Revealing the Environmental Dependence of Molecular Gas Content in a Distant X-Ray Cluster at z = 2.51

Wang, Tao; Elbaz, D.; Daddi, E.; Liu, Daizhong; Kodama, Tadayuki; Tanaka, Ichi; Schreiber, C.; Zanella, Anita; Valentino, F.; Sargent, M.; Kohno, Kotaro; Xiao, Mengyuan; Pannella, M.; Ciesla, L.; Gobat, R.; Koyama, Yusei

doi:10.3847/2041-8213/aaeb2c

Cited by 66 publications

(122 citation statements)

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“…In contrast, it has been shown that at high-redshift massive galaxies (often residing in the proto-clusters, i.e., the progenitors of the clusters at redshift zero) can have efficient star formation (e.g. Miller et al 2018;Wang et al 2018). Because the lognormal parametrisation leaves a tail on the high mass end, it might mimic this effect, and the choice of the this shape is therefore justified.…”

Section: From Accretion Onto the Dark Matter Haloes To Sfrmentioning

confidence: 99%

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

Maniyar

Béthermin

Lagache

2021

A&A

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Modelling the anisotropies in the cosmic infrared background (CIB) on all the scales is a challenging task because the nature of the galaxy evolution is complex and too many parameters are therefore often required to fit the observational data. We present a new halo model for the anisotropies of the CIB using only four parameters. Our model connects the mass accretion on the dark matter haloes to the star formation rate. Despite its relative simplicity, it is able to fit both the Planck and Herschel CIB power spectra and is consistent with the external constraints for the obscured star formation history derived from infrared deep surveys used as priors for the fit. Using this model, we find that the halo mass with the maximum efficiency for converting the accreted baryons into stars is log 10 M max = 12.94 +0.02 −0.02 M , consistent with other studies. Accounting for the mass loss through stellar evolution, we find for an intermediate-age galaxy that the star formation efficiency defined as M (z)/M b (z) is equal to 0.19 and 0.21 at redshift 0.1 and 2, respectively, which agrees well with the values obtained by previous studies. A CIB model is used for the first time to simultaneously fit Planck and Herschel CIB power spectra. The high angular resolution of Herschel allows us to reach very small scales, making it possible to constrain the shot noise and the one-halo term separately, which is difficult to do using the Planck data alone. However, we find that large angular scale Planck and Herschel data are not fully compatible with the small-scale Herschel data (for > 3000). The CIB is expected to be correlated with the thermal Sunyaev-Zel'dovich (tSZ) signal of galaxy clusters. Using this halo model for the CIB and a halo model for the tSZ with a single parameter, we also provide a consistent framework for calculating the CIB × tSZ cross correlation, which requires no additional parameter. To a certain extent, the CIB at high frequencies traces galaxies at low redshifts that reside in the clusters contributing to the tSZ, giving rise to the one-halo term of this correlation, while the two-halo term comes from the overlap in the redshift distribution of the tSZ clusters and CIB galaxies. The CIB × tSZ correlation is thus found to be higher when inferred with a combination of two widely spaced frequency channels (e.g. 143 × 857 GHz). We also find that even at ∼ 2000, the two-halo term of this correlation is still comparable to the one-halo term and has to be accounted for in the total cross-correlation. The CIB, tSZ, and CIB × tSZ act as foregrounds when the kinematic SZ (kSZ) power spectrum is measured from the cosmic microwave background power spectrum and need to be removed. Because of its simplistic nature and the low number of parameters, the halo model formalism presented here for these foregrounds is quite useful for such an analysis to measure the kSZ power spectrum accurately.

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Section: From Accretion Onto the Dark Matter Haloes To Sfrmentioning

confidence: 99%

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

Maniyar

Béthermin

Lagache

2021

A&A

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“…In addition, a comparison with galaxies in the field, in clusters, and in other proto-clusters can provide insights into the role played by the environment. To this end, we collected CO data from the literature for galaxies in clusters (62 galaxies in 11 clusters, Wang et al 2018;Rudnick et al 2017;Stach et al 2017;Aravena et al 2012;Casasola et al 2013;Castignani et al 2018;Coogan et al 2018;Hayashi et al 2017;Webb et al 2017) and in proto-clusters (16 galaxies in four proto-clusters, Dannerbauer et al 2017;Ivison et al 2013;Tadaki et al 2014;Lee et al 2017), and of SMGs and AGN in the z = 1-3 redshift range (31 SMGs, 15 AGN, and 38 obscured AGN, Perna et al 2018). In order to represent normal star-forming galaxies and SB galaxies, we used the SFR-M rela-tion 5 from Speagle et al (2014), and the L CO − L IR relation from MS and SB galaxies as derived by Sargent et al (2014) 6 For estimating molecular gas masses, we converted all high transition CO luminosities to L CO(1−0) , when not available, using the median brightness temperature ratios derived by Bothwell et al (2013).…”

Section: Co Line Propertiesmentioning

confidence: 99%

“…Gas masses are derived using M gas = α CO L CO(1−0) . The adopted α CO value for each galaxy is that reported in earlier studies (Tadaki et al 2014;Dannerbauer et al 2017;Wang et al 2018;Lee et al 2017;Ivison et al 2013), and had been fixed to either α CO = 0.8, typical of SB galaxies, or α CO = 4.0-4.36, typical of normal SFGs. We remind that we consider as an SB any source with SFR > 3 × SFR MS , but this definition might not match what was found in other published samples.…”

Section: Co Line Propertiesmentioning

confidence: 99%

“…Until recently, the limited number of CO detections in high-redshift (z 1.5-2) structures had not provided a consensus on the influence of the environment on the gas contents of galaxies (Aravena et al 2012;Wagg et al 2012;Casasola et al 2013;Stach et al 2017;Noble et al 2017;Coogan et al 2018;Tadaki et al 2014;Lee et al 2017;Dannerbauer et al 2017). However, a recent study by Wang et al (2018) of a cluster at z = 2.51, known as CL J1001+0220, has clearly shown that the molecular gas properties of cluster members are correlated with their location, that is with their distance from the cluster core (see also Hayashi et al 2017, for XMMXCS J2215.9−1738 at z = 1.46). Thus galaxies remain relatively gas-rich when they first enter the cluster, but their gas content is rapidly reduced as they approach the cluster centre.…”

Section: Introductionmentioning

confidence: 99%

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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

A&A

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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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“…Evidence for direct, resolved stripping of CO has also been observed in a handful of galaxies (Lee & Chung 2018;Moretti et al 2018;Cramer et al 2020;Jáchym et al 2019), while additional cases of molecular disturbances have been found in Virgo (Lee et al 2017a). Broadly speaking, at intermediate and higher redshifts, reports are even more varied, with some suggestions that (proto)clusters favour H2-poor galaxies (Jablonka et al 2013;Castignani et al 2018;Coogan et al 2018), others that they favour H2-rich galaxies (Noble et al 2017;Hayashi et al 2018), others that they favour H2normal galaxies (Dannerbauer et al 2017;Lee et al 2017b;Rudnick et al 2017;Darvish et al 2018;Wu et al 2018), or a mass-dependent/phase-space-dependent combination thereof (Hayashi et al 2017;Wang et al 2018;Tadaki et al 2019).…”

mentioning

confidence: 99%

Molecular hydrogen in IllustrisTNG galaxies: carefully comparing signatures of environment with local CO and SFR data

Stevens

Lagos

Cortese

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We examine how the post-processed content of molecular hydrogen (H2) in galaxies from the TNG100 cosmological, hydrodynamic simulation changes with environment at z = 0, assessing central/satellite status and host halo mass. We make close comparisons with the carbon monoxide (CO) emission survey xCOLD GASS where possible, having mock-observed TNG100 galaxies to match the survey’s specifications. For a representative sample of host haloes across 1011 ≲ M200c/M⊙ < 1014.6, TNG100 predicts that satellites with m* ≥ 109 M⊙ should have a median deficit in their H2fractions of ∼0.6 dex relative to centrals of the same stellar mass. Once observational and group-finding uncertainties are accounted for, the signature of this deficit decreases to ∼0.2 dex. Remarkably, we calculate a deficit in xCOLD GASS satellites’ H2content relative to centrals of 0.2–0.3 dex, in line with our prediction. We further show that TNG100 and SDSS data exhibit continuous declines in the average star formation rates of galaxies at fixed stellar mass in denser environments, in quantitative agreement with each other. By tracking satellites from their moment of infall in TNG100, we directly show that atomic hydrogen (H i) is depleted at fractionally higher rates than H2on average. Supporting this picture, we find that the H2/H i mass ratios of satellites are elevated relative to centrals in xCOLD GASS. We provide additional predictions for the effect of environment on H2 — both absolute and relative to H i — that can be tested with spectral stacking in future CO surveys.

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Revealing the Environmental Dependence of Molecular Gas Content in a Distant X-Ray Cluster at z = 2.51

Cited by 66 publications

References 50 publications

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

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

Molecular hydrogen in IllustrisTNG galaxies: carefully comparing signatures of environment with local CO and SFR data

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