Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2

Strazzullo, V.; Coogan, R. T.; Daddi, E.; Sargent, M.; Gobat, R.; Valentino, F.; Béthermin, M.; Pannella, M.; Dickinson, Mark; Renzini, A.; Arimoto, N.; Cimatti, A.; Dannerbauer, H.; Finoguenov, A.; Liu, Daizhong; Onodera, Makoto

doi:10.3847/1538-4357/aacd10

Cited by 37 publications

(31 citation statements)

References 131 publications

(179 reference statements)

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“…We stress here that the BCG candidate of the cluster Cl J1449+0856 at z = 2 was first described by Gobat et al (2011) and has recently been observed with ALMA Strazzullo et al 2018). No stellar mass estimate is reported for this source in these studies.…”

Section: Molecular Gas Diagramsmentioning

confidence: 77%

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Castignani

Combes

Salomé

et al. 2019

A&A

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Context. Low luminosity radio galaxies (LLRGs) typically reside in dense megaparsec-scale environments and are often associated with brightest cluster galaxies (BCGs). They are an excellent tool to study the evolution of molecular gas reservoirs in giant ellipticals, even close to the active galactic nucleus. Aims. We investigate the role of dense megaparsec-scale environment in processing molecular gas in LLRGs in the cores of galaxy (proto-)clusters. To this aim we selected within the COSMOS and DES surveys a sample of five LLRGs at z = 0.4 − 2.6 that show evidence of ongoing star formation on the basis of their far-infrared (FIR) emission. Methods. We assembled and modeled the FIR-to-UV spectral energy distributions (SEDs) of the five radio sources to characterize their host galaxies in terms of stellar mass and star formation rate. We observed the LLRGs with the IRAM-30m telescope to search for CO emission. We then searched for dense megaparsec-scale overdensities associated with the LLRGs using photometric redshifts of galaxies and the Poisson Probability Method, which we have upgraded using an approach based on the wavelet-transform (wPPM), to ultimately characterize the overdensity in the projected space and estimate the radio galaxy miscentering. Color-color and colormagnitude plots were then derived for the fiducial cluster members, selected using photometric redshifts. Results. Our IRAM-30m observations yielded upper limits to the CO emission of the LLRGs, at z = 0.39, 0.61, 0.91, 0.97, and 2.6. For the most distant radio source, COSMOS-FRI 70 at z = 2.6, a hint of CO(7→6) emission is found at 2.2σ. The upper limits found for the molecular gas content M(H 2 )/M <0.11, 0.09, 1.8, 1.5, and 0.29, respectively, and depletion time τ dep (0.2 − 7) Gyr of the five LLRGs are overall consistent with the corresponding values of main sequence field galaxies. Our SED modeling implies large stellar-mass estimates in the range log(M /M ) = 10.9 − 11.5, typical for giant ellipticals. Both our wPPM analysis and the cross-matching of the LLRGs with existing cluster/group catalogs suggest that the megaparsec-scale overdensities around our LLRGs are rich ( 10 14 M ) groups and show a complex morphology. The color-color and color-magnitude plots suggest that the LLRGs are consistent with being star forming and on the high-luminosity tail of the red sequence. The present study thus increases the still limited statistics of distant cluster core galaxies with CO observations. Conclusions. The radio galaxies of this work are excellent targets for ALMA as well as next-generation telescopes such as the James Webb Space Telescope.

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Section: Molecular Gas Diagramsmentioning

confidence: 77%

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Castignani

Combes

Salomé

et al. 2019

A&A

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“…Webb et al (2017) recently detected CO(2→1) with the Large Millimeter Telescope (LMT), which is associated with a large reservoir (∼ 10 11 M ) of molecular gas that is possibly associated with the BCG and/or its nearby cluster core companions within the 25 arcsec diameter (i.e., ∼ 200 kpc at z = 1.7) beam of the LMT. By spatially resolving, both in continuum and in CO, the BCG from each of its nearby companions separately, the present study the present study is one of the first to probe both molecular gas and dust reservoirs of z 1 BCGs in detail (Emonts et al 2013(Emonts et al , 2016Coogan et al 2018;Strazzullo et al 2018;Castignani et al 2019). We thus aim to unveil the mechanisms at play for the assembly and the star formation fueling of the most distant BCGs.…”

Section: Introductionmentioning

confidence: 95%

Environmental processing in cluster core galaxies at z = 1.7

Castignani

Combes

Salomé

2020

A&A

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Today, the brightest cluster galaxies (BCGs) are passive and very massive galaxies at the center of their clusters, and they still accrete mass through swallowing companions and gas from cooling flows. However their formation history is not well known. We report CO(4→3) and continuum map observations of the SpARCS1049+56 BCG at z = 1.709, one of the most distant known BCGs. Our observations yield M H 2 < 1.1 × 10 10 M for the BCG; while in CO(4→3), we detect two gas-rich companions at the northeast and southeast of the BCG, within 20 kpc, with L CO(4→3) = (5.8 ± 0.6) × 10 9 K km s −1 pc 2 and (7.4 ± 0.7) × 10 9 K km s −1 pc 2 , respectively. The northern companion is associated with a pair of merging cluster galaxies, while the southern one shows a southern tail in CO(4→3), which was also detected in continuum, and we suggest it to be the most distant jellyfish galaxy for which ram pressure stripping is effectively able to strip off its dense molecular gas. This study probes the presence of rare gas-rich systems in the very central region of a distant cluster core, which will potentially merge into the BCG itself. Currently, we may thus be seeing the reversal of the star formation versus density relation at play in the distant universe. This is the first time the assembly of high-z progenitors of our local BCGs can be studied in such great detail.

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“…Therefore, massive galaxy clusters must have formed the bulk of their member galaxies' stellar mass at early times (e.g., Archibald et al 2001;Hopkins & Beacom 2006). At high-redshift, a significant amount of enhancement of star formation is observed in galaxies residing in candidate protoclusters -the progenitors of massive local galaxy clusters (e.g., Steidel et al 2000;Geach et al 2005;Chapman et al 2009;Capak et al 2011;Muzzin et al 2011;Clements et al 2014;Smail et al 2014;Webb et al 2013;Casey et al 2015;Ma et al 2015;Daddi et al 2017;Umehata et al 2017;Stach et al 2017Stach et al , 2018Strazzullo et al 2018). Thus, there is some evidence that at high redshift, galaxy evolution is accelerated at early times in regions of strong overdensity.…”

Section: Introductionmentioning

confidence: 99%

Two sub-millimetre bright protoclusters bounding the epoch of peak star-formation activity

Lacaille

Chapman

Smail

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present James Clerk Maxwell Telescope Submillimetre Common-User Bolometer Array 2 (SCUBA-2) 850 & 450 µm observations (σ 850 ∼ 0.5 mJy, σ 450 ∼ 5 mJy) of the HS1549+19 and HS1700+64 survey fields containing two of the largest known galaxy over-densities at z = 2.85 and 2.30, respectively. We detect 56 sub-millimetre galaxies (SMGs) with SNR > 4 over ∼ 50 arcmin 2 at 850 µm with flux densities of 3 -17 mJy. The number counts indicate over-densities in the 3-arcmin diameter core region (∼ 1.5 Mpc at z = 2.5) of 6 +4 −2 × (HS1549) and 4 +6 −2 × (HS1700) compared to blank field surveys. Within these core regions, we spectroscopically confirm that approximately one third of the SMGs lie at the protocluster redshifts for both HS1549 and HS1700. We use statistical identifications of other SMGs in the wider fields to constrain an additional four candidate protocluster members in each system. We combine multi wavelength estimates of the star-formation rates (SFRs) from Lyman-break dropout-and narrowband-selected galaxies, and the SCUBA-2 SMGs, to estimate total SFRs of 12,500 ± 2800 M yr −1 (4900 ± 1200 M yr −1 ) in HS1549 (HS1700), and SFR densities (SFRDs) within the central 1.5-Mpc diameter of each protocluster to be 3000 ± 900 M yr −1 Mpc −3 (1300 ± 400 M yr −1 Mpc −3 ) in the HS1549 (HS1700) protocluster, ∼ 10 4 × larger than the global SFRDs found at their respective epochs, due to the concentration of starforming galaxies in the small volume of the dense cluster cores. Our results suggest centrally concentrated starbursts within protoclusters may be a relatively common scenario for the build up of mass in rich clusters assembling at z 2.

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Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2

Cited by 37 publications

References 131 publications

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Molecular gas in radio galaxies in dense megaparsec-scale environments at z = 0.4–2.6

Environmental processing in cluster core galaxies at z = 1.7

Two sub-millimetre bright protoclusters bounding the epoch of peak star-formation activity

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