ALMA Pinpoints a Strong Overdensity of U/LIRGs in the Massive Cluster XCS J2215 at z = 1.46

Stach, S. M.; Swinbank, A. M.; Smail, Ian; Hilton, Matthew; Simpson, J. M.; Cooke, Elizabeth A.

doi:10.3847/1538-4357/aa93f6

Cited by 47 publications

(63 citation statements)

References 83 publications

(148 reference statements)

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“…That the environmental quenching efficiency for lower-M * declines rapidly over this window perhaps suggests a similar decline for higher-M * at even higher redshifts than are studied here. Such a picture is consistent with several works studying clusters at z > ∼ 1.4, in which the average star formation is seen in many cases to be unperturbed or even enhanced relative to field environments (e.g., Brodwin et al 2013;Alberts et al 2014Alberts et al , 2016Santos et al 2014;Wang et al 2016;Stach et al 2017;Coogan et al 2018).…”

Section: Environmental Quenching Efficiencysupporting

confidence: 91%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼5000 spectroscopically-confirmed galaxies drawn from the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey we investigate the relationship between color and galaxy density for galaxy populations of various stellar masses in the redshift range 0.55 ≤ z ≤ 1.4. The fraction of galaxies with colors consistent with no ongoing star formation ( f q ) is broadly observed to increase with increasing stellar mass, increasing galaxy density, and decreasing redshift, with clear differences observed in f q between field and group/cluster galaxies at the highest redshifts studied. We use a semi-empirical model to generate a suite of mock group/cluster galaxies unaffected by environmentally-specific processes and compare these galaxies at fixed stellar mass and redshift to observed populations to constrain the efficiency of environmentally-driven quenching (Ψ convert ). High-density environments from 0.55 ≤ z ≤ 1.4 appear capable of efficiently quenching galaxies with log(M * /M ⊙ ) > 10.45. Lower stellar mass galaxies also appear efficiently quenched at the lowest redshifts studied here, but this quenching efficiency is seen to drop precipitously with increasing redshift. Quenching efficiencies, combined with simulated group/cluster accretion histories and results on the star formation rate-density relation from a companion ORELSE study, are used to constrain the average time from group/cluster accretion to quiescence and the elapsed time between accretion and the inception of the quenching event. These timescales were constrained to be t convert = 2.4 ± 0.3 and t delay = 1.3 ± 0.4 Gyr, respectively, for galaxies with log(M * /M ⊙ ) > 10.45 and t convert = 3.3 ± 0.3 and t delay = 2.2 ± 0.4 Gyr for lower stellar mass galaxies. These quenching efficiencies and associated timescales are used to rule out certain environmental mechanisms as being the primary processes responsible for transforming the star-formation properties of galaxies over this 4 Gyr window in cosmic time.

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Section: Environmental Quenching Efficiencysupporting

confidence: 91%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In Figure 2 we show the CO(3-2) luminosity (L CO(3−2) ) and infrared luminosity (L IR ) derived from the 250-870 µm photometry (Swinbank et al 2014) for 870-µm selected SMGs with detected 12 CO. Included for comparison are starforming galaxies with CO(2-1), CO(3-2), or CO(4-3) measurements (Bothwell et al 2013;Daddi et al 2015;Papovich et al 2016;Lee et al 2017;Stach et al 2017;Hayashi et al 2017). Where CO(3-2) observations are unavailable, CO(2-1) and CO(4-3) luminosities are converted to L CO(3−2) using the brightness temperature ratios for the SMGs compiled by Carilli & Walter (2013).…”

Section: Analysis and Discussionmentioning

confidence: 99%

An ALMA survey of CO in submillimetre galaxies: companions, triggering, and the environment in blended sources

Wardlow

Simpson

Smail

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present ALMA observations of the mid-J 12 CO emission from six single-dish selected 870-µm sources in the Extended Chandra Deep Field-South (ECDFS) and UKIDSS Ultra-Deep Survey (UDS) fields. These six single-dish submillimetre sources were selected based on previous ALMA continuum observations, which showed that each comprised a blend of emission from two or more individual submillimetre galaxies (SMGs), separated on 5-10 scales. The six single-dish submillimetre sources targeted correspond to a total of 14 individual SMGs, of which seven have previouslymeasured robust optical/near-infrared spectroscopic redshifts, which were used to tune our ALMA observations. We detect CO(3-2) or CO(4-3) at z = 2.3-3.7 in seven of the 14 SMGs, and in addition serendipitously detect line emission from three gasrich companion galaxies, as well as identify four new 3.3-mm selected continuum sources in the six fields. Joint analysis of our CO spectroscopy and existing data suggests that 64(±18)% of the SMGs in blended submillimetre sources are unlikely to be physically associated. However, three of the SMG fields (50%) contain new, serendipitously-detected CO-emitting (but submillimetre-faint) sources at similar redshifts to the 870-µm selected SMGs we targeted. These data suggest that the SMGs inhabit overdense regions, but that these are not sufficiently overdense on ∼ 100 kpc scales to influence the source blending given the short lifetimes of SMGs. We find that 21 ± 12% of SMGs have spatially-distinct and kinematically-close companion galaxies (∼ 8-150 kpc and 300 km s −1 ), which may have enhanced their star-formation via gravitational interactions.

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“…Their work includes CO results from Hayashi et al (2017). The sample of Stach et al (2017) comprising six sources with independent CO detections from the same cluster is also entirely included in Hayashi et al (2018). Therefore, concerning XMMXCS J2215.9-1738 cluster galaxies, we consider their more recent results.…”

Section: Effective Radiimentioning

confidence: 99%

Molecular gas in two companion cluster galaxies at z = 1.2

Castignani

Combes

Salomé

et al. 2018

A&A

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Context. Probing both star formation history and evolution of distant cluster galaxies is essential to evaluate the effect of dense environment on shaping the galaxy properties we observe today. Aims. We investigate the effect of cluster environment on the processing of the molecular gas in distant cluster galaxies. We study the molecular gas properties of two star-forming galaxies separated by 6 kpc in the projected space and belonging to a galaxy cluster selected from the Irac Shallow Cluster Survey, at a redshift z = 1.2, that is, ∼ 2 Gyr after the cosmic star formation density peak. This work describes the first CO detection from 1 < z < 1.4 star-forming cluster galaxies with no clear reported evidence of active galactic nuclei. Methods. We exploit observations taken with the NOEMA interferometer at ∼ 3 mm to detect CO(2-1) line emission from the two selected galaxies, unresolved by our observations. Results. Based on the CO(2-1) spectrum, we estimate a total molecular gas mass M(H 2 ) = (2.2 +0.5 −0.4 ) × 10 10 M , where fully excited gas is assumed, and a dust mass M dust < 4.2 × 10 8 M for the two blended sources. The two galaxies have similar stellar masses and Hα-based star formation rates (SFRs) found in previous work, as well as a large relative velocity of ∼400 km/s estimated from the CO(2-1) line width. These findings tend to privilege a scenario where both sources contribute to the observed CO(2-1). Using the archival Spitzer MIPS flux at 24 µm we estimate an SFR(24µm) = (28 +12 −8 ) M /yr for each of the two galaxies. Assuming that the two sources contribute equally to the observed CO(2-1), our analysis yields a depletion timescale of τ dep = (3.9 +1.4 −1.8 ) × 10 8 yr, and a molecular gas to stellar mass ratio of 0.17 ± 0.13 for each of two sources, separately. We also provide a new, more precise measurement of an unknown weighted mean of the redshifts of the two galaxies, z = 1.163 ± 0.001. Conclusions. Our results are in overall agreement with those of other distant cluster galaxies and with model predictions for main sequence (MS) field galaxies at similar redshifts. The two target galaxies have molecular gas mass and depletion times that are marginally compatible with, but smaller than those of MS field galaxies, suggesting that the molecular gas has not been sufficiently refueled. We speculate that the cluster environment might have played a role in preventing the refueling via environmental mechanisms such as galaxy harassment, strangulation, ram-pressure, or tidal stripping. Higher-resolution and higher-frequency observations will enable us to spatially resolve the two sources and possibly distinguish between different gas processing mechanisms.

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ALMA Pinpoints a Strong Overdensity of U/LIRGs in the Massive Cluster XCS J2215 at z = 1.46

Cited by 47 publications

References 83 publications

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

An ALMA survey of CO in submillimetre galaxies: companions, triggering, and the environment in blended sources

Molecular gas in two companion cluster galaxies at z = 1.2

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