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1. The CatWISE2020 Catalog

Author

Marocco, Federico, Eisenhardt, Peter RM, Fowler, John W, Kirkpatrick, J Davy, Meisner, Aaron M, Schlafly, Edward F, Stanford, SA, Garcia, Nelson, Caselden, Dan, Cushing, Michael C, Cutri, Roc M, Faherty, Jacqueline K, Gelino, Christopher R, Gonzalez, Anthony H, Jarrett, Thomas H, Koontz, Renata, Mainzer, Amanda, Marchese, Elijah J, Mobasher, Bahram, Schlegel, David J, Stern, Daniel, Teplitz, Harry I, and Wright, Edward L

Subjects
Space Sciences, Physical Sciences, Astronomy databases, Infrared astronomy, Infrared photometry, Catalogs, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences
Abstract

The CatWISE2020 Catalog consists of 1,890,715,640 sources over the entire sky selected from Wide-field Infrared Survey Explorer (WISE) and NEOWISE survey data at 3.4 and 4.6 μm (W1 and W2) collected from 2010 January 7 to 2018 December 13. This data set adds two years to that used for the CatWISE Preliminary Catalog, bringing the total to six times as many exposures spanning over 16 times as large a time baseline as the AllWISE catalog. The other major change from the CatWISE Preliminary Catalog is that the detection list for the CatWISE2020 Catalog was generated using crowdsource from Schlafly et al., while the CatWISE Preliminary Catalog used the detection software used for AllWISE. These two factors result in roughly twice as many sources in the CatWISE2020 Catalog. The scatter with respect to Spitzer photometry at faint magnitudes in the COSMOS field, which is out of the Galactic Plane and at low ecliptic latitude (corresponding to lower WISE coverage depth) is similar to that for the CatWISE Preliminary Catalog. The 90% completeness depth for the CatWISE2020 Catalog is at W1 = 17.7 mag and W2 = 17.5 mag, 1.7 mag deeper than in the CatWISE Preliminary Catalog. In comparison to Gaia, CatWISE2020 motions are accurate at the 20 mas yr-1 level for W1∼15 mag sources and at the ∼100 mas yr-1 level for W1∼17 mag sources. This level of accuracy represents a 12 improvement over AllWISE. The CatWISE catalogs are available in the WISE/NEOWISE Enhanced and Contributed Products area of the NASA/IPAC Infrared Science Archive.

Published
2021

2. The CatWISE Preliminary Catalog: Motions from WISE and NEOWISE Data

Author

Eisenhardt, PRM, Marocco, F, Fowler, JW, Meisner, AM, Kirkpatrick, JD, Garcia, N, Jarrett, TH, Koontz, R, Marchese, EJ, Stanford, SA, Caselden, D, Cushing, MC, Cutri, RM, Faherty, JK, Gelino, CR, Gonzalez, AH, Mainzer, A, Mobasher, B, Schlegel, DJ, Stern, D, Teplitz, HI, and Wright, EL

Subjects
Catalogs, Sky surveys, Proper motions, Brown dwarfs, Infrared astronomy, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

CatWISE is a program to catalog sources selected from combined WISE and NEOWISE all-sky survey data at 3.4 and 4.6 μm (W1 and W2). The CatWISE Preliminary Catalog consists of 900,849,014 sources measured in data collected from 2010 to 2016. This data set represents four times as many exposures and spans over 10 times as large a time baseline as that used for the AllWISE Catalog. CatWISE adapts AllWISE software to measure the sources in coadded images created from six-month subsets of these data, each representing one coverage of the inertial sky, or epoch. The catalog includes the measured motion of sources in eight epochs over the 6.5 yr span of the data. From comparison to Spitzer, signal-to-noise ratio = 5 limits in magnitudes in the Vega system are W1 = 17.67 and W2 = 16.47, compared to W1 = 16.96 and W2 = 16.02 for AllWISE. From comparison to Gaia, CatWISE positions have typical accuracies of 50 mas for stars at W1 = 10 mag and 275 mas for stars at W1 = 15.5 mag. Proper motions have typical accuracies of 10 mas yr-1 and 30 mas yr-1 for stars with these brightnesses, an order of magnitude better than from AllWISE. The catalog is available in the WISE/NEOWISE Enhanced and Contributed Products area of the NASA/IPAC Infrared Science Archive.

Published
2020

3. The Massive and Distant Clusters of WISE Survey. I. Survey Overview and a Catalog of >2000 Galaxy Clusters at z ≃ 1

Author

Gonzalez, AH, Gettings, DP, Brodwin, M, Eisenhardt, PRM, Stanford, SA, Wylezalek, D, Decker, B, Marrone, DP, Moravec, E, O'Donnell, C, Stalder, B, Stern, D, Abdulla, Z, Brown, G, Carlstrom, J, Chambers, KC, Hayden, B, Lin, YT, Magnier, E, Masci, FJ, Mantz, AB, McDonald, M, Mo, W, Perlmutter, S, Wright, EL, and Zeimann, GR

Subjects
Space Sciences, Physical Sciences, Life Below Water, galaxies: clusters: general, galaxies: distances and redshifts, galaxies: evolution, surveys, astro-ph.CO, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences
Abstract

© 2019. The American Astronomical Society. All rights reserved. We present the Massive and Distant Clusters of WISE Survey (MaDCoWS), a search for galaxy clusters at 0.7 ≲ z ≲ 1.5 based upon data from the Wide-field Infrared Survey Explorer (WISE) mission. MaDCoWS is the first cluster survey capable of discovering massive clusters at these redshifts over the full extragalactic sky. The search is divided into two regions - the region of the extragalactic sky covered by Pan-STARRS (δ > -30°) and the remainder of the southern extragalactic sky at δ < -30° for which shallower optical data from the SuperCOSMOS Sky Survey is available. In this paper, we describe the search algorithm, characterize the sample, and present the first MaDCoWS data release - catalogs of the 2433 highest amplitude detections in the WISE-Pan-STARRS region and the 250 highest amplitude detections in the WISE-SuperCOSMOS region. A total of 1723 of the detections from the WISE-Pan-STARRS sample have also been observed with the Spitzer Space Telescope, providing photometric redshifts and richnesses, and an additional 64 detections within the WISE-SuperCOSMOS region also have photometric redshifts and richnesses. Spectroscopic redshifts for 38 MaDCoWS clusters with IRAC photometry demonstrate that the photometric redshifts have an uncertainty of σ z /(1 + z) ≃ 0.036. Combining the richness measurements with Sunyaev-Zel'dovich observations of MaDCoWS clusters, we also present a preliminary mass-richness relation that can be used to infer the approximate mass distribution of the full sample. The estimated median mass for the WISE-Pan-STARRS catalog is , with the Sunyaev-Zel'dovich data confirming that we detect clusters with masses up to M 500 ∼ 5 ×10 14 M (M 200 ∼ 10 15 M ).

Published
2019

4. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author

Rubin, D, Hayden, B, Huang, X, Aldering, G, Amanullah, R, Barbary, K, Boone, K, Brodwin, M, Deustua, SE, Dixon, S, Eisenhardt, P, Fruchter, AS, Gonzalez, AH, Goobar, A, Gupta, RR, Hook, I, Jee, MJ, Kim, AG, Kowalski, M, Lidman, CE, Linder, E, Luther, K, Nordin, J, Pain, R, Perlmutter, S, Raha, Z, Rigault, M, Ruiz-Lapuente, P, Saunders, CM, Sofiatti, C, Spadafora, AL, Stanford, SA, Stern, D, Suzuki, N, and Williams, SC

Subjects
Space Sciences, Physical Sciences, Astronomical Sciences, cosmology: observations, galaxies: clusters: individual (MOO J1014+0038) supernovae: general, gravitational lensing: weak, astro-ph.GA, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of (1.10 0.23 mag) - compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from ΛCDM simulations - making it the most amplified SN Ia discovered behind a galaxy cluster.

Published
2018

5. THE HUBBLE SPACE TELESCOPE**Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. The observations are associated with program GO-10496. CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

Author

Barbary, K, Aldering, G, Amanullah, R, Brodwin, M, Connolly, N, Dawson, KS, Doi, M, Eisenhardt, P, Faccioli, L, Fadeyev, V, Fakhouri, HK, Fruchter, AS, Gilbank, DG, Gladders, MD, Goldhaber, G, Goobar, A, Hattori, T, Hsiao, E, Huang, X, Ihara, Y, Kashikawa, N, Koester, B, Konishi, K, Kowalski, M, Lidman, C, Lubin, L, Meyers, J, Morokuma, T, Oda, T, Panagia, N, Perlmutter, S, Postman, M, Ripoche, P, Rosati, P, Rubin, D, Schlegel, DJ, Spadafora, AL, Stanford, SA, Strovink, M, Suzuki, N, Takanashi, N, Tokita, K, and Yasuda, and N

Subjects
Space Sciences, Physical Sciences, cosmology: observations, supernovae: general, white dwarfs, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 1 cluster SNeIa, we determine an SN Ia rate of 0.50+0.23-0.19 (stat) +0.10-0.09 (sys) h 270 SNuB (SNuB ≡ 10-12 SNe L -1, Byr-1). In units of stellar mass, this translates to 0.36+0.16-0.13 (stat) +0.07-0.06 (sys) h 270 SNuM (SNuM ≡ 10 -12 SNe M -1⊙yr-1). This represents a factor of 5 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Ψ(t)ts . Under the approximation of a single-burst cluster formation redshift of zf = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41 +0.47-0.40, consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts. © 2012. The American Astronomical Society. All rights reserved..

Published
2012

6. THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

Author

Barbary, K, Aldering, G, Amanullah, R, Brodwin, M, Connolly, N, Dawson, KS, Doi, M, Eisenhardt, P, Faccioli, L, Fadeyev, V, Fakhouri, HK, Fruchter, AS, Gilbank, DG, Gladders, MD, Goldhaber, G, Goobar, A, Hattori, T, Hsiao, E, Huang, X, Ihara, Y, Kashikawa, N, Koester, B, Konishi, K, Kowalski, M, Lidman, C, Lubin, L, Meyers, J, Morokuma, T, Oda, T, Panagia, N, Perlmutter, S, Postman, M, Ripoche, P, Rosati, P, Rubin, D, Schlegel, DJ, Spadafora, AL, Stanford, SA, Strovink, M, Suzuki, N, Takanashi, N, Tokita, K, Yasuda, N, and Project, Supernova Cosmology

Subjects
cosmology: observations, supernovae: general, white dwarfs, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We report a measurement of the Type Ia supernova (SN Ia) rate in galaxyclusters at 0.9 < z < 1.45 from the Hubble Space Telescope (HST) ClusterSupernova Survey. This is the first cluster SN Ia rate measurement withdetected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine a SN Ia rateof 0.50 +0.23-0.19 (stat) +0.10-0.09 (sys) SNuB (SNuB = 10^-12 SNe L_{sun,B}^-1yr^-1). In units of stellar mass, this translates to 0.36 +0.16-0.13 (stat)+0.07-0.06 (sys) SNuM (SNuM = 10^-12 SNe M_sun^-1 yr^-1). This represents afactor of approximately 5 +/- 2 increase over measurements of the cluster rateat z < 0.2. We parameterize the late-time SN Ia delay time distribution with apower law (proportional to t^s). Under the assumption of a cluster formationredshift of z_f = 3, our rate measurement in combination with lower-redshiftcluster SN Ia rates constrains s = -1.41 +0.47/-0.40, consistent withmeasurements of the delay time distribution in the field. This measurement isgenerally consistent with expectations for the "double degenerate" scenario andinconsistent with some models for the "single degenerate" scenario predicting asteeper delay time distribution at large delay times. We check forenvironmental dependence and the influence of younger stellar populations bycalculating the rate specifically in cluster red-sequence galaxies and inmorphologically early-type galaxies, finding results similar to the fullcluster rate. Finally, the upper limit of one host-less cluster SN Ia detectedin the survey implies that the fraction of stars in the intra-cluster medium isless than 0.47 (95% confidence), consistent with measurements at lowerredshifts.

Published
2012

7. MID-INFRARED VARIABILITY FROM THE SPITZER DEEP WIDE-FIELD SURVEY

Author

Kozłowski, Szymon, Kochanek, Christopher S, Stern, Daniel, Ashby, Matthew LN, Assef, Roberto J, Bock, JJ, Borys, C, Brand, K, Brodwin, M, Brown, MJI, Cool, R, Cooray, A, Croft, S, Dey, Arjun, Eisenhardt, PR, Gonzalez, A, Gorjian, V, Griffith, R, Grogin, N, Ivison, R, Jacob, J, Jannuzi, BT, Mainzer, A, Moustakas, L, Röttgering, H, Seymour, N, Smith, HA, Stanford, SA, Stauffer, JR, Sullivan, IS, van Breugel, W, Willner, SP, and Wright, EL

Subjects
cosmology: observations, galaxies: active, infrared: galaxies, quasars: general, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We use the multi-epoch, mid-infrared Spitzer Deep Wide-Field Survey to investigate the variability of objects in 8.1 deg2 of the NOAO Deep Wide Field Survey Boötes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 μm bands. Out of 474, 179 analyzed sources, 1.1% meet our standard variability selection criteria that the two light curves are strongly correlated (r>0.8) and that their joint variance (σ12) exceeds that for all sources with the same magnitude by 2σ. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBoötes survey, radio catalogs, 24 μm selected active galactic nucleus (AGN) candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects, although most of the stellar, galaxy, and unclassified sources are false positives. For our standard selection criteria, 11%-12% of the mid-IR counterparts to X-ray sources, 24 μm AGN candidates, and spectroscopically identified AGNs show variability. The exact fractions depend on both the search depth and the selection criteria. For example, 12% of the 1131 known z>1 AGNs in the field and 14%-17% of the known AGNs with well-measured fluxes in all four Infrared Array Camera bands meet our standard selection criteria. The mid-IR AGN variability can be well described by a single power-law structure function with an index of γ ≈ 0.5 at both 3.6 and 4.5 μm, and an amplitude of S 0 ≃ 0.1 mag on rest-frame timescales of 2 yr. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities. © 2010. The American Astronomical Society. All rights reserved.

Published
2010

8. THE SPITZER DEEP, WIDE-FIELD SURVEY

Author

Ashby, MLN, Stern, D, Brodwin, M, Griffith, R, Eisenhardt, P, Kozłowski, S, Kochanek, CS, Bock, JJ, Borys, C, Brand, K, Brown, MJI, Cool, R, Cooray, A, Croft, S, Dey, A, Eisenstein, D, Gonzalez, AH, Gorjian, V, Grogin, NA, Ivison, RJ, Jacob, J, Jannuzi, BT, Mainzer, A, Moustakas, LA, Röttgering, HJA, Seymour, N, Smith, HA, Stanford, SA, Stauffer, JR, Sullivan, I, van Breugel, W, Willner, SP, and Wright, EL

Subjects
infrared: galaxies, infrared: stars, surveys, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg2 in the Boötes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit - for the first time - the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ∼ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ∼ 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 × 105 distinct sources detected to the average 5σ, 4″-diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0μm, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, >50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and >80% of on-axis XBoötes sources are detected out to 8.0μm. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class. © 2009. The American Astronomical Society. All rights reserved.

Published
2009

9. The Massive and Distant Clusters of WISE Survey. I. Survey Overview and a Catalog of >2000 Galaxy Clusters at z ≃ 1

Author

MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Gonzalez, Anthony H, Gettings, Daniel P, Brodwin, Mark, Eisenhardt, Peter RM, Stanford, SA, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P, Moravec, Emily, O’Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C, Hayden, Brian, Lin, Yen-ting, Magnier, Eugene, Masci, Frank J, Mantz, Adam B, McDonald, Michael A., Mo, Wenli, Perlmutter, Saul, Wright, Edward L, Zeimann, Gregory R, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Gonzalez, Anthony H, Gettings, Daniel P, Brodwin, Mark, Eisenhardt, Peter RM, Stanford, SA, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P, Moravec, Emily, O’Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C, Hayden, Brian, Lin, Yen-ting, Magnier, Eugene, Masci, Frank J, Mantz, Adam B, McDonald, Michael A., Mo, Wenli, Perlmutter, Saul, Wright, Edward L, and Zeimann, Gregory R

Published
2022

10. The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters

Author

MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, McDonald, Michael A., MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A.

Abstract

© 2019. The American Astronomical Society. All rights reserved. We present measurements of the stellar mass fractions ( f∗) for a sample of high-redshift (0.93≤.z≤1.32) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel-dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean f∗ between the two selection methods; though, we do find an unexpectedly large range in f∗ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find m∗ = 19.41 ± 0.07, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at z = 1.31, is the most distant MaDCoWS cluster confirmed to date.

Published
2022

11. Galaxy populations in the most distant SPT-SZ clusters: I. Environmental quenching in massive clusters at 1.4 ≲ z ≲ 1.7

Author

MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, Matthew B, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, Michael A., Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, Stalder, B, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, Matthew B, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, Michael A., Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, and Stalder, B

Abstract

© 2019 ESO. We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg 2 South Pole Telescope Sunyaev Zel'dovich effect (SPT-SZ) survey, which is sensitive to M 500 ≳ 3 × 10 14 M · clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z≳ 1.4, S/N SZE > 5 clusters, that are among the rarest most massive clusters known at this redshift. All five clusters show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates, although one (SPT-CLJ0607-4448) shows a galaxy concentration much less prominent than the others. The highest redshift cluster in this sample, SPT-CLJ0459-4947 at z ∼ 1.72, is the most distant M 500 > 10 14 M · cluster discovered thus far through its intracluster medium, and is one of only three known clusters in this mass range at z≳ 1.7, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, we find that the quiescent fraction in the cluster central regions (r/r 500 < 0.7) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range ∼0.5 - 0.8 for stellar masses log(M/M · ) > 10.85. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/N SZE > 5, even if they had the same quiescent fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in the central regions of the most massive clusters, occurring already earlier than z ∼ 1.5.

Published
2022

12. The Massive and Distant Clusters of WISE Survey. I. Survey Overview and a Catalog of >2000 Galaxy Clusters at z ≃ 1

Author

Gonzalez, Anthony H, Gettings, Daniel P, Brodwin, Mark, Eisenhardt, Peter RM, Stanford, SA, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P, Moravec, Emily, O’Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C, Hayden, Brian, Lin, Yen-ting, Magnier, Eugene, Masci, Frank J, Mantz, Adam B, McDonald, Michael, Mo, Wenli, Perlmutter, Saul, Wright, Edward L, Zeimann, Gregory R, Gonzalez, Anthony H, Gettings, Daniel P, Brodwin, Mark, Eisenhardt, Peter RM, Stanford, SA, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P, Moravec, Emily, O’Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C, Hayden, Brian, Lin, Yen-ting, Magnier, Eugene, Masci, Frank J, Mantz, Adam B, McDonald, Michael, Mo, Wenli, Perlmutter, Saul, Wright, Edward L, and Zeimann, Gregory R

Published
2021

13. The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters

Author

Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, McDonald, Michael A, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A

Abstract

© 2019. The American Astronomical Society. All rights reserved. We present measurements of the stellar mass fractions ( f∗) for a sample of high-redshift (0.93≤.z≤1.32) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel-dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean f∗ between the two selection methods; though, we do find an unexpectedly large range in f∗ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find m∗ = 19.41 ± 0.07, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at z = 1.31, is the most distant MaDCoWS cluster confirmed to date.

Published
2021

14. Baryon content of massive galaxy clusters at 0.57

Author

MIT Kavli Institute for Astrophysics and Space Research, Chiu, I, Mohr, J, McDonald, M, Bocquet, S, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Brodwin, M, Desai, S, Dietrich, JP, Forman, WR, Gangkofner, C, Gonzalez, AH, Hennig, C, Liu, J, Reichardt, CL, Saro, A, Stalder, B, Stanford, SA, Song, J, Schrabback, T, Šuhada, R, Strazzullo, V, Zenteno, A, MIT Kavli Institute for Astrophysics and Space Research, Chiu, I, Mohr, J, McDonald, M, Bocquet, S, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Brodwin, M, Desai, S, Dietrich, JP, Forman, WR, Gangkofner, C, Gonzalez, AH, Hennig, C, Liu, J, Reichardt, CL, Saro, A, Stalder, B, Stanford, SA, Song, J, Schrabback, T, Šuhada, R, Strazzullo, V, and Zenteno, A

Abstract

© 2015 The Authors. We study the stellar, brightest cluster galaxy (BCG) and intracluster medium (ICM) masses of 14 South Pole Telescope (SPT) selected galaxy clusters with median redshift z = 0.9 and mass M500 = 6 × 1014M⊙. We estimate stellar masses for each cluster and BCG using six photometric bands, the ICM mass using X-ray observations and the virial masses using the SPT Sunyaev-Zel'dovich effect signature. At z = 0.9, the BCG mass M*BCG constitutes 0.12 ± 0.01 per cent of the halo mass for a 6 × 1014M⊙ cluster, and this fraction falls as M 500-0.58±0.07. The cluster stellar mass function has a characteristic mass M0 = 1011.0 ± 0.1M⊙, and the number of galaxies per unit mass in clusters is larger than in the field by a factor of 1.65 ± 0.20. We combine our SPT sample with previously published samples at low redshift and correct to a common initial mass function and for systematic virial mass differences. We then explore mass and redshift trends in the stellar fraction f*, the ICM fraction fICM, the collapsed baryon fraction fc and the baryon fraction fb. At a pivot mass of 6 × 1014M⊙ and redshift z = 0.9, the characteristic values are f* = 1.1 ± 0.1 per cent, fICM = 9.6 ± 0.5 per cent, fc = 10.7 ± 1.1 per cent and fb = 10.7 ± 0.6 per cent. These fractions all vary with cluster mass at high significance, with higher mass clusters having lower f* and fc and higher fICM and fb. When accounting for a 15 per cent systematic virial mass uncertainty, there is no statistically significant redshift trend at fixed mass. Our results support the scenario where clusters grow through accretion from subclusters (higher f*, lower fICM) and the field (lower f*, higher fICM), balancing to keep f* and fICM approximately constant since z ~ 0.9.

Published
2021

15. Galaxy populations in the most distant SPT-SZ clusters: I. Environmental quenching in massive clusters at 1.4 ≲ z ≲ 1.7

Author

Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, MB, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, M, Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, Stalder, B, Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, MB, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, M, Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, and Stalder, B

Abstract

© 2019 ESO. We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg 2 South Pole Telescope Sunyaev Zel'dovich effect (SPT-SZ) survey, which is sensitive to M 500 ≳ 3 × 10 14 M · clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z≳ 1.4, S/N SZE > 5 clusters, that are among the rarest most massive clusters known at this redshift. All five clusters show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates, although one (SPT-CLJ0607-4448) shows a galaxy concentration much less prominent than the others. The highest redshift cluster in this sample, SPT-CLJ0459-4947 at z ∼ 1.72, is the most distant M 500 > 10 14 M · cluster discovered thus far through its intracluster medium, and is one of only three known clusters in this mass range at z≳ 1.7, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, we find that the quiescent fraction in the cluster central regions (r/r 500 < 0.7) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range ∼0.5 - 0.8 for stellar masses log(M/M · ) > 10.85. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/N SZE > 5, even if they had the same quiescent fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in the central regions of the most massive clusters, occurring already earlier than z ∼ 1.5.

Published
2021

16. Galaxy populations in the most distant SPT-SZ clusters I. Environmental quenching in massive clusters at 1.4 less than or similar to z less than or similar to 1.7

Author

Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, MB, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, M, Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, Stalder, B, Strazzullo, V, Pannella, M, Mohr, JJ, Saro, A, Ashby, MLN, Bayliss, MB, Bocquet, S, Bulbul, E, Khullar, G, Mantz, AB, Stanford, SA, Benson, BA, Bleem, LE, Brodwin, M, Canning, REA, Capasso, R, Chiu, I, Gonzalez, AH, Gupta, N, Hlavacek-Larrondo, J, Klein, M, McDonald, M, Noordeh, E, Rapetti, D, Reichardt, CL, Schrabback, T, Sharon, K, and Stalder, B

Abstract

We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg 2 South Pole Telescope Sunyaev Zel'dovich effect (SPT-SZ) survey, which is sensitive to M 500 ≳ 3 × 10 14 M · clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z≳ 1.4, S/N SZE > 5 clusters, that are among the rarest most massive clusters known at this redshift. All five clusters show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates, although one (SPT-CLJ0607-4448) shows a galaxy concentration much less prominent than the others. The highest redshift cluster in this sample, SPT-CLJ0459-4947 at z ∼ 1.72, is the most distant M 500 > 10 14 M · cluster discovered thus far through its intracluster medium, and is one of only three known clusters in this mass range at z≳ 1.7, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, we find that the quiescent fraction in the cluster central regions (r/r 500 < 0.7) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range ∼0.5 - 0.8 for stellar masses log(M/M · ) > 10.85. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/N SZE > 5, even if they had the same quiescent fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in the central regions of the most massive clusters, occurring already earlier than z ∼ 1.5.

Published
2019

17. Baryon content of massive galaxy clusters at 0.57

Author

Chiu, I, Mohr, J, McDonald, M, Bocquet, S, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Brodwin, M, Desai, S, Dietrich, JP, Forman, WR, Gangkofner, C, Gonzalez, AH, Hennig, C, Liu, J, Reichardt, CL, Saro, A, Stalder, B, Stanford, SA, Song, J, Schrabback, T, Šuhada, R, Strazzullo, V, and Zenteno, A

Abstract

© 2015 The Authors. We study the stellar, brightest cluster galaxy (BCG) and intracluster medium (ICM) masses of 14 South Pole Telescope (SPT) selected galaxy clusters with median redshift z = 0.9 and mass M500 = 6 × 1014M⊙. We estimate stellar masses for each cluster and BCG using six photometric bands, the ICM mass using X-ray observations and the virial masses using the SPT Sunyaev-Zel'dovich effect signature. At z = 0.9, the BCG mass M*BCG constitutes 0.12 ± 0.01 per cent of the halo mass for a 6 × 1014M⊙ cluster, and this fraction falls as M 500-0.58±0.07. The cluster stellar mass function has a characteristic mass M0 = 1011.0 ± 0.1M⊙, and the number of galaxies per unit mass in clusters is larger than in the field by a factor of 1.65 ± 0.20. We combine our SPT sample with previously published samples at low redshift and correct to a common initial mass function and for systematic virial mass differences. We then explore mass and redshift trends in the stellar fraction f*, the ICM fraction fICM, the collapsed baryon fraction fc and the baryon fraction fb. At a pivot mass of 6 × 1014M⊙ and redshift z = 0.9, the characteristic values are f* = 1.1 ± 0.1 per cent, fICM = 9.6 ± 0.5 per cent, fc = 10.7 ± 1.1 per cent and fb = 10.7 ± 0.6 per cent. These fractions all vary with cluster mass at high significance, with higher mass clusters having lower f* and fc and higher fICM and fb. When accounting for a 15 per cent systematic virial mass uncertainty, there is no statistically significant redshift trend at fixed mass. Our results support the scenario where clusters grow through accretion from subclusters (higher f*, lower fICM) and the field (lower f*, higher fICM), balancing to keep f* and fICM approximately constant since z ~ 0.9.

Published
2016

18. Galaxy populations in massive galaxy clusters to z=1.1: colour distribution, concentration, halo occupation number and red sequence fraction

Author

Hennig, C, Mohr, JJ, Zenteno, A, Desai, S, Dietrich, JP, Bocquet, S, Strazzullo, V, Saro, A, Abbott, TMC, Abdalla, FB, Bayliss, M, Benoit-Levy, A, Bernstein, RA, Bertin, E, Brooks, D, Capasso, R, Capozzi, D, Carnero, A, Kind, MC, Carretero, J, Chiu, I, D'Andrea, CB, daCosta, LN, Diehl, HT, Doel, P, Eifler, TF, Evrard, AE, Fausti-Neto, A, Fosalba, P, Frieman, J, Gangkofner, C, Gonzalez, A, Gruen, D, Gruendl, RA, Gupta, N, Gutierrez, G, Honscheid, K, Hlavacek-Larrondo, J, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, March, M, Marshall, JL, Martini, P, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Neilsen, E, Nord, B, Ogando, R, Plazas, AA, Reichardt, C, Romer, AK, Rozo, E, Rykoff, ES, Sanchez, E, Santiago, B, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Stalder, B, Stanford, SA, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, Zhang, Y, Hennig, C, Mohr, JJ, Zenteno, A, Desai, S, Dietrich, JP, Bocquet, S, Strazzullo, V, Saro, A, Abbott, TMC, Abdalla, FB, Bayliss, M, Benoit-Levy, A, Bernstein, RA, Bertin, E, Brooks, D, Capasso, R, Capozzi, D, Carnero, A, Kind, MC, Carretero, J, Chiu, I, D'Andrea, CB, daCosta, LN, Diehl, HT, Doel, P, Eifler, TF, Evrard, AE, Fausti-Neto, A, Fosalba, P, Frieman, J, Gangkofner, C, Gonzalez, A, Gruen, D, Gruendl, RA, Gupta, N, Gutierrez, G, Honscheid, K, Hlavacek-Larrondo, J, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, March, M, Marshall, JL, Martini, P, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Neilsen, E, Nord, B, Ogando, R, Plazas, AA, Reichardt, C, Romer, AK, Rozo, E, Rykoff, ES, Sanchez, E, Santiago, B, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Stalder, B, Stanford, SA, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, and Zhang, Y

Abstract

We study the galaxy populations in 74 Sunyaev–Zeldovich effect selected clusters from the South Pole Telescope survey, which have been imaged in the science verification phase of the Dark Energy Survey. The sample extends up to z ∼ 1.1 with 4 × 1014 M⊙ ≤ M200 ≤ 3 × 1015M⊙. Using the band containing the 4000 Å break and its redward neighbour, we study the colour–magnitude distributions of cluster galaxies to ∼m* + 2, finding that: (1)The intrinsic rest frame g − r colour width of the red sequence (RS) population is ∼0.03 out to z ∼ 0.85 with a preference for an increase to ∼0.07 at z = 1, and (2) the prominence of the RS declines beyond z ∼ 0.6. The spatial distribution of cluster galaxies is well described by the NFW profile out to 4R200 with a concentration of cg=3.59+0.20−0.18⁠, 5.37+0.27−0.24 and 1.38+0.21−0.19 for the full, the RS and the blue non-RS populations, respectively, but with ∼40 per cent to 55 per cent cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region N200 exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The RS fraction within R200 is (68 ± 3) per cent at z = 0.46, varies from ∼55 per cent at z = 1 to ∼80 per cent at z = 0.1 and exhibits intrinsic variation among clusters of ∼14 per cent. We discuss a model that suggests that the observed redshift trend in RS fraction favours a transformation time-scale for infalling field galaxies to become RS galaxies of 2–3 Gyr.

Published
2017

19. Comparing dynamical and photometric-stellar masses of early-type galaxies at z similar to 1

Author

Rettura, A, Rosati, P, Strazzullo, V, Dickinson, M, Fosbury, Rae, Rocca-Volmerange, B, Cimatti, A, Alighieri, Sds, Kuntschner, H, Lanzoni, B, Nonino, M, Popesso, P, Stern, D, Eisenhardt, Pr, Lidman, C, Stanford, Sa, Rettura, A, Rosati, P, Strazzullo, V, Dickinson, M, Fosbury, Rae, Rocca-Volmerange, B, Cimatti, A, Alighieri, Sd, Kuntschner, H, Lanzoni, B, Nonino, M, Popesso, P, Stern, D, Eisenhardt, Pr, Lidman, C, and Stanford, Sa

Abstract

Aims. The purpose of this study is to explore the relationship between galaxy stellar masses, based on multiwavelength photometry spectral template fitting and dynamical masses based on published velocity dispersion measurements, for a sample of 48 early-type galaxies at z similar to 1 with HST/ACS morphological information. Methods. We determine photometric-stellar masses and perform a quantitative morphological analysis of cluster and field galaxies at redshift 0.6 < z < 1.2, using ground- and space-based multiwavelength data available on the GOODS-S field and on the field around the X-ray luminous cluster RDCS1252.9-2927 at z = 1.24. We use multi-band photometry over 0.4-8 mu m from HST/ACS, VLT/ISAAC and Spitzer/IRAC to estimate photometric-stellar masses using Composite Stellar Population ( CSP) templates computed with PEGASE. 2 ( Fioc & Rocca-Volmerange 1997) models. We compare stellar masses with those obtained using CSPs built with Bruzual & Charlot ( 2003, MNRAS, 344, 1000; BC03) and Maraston ( 2005, MNRAS, 362, 799; M05) models. We then compare photometric-stellar mass and dynamical mass estimates as a function of morphological parameters obtained from HST/ACS imaging. Results. Based on our sample, which spans the mass range log M-phot similar or equal to [ 10, 11.5], we find that 1) PEGASE. 2, BC03, M05 yield consistent photometric-stellar masses for early-type galaxies at z similar to 1 with a small scatter ( 0.15 dex rms); 2) adopting a Kroupa IMF, photometric-stellar masses match dynamical mass estimates for early-type galaxies with an average offset of 0.27 dex; 3) assuming a constant IMF, increasing dark matter fraction with the increasing galaxy mass can explain the observed trend; 4) we observe that early- type galaxies with significant disk components ( Sa/Sab) or with signs of dynamical interaction tend to have the largest deviation from a one-to-one M-dyn vs. M-phot relation.

Published
2006

20. COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY

Author

de Haan, T, Benson, BA, Bleem, LE, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zenteno, A, de Haan, T, Benson, BA, Bleem, LE, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, and Zenteno, A

Published
2016

21. STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

Author

McDonald, M, Stalder, B, Bayliss, M, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chiu, I, Desai, S, Gonzalez, AH, Hlavacek-Larrondo, J, Holzapfel, WL, Marrone, DP, Miller, ED, Reichardt, CL, Saliwanchik, BR, Saro, A, Schrabback, T, Stanford, SA, Stark, AA, Vieira, JD, Zenteno, A, McDonald, M, Stalder, B, Bayliss, M, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chiu, I, Desai, S, Gonzalez, AH, Hlavacek-Larrondo, J, Holzapfel, WL, Marrone, DP, Miller, ED, Reichardt, CL, Saliwanchik, BR, Saro, A, Schrabback, T, Stanford, SA, Stark, AA, Vieira, JD, and Zenteno, A

Published
2016

22. Baryon content of massive galaxy clusters at 0.57 < z < 1.33

Author

Chiu, I, Mohr, J, McDonald, M, Bocquet, S, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Brodwin, M, Desai, S, Dietrich, JP, Forman, WR, Gangkofner, C, Gonzalez, AH, Hennig, C, Liu, J, Reichardt, CL, Saro, A, Stalder, B, Stanford, SA, Song, J, Schrabback, T, Suhada, R, Strazzullo, V, Zenteno, A, Chiu, I, Mohr, J, McDonald, M, Bocquet, S, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Brodwin, M, Desai, S, Dietrich, JP, Forman, WR, Gangkofner, C, Gonzalez, AH, Hennig, C, Liu, J, Reichardt, CL, Saro, A, Stalder, B, Stanford, SA, Song, J, Schrabback, T, Suhada, R, Strazzullo, V, and Zenteno, A

Published
2016

23. SPT-GMOS: A GEMINI/GMOS-SOUTH SPECTROSCOPIC SURVEY OF GALAXY CLUSTERS IN THE SPT-SZ SURVEY

Author

Bayliss, MB, Ruel, J, Stubbs, CW, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Capasso, R, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zenteno, A, Bayliss, MB, Ruel, J, Stubbs, CW, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Capasso, R, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, and Zenteno, A

Published
2016

24. A MEASUREMENT OF GRAVITATIONAL LENSING OF THE COSMIC MICROWAVE BACKGROUND BY GALAXY CLUSTERS USING DATA FROM THE SOUTH POLE TELESCOPE

Author

Baxter, EJ, Keisler, R, Dodelson, S, Aird, KA, Allen, SW, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Jones, C, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Baxter, EJ, Keisler, R, Dodelson, S, Aird, KA, Allen, SW, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Jones, C, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

Clusters of galaxies are expected to gravitationally lens the cosmic microwave background (CMB) and thereby generate a distinct signal in the CMB on arcminute scales. Measurements of this effect can be used to constrain the masses of galaxy clusters with CMB data alone. Here we present a measurement of lensing of the CMB by galaxy clusters using data from the South Pole Telescope (SPT). We develop a maximum likelihood approach to extract the CMB cluster lensing signal and validate the method on mock data. We quantify the effects on our analysis of several potential sources of systematic error and find that they generally act to reduce the best-fit cluster mass. It is estimated that this bias to lower cluster mass is roughly $0.85\sigma$ in units of the statistical error bar, although this estimate should be viewed as an upper limit. We apply our maximum likelihood technique to 513 clusters selected via their SZ signatures in SPT data, and rule out the null hypothesis of no lensing at $3.1\sigma$. The lensing-derived mass estimate for the full cluster sample is consistent with that inferred from the SZ flux: $M_{200,\mathrm{lens}} = 0.83_{-0.37}^{+0.38}\, M_{200,\mathrm{SZ}}$ (68% C.L., statistical error only).

Published
2015

25. MEASUREMENT OF GALAXY CLUSTER INTEGRATED COMPTONIZATION AND MASS SCALING RELATIONS WITH THE SOUTH POLE TELESCOPE

Author

Saliwanchik, BR, Montroy, TE, Aird, KA, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Saliwanchik, BR, Montroy, TE, Aird, KA, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We describe a method for measuring the integrated Comptonization (YSZ) of clusters of galaxies from measurements of the Sunyaev-Zel'dovich (SZ) effect in multiple frequency bands and use this method to characterize a sample of galaxy clusters detected in South Pole Telescope (SPT) data. We test this method on simulated cluster observations and verify that it can accurately recover cluster parameters with negligible bias. In realistic simulations of an SPT-like survey, with realizations of cosmic microwave background anisotropy, point sources, and atmosphere and instrumental noise at typical SPT-SZ survey levels, we find that YSZ is most accurately determined in an aperture comparable to the SPT beam size. We demonstrate the utility of this method to measure YSZ and to constrain mass scaling relations using X-ray mass estimates for a sample of 18 galaxy clusters from the SPT-SZ survey. Measuring YSZ within a 0.75' radius aperture, we find an intrinsic log-normal scatter of 21+/-11% in YSZ at a fixed mass. Measuring YSZ within a 0.3 Mpc projected radius (equivalent to 0.75' at the survey median redshift z = 0.6), we find a scatter of 26+/-9%. Prior to this study, the SPT observable found to have the lowest scatter with mass was cluster detection significance. We demonstrate, from both simulations and SPT observed clusters, that YSZ measured within an aperture comparable to the SPT beam size is equivalent, in terms of scatter with cluster mass, to SPT cluster detection significance.

Published
2015

26. GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY

Author

Bleem, LE, Stalder, B, de Haan, T, Aird, KA, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Bleem, LE, Stalder, B, de Haan, T, Aird, KA, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We present a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg$^2$ of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500-square-degree SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold of $\xi$ =4.5 (5.0). Ground- and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the $\xi$>4.5 candidates and 387 (or 95%) of the $\xi$>5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. We estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; we additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above $z$~0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is $M_{\scriptsize 500c}(\rho_\mathrm{crit})$ ~ 3.5 x 10$^{14} M_\odot h^{-1}$, the median redshift is $z_{med}$ =0.55, and the highest-redshift systems are at $z$>1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution.

Published
2015

27. The nascent red sequence at z ~ 2

Author

Zirm, Andrew W, Stanford, SA, Postman, M, Overzier, RA, Blakeslee, JP, Rosati, P, Kurk, J, Pentericci, L, Venemans, B, Miley, GK, Roettgering, HJA, Franx, M, van der Wel, Arjen, Demarco, R, and van Breugel, W

Subjects
H-ALPHA EMITTERS, formation [galaxies], CLUSTER SURVEY, Astrophysics::Cosmology and Extragalactic Astrophysics, stellar content [galaxies], STAR-FORMATION, PROTO-CLUSTER, Physics and Astronomy, Z=2.16, SEARCH, clusters : individual (MRC 1138-262) [galaxies], Astrophysics::Solar and Stellar Astrophysics, EARLY-TYPE GALAXIES, PHOTOMETRY, COMBO-17, HIGH-REDSHIFT, Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies]
Abstract

We present new constraints on the evolution of the early-type galaxy color-magnitude relation (CMR) based on deep near-infrared imaging of a galaxy protocluster at z = 2.16 obtained using NICMOS on board the Hubble Space Telescope. This field contains a spectroscopically confirmed space overdensity of Ly alpha- and H alpha-emitting galaxies that surrounds the powerful radio galaxy MRC 1138-262. Using these NICMOS data we identify a significant surface overdensity (=6.2 times) of red J(110) - H(160) galaxies in the color-magnitude diagram (when compared with deep NICMOS imaging from the HDF-N and UDF). The optical-NIR colors of these prospective red-sequence galaxies indicate the presence of ongoing dust-obscured star formation or recently formed (less than or similar to 1.5 Gyr) stellar populations in a majority of the red galaxies. We measure the slope and intrinsic scatter of the CMR for three different red galaxy samples selected by a wide color cut and using photometric redshifts both with and without restrictions on rest-frame optical morphology. In all three cases both the rest-frame U - B slope and intrinsic color scatter are considerably higher than corresponding values for lower redshift galaxy clusters. These results suggest that while some relatively quiescent galaxies do exist in this protocluster both the majority of the galaxy population and hence the color-magnitude relation are still in the process of forming, as expected.

Published
2008

29. Optical Spectroscopy and Velocity Dispersions of Galaxy Clusters from the SPT-SZ Survey

Author

Ruel, J, Bazin, G, Bayliss, M, Brodwin, M, Foley, RJ, Stalder, B, Aird, KA, Armstrong, R, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Chapman, SC, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, v Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Starsk, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Ruel, J, Bazin, G, Bayliss, M, Brodwin, M, Foley, RJ, Stalder, B, Aird, KA, Armstrong, R, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Chapman, SC, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, v Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Starsk, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We present optical spectroscopy of galaxies in clusters detected through the Sunyaev-Zel'dovich (SZ) effect with the South Pole Telescope (SPT). We report our own measurements of $61$ spectroscopic cluster redshifts, and $48$ velocity dispersions each calculated with more than $15$ member galaxies. This catalog also includes $19$ dispersions of SPT-observed clusters previously reported in the literature. The majority of the clusters in this paper are SPT-discovered; of these, most have been previously reported in other SPT cluster catalogs, and five are reported here as SPT discoveries for the first time. By performing a resampling analysis of galaxy velocities, we find that unbiased velocity dispersions can be obtained from a relatively small number of member galaxies ($\lesssim 30$), but with increased systematic scatter. We use this analysis to determine statistical confidence intervals that include the effect of membership selection. We fit scaling relations between the observed cluster velocity dispersions and mass estimates from SZ and X-ray observables. In both cases, the results are consistent with the scaling relation between velocity dispersion and mass expected from dark-matter simulations. We measure a $\sim$30% log-normal scatter in dispersion at fixed mass, and a $\sim$10% offset in the normalization of the dispersion-mass relation when compared to the expectation from simulations, which is within the expected level of systematic uncertainty.

Published
2014

30. THE REDSHIFT EVOLUTION OF THE MEAN TEMPERATURE, PRESSURE, AND ENTROPY PROFILES IN 80 SPT-SELECTED GALAXY CLUSTERS

Author

McDonald, M, Benson, BA, Vikhlinin, A, Aird, KA, Allen, SW, Bautz, M, Bayliss, M, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McMahon, JJ, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Zenteno, A, McDonald, M, Benson, BA, Vikhlinin, A, Aird, KA, Allen, SW, Bautz, M, Bayliss, M, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McMahon, JJ, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, and Zenteno, A

Published
2014

31. SPT-CL J2040-4451: AN SZ-SELECTED GALAXY CLUSTER AT z=1.478 WITH SIGNIFICANT ONGOING STAR FORMATION

Author

Bayliss, MB, Ashby, MLN, Ruel, J, Brodwin, M, Aird, KA, Bautz, MW, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiattii, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, de Haan, T, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, Mawatari, K, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Stalder, B, Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, R, Zenteno, A, Bayliss, MB, Ashby, MLN, Ruel, J, Brodwin, M, Aird, KA, Bautz, MW, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiattii, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, de Haan, T, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, Mawatari, K, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Stalder, B, Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, R, and Zenteno, A

Abstract

SPT-CLJ2040-4451 -- spectroscopically confirmed at z = 1.478 -- is the highest redshift galaxy cluster yet discovered via the Sunyaev-Zel'dovich effect. SPT-CLJ2040-4451 was a candidate galaxy cluster identified in the first 720 deg^2 of the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, and confirmed in follow-up imaging and spectroscopy. From multi-object spectroscopy with Magellan-I/Baade+IMACS we measure spectroscopic redshifts for 15 cluster member galaxies, all of which have strong [O II] 3727 emission. SPT-CLJ2040-4451 has an SZ-measured mass of M_500,SZ = 3.2 +/- 0.8 X 10^14 M_Sun/h_70, corresponding to M_200,SZ = 5.8 +/- 1.4 X 10^14 M_Sun/h_70. The velocity dispersion measured entirely from blue star forming members is sigma_v = 1500 +/- 520 km/s. The prevalence of star forming cluster members (galaxies with > 1.5 M_Sun/yr) implies that this massive, high-redshift cluster is experiencing a phase of active star formation, and supports recent results showing a marked increase in star formation occurring in galaxy clusters at z >1.4. We also compute the probability of finding a cluster as rare as this in the SPT-SZ survey to be >99%, indicating that its discovery is not in tension with the concordance Lambda-CDM cosmological model.

Published
2014

32. SPT-CL J0205-5829: A z=1.32 EVOLVED MASSIVE GALAXY CLUSTER IN THE SOUTH POLE TELESCOPE SUNYAEV-ZEL'DOVICH EFFECT SURVEY

Author

Stalder, B, Ruel, J, Suhada, R, Brodwin, M, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Stalder, B, Ruel, J, Suhada, R, Brodwin, M, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

The galaxy cluster SPT-CL J0205-5829 currently has the highest spectroscopically-confirmed redshift, z=1.322, in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. XMM-Newton observations measure a core-excluded temperature of Tx=8.7keV producing a mass estimate that is consistent with the Sunyaev-Zel'dovich derived mass. The combined SZ and X-ray mass estimate of M500=(4.9+/-0.8)e14 h_{70}^{-1} Msun makes it the most massive known SZ-selected galaxy cluster at z>1.2 and the second most massive at z>1. Using optical and infrared observations, we find that the brightest galaxies in SPT-CL J0205-5829 are already well evolved by the time the universe was <5 Gyr old, with stellar population ages >3 Gyr, and low rates of star formation (<0.5Msun/yr). We find that, despite the high redshift and mass, the existence of SPT-CL J0205-5829 is not surprising given a flat LambdaCDM cosmology with Gaussian initial perturbations. The a priori chance of finding a cluster of similar rarity (or rarer) in a survey the size of the 2500 deg^2 SPT-SZ survey is 69%.

Published
2013

33. Supplementary online material for article, "Erratum: �The Spitzer South Pole Telescope Deep Field: Survey Design and Infrared Array Camera Catalogs'

Author

Ashby, MLN, primary, Stanford, SA, additional, Brodwin, M, additional, Gonzalez, AH, additional, Martinez-Manzo, J, additional, Bartlett, JG, additional, Benson, BA, additional, Bleem, LE, additional, Crawford, TM, additional, Dey, A, additional, Dressler, A, additional, Eisenhardt, PRM, additional, Galametz, A, additional, Januzzi, BT, additional, Marrone, DP, additional, Mei, S, additional, Muzzin, A, additional, Pacaud, F, additional, Pierre, M, additional, Stern, D, additional, and Viera, JD, additional

Published
2014
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34. DYNAMIC SIMULATIONS OF THE INTERACTING GALAXIES IN THE NGC-520 UGC-957 SYSTEM

Author

STANFORD, SA, BALCELLS, M, and Kapteyn Astronomical Institute

Subjects
MODELS, CLOUDS, GALAXIES-STRUCTURE, Astrophysics::Cosmology and Extragalactic Astrophysics, APERTURE SYNTHESIS, MOLECULAR GAS, GALAXIES-INTERACTIONS, BINARY GALAXIES, PAIR, STAR FORMATION, Astrophysics::Earth and Planetary Astrophysics, GALAXIES-INDIVIDUAL (NGC-520, UGC-957), EMISSION, Astrophysics::Galaxy Astrophysics
Abstract

Numerical simulations of the interacting galaxies in the NGC 520/UGC 957 system are presented. Two sets of models were produced to investigate the postulated three-galaxy system of two colliding disk galaxies within NGC 520 and the dwarf galaxy UGC 957. The morphology and kinematics of the models are compared with previously obtained optical, infrared, and 21 cm imaging and spectroscopy to choose best-fitting simulations. The first set of models simulated a dwarf perturbing one-disk galaxy, which tested the possibility that NGC 520 contains only one galaxy disturbed by the passage of UGC 957. The resulting morphology of the perturbed single disk in the simulation fails to reproduce the observed tidal tails and northwest mass condensation of NGC 520. A second set of models simulated two colliding disks, which tested the hypothesis that NGC 520 itself contains two galaxies in a strong collision and UGC 957 is unimportant to the interaction. These disk-disk models produced a good match to the morphology of the present NGC 520. A detailed match of the internal kinematics could not be reached, at least partly due to the restrictions of the modeling technique. Also, the southern tidal in the disk-disk simulation was too short. We conclude that (1) NGC 520 contains two colliding disk galaxies which have produced the brighter southern half of the long tidal tail and (2) UGC 957, which may originally have been a satellite of one of the disk galaxies, formed the diffuse northern tail as it orbited NGC 520. The time scale for the collision of the two disks is approximately 3 x 10(8) years. Implications of the disks' collision for their gas components and the apparently enhanced star formation rate are discussed.

Published
1991

35. Evolution of the Color‐Magnitude Relation in High‐Redshift Clusters: Blue Early‐Type Galaxies and Red Pairs in RDCS J0910+5422

Author

S. Mei, J. P. Blakeslee, S. A. Stanford, B. P. Holden, P. Rosati, V. Strazzullo, N. Homeier, M. Postman, M. Franx, A. Rettura, H. Ford, G. D. Illingworth, S. Ettori, R. J. Bouwens, R. Demarco, A. R. Martel, M. Clampin, G. F. Hartig, P. Eisenhardt, D. R. Ardila, F. Bartko, N. Benitez, L. D. Bradley, T. J. Broadhurst, R. A. Brown, C. J. Burrows, E. S. Cheng, N. J. G. Cross, P. D. Feldman, D. A. Golimowski, T. Goto, C. Gronwall, L. Infante, R. A. Kimble, J. E. Krist, M. P. Lesser, F. Menanteau, G. R. Meurer, G. K. Miley, V. Motta, M. Sirianni, W. B. Sparks, H. D. Tran, Z. I. Tsvetanov, R. L. White, W. Zheng, Mei, S, Blakeslee, Jp, Stanford, Sa, Holden, Bp, Rosati, P, Strazzullo, V, Homeier, N, Postman, M, Franx, M, Rettura, A, Ford, H, Illingworth, Gd, Ettori, S, Bouwens, Rj, Demarco, R, Martel, Ar, Clampin, M, Hartig, Gf, Eisenhardt, P, Ardila, Dr, Bartko, F, Benitez, N, Bradley, Ld, Broadhurst, Tj, Brown, Ra, Burrows, Cj, Cheng, E, Cross, Njg, Feldman, Pd, Golimowski, Da, Goto, T, Gronwall, C, Infante, L, Kimble, Ra, Krist, Je, Lesser, Mp, Menanteau, F, Meurer, Gr, Miley, Gk, Motta, V, Sirianni, M, Sparks, Wb, Tran, Hd, Tsvetanov, Zi, White, Rl, and Zheng, W

Subjects
Physics, education.field_of_study, Star formation, Metallicity, Astrophysics (astro-ph), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Space and Planetary Science, Elliptical galaxy, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract

The color-magnitude relation has been determined for the RDCS J0910+5422 cluster of galaxies at redshift z = 1.106. Cluster members were selected from HST ACS images, combined with ground--based near--IR imaging and optical spectroscopy. The observed early--type color--magnitude relation (CMR) in (i_775 -z_850) versus z_850 shows intrinsic scatters in color of 0.042 +/- 0.010 mag and 0.044 +/- 0.020 mag for ellipticals and S0s, respectively. From the scatter about the CMR, a mean luminosity--weighted age t > 3.3 Gyr (z > 3) is derived for the elliptical galaxies. Strikingly, the S0 galaxies in RDCS J0910+5422 are systematically bluer in (i_775 - z_850) by 0.07 +/- 0.02 mag, with respect to the ellipticals. The ellipticity distribution as a function of color indicates that the face-on S0s in this particular cluster have likely been classified as elliptical. Thus, if anything, the offset in color between the elliptical and S0 populations may be even more significant. The color offset between S0 and E corresponds to an age difference of ~1 Gyr, for a single-burst solar metallicity model. A solar metallicity model with an exponential decay in star formation will reproduce the offset for an age of 3.5 Gyr, i.e. the S0s have evolved gradually from star forming progenitors. The early--type population in this cluster appears to be still forming. The blue early-type disk galaxies in RDCS J0910+5422 likely represent the direct progenitors of the more evolved S0s that follow the same red sequence as ellipticals in other clusters. Thirteen red galaxy pairs are observed and the galaxies associated in pairs constitute ~40% of the CMR galaxies in this cluster., ApJ, in press

Published
2006
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36. The near-infrared luminosity function of cluster galaxies beyond redshift one

Author

Piero Rosati, Mario Nonino, P. E. Eisenhardt, Ricardo Demarco, Christopher Lidman, V. Strazzullo, Sune Toft, S. A. Stanford, V. Mainieri, Stefano Ettori, Strazzullo, V, Rosati, P, Stanford, Sa, Lidman, C, Nonino, M, Demarco, R, Eisenhardt, Pe, Ettori, S, Mainieri, V, and Toft, S

Subjects
Physics, Stellar mass, media_common.quotation_subject, Astrophysics (astro-ph), Near-infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Universe, Redshift, Stars, Space and Planetary Science, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), media_common
Abstract

We determined the K band luminosity function (LF) of cluster galaxies at redshift z~1.2, using near-infrared images of three X-ray luminous clusters at z=1.11,1.24,1.27. The composite LF was derived down to M*+4, by means of statistical background subtraction, and is well described by a Schechter function with K*=20.5 AB mag and alpha=-1. From the K band composite LF we derived the stellar mass function of cluster galaxies. Using available X-ray mass profiles we determined the M/L ratios of these three clusters, which tend to be lower than those measured in the local universe. With these data, no significant difference can be seen between the shapes of the cluster galaxies LF and the LF of field galaxies at similar redshift. We also found no significant evolution out to z ~1.2 in the bright (2. The results obtained in this work support and extend previous findings that most of the stars in bright galaxies were formed at high redshift, and that K-bright (M>10^11 Msun) galaxies were already in place at z ~ 1.2, at least in the central regions of X-ray luminous clusters. Together with recent results on the field galaxies stellar mass function, this implies that most of the stellar mass is already assembled in massive galaxies by z ~ 1, both in low and high density environments., Comment: 16 pages, 10 figures, to appear in A&A

Published
2006

37. Spectroscopic confirmation of a mature galaxy cluster at a redshift of 2.

Author

Willis JP, Canning REA, Noordeh ES, Allen SW, King AL, Mantz A, Morris RG, Stanford SA, and Brammer G

Abstract

Galaxy clusters are the most massive virialized structures in the Universe and are formed through the gravitational accretion of matter over cosmic time 1 . The discovery 2 of an evolved galaxy cluster at redshift z = 2, corresponding to a look-back time of 10.4 billion years, provides an opportunity to study its properties. The galaxy cluster XLSSC 122 was originally detected as a faint, extended X-ray source in the XMM Large Scale Structure survey and was revealed to be coincident with a compact over-density of galaxies 2 with photometric redshifts of 1.9 ± 0.2. Subsequent observations 3 at millimetre wavelengths detected a Sunyaev-Zel'dovich decrement along the line of sight to XLSSC 122, thus confirming the existence of hot intracluster gas, while deep imaging spectroscopy from the European Space Agency's X-ray Multi-Mirror Mission (XMM-Newton) revealed 4 an extended, X-ray-bright gaseous atmosphere with a virial temperature of 60 million Kelvin, enriched with metals to the same extent as are local clusters. Here we report optical spectroscopic observations of XLSSC 122 and identify 37 member galaxies at a mean redshift of 1.98, corresponding to a look-back time of 10.4 billion years. We use photometry to determine a mean, dust-free stellar age of 2.98 billion years, indicating that star formation commenced in these galaxies at a mean redshift of 12, when the Universe was only 370 million years old. The full range of inferred formation redshifts, including the effects of dust, covers the interval from 7 to 13. These observations confirm that XLSSC 122 is a remarkably mature galaxy cluster with both evolved stellar populations in the member galaxies and a hot, metal-rich gas composing the intracluster medium.

Published
2020
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38. Weeding Out the Truth: Adolescents and Cannabis.

Author

Ammerman S and Tau G

Subjects
Adolescent, Animals, Brain drug effects, Brain growth & development, Brain metabolism, Diagnostic and Statistical Manual of Mental Disorders, History, 20th Century, History, 21st Century, Humans, Marijuana Smoking adverse effects, Marijuana Smoking history, Medical Marijuana administration & dosage, United States epidemiology, Adolescent Behavior, Legislation, Drug history, Marijuana Abuse diagnosis, Marijuana Abuse epidemiology, Marijuana Smoking epidemiology, Marijuana Smoking legislation & jurisprudence
Abstract

The use of cannabis for both legal (similar to alcohol) and medical purposes is becoming more common. Although cannabis remains an illegal Schedule 1 drug federally, as of November 2015, 23 states and the District of Columbia have legalized "medical" cannabis, and 4 states and the District of Columbia have legalized the use of cannabis for adults aged 21 years and older. It is very likely that more and more states will sooner rather than later allow cannabis for both medical and legal purposes. This review article will focus on a variety of issues relevant to the current debate about cannabis, and will address the following.

Published
2016
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39. Early assembly of the most massive galaxies.

Author

Collins CA, Stott JP, Hilton M, Kay ST, Stanford SA, Davidson M, Hosmer M, Hoyle B, Liddle A, Lloyd-Davies E, Mann RG, Mehrtens N, Miller CJ, Nichol RC, Romer AK, Sahlén M, Viana PT, and West MJ

Abstract

The current consensus is that galaxies begin as small density fluctuations in the early Universe and grow by in situ star formation and hierarchical merging. Stars begin to form relatively quickly in sub-galactic-sized building blocks called haloes which are subsequently assembled into galaxies. However, exactly when this assembly takes place is a matter of some debate. Here we report that the stellar masses of brightest cluster galaxies, which are the most luminous objects emitting stellar light, some 9 billion years ago are not significantly different from their stellar masses today. Brightest cluster galaxies are almost fully assembled 4-5 billion years after the Big Bang, having grown to more than 90 per cent of their final stellar mass by this time. Our data conflict with the most recent galaxy formation models based on the largest simulations of dark-matter halo development. These models predict protracted formation of brightest cluster galaxies over a Hubble time, with only 22 per cent of the stellar mass assembled at the epoch probed by our sample. Our findings suggest a new picture in which brightest cluster galaxies experience an early period of rapid growth rather than prolonged hierarchical assembly.

Published
2009
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40. Evidence against a redshift z > 6 for the galaxy STIS123627+621755.

Author

Stern D, Eisenhardt P, Spinrad H, Dawson S, van Breugel W, Dey A, de Vries W, and Stanford SA

Abstract

The identification of galaxies at extreme distances provides the most direct information about the earliest phases of galaxy formation. But at redshifts z > 5 even the most luminous galaxies appear faint; the interpretation of low signal-to-noise ratio data is difficult and misidentifications do occur. Here we report optical and near-infrared observations of the source STIS123627+621755, which was previously suggested to be at a redshift of 6.68 (ref. 1). At that redshift, and with the reported spectral energy distribution, the galaxy should be essentially invisible at wavelengths less than 9,300 A, because the intervening intergalactic medium absorbs almost all light energetic enough to ionize neutral hydrogen--that is, with wavelengths less than the redshifted Lyman limit of lambda = (1 + z) x 912A. At near-infrared wavelengths, however, the galaxy should be relatively bright. Here we report a detection of the galaxy at 6,700 A and a non-detection at a wavelength of 1.2 microm, contrary to expectations for z approximately 6.68. The data conservatively require that STIS123627+621755 has a redshift z < 6.

Published
2000
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41. Discovery of a Color-selected Quasar at z = 5.50.

Author

Stern D, Spinrad H, Eisenhardt P, Bunker AJ, Dawson S, Stanford SA, and Elston R

Abstract

We present observations of RD J030117+002025, a quasar at z=5.50 discovered from deep, multicolor, ground-based observations covering 74 arcmin2. This is the most distant quasar or active galaxy currently known. The object was targeted as an R-band dropout, with RAB>26.3 (3 sigma limit in a 3&arcsec; diameter region), IAB=23.8, and zAB=23.4. The Keck/Low-Resolution Imaging Spectrometer spectrum shows broad Lyalpha/N v lambda1240 emission and sharp absorption decrements from the highly redshifted hydrogen forests. The fractional continuum depression due to the Lyalpha forest is DA=0.90. RD J030117+002025 is the least luminous high-redshift quasar known (MB approximately -22.7).

Published
2000
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42. Functional association of class II antigens with cell surface binding of Epstein-Barr virus.

Author

Reisert PS, Spiro RC, Townsend PL, Stanford SA, Sairenji T, and Humphreys RE

Subjects
Animals, Antibodies, Neoplasm physiology, Antigens, Surface immunology, Antilymphocyte Serum pharmacology, Binding, Competitive, Burkitt Lymphoma immunology, Burkitt Lymphoma microbiology, Cell Line, Electrophoresis, Polyacrylamide Gel, HLA-DR Antigens, Histocompatibility Antigens Class II immunology, Humans, Membrane Proteins analysis, Neoplasm Proteins analysis, Rabbits, Receptors, Complement 3d, Receptors, Virus analysis, Antigens, Surface analysis, Herpesvirus 4, Human metabolism, Histocompatibility Antigens Class II analysis, Receptors, Virus physiology
Abstract

A functional role of class II antigen in the binding of Epstein-Barr virus (EBV) was deduced from the study of membrane proteins on Jijoye, an EBV receptor (EBVR)-positive B cell line, and its mutant, EBVR-negative daughter cell line, P3HR-1. From gel electrophoresis of radiolabeled microsomal membrane proteins and immunoprecipitates, we identified class II antigen on Jijoye but not on P3HR-1 cells and the presence of Ii on both cell lines. The role of these molecules in EBVR function was tested by antibody blocking of virus adsorption. Anti-p23,30 serum (to class II antigen) was found to block binding of EBV to B lymphoblasts under conditions in which normal rabbit serum, rabbit antiserum to butyrate-treated P3HR-1 cells (with ample anti-Ii antibodies), and rabbit anti-p44,12 (to class I antigen and beta 2-microglobulin) serum did not block virus binding. Only one of four commercial monoclonal antibodies (MoAb) to framework epitopes on class II antigens blocked binding of EBV, whereas all four MoAb demonstrated immunofluorescent reactivity with the EBVR+ Raji cells. In previous studies of binding of EBV to hairy leukemic cells, a substantial subpopulation of HLA-DR+, EBVR- cells was identified, in addition to HLA-DR+, EBVR+ cells. These findings were consistent with the view that the HLA-DR complex has a role in the binding of EBV but that other components are also needed for the expression of EBVR function.

Published
1985

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