The SCUBA-2 Cluster Snapshot Survey – I. Catalogue of lensed galaxies and submillimetre-bright central galaxies
AuthorCheale, Ryan A
Geach, James E
Edge, Alastair C
Blain, Andrew W
Chapman, Scott C
Hogan, Mike T
Rawle, Timothy D
Webb, Tracy M A
AffiliationUniv Arizona, Steward Observ
galaxies: clusters: general
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationRyan A Cheale, James E Geach, Alastair C Edge, Andrew W Blain, Scott C Chapman, Eiichi Egami, Mike T Hogan, Timothy D Rawle, Tracy M A Webb, The SCUBA-2 Cluster Snapshot Survey – I. Catalogue of lensed galaxies and submillimetre-bright central galaxies, Monthly Notices of the Royal Astronomical Society, Volume 484, Issue 2, April 2019, Pages 2757–2778, https://doi.org/10.1093/mnras/stz011
Rights© 2019 The Author(s).
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractThe SCUBA-2 Cluster Snapshot Survey (S2CSS) observed 202 rich clusters of galaxies at 850 mu m in relatively poor submillimetre observing conditions (tau(225) (GHz) > 0.1) with the aim of identifying rare examples of bright (tens of mJy) gravitationally lensed submillimetre galaxies. The S2CSS covered over 0.33 deg(2) to an average depth of sigma(850) approximate to 12 mJy beam(-1). Here we present a sample of 97 bright 850-mu m point sources selected from the S2CSS that are potentially gravitationally lensed, and eight sources for which the strong submillimetre emission is co-located with the central brightest cluster galaxy (BCG). We construct far-infrared spectral energy distributions for those sources with Herschel SPIRE coverage and use these distributions to estimate the redshifts and luminosities of the sources. The bright submillimetre flux density of our sources makes them excellent targets for detailed follow-up work that will allow the detection of spectral features in the submillimetre/millimetre that would otherwise be too faint to detect. Through a stacking analysis, we also investigate the average submillimetre/radio properties of BCGs, determining the average 850-mu m flux of BCGs as a function of radio luminosity.
VersionFinal published version
SponsorsRoyal Society; Royal Society University Research Fellowship; STFC [ST/P000J41/1]; ERC Advanced Grant [ST/P000J41/1, 321334]; Royal Society/Wolfson Merit Award; Chinese Academy of Sciences [XDB09000000]; Science and Technology Facilities Council of the United Kingdom
Showing items related by title, author, creator and subject.
Evidence from APOGEE for the presence of a major building block of the halo buried in the inner GalaxyHorta, D.; Schiavon, R.P.; MacKereth, J.T.; Pfeffer, J.; Mason, A.C.; Kisku, S.; Fragkoudi, F.; Allende Prieto, C.; Cunha, K.; Hasselquist, S.; et al. (Oxford University Press, 2021)We report evidence from APOGEE for the presence of a new metal-poor stellar structure located within ∼4 kpc of the Galactic Centre. Characterized by a chemical composition resembling those of low-mass satellites of the Milky Way, this new inner Galaxy structure (IGS) seems to be chemically and dynamically detached from more metal-rich populations in the inner Galaxy. We conjecture that this structure is associated with an accretion event that likely occurred in the early life of the Milky Way. Comparing the mean elemental abundances of this structure with predictions from cosmological numerical simulations, we estimate that the progenitor system had a stellar mass of ∼5 × 108 M, or approximately twice the mass of the recently discovered Gaia-Enceladus/Sausage system. We find that the accreted:in situ ratio within our metal-poor ([Fe/H] <-0.8) bulge sample is somewhere between 1:3 and 1:2, confirming predictions of cosmological numerical simulations by various groups. © 2021 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
STELLAR MASS–GAS-PHASE METALLICITY RELATION AT 0.5 ≤ z ≤ 0.7: A POWER LAW WITH INCREASING SCATTER TOWARD THE LOW-MASS REGIMEGuo, Yicheng; Koo, David C.; Lu, Yu; Forbes, John C.; Rafelski, Marc; Trump, Jonathan R.; Amorín, Ricardo; Barro, Guillermo; Davé, Romeel; Faber, S. M.; et al. (IOP PUBLISHING LTD, 2016-05-11)We present the stellar mass (M-*)-gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 <= z <= 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M-* of this magnitude-limited (R less than or similar to 24 AB) sample are representative of normal star-forming galaxies. For masses below 10(9) M-circle dot, our sample of 237 galaxies is similar to 10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 10(8) M-circle dot < M-* < 10(11) M-circle dot: 12 + log (O/H) = (5.83 +/- 0.19)+(0.30 +/- 0.02) log (M-*/M-circle dot). At 10(9) M-circle dot < M-* < 10(10.5) M-circle dot, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 10(9) M-circle dot. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as M-* decreases. Our result implies that either the scatter of the baryonic accretion rate (sigma((M) over dot)) or the scatter of the M-*-M-halo relation (sigma(SHMR)) increases as M-* decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both sigma((M) over dot) and sigma(SHMR) remain unchanged from z = 0.7 to z = 0.
STAR FORMATION AND AGN ACTIVITY IN GALAXY CLUSTERS FROM z = 1–2: A MULTI-WAVELENGTH ANALYSIS FEATURING HERSCHEL /PACSAlberts, Stacey; Pope, Alexandra; Brodwin, Mark; Chung, Sun Mi; Cybulski, Ryan; Dey, Arjun; Eisenhardt, Peter R. M.; Galametz, Audrey; Gonzalez, Anthony H.; Jannuzi, Buell T.; et al. (IOP PUBLISHING LTD, 2016-06-30)We present a detailed, multi-wavelength study of star formation (SF) and active galactic nucleus (AGN) activity in 11 near-infrared (IR) selected, spectroscopically confirmed massive (greater than or similar to 10(14)M(circle dot)) galaxy clusters at 1 < z < 1.75. Using new deep Herschel/PACS imaging, we characterize the optical to far-IR spectral energy distributions (SEDs) for IR-luminous cluster galaxies, finding that they can, on average, be well described by field galaxy templates. Identification and decomposition of AGNs through SED fittings allows us to include the contribution to cluster SF from AGN host galaxies. We quantify the star-forming fraction, dust-obscured SF rates (SFRs) and specific SFRs for cluster galaxies as a function of cluster-centric radius and redshift. In good agreement with previous studies, we find that SF in cluster galaxies at z greater than or similar to 1.4 is largely consistent with field galaxies at similar epochs, indicating an era before significant quenching in the cluster cores (r < 0.5 Mpc). This is followed by a transition to lower SF activity as environmental quenching dominates by z similar to 1. Enhanced SFRs are found in lower mass (10.1< logM(kappa)/M-circle dot < 10.8) cluster galaxies. We find significant variation in SF from cluster to cluster within our uniformly selected sample, indicating that caution should be taken when evaluating individual clusters. We examine AGNs in clusters from z = 0.5-2, finding an excess AGN fraction at z greater than or similar to 1, suggesting environmental triggering of AGNs during this epoch. We argue that our results-a transition from field-like to quenched SF, enhanced SF in lower mass galaxies in the cluster cores, and excess AGNs-are consistent with a co-evolution between SF and AGNs in clusters and an increased merger rate in massive halos at high redshift.