 publications

References 192 publications

Mapping the “invisible” circumgalactic medium around a z ∼ 4.5 radio galaxy with MUSE

Mapping the “invisible” circumgalactic medium around a z ∼ 4.5 radio galaxy with MUSE

Evolution of CIV Absorbers. II. Where does CIV live?

A Complex Multiphase DLA Associated with a Compact Group at z=2.431 Traces Accretion, Outflows, and Tidal Streams

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