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

Castignani, G.; Combes, F.; Salomé, P.; Benoist, Christophe; Chiaberge, M.; Freundlich, Jonathan; Zotti, G. de

doi:10.1051/0004-6361/201834066

Cited by 21 publications

(52 citation statements)

References 201 publications

(288 reference statements)

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“…Although the time scales are formally consistent with those of MS galaxies, as seen in Figs. 4, 5 the two BCGs tend to populate the regions occupied by other rare distant star forming BCGs (e.g., Castignani et al 2019Castignani et al , 2020a, with large molecular gas reservoirs and strong star formation activity.…”

Section: Star Formation and Depletion Timementioning

confidence: 99%

“…Among the distant 64 cluster galaxies with CO observations and stellar mass estimates considered in the previous Section there are only a few BCG candidates. As discussed in Castignani et al (2019Castignani et al ( , 2020a they are:…”

Section: Distant Bcgs Observed In Comentioning

confidence: 99%

“…• We have also included for our comparison six additional BCG (candidates) at z ∼ 0.4 − 1 that were observed by Castignani et al (2019Castignani et al ( , 2020a using the IRAM-30m as part of a large search for CO in distant star forming BCGs, which were selected from several surveys (DES, SDSS, COSMOS, and SpARCS). These six sources are DES-RG 399 (z = 0.39), DES-RG 708 (z = 0.61), COSMOS-FRI 16 (z = 0.97), COSMOS-FRI 31 (z = 0.91), 3C 244.1 (z = 0.43), and SDSS J161112.65+550823.5 (z = 0.91), for which in our previous studies we set robust upper limits to their molecular gas content.…”

Section: Distant Bcgs Observed In Comentioning

confidence: 99%

“…4. For a comparison, BCGs candidates from our recent IRAM-30m campaign Castignani et al (2019Castignani et al ( , 2020a, at similar redshifts of z ∼ 0.4 − 0.1 than CLASH BCGs, have indeed upper limits ranging from M H 2 /M 2 (COSMOS-FRI 16, 31 at z ∼ 0.9 − 1), down to lower values of M H 2 /M ∼ 0.1 − 0.2 (SDSS J161112.65+550823.5, 3C 244.1, DES-RG 399, and DES-RG 708 at z ∼ 0.4 − 0.9). SpARCS 104922.6+564032.5 BCG at z = 1.7 which we included in our comparison sample represents a remarkable exception.…”

Section: Molecular Gas Reservoirsmentioning

confidence: 99%

“…This work is part of a larger search done over a wide range of redshifts, z ∼ 0.4 − 2.6, to detect molecular gas in distant BCGs (Castignani et al 2019(Castignani et al , 2020a. The paper is structured as follows: in Sect.…”

Section: Introductionmentioning

confidence: 99%

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Molecular gas in distant brightest cluster galaxies

Castignani

Combes

Salomé

et al. 2020

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Brightest cluster galaxies (BCGs) are excellent laboratories to study galaxy evolution in dense Mpc-scale environments. We have observed in CO(1→0), CO(2→1), CO(3→2), or CO(4→3), with the IRAM-30m, 18 BCGs at z ∼ 0.2 − 0.9 that are drawn from the Cluster Lensing And Supernova survey with Hubble (CLASH) survey. Our sample includes RX1532, which is our primary target, being among the BCGs with the highest star formation rate (SFR 100 M /yr) in the CLASH sample. We unambiguously detected both CO(1→0) and CO(3→2) in RX1532, yielding a large reservoir of molecular gas, M H 2 = (8.7 ± 1.1) × 10 10 M , and a high level of excitation r 31 = 0.75 ± 0.12. A morphological analysis of the Hubble Space Telescope I-band image of RX1532 reveals the presence of clumpy substructures both within and outside the half-light radius r e = (11.6 ± 0.3) kpc, similarly to those found independently both in ultraviolet and in H α in previous work. We tentatively detected CO(1→0) or CO(2→1) in four other BCGs, with molecular gas reservoirs in the range M H 2 = 2 × 10 10−11 M . For the remaining 13 BCGs we set robust upper limits of M H 2 /M 0.1, which are among the lowest molecular gas to stellar mass ratios found for distant ellipticals and BCGs. By comparison with distant cluster galaxies observed in CO our study shows that RX1532 (M H 2 /M = 0.40 ± 0.05) belongs to the rare population of star forming and gas-rich BCGs in the distant universe. By using available X-ray based estimates of the central intra-cluster medium entropy, we show that the detection of large reservoirs of molecular gas M H 2 10 10 M in distant BCGs is possible when the two conditions are met: i) high SFR and ii) low central entropy, which favors the condensation and the inflow of gas onto the BCGs themselves, similarly to what has been previously found for some local BCGs.

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Section: Star Formation and Depletion Timementioning

confidence: 99%

Section: Distant Bcgs Observed In Comentioning

confidence: 99%

Section: Distant Bcgs Observed In Comentioning

confidence: 99%

Section: Molecular Gas Reservoirsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Molecular gas in distant brightest cluster galaxies

Castignani

Combes

Salomé

et al. 2020

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Using ALMA to resolve the nature of the early star-forming large-scale structure PLCK G073.4−57.5

Kneißl

Polletta

Martinache

et al. 2019

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Galaxy clusters at high redshift are key targets for understanding matter assembly in the early Universe, yet they are challenging to locate. A sample of more than 2000 high-z candidate structures has been found using Planck's all-sky submillimetre maps, and a sub-set of 234 have been followed up with Herschel-SPIRE, which showed that the emission can be attributed to large overdensities of dusty star-forming galaxies. As a next step, we need to resolve and characterise the individual galaxies giving rise to the emission seen by Planck and Herschel, and to find out whether they constitute the progenitors of present-day, massive galaxy clusters. Thus, we targeted the eight brightest Herschel-SPIRE sources in the centre of the Planck peak PLCK G073.4−57.5 using ALMA at 1.3 mm, and complemented these observations with multi-wavelength data from Spitzer-IRAC, CFHT-WIRCam in the J and K s bands, and JCMT's SCUBA-2 instrument. We detected a total of 18 millimetre galaxies brighter than 0.3 mJy within the 2.4 arcmin 2 ALMA pointings, corresponding to an ALMA source density 8-30 times higher than average background estimates and larger than seen in typical 'proto-cluster' fields. We were able to match all but one of the ALMA sources to a near infrared (NIR) counterpart. The four most significant SCUBA-2 sources are not included in the ALMA pointings, but we find an 8 σ stacking detection of the ALMA sources in the SCUBA-2 map at 850 µm. We derive photometric redshifts, infrared (IR) luminosities, star-formation rates (SFRs), stellar masses (M), dust temperatures, and dust masses for all of the ALMA galaxies. Photometric redshifts identify two groups each of five sources, concentrated around z 1.5 and 2.4. The two groups show two 'red sequences', that is similar near-IR [3.6] − [4.5] colours and different J − K s colours. The majority of the ALMA-detected galaxies are on the SFR versus M main sequence (MS), and half of the sample is more massive than the characteristic M * at the corresponding redshift. We find that the z 1.5 group has total SFR = 840 +120 −100 M yr −1 and M = 5.8 +1.7 −2.4 × 10 11 M , and that the z 2.4 group has SFR = 1020 +310 −170 M yr −1 and M = 4.2 +1.5 −2.1 × 10 11 M , but the latter group is more scattered in stellar mass and around the MS. Serendipitous CO line detections in two of the galaxies appear to match their photometric redshifts at z = 1.54. We performed an analysis of star-formation efficiencies (SFEs) and CO-and mm-continuum-derived gas fractions of our ALMA sources, combined with a sample of 1 < z < 3 cluster and proto-cluster members, and observed trends in both quantities with respect to stellar masses and in comparison to field galaxies. A dedicated Herschel (Pilbratt et al. 2010) follow-up programme with the SPIRE instrument for 234 Planck targets (Planck Collab. XXXVII 2015) found a significant excess of 'red' sources (where red means S 350 / S 250 > 0.7 and S 500 / S 350 > 0.6, which is consistent with z > ∼ 2 SFGs), in comparison to reference SPIRE fields. Assuming a single com...

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Environmental processing in cluster core galaxies at z = 1.7

Castignani

Combes

Salomé

2020

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

Cited by 21 publications

References 201 publications

Molecular gas in distant brightest cluster galaxies

Molecular gas in distant brightest cluster galaxies

Using ALMA to resolve the nature of the early star-forming large-scale structure PLCK G073.4−57.5

Environmental processing in cluster core galaxies at z = 1.7

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