GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Gómez-Guijarro, Carlos; Elbaz, D.; Xiao, Mengyuan; Béthermin, M.; Franco, Maximilien; Magnelli, B.; Daddi, E.; Dickinson, Mark; Demarco, R.; Inami, Hanae; Rujopakarn, W.; Magdis, G.; Shu, Xinwen; Chary, R.-R.; Zhou, Luwenjia; Alexander, D. M.; Bournaud, F.; Ciesla, L.; Ferguson, Harry; Finkelstein, Steven L.; Giavalisco, Mauro; Iono, Daisuke; Juneau, Stéphanie; Kartaltepe, Jeyhan S.; Lagache, G.; Floc’h, E. Le; Leiton, R.; Lin, Lihwai; Motohara, Kentaro; Mullaney, James; Okumura, K.; Pannella, M.; Papovich, C.; Pope, Alexandra; Sargent, M.; Silverman, John D.; Treister, Ezequiel; Wang, Tao

doi:10.1051/0004-6361/202141615

Cited by 56 publications

(77 citation statements)

References 178 publications

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“…One possible class of progenitors could be dusty, extreme starbursts, or "submillimeter galaxies" (Toft et al 2012(Toft et al , 2014Wild et al 2020), which have the extremely high star formation rates and feedback necessary to produce galaxies like those in  L SQuIGG E (Spilker et al 2020a(Spilker et al , 2020b. At high redshift, submillimeter galaxies also lie slightly below quiescent galaxies in the mass-size plane (Gómez-Guijarro et al 2022). If they shut off their rapid star formation abruptly and uniformly, submillimeter galaxies would likely result in poststarburst SEDs and flat age gradients similar to those measured in  L SQuIGG E galaxies (Setton et al 2020).…”

Section: Preferential Fast Quenching In Compact Star-forming Galaxiesmentioning

confidence: 99%

The Compact Structures of Massive z ∼ 0.7 Post-starburst Galaxies in the SQuIGGL⃗E Sample

Setton

Verrico

Bezanson

et al. 2022

ApJ

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We present structural measurements of 145 spectroscopically selected intermediate-redshift (z ∼ 0.7), massive (M ⋆ ∼ 1011 M ⊙) post-starburst galaxies from the SQuIGG L ⃗ E sample measured using wide-depth Hyper Suprime-Cam i-band imaging. This deep imaging allows us to probe the sizes and structures of these galaxies, which we compare to a control sample of star-forming and quiescent galaxies drawn from the LEGA-C Survey. We find that post-starburst galaxies systematically lie ∼0.1 dex below the quiescent mass–size (half-light radius) relation, with a scatter of ∼0.2 dex. This finding is bolstered by nonparametric measures, such as the Gini coefficient and the concentration, which also reveal these galaxies to have more compact light profiles than both quiescent and star-forming populations at similar mass and redshift. The sizes of post-starburst galaxies show either negative or no correlation with the time since quenching, such that more recently quenched galaxies are larger or similarly sized. This empirical finding disfavors the formation of post-starburst galaxies via a purely central burst of star formation that simultaneously shrinks the galaxy and shuts off star formation. We show that the central densities of post-starburst and quiescent galaxies at this epoch are very similar, in contrast with their effective radii. The structural properties of z ∼ 0.7 post-starburst galaxies match those of quiescent galaxies that formed in the early universe, suggesting that rapid quenching in the present epoch is driven by a similar mechanism to the one at high redshift.

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Section: Preferential Fast Quenching In Compact Star-forming Galaxiesmentioning

confidence: 99%

The Compact Structures of Massive z ∼ 0.7 Post-starburst Galaxies in the SQuIGGL⃗E Sample

Setton

Verrico

Bezanson

et al. 2022

ApJ

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“…We compare our combined counts to results from recent ALMA observations that probe down to the sub-mJy level, as well as to predictions by state-of-the-art galaxy evolution models. To the literature data already compared in Paper IV at 1.1 − 1.3 mm (for details see Paper IV and references therein), we add number counts derived from six new dedicated surveys and three new models: a 20 arcmin 2 survey at 1.1 mm that contains a z = 3.09 protocluster (ALMA deep field in SSA22, Umehata et al 2018); a 69 arcmin 2 survey at 1.1 mm in the deepest HST-WFC3 H-band part of the GOODS-South field (GOODS-ALMA, Franco et al 2018); a 26 arcmin 2 survey at 1.2 mm in the GOODS-South field (ASAGAO, Hatsukade et al 2018); a 4.2 arcmin 2 survey at 1.2 mm in the HUDF (ASPECS-LP, González-López et al 2020); a 25 arcmin 2 serendipitous survey at 850 µm around a sample of spectroscopically confirmed star-forming galaxies in the COSMOS and CDF-South fields (ALPINE, Béthermin et al 2020); a 72 arcmin 2 survey at 1.1 mm in the GOODS-South field, including both small and large spatial scales (GOODS-ALMA 2.0, Gómez-Guijarro et al 2022); a semi-empirical model for the dust continuum number counts of galaxies (Popping et al 2020); a semi-analytic model of galaxy formation that includes Band 6 number counts predictions (Lagos et al 2020); and a cosmological hydrodynamical simulation that predicts 850 µm number counts (Hayward et al 2021). Since we include in our comparison counts derived at wavelengths other than 1.1 mm, we scale their estimates as S 1.1 mm = 1.59 × S 1.3 mm , S 1.1 mm = 1.27 × S 1.2 mm , and S 1.1 mm = 0.51 × S 850 µm .…”

Section: Comparison To Previous Workmentioning

confidence: 99%

“…Arrows indicate 3σ upper limits for flux densities having zero median counts and non-zero values at the 84th percentile. We show previous results reported by Ono et al (2014) as dark magenta crosses, Carniani et al (2015) as dark teal squares, Fujimoto et al (2016) as magenta diamonds, Oteo et al (2016) as teal triangles, Hatsukade et al (2016) as purple crosses, Aravena et al (2016) as blue squares, Umehata et al (2018) as dark magenta diamonds, Franco et al (2018) as teal triangles, Hatsukade et al (2018) as magenta crosses, González-López et al (2020) as teal squares (with their best fit from a P(D) analysis shown as a black dotted line), Béthermin et al (2020) as purple diamonds, Gómez-Guijarro et al (2022) as blue triangles, and Dunlop et al (2017) as a black solid curve. We show number counts predicted by the galaxy evolution models from Cowley et al (2015) (yellow line), Béthermin et al (2017) trapolating their data to 0.01 mJy (see Fig.…”

Section: Comparison To Previous Workmentioning

confidence: 99%

The ALMA Frontier Fields Survey. VI. Lensing-corrected 1.1mm number counts in Abell 2744, MACSJ0416.1-2403, MACSJ1149.5+2223, Abell 370 and Abell S1063

Arancibia¹,

González-López²,

Ibar³

et al. 2022

Preprint

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Context. Probing the faint end of the number counts at mm wavelengths is important to identify the origin of the extragalactic background light in this regime. Aided by strong gravitational lensing, ALMA observations towards massive galaxy clusters have opened a window to disentangle this origin, allowing to resolve sub-mJy dusty star-forming galaxies. Aims. We aim to derive number counts at 1.1 mm down to flux densities fainter than 0.1 mJy, based on ALMA observations towards five Hubble Frontier Fields (FF) galaxy clusters, following a statistical approach to correct for lensing effects. Methods. We created a source catalog that includes ALMA 1.1 mm continuum detections around two new FF galaxy clusters, together with the sources previously detected around three FF galaxy clusters, making a total of 29 detected sources down to a 4.5σ significance. ALMA 1.1mm mosaics used for our source extraction covered the inner ≈ 2 × 2 FF regions, reached rms depths of ≈ 55 − 71 µJy beam −1 , and had synthesized beam sizes between ≈ 0 . 5 − 1 . 5 (natural weighting). We derived source intrinsic flux densities using public lensing models. We folded the uncertainties in both magnifications and source redshifts into the number counts through Monte Carlo simulations. Results. Using the combination of all cluster fields, we derive cumulative number counts over two orders of magnitude down to ≈ 0.01 mJy after correction for lensing effects. Cosmic variance estimates are all exceeded by uncertainties in our median combined cumulative counts that come from both our Monte Carlo simulations and Poisson statistics. Our number counts agree at a 1σ level with our previous estimates using ALMA observations of the first three FFs, exhibiting a similar flattening at faint flux densities. They are also consistent to 1σ with most of recent ALMA estimates and galaxy evolution models. However, below ≈ 0.1 mJy, our cumulative number counts are lower by ≈ 0.4 dex compared to all deep ALMA studies but the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field Large Program (ASPECS-LP). Importantly, the flattening found for our cumulative counts extends further to ≈ 0.01 mJy, i.e., ≈ 0.4 dex fainter than ASPECS-LP, and remains in agreement with extrapolations of their number counts down to this flux limit. We find a median contribution to the extragalactic background light (EBL) of 14 +12 −8 Jy deg −2 resolved in our demagnified sources down to ≈ 0.01 mJy, representing 75 − 86% of Planck-derived extragalactic EBL estimates at 1.1 mm. Conclusions. We estimate cumulative 1.1 mm number counts down to ≈ 0.01 mJy, along the line of sight of five galaxy clusters that benefit from having rich deep multiwavelength data. They bring further support in line of the flattening of the number counts reported previously by us and ASPECS-LP, which has been interpreted by a recent galaxy evolution model as a measurement of the "knee" of the infrared luminosity function at high redshift. Our estimates of the contribution to the EBL associated with 1.1 mm galaxies i...

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“…Assuming a lack of significant size variation between the CO and dust continuum (e.g., Puglisi et al 2019), we compared the molecular gas size (and/or dust size) of our sources with the literature. The typical dust size for galaxies at z = 2.5 with a stellar mass of 10 10.9 M is 0.99 ± 0.34 kpc in radius from the GOODS-ALMA 1.1 mm survey (Figure 15 in Gómez-Guijarro et al 2022a). The dust distribution in the GOODS-ALMA sample was considered to be compact relative to the stellar distribution (van der Wel et al 2014) in Gómez-Guijarro et al (2022a).…”

Section: Structural Properties Of the Molecular Gasmentioning

confidence: 99%

“…The typical dust size for galaxies at z = 2.5 with a stellar mass of 10 10.9 M is 0.99 ± 0.34 kpc in radius from the GOODS-ALMA 1.1 mm survey (Figure 15 in Gómez-Guijarro et al 2022a). The dust distribution in the GOODS-ALMA sample was considered to be compact relative to the stellar distribution (van der Wel et al 2014) in Gómez-Guijarro et al (2022a). By further using the submillimeter compactness criterion (Puglisi et al 2021), which is used to select compact galaxies, defined as a ratio of the stellar size (van der Wel et al 2014) larger than the molecular gas size by a factor of 2.2, we conclude that the two SBs do not show compact gas disks.…”

Section: Structural Properties Of the Molecular Gasmentioning

confidence: 99%

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z=2.51

Xiao,

Wang,

Elbaz

et al. 2022

Preprint

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One of the most prominent features of galaxy clusters is the presence of a dominant population of massive ellipticals in their cores. Stellar archaeology suggests that these gigantic beasts assembled most of their stars in the early Universe via starbursts. However, the role of dense environments and their detailed physical mechanisms in triggering starburst activities remain unknown. Here we report spatially resolved Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO J = 3−2 emission line, with a resolution of about 2.5 kiloparsecs, toward a forming galaxy cluster core with starburst galaxies at z = 2.51. In contrast to starburst galaxies in the field often associated with galaxy mergers or highly turbulent gaseous disks, our observations show that the two starbursts in the cluster exhibit dynamically cold (rotation-dominated) gas-rich disks. Their gas disks have extremely low velocity dispersion (σ 0 ∼ 20 − 30 km s −1 ), which is three times lower than their field counterparts at similar redshifts. The high gas fraction and suppressed velocity dispersion yield gravitationally unstable gas disks, which enables highly efficient star formation. The suppressed velocity dispersion, likely induced by the accretion of corotating and coplanar cold gas, might serve as an essential avenue to trigger starbursts in massive halos at high redshifts.

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GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Cited by 56 publications

References 178 publications

The Compact Structures of Massive z ∼ 0.7 Post-starburst Galaxies in the SQuIGGL⃗E Sample

The Compact Structures of Massive z ∼ 0.7 Post-starburst Galaxies in the SQuIGGL⃗E Sample

The ALMA Frontier Fields Survey. VI. Lensing-corrected 1.1mm number counts in Abell 2744, MACSJ0416.1-2403, MACSJ1149.5+2223, Abell 370 and Abell S1063

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z=2.51

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