Millimeter-wave Point Sources from the 2500 Square Degree SPT-SZ Survey: Catalog and Population Statistics

Everett, W.; Zhang, L.; Crawford, T. M.; Vieira, J. D.; Aravena, M.; Archipley, Melanie; Austermann, J. E.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chapman, Scott; Crites, A. T.; Haan, T. de; Dobbs, M.; George, E. M.; Halverson, N. W.; Harrington, N. L.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Knox, L.; Lee, A. T.; Luong-Van, D.; Mangian, A. C.; Marrone, Daniel P.; McMahon, Jeff; Meyer, S. S.; Mocanu, L. M.; Mohr, J. J.; Natoli, T.; Padin, S.; Pryke, C.; Reichardt, Christian; Reuter, C.; Ruhl, J. E.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Spilker, Justin; Stalder, B.; Staniszewski, Z.; Stark, A. A.; Story, K. T.; Switzer, Eric R.; Vanderlinde, K.; Weiß, A.; Williamson, A. R.

doi:10.3847/1538-4357/ab9df7

Cited by 61 publications

(61 citation statements)

References 89 publications

(133 reference statements)

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“…It is challenging not only to homogeneously measure environments and systemically search for protoclusters, due to the small number of galaxies, but also to confirm galaxies in those structures without biases on the galaxy population (see review paper in Overzier 2016). There is an increasing number of surveys using various methods to search for protoclusters or high-redshift clusters, such as surveying galaxies around quasars or radio galaxies (e.g., Venemans et al 2007;Overzier et al 2008;Wylezalek et al 2013Wylezalek et al , 2014Cooke et al 2015Cooke et al , 2016, using Lyα emitters or dropout galaxies to trace large-scale structures (e.g., Steidel et al 1998;Toshikawa et al 2016Toshikawa et al , 2018Higuchi et al 2019;Hu et al 2021), searching for high-redshift overdensities using large deep photometric and spectroscopic surveys (e.g., Lemaux et al 2014aLemaux et al , 2018Cucciati et al 2018;Darvish et al 2020;Toshikawa et al 2020), and selecting via the Sunyaev-Zel'dovich effect signature (e.g., Bleem et al 2015;Everett et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Shen

Lemaux

Lubin

et al. 2021

ApJ

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Radio active galactic nuclei (RAGNs) are mainly found in dense structures (i.e., clusters/groups) at redshifts of z < 2 and are commonly used to detect protoclusters at higher redshift. Here, we attempt to study the host and environmental properties of two relatively faint (L 1.4 GHz ∼ 1025 W Hz−1) RAGNs in a known protocluster at z = 3.3 in the PCl J0227-0421 field, detected using the latest radio observation obtained as part of the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. Using new spectroscopic observations obtained from the Keck/Multi-Object Spectrometer for Infra-Red Exploration as part of the Charting Cluster Construction with the VIMOS Ultra-Deep Survey (VUDS) and ORELSE (C3VO) survey and previous spectroscopic data obtained as part of the VIMOS-Very Large Telescope Deep Survey and VUDS, we revise the three-dimensional overdensity field around this protocluster. The protocluster is embedded in a large-scale overdensity protostructure. This protostructure has an estimated total mass of ∼2.6 × 1015 M ⊙ and contains several overdensity peaks. Both RAGNs are hosted by very bright and massive galaxies, while their hosts show extreme differences in color, indicating that they are of different ages and are in different evolutionary stages. Furthermore, we find that they are not in the most locally dense parts of the protostructure, but are fairly close to the centers of their parent overdensity peaks. We propose a scenario where merging might have already happened in both cases, which lowered the local density of their surrounding area and boosted their stellar mass. This work is the first time that two RAGNs at low luminosity have been found and studied within a high-redshift protostructure.

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Section: Introductionmentioning

confidence: 99%

Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Shen

Lemaux

Lubin

et al. 2021

ApJ

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“…[9] and fluxfrequency scaling relations from Ref. [53]. We neglect Galactic foregrounds for these simulations, as the expected polarized power from dust within our survey region is 1-2 orders of magnitude smaller than the E-mode signal over the multipoles and observing frequencies considered here (Galactic dust is accounted for in the likelihood; see Sec.…”

Section: Simulationsmentioning

confidence: 98%

Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data

Dutcher¹,

Balkenhol²,

Ade³

et al. 2021

Phys. Rev. D

Self Cite

183

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We present measurements of the E-mode (EE) polarization power spectrum and temperature-E-mode (TE) cross-power spectrum of the cosmic microwave background using data collected by SPT-3G, the latest instrument installed on the South Pole Telescope. This analysis uses observations of a 1500 deg 2 region at 95, 150, and 220 GHz taken over a four-month period in 2018. We report binned values of the EE and TE power spectra over the angular multipole range 300 ≤ l < 3000, using the multifrequency data to construct six semi-independent estimates of each power spectrum and their minimum-variance combination. These measurements improve upon the previous results of SPTpol across the multipole ranges 300 ≤ l ≤ 1400 for EE and 300 ≤ l ≤ 1700 for TE, resulting in constraints on cosmological parameters comparable to those from other current leading ground-based experiments. We find that the SPT-3G data set is well fit by a ΛCDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find H 0 ¼ 68.8 AE 1.5 km s −1 Mpc −1 and σ 8 ¼ 0.789 AE 0.016, with a gravitational lensing amplitude consistent with the ΛCDM prediction (A L ¼ 0.98 AE 0.12). We combine the SPT-3G and the Planck data sets and obtain joint constraints on the ΛCDM model. The volume of the 68% confidence region in six-dimensional ΛCDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with no significant shifts in central values. We note that the results presented here are obtained from data collected during just half of a typical observing season with only part of the focal plane operable, and that the active detector count has since nearly doubled for observations made with SPT-3G after 2018.

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“…The point source and cluster potential of these maps will be explored in two upcoming papers, but a preliminary search has 4 000 confirmed clusters (Hilton et al, 2020, in prep) and 18 500 point source candidates at > 5σ. For comparison, the largest published point source catalog at these frequencies is Everett et al (2020) with 4845 point sources at > 4.5σ, and the largest published SZ-detected cluster catalog, PSZ2, has 1203 confirmed clusters (Planck Collaboration, 2016b).…”

Section: Map Images and Featuresmentioning

confidence: 99%

The Atacama Cosmology Telescope: arcminute-resolution maps of 18 000 square degrees of the microwave sky from ACT 2008–2018 data combined with Planck

Næss

Aiola

Austermann

et al. 2020

J. Cosmol. Astropart. Phys.

120

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This paper presents a maximum-likelihood algorithm for combining sky maps with disparate sky coverage, angular resolution and spatially varying anisotropic noise into a single map of the sky. We use this to merge hundreds of individual maps covering the 2008-2018 ACT observing seasons, resulting in by far the deepest ACT maps released so far. We also combine the maps with the full Planck maps, resulting in maps that have the best features of both Planck and ACT: Planck's nearly white noise on intermediate and large angular scales and ACT's high-resolution and sensitivity on small angular scales. The maps cover over 18 000 square degrees, nearly half the full sky, at 100, 150 and 220 GHz. They reveal 4 000 optically-confirmed clusters through the Sunyaev Zel'dovich effect (SZ) and 18 500 point source candidates at > 5σ, the largest single collection of SZ clusters and millimeter wave sources to date. The multi-frequency maps provide millimeter images of nearby galaxies and individual Milky Way nebulae, and even clear detections of several nearby stars. Other anticipated uses of these maps include, for example, thermal SZ and kinematic SZ cluster stacking, CMB cluster lensing and galactic dust science. The method itself has negligible bias. However, due to the preliminary nature of some of the component data sets, we caution that these maps should not be used for precision cosmological analysis. The maps are part of ACT DR5, and will be made available on LAMBDA 1 no later than three months after the journal publication of this article, along with an interactive sky atlas.

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Millimeter-wave Point Sources from the 2500 Square Degree SPT-SZ Survey: Catalog and Population Statistics

Cited by 61 publications

References 89 publications

Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data

The Atacama Cosmology Telescope: arcminute-resolution maps of 18 000 square degrees of the microwave sky from ACT 2008–2018 data combined with Planck

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