ALMA Observations of Gas-rich Galaxies in z ∼ 1.6 Galaxy Clusters: Evidence for Higher Gas Fractions in High-density Environments

Noble, Allison; McDonald, Michael; Muzzin, Adam; Nantais, Julie; Rudnick, G.; Kampen, E. van; Webb, Tracy; Wilson, Gillian; Yee, H. K. C.; Boone, K.; Cooper, M. C.; DeGroot, A.; Delahaye, Anna; Demarco, R.; Foltz, Ryan; Hayden, Brian; Lidman, C.; Manilla-Robles, A.; Perlmutter, S.

doi:10.3847/2041-8213/aa77f3

Cited by 97 publications

(154 citation statements)

References 63 publications

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“…The rest of galaxies (including all those with M ⋆ > 10 11 M ⊙ ) are in agreement with the field relations. In line with these results, Noble et al (2017) found depletion timescales systematically higher than the scaling relation for nine CO(3 − 2)-detected galaxies in a cluster at z ∼ 1.6, although most are within a one standard deviation of the relation (plus several non-detection whose upper limits are in agreement with the field). Similarly, Hayashi et al (2018) presented CO(3 − 2) observations in several cluster galaxies at z ∼ 1.5 finding again systematically longer depletion timescales, although ∼ 50% of their sample might be in agreement the expected relation for the field (when non-detections are taken into account).…”

Section: The Star Formation Efficiencysupporting

confidence: 77%

“…A thorough characterization of the star formation activity requires a census of the molecular gas mass, the main ingredient from which stars are formed. While some pioneering studies on the gas content of (proto-)cluster structures at z 1.5 have been carried out, they have focused on extreme, rare sources like Dusty Star-Forming Galaxies (DSFGs) or Active Galactic Nucleus hosts (AGN), or on samples of a few targets (Aravena et al 2012;Casasola et al 2013;Dannerbauer et al 2017;Noble et al 2017;Rudnick et al 2017;Stach et al 2017;Wang et al 2018). Despite these significant efforts, the physical properties of less extreme star-forming galaxies and the impact of the environment on their formation and evolution are still far from understood.…”

Section: Introductionmentioning

confidence: 99%

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On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

Zavala

Casey

Scoville

et al. 2019

ApJ

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We present ALMA Band 6 (ν = 233 GHz, λ = 1.3 mm) continuum observations towards 68 'normal' star-forming galaxies within two Coma-like progenitor structures at z = 2.10 and 2.47, from which ISM masses are derived, providing the largest census of molecular gas mass in overdense environments at these redshifts. Our sample comprises galaxies with a stellar mass range of 1 × 10 9 M ⊙ − 4 × 10 11 M ⊙ with a mean M ⋆ ≈ 6 × 10 10 M ⊙ . Combining these measurements with multiwavelength observations and SED modeling, we characterize the gas mass fraction and the star formation efficiency, and infer the impact of the environment on galaxies' evolution. Most of our detected galaxies ( 70%) have star formation efficiencies and gas fractions similar to those found for coeval field galaxies and in agreement with the field scaling relations. However, we do find that the proto-clusters contain an increased fraction of massive, gas-poor galaxies, with low gas fractions (f gas 6 − 10 %) and red rest-frame ultraviolet/optical colors typical of post-starburst and passive galaxies. The relatively high abundance of passive galaxies suggests an accelerated evolution of massive galaxies in proto-cluster environments. The large fraction of quenched galaxies in these overdense structures also implies that environmental quenching takes place during the early phases of cluster assembly, even before virialization. From our data, we derive a quenching efficiency of ǫ q ≈ 0.45 and an upper limit on the quenching timescale of τ q < 1 Gyr.

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Section: The Star Formation Efficiencysupporting

confidence: 77%

Section: Introductionmentioning

confidence: 99%

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

Zavala

Casey

Scoville

et al. 2019

ApJ

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“…A question arises about what mechanisms may be responsible for this enhancement. Several physical mechanisms might contribute to a larger cross section of Mg ii in group galaxies, including higher gas fractions for satellite galaxies in dense environments (Noble et al 2017) or stronger outflows from stellar winds due to enhanced star-formation (McGee et al 2014). There seems however to be no clear consensus on the relevance of these mechanisms in groups at z ≈ 1 (Wetzel et al 2012;Rudnick et al 2017;Fossati et al 2017).…”

Section: The Origin Of Enhanced Cold Gas In Galaxy Groupsmentioning

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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“…Gas-rich galaxies have been observed in high-z clusters and protoclusters (Hayashi et al 2017;Noble et al 2017), with star formation rates up to 800 M yr −1 (Santos et al 2015). A large reservoir of diffuse cold and metal-rich molecular gas (M H 2 ∼ 10 11 M ) extending for 50-70 kpc was found around the radio galaxy at the center of the z=2.2 Spiderweb protocluster (Emonts et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Discovery of a galaxy overdensity around a powerful, heavily obscured FRII radio galaxy atz= 1.7: star formation promoted by large-scale AGN feedback?

Gilli¹,

Mignoli²,

Peca³

et al. 2019

A&A

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We report the discovery of a galaxy overdensity around a Compton-thick Fanaroff-Riley type II (FRII) radio galaxy at z=1.7 in the deep multiband survey around the z=6.3 quasi-stellar object (QSO) SDSS J1030+0524. Based on a 6hr VLT/MUSE and on a 4hr LBT/LUCI observation, we identify at least eight galaxy members in this structure with spectroscopic redshift z=1.687-1.699, including the FRII galaxy at z=1.699. Most members are distributed within 400 kpc from the FRII core. Nonetheless, the whole structure is likely much more extended, as one of the members was serendipitously found at ∼800 kpc projected separation. The classic radio structure of the FRII itself extends for ∼ 600 kpc across the sky. Most of the identified overdensity members are blue, compact galaxies that are actively forming stars at rates of ∼8-60 M yr −1 . For the brightest of them, a half-light radius of 2.2±0.8 kpc at 8000Å rest-frame was determined based on adaptive optics-assisted observations with LBT/SOUL in the Ks band. We do not observe any strong galaxy morphological segregation or concentration around the FRII core. This suggests that the structure is far from being virialized and likely constitutes the progenitor of a local massive galaxy group or cluster caught in its main assembly phase. Based on a 500ks Chandra ACIS-I observation, we found that the FRII nucleus hosts a luminous QSO (L 2−10keV = 1.3 × 10 44 erg s −1 , intrinsic and rest-frame) that is obscured by Compton-thick absorption (N H = 1.5±0.6×10 24 cm −2 ). Under standard bolometric corrections, the total measured radiative power (L rad ∼ 4 × 10 45 erg s −1 ) is similar to the jet kinetic power that we estimated from radio observations at 150MHz (P kin = 6.3 × 10 45 erg s −1 ), in agreement with what is observed in powerful jetted AGN. Our Chandra observation is the deepest so far for a distant FRII within a galaxy overdensity. It revealed significant diffuse X-ray emission within the region that is covered by the overdensity. In particular, X-ray emission extending for ∼240 kpc is found around the eastern lobe of the FRII. Four out of the six MUSE star-forming galaxies in the overdensity are distributed in an arc-like shape at the edge of this diffuse X-ray emission. These objects are concentrated within 200 kpc in the plane of the sky and within 450 kpc in radial separation. Three of them are even more concentrated and fall within 60 kpc in both transverse and radial distance. The probability of observing four out of the six z = 1.7 sources by chance at the edge of the diffuse emission is negligible. In addition, these four galaxies have the highest specific star formation rates of the MUSE galaxies in the overdensity and lie above the main sequence of field galaxies of equal stellar mass at z=1.7. We propose that the diffuse X-rays originate from an expanding bubble of gas that is shock heated by the FRII jet, and that star formation is promoted by the compression of the cold interstellar medium of the galaxies around the bubble, which may be remarkable evidence of pos...

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ALMA Observations of Gas-rich Galaxies in z ∼ 1.6 Galaxy Clusters: Evidence for Higher Gas Fractions in High-density Environments

Cited by 97 publications

References 63 publications

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

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

Discovery of a galaxy overdensity around a powerful, heavily obscured FRII radio galaxy atz= 1.7: star formation promoted by large-scale AGN feedback?

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ALMA Observations of Gas-rich Galaxies in z ∼ 1.6 Galaxy Clusters: Evidence for Higher Gas Fractions in High-density Environments

Cited by 97 publications

References 63 publications

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z ≈ 2.0–2.5

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

Discovery of a galaxy overdensity around a powerful, heavily obscured FRII radio galaxy atz= 1.7: star formation promoted by large-scale AGN feedback?

Contact Info

Product

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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