From Clusters to Proto-Clusters: The Infrared Perspective on Environmental Galaxy Evolution

Alberts, Stacey; Noble, Allison

doi:10.3390/universe8110554

Cited by 25 publications

(6 citation statements)

References 907 publications

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“…Compared to clusters at lower redshifts, we find that ΣSFR/M halo rises rapidly with redshift, as predicted by Alberts et al (2014; see a discussion in Popesso et al 2015;Alberts & Noble 2022). This indicates vigorous star formation in the structures in the early Universe.…”

Section: Properties Of Lh-sbc3supporting

confidence: 75%

Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z = 3.95

Zhou,

Wang,

Daddi

et al. 2024

A&A

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The study of distant galaxy groups and clusters at the peak epoch of star formation is limited by the lack of a statistically and homogeneously selected and spectroscopically confirmed sample. Recent discoveries of concentrated starburst activities in cluster cores have opened a new window to hunt for these structures based on their integrated IR luminosities. Here, we carry out a large NOEMA (NOrthern Extended Millimeter Array) program targeting a statistical sample of infrared-luminous sources associated with overdensities of massive galaxies at $z$\,>\,2, the Noema formIng Cluster survEy (NICE). We present the first result from the ongoing NICE survey, a compact group at $z$\,=\,3.95 in the Lockman Hole field (LH-SBC3), confirmed via four massive star $\,gtrsim odot $) galaxies detected in the CO(4-3) and CI odot odot $/yr. In addition, the most massive galaxy hosts a radio-loud active galactic nucleus with $L_ 1.4GHz, rest $\,=\,3.0\,times $. The discovery of LH-SBC3 demonstrates the feasibility of our method to efficiently identify high-$z$ compact groups or cluster cores undergoing formation. The existence of these starbursting cluster cores up to $z$\,sim \,$4$ provides critical insights into the mass assembly history of the central massive galaxies in clusters.

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Section: Properties Of Lh-sbc3supporting

confidence: 75%

Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z = 3.95

Zhou,

Wang,

Daddi

et al. 2024

A&A

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“…Most models for quenching dwarf galaxies have focused on environmental effects (Bahé & McCarthy 2015;Alberts & Noble 2022) such as ram pressure stripping (e.g., Gunn & Gott 1972;Bekki 2009;Fillingham et al 2016;Boselli et al 2022), strangulation (Larson et al 1980;Kawata & Mulchaey 2008), or tidal stripping (Moore et al 1996). However, recent observations of large numbers of ultra-diffuse galaxies have prompted the development of internal quenching mechanisms, such as strong feedback (Mori et al 2002).…”

Section: Discussionmentioning

confidence: 99%

PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc

Carleton,

Ellsworth-Bowers,

Windhorst

et al. 2024

ApJL

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A wealth of observations have long suggested that the vast majority of isolated classical dwarf galaxies (M * = 107–109 M ⊙) are currently star forming. However, recent observations of the large abundance of “ultra-diffuse galaxies” beyond the reach of previous large spectroscopic surveys suggest that our understanding of the dwarf galaxy population may be incomplete. Here we report the serendipitous discovery of an isolated quiescent dwarf galaxy in the nearby Universe, which was imaged as part of the JWST PEARLS Guaranteed Time Observation program. Remarkably, individual red-giant branch stars are visible in this near-IR imaging, suggesting a distance of 30 ± 4 Mpc, and a wealth of archival photometry point to an sSFR of 2 × 10−11 yr−1 and star formation rate of 4 × 10−4 M ⊙ yr−1. Spectra obtained with the Lowell Discovery Telescope find a recessional velocity consistent with the Hubble Flow and >1500 km s−1 separated from the nearest massive galaxy in Sloan Digital Sky Survey suggesting that this galaxy was either quenched from internal mechanisms or had a very high-velocity (≳1000 km s−1) interaction with a nearby massive galaxy in the past. This analysis highlights the possibility that many nearby quiescent dwarf galaxies are waiting to be discovered and that JWST has the potential to resolve them.

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“…The star formation rate density (SFRD) of the PC15 protocluster candidates, including lower-z and higher-z subsamples, and the LBG selected Hyper Suprime-Cam protocluster candidates (Kubo et al 2019) in comparison to the projected SFRD for protoclusters with a z = 0 halo mass of scaled from Chiang et al (2017) and the observational measurements of field galaxies (Madau & Dickinson 2014). This figure is adapted from Alberts & Noble (2022). different methods, determine how much star formation there is within populations of protoclusters, and determine where the cosmic SFRD of protoclusters peaks.…”

Section: Discussionmentioning

confidence: 99%

Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters

Popescu,

Pope,

Lee

et al. 2023

ApJ

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As the progenitors of present-day galaxy clusters, protoclusters are excellent laboratories to study galaxy evolution. Since existing observations of protoclusters are limited to the detected constituent galaxies at UV and/or infrared wavelengths, the details of how typical galaxies grow in these young, pre-virialized structures remain uncertain. We measure the total stellar mass and star formation within protoclusters, including the contribution from faint undetected members by performing a stacking analysis of 211 z = 2–4 protoclusters selected as Planck cold sources. We stack Wide-field Infrared Survey Explorer and Herschel/SPIRE images to measure the angular size and the spectral energy distribution of the integrated light from the protoclusters. The fluxes of protoclusters selected as Planck cold sources can be contaminated by line-of-sight interlopers. Using the WebSky simulation, we estimate that a single protocluster contributes 33% ± 15% of the flux of a Planck cold source on average. After this correction, we obtain a total star formation rate of 7.3 ± 3.2 × 103 M ⊙yr−1 and a total stellar mass of 4.9 ± 2.2 × 1012 M ⊙. Our results indicate that protoclusters have, on average, 2× more star formation and 4× more stellar mass than the total contribution from individually detected galaxies in spectroscopically confirmed protoclusters. This suggests that much of the total flux within z = 2–4 protoclusters comes from galaxies with luminosities lower than the detection limit of SPIRE (L IR < 3 × 1012 L ⊙). Lastly, we find that protoclusters subtend a half-light radius of 2.′8 (4.2–5.8 cMpc), which is consistent with simulations.

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From Clusters to Proto-Clusters: The Infrared Perspective on Environmental Galaxy Evolution

Cited by 25 publications

References 907 publications

Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z = 3.95

Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z = 3.95

PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc

Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters

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