Author: "Pryke, C." / Publisher: iop publishing ltd - Searchworks@Jio Institute Digital Library Search Results

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37 results on '"Pryke, C."'

1. Measurements of the Cross-spectra of the Cosmic Infrared and Microwave Backgrounds from 95 to 1200 GHz

Author: Viero, MP, Reichardt, CL, Benson, BA, Bleem, LE, Bock, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, G, Holzapfel, WL, Hou, Z, Hrubes, JD, Knox, L, Lee, AT, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Moncelsi, L, Padin, S, Pryke, C, Ruhl, JE, Schaffer, KK, Serra, P, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, Zemcov, M, Viero, MP, Reichardt, CL, Benson, BA, Bleem, LE, Bock, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, G, Holzapfel, WL, Hou, Z, Hrubes, JD, Knox, L, Lee, AT, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Moncelsi, L, Padin, S, Pryke, C, Ruhl, JE, Schaffer, KK, Serra, P, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, and Zemcov, M
Published: 2019

2. Maps of the Southern Millimeter-wave Sky from Combined 2500 deg(2) SPT-SZ and Planck Temperature Data

Author: Chown, R, Omori, Y, Aylor, K, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Henning, JW, Halverson, NW, Harrington, NL, Holder, G, Holzapfel, WL, Hou, Z, Hrubes, JD, Knox, L, Lee, AT, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Simard, G, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, Wu, WLK, Chown, R, Omori, Y, Aylor, K, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Henning, JW, Halverson, NW, Harrington, NL, Holder, G, Holzapfel, WL, Hou, Z, Hrubes, JD, Knox, L, Lee, AT, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Simard, G, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, and Wu, WLK
Abstract: We present three maps of the millimeter-wave sky created by combining data from the South Pole Telescope (SPT) and the Planck satellite. We use data from the SPT-SZ survey, a survey of 2540 deg 2 of the the sky with arcminute resolution in three bands centered at 95, 150, and 220 GHz, and the full-mission Planck temperature data in the 100, 143, and 217 GHz bands. A linear combination of the SPT-SZ and Planck data is computed in spherical harmonic space, with weights derived from the noise of both instruments. This weighting scheme results in Planck data providing most of the large-angular-scale information in the combined maps, with the smaller-scale information coming from SPT-SZ data. A number of tests have been done on the maps. We find their angular power spectra to agree very well with theoretically predicted spectra and previously published results
Published: 2018

3. Constraints on Cosmological Parameters from the Angular Power Spectrum of a Combined 2500 deg(2) SPT-SZ and Planck Gravitational Lensing Map

Author: Simard, G, Omori, Y, Aylor, K, Baxter, EJ, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Henning, JW, Holder, GP, Hou, Z, Holzapfel, WL, Hrubes, JD, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Manzotti, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, Wu, WLK, Simard, G, Omori, Y, Aylor, K, Baxter, EJ, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Henning, JW, Holder, GP, Hou, Z, Holzapfel, WL, Hrubes, JD, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Manzotti, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, and Wu, WLK
Published: 2018

4. A Comparison of Maps and Power Spectra Determined from South Pole Telescope and Planck Data

Author: Hou, Z, Aylor, K, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, Follin, B, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Omori, Y, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, Hou, Z, Aylor, K, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, Follin, B, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Omori, Y, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, and Williamson, R
Published: 2018

5. Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

Author: Henning, JW, Sayre, JT, Reichardt, CL, Ade, PAR, Anderson, AJ, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Moran, CC, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, Yefremenko, V, Henning, JW, Sayre, JT, Reichardt, CL, Ade, PAR, Anderson, AJ, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Moran, CC, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V
Published: 2018

6. CMB Polarization B-mode Delensing with SPTpol and Herschel

Author: Manzotti, A, Story, KT, Wu, WLK, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Bock, JJ, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Conley, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dodelson, S, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, LM, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Vanderlinde, K, Vieira, JD, Viero, MP, Wang, G, Whitehorn, N, Yefremenko, V, Zemcov, M, Manzotti, A, Story, KT, Wu, WLK, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Bock, JJ, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Conley, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dodelson, S, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, LM, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Vanderlinde, K, Vieira, JD, Viero, MP, Wang, G, Whitehorn, N, Yefremenko, V, and Zemcov, M
Published: 2017

7. A Comparison of Cosmological Parameters Determined from CMB Temperature Power Spectra from the South Pole Telescope and the &ITPlanck&IT Satellite

Author: Aylor, K, Hou, Z, Knox, L, Story, KT, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hrubes, JD, Keisler, R, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Omori, Y, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Scaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, Williamson, R, Aylor, K, Hou, Z, Knox, L, Story, KT, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Chown, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hrubes, JD, Keisler, R, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Natoli, T, Omori, Y, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Scaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, and Williamson, R
Published: 2017

8. A 2500 deg(2) CMB Lensing Map from Combined South Pole Telescope and Planck Data

Author: Omori, Y, Chown, R, Simard, G, Story, KT, Aylor, K, Baxter, EJ, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Hou, Z, Holzapfel, WL, Hrubes, JD, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Manzotti, A, Marrone, DP, McMahon, JJ, Meyer, SS, Moeanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Omori, Y, Chown, R, Simard, G, Story, KT, Aylor, K, Baxter, EJ, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Hou, Z, Holzapfel, WL, Hrubes, JD, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Manzotti, A, Marrone, DP, McMahon, JJ, Meyer, SS, Moeanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Published: 2017

9. 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

10. MAPS OF THE MAGELLANIC CLOUDS FROM COMBINED SOUTH POLE TELESCOPE AND PLANCK DATA

Author: Crawford, TM, Chown, R, Holder, GP, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, George, EM, Halverson, NW, Harrington, NL, Holzapfel, WL, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Williamson, R, Crawford, TM, Chown, R, Holder, GP, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, George, EM, Halverson, NW, Harrington, NL, Holzapfel, WL, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, and Williamson, R
Published: 2016

11. MILLIMETER TRANSIENT POINT SOURCES IN THE SPTpol 100 SQUARE DEGREE SURVEY

Author: Whitehorn, N, Natoli, T, Ade, PAR, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, L, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Yefremenko, V, Whitehorn, N, Natoli, T, Ade, PAR, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, L, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, and Yefremenko, V
Published: 2016

12. 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

13. A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND GRAVITATIONAL LENSING POTENTIAL FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author: Story, KT, Hanson, D, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenk, V, Zahn, O, Story, KT, Hanson, D, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenk, V, and Zahn, O
Abstract: We present a measurement of the cosmic microwave background (CMB) gravitational lensing potential using data from the first two seasons of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope (SPT). The observations used in this work cover 100 deg$^2$ of sky with arcminute resolution at 150 GHz. Using a quadratic estimator, we make maps of the CMB lensing potential from combinations of CMB temperature and polarization maps. We combine these lensing potential maps to form a minimum-variance (MV) map. The lensing potential is measured with a signal-to-noise ratio of greater than one for angular multipoles between $100< L <250$. This is the highest signal-to-noise mass map made from the CMB to date and will be powerful in cross-correlation with other tracers of large-scale structure. We calculate the power spectrum of the lensing potential for each estimator, and we report the value of the MV power spectrum between $100< L <2000$ as our primary result. We constrain the ratio of the spectrum to a fiducial $\Lambda$CDM model to be $A_{\rm MV}=0.92 \pm 0.14 {\rm\, (Stat.)} \pm 0.08 {\rm\, (Sys.)}$. Restricting ourselves to polarized data only, we find $A_{\rm POL}=0.92 \pm 0.24 {\rm\, (Stat.)} \pm 0.11 {\rm\, (Sys.)}$. This measurement rejects the hypothesis of no lensing at $5.9 \sigma$ using polarization data alone, and at $14 \sigma$ using both temperature and polarization data.
Published: 2015

14. 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

15. 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

16. MEASUREMENTS OF SUB-DEGREE B-MODE POLARIZATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author: Keisler, R, Hoover, S, Harrington, N, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Leitch, EM, Li, D, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, Zahn, O, Keisler, R, Hoover, S, Harrington, N, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Leitch, EM, Li, D, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, and Zahn, O
Abstract: We present a measurement of the $B$-mode polarization power spectrum (the $BB$ spectrum) from 100 $\mathrm{deg}^2$ of sky observed with SPTpol, a polarization-sensitive receiver currently installed on the South Pole Telescope. The observations used in this work were taken during 2012 and early 2013 and include data in spectral bands centered at 95 and 150 GHz. We report the $BB$ spectrum in five bins in multipole space, spanning the range $300 \le \ell \le 2300$, and for three spectral combinations: 95 GHz $\times$ 95 GHz, 95 GHz $\times$ 150 GHz, and 150 GHz $\times$ 150 GHz. We subtract small ($< 0.5 \sigma$ in units of statistical uncertainty) biases from these spectra and account for the uncertainty in those biases. The resulting power spectra are inconsistent with zero power but consistent with predictions for the $BB$ spectrum arising from the gravitational lensing of $E$-mode polarization. If we assume no other source of $BB$ power besides lensed $B$ modes, we determine a preference for lensed $B$ modes of $4.9 \sigma$. After marginalizing over tensor power and foregrounds, namely polarized emission from galactic dust and extragalactic sources, this significance is $4.3 \sigma$. Fitting for a single parameter, $A_\mathrm{lens}$, that multiplies the predicted lensed $B$-mode spectrum, and marginalizing over tensor power and foregrounds, we find $A_\mathrm{lens} = 1.08 \pm 0.26$, indicating that our measured spectra are consistent with the signal expected from gravitational lensing. The data presented here provide the best measurement to date of the $B$-mode power spectrum on these angular scales.
Published: 2015

17. 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

18. A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY

Author: George, EM, Reichardt, CL, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, George, EM, Reichardt, CL, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, Halverson, NW, Harrington, NL, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Abstract: We present measurements of secondary cosmic microwave background (CMB) anisotropies and cosmic infrared background (CIB) fluctuations using data from the South Pole Telescope (SPT) covering the complete 2540 sq.deg. SPT-SZ survey area. Data in the three SPT-SZ frequency bands centered at 95, 150, and 220 GHz, are used to produce six angular power spectra (three single-frequency auto-spectra and three cross-spectra) covering the multipole range 2000 < ell < 11000 (angular scales 5' > \theta > 1'). These are the most precise measurements of the angular power spectra at ell > 2500 at these frequencies. The main contributors to the power spectra at these angular scales and frequencies are the primary CMB, CIB, thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ), and radio galaxies. We include a constraint on the tSZ power from a measurement of the tSZ bispectrum from 800 sq.deg. of the SPT-SZ survey. We measure the tSZ power at 143 GHz to be DtSZ = 4.08 +0.58 -0.67 \mu K^2 and the kSZ power to be DkSZ = 2.9 +- 1.3 \mu K^2. The data prefer positive kSZ power at 98.1% CL. We measure a correlation coefficient of \xi = 0.113 +0.057 -0.054 between sources of tSZ and CIB power, with \xi < 0 disfavored at a confidence level of 99.0%. The constraint on kSZ power can be interpreted as an upper limit on the duration of reionization. When the post-reionization homogeneous kSZ signal is accounted for, we find an upper limit on the duration \Delta z < 5.4 at 95% CL.
Published: 2015

19. MEASUREMENTS OF E-MODE POLARIZATION AND TEMPERATURE-E-MODE CORRELATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author: Crites, AT, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, De Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, Zahn, O, Crites, AT, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, De Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, and Zahn, O
Abstract: We present measurements of $E$-mode polarization and temperature-$E$-mode correlation in the cosmic microwave background (CMB) using data from the first season of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope (SPT). The observations used in this work cover 100~\sqdeg\ of sky with arcminute resolution at $150\,$GHz. We report the $E$-mode angular auto-power spectrum ($EE$) and the temperature-$E$-mode angular cross-power spectrum ($TE$) over the multipole range $500 < \ell \leq5000$. These power spectra improve on previous measurements in the high-$\ell$ (small-scale) regime. We fit the combination of the SPTpol power spectra, data from \planck\, and previous SPT measurements with a six-parameter \LCDM cosmological model. We find that the best-fit parameters are consistent with previous results. The improvement in high-$\ell$ sensitivity over previous measurements leads to a significant improvement in the limit on polarized point-source power: after masking sources brighter than 50\,mJy in unpolarized flux at 150\,GHz, we find a 95\% confidence upper limit on unclustered point-source power in the $EE$ spectrum of $D_\ell = \ell (\ell+1) C_\ell / 2 \pi < 0.40 \ \mu{\mbox{K}}^2$ at $\ell=3000$, indicating that future $EE$ measurements will not be limited by power from unclustered point sources in the multipole range $\ell < 3600$, and possibly much higher in $\ell.$
Published: 2015

20. 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

21. A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg(2) OF SOUTH POLE TELESCOPE DATA

Author: Crawford, TM, Schaffer, KK, Bhattacharya, S, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Crawford, TM, Schaffer, KK, Bhattacharya, S, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mocanu, LM, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Abstract: We present a measurement of the angular bispectrum of the millimeter-wave sky in observing bands centered at roughly 95, 150, and 220 GHz, on angular scales of $1^\prime \lesssim \theta \lesssim 10^\prime$ (multipole number $1000 \lesssim l \lesssim 10000$). At these frequencies and angular scales, the main contributions to the bispectrum are expected to be the thermal Sunyaev-Zel'dovich (tSZ) effect and emission from extragalactic sources, predominantly dusty, star-forming galaxies (DSFGs) and active galactic nuclei. We measure the bispectrum in 800 $\mathrm{deg}^2$ of three-band South Pole Telescope data, and we use a multi-frequency fitting procedure to separate the bispectrum of the tSZ effect from the extragalactic source contribution. We simultaneously detect the bispectrum of the tSZ effect at $>$10$\sigma$, the unclustered component of the extragalactic source bispectrum at $>$5$\sigma$ in each frequency band, and the bispectrum due to the clustering of DSFGs---i.e., the clustered cosmic infrared background (CIB) bispectrum---at $>$5$\sigma$. This is the first reported detection of the clustered CIB bispectrum. We use the measured tSZ bispectrum amplitude, compared to model predictions, to constrain the normalization of the matter power spectrum to be $\sigma_8 = 0.787 \pm 0.031$ and to predict the amplitude of the tSZ power spectrum at $l = 3000$. This prediction improves our ability to separate the thermal and kinematic contributions to the total SZ power spectrum. The addition of bispectrum data improves our constraint on the tSZ power spectrum amplitude by a factor of two compared to power spectrum measurements alone and demonstrates a preference for a nonzero kinematic SZ (kSZ) power spectrum, with a derived constraint on the kSZ amplitude at $l=3000$ of A_kSZ $ = 2.9 \pm 1.6 \ \mu$K$^2$, or A_kSZ $ = 2.6 \pm 1.8 \ \mu$K$^2$ if the default A_kSZ > 0 prior is removed.
Published: 2014

22. 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

23. 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

24. CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg(2) SPT-SZ SURVEY

Author: Hou, Z, Reichardt, CL, Story, KT, Follin, B, Keisler, R, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, De Haan, T, De Putter, R, Dobbs, MA, Dodelson, S, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Hou, Z, Reichardt, CL, Story, KT, Follin, B, Keisler, R, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, De Haan, T, De Putter, R, Dobbs, MA, Dodelson, S, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Published: 2014

25. 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

26. COSMOLOGICAL CONSTRAINTS FROM SUNYAEV-ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg(2) OF THE SOUTH POLE TELESCOPE SURVEY

Author: Benson, BA, de Haan, T, Dudley, JP, Reichardt, CL, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, N, 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, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Benson, BA, de Haan, T, Dudley, JP, Reichardt, CL, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, N, 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, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A
Abstract: We use measurements from the South Pole Telescope (SPT) Sunyaev Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg2 of the 2500 deg2 SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM. Assuming a spatially flat LCDM cosmological model, we find the SPT cluster sample constrain sigma_8 (Omega_m/0.25)^0.30 = 0.785 +- 0.037. In combination with measurements of the CMB power spectrum from the SPT and the seven-year WMAP data, the SPT cluster sample constrain sigma_8 = 0.795 +- 0.016 and Omega_m = 0.255 +- 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the LCDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (sum mnu), the effective number of relativistic species (Neff), and a primordial non-Gaussianity (fNL). We find that adding the SPT cluster data significantly improves the constraints on w and sum mnu beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w=-0.973 +- 0.063 and the sum of neutrino masses sum mnu < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. [abbrev.]
Published: 2013

27. GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY

Author: Reichardt, CL, Stalder, B, Bleem, LE, Montroy, TE, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, 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, 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, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Reichardt, CL, Stalder, B, Bleem, LE, Montroy, TE, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, 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, 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, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A
Abstract: We present a catalog of 224 galaxy cluster candidates, selected through their Sunyaev-Zel'dovich (SZ) effect signature in the first 720 deg2 of the South Pole Telescope (SPT) survey. This area was mapped with the SPT in the 2008 and 2009 austral winters to a depth of 18 uK-arcmin at 150 GHz; 550 deg2 of it was also mapped to 44 uK-arcmin at 95 GHz. Based on optical imaging of all candidates and near-infrared imaging of the majority of candidates, we have found optical and/or infrared counterparts for 158 clusters. Of these, 135 were first identified as clusters in SPT data, including 117 new discoveries reported in this work. This catalog triples the number of confirmed galaxy clusters discovered through the SZ effect. We report photometrically derived (and in some cases spectroscopic) redshifts for confirmed clusters and redshift lower limits for the remaining candidates. The catalog extends to high redshift with a median redshift of z = 0.55 and maximum redshift of z = 1.37. Based on simulations, we expect the catalog to be nearly 100% complete above M500 ~ 5e14 Msun h_{70}^-1 at z > 0.6. There are 121 candidates detected at signal-to-noise greater than five, at which the catalog purity is measured to be 95%. From this high-purity subsample, we exclude the z < 0.3 clusters and use the remaining 100 candidates to improve cosmological constraints following the method presented by Benson et al., 2011. Adding the cluster data to CMB+BAO+H0 data leads to a preference for non-zero neutrino masses while only slightly reducing the upper limit on the sum of neutrino masses to sum mnu < 0.38 eV (95% CL). For a spatially flat wCDM cosmological model, the addition of this catalog to the CMB+BAO+H0+SNe results yields sigma8=0.807+-0.027 and w = -1.010+-0.058, improving the constraints on these parameters by a factor of 1.4 and 1.3, respectively. [abbrev]
Published: 2013

28. IMPROVED CONSTRAINTS ON COSMIC MICROWAVE BACKGROUND SECONDARY ANISOTROPIES FROM THE COMPLETE 2008 SOUTH POLE TELESCOPE DATA

Author: Shirokoff, E, Reichardt, CL, Shaw, L, Millea, M, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Shirokoff, E, Reichardt, CL, Shaw, L, Millea, M, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Abstract: We report measurements of the cosmic microwave background (CMB) power spectrum from the complete 2008 South Pole Telescope (SPT) data set. We analyze twice as much data as the first SPT power spectrum analysis, using an improved cosmological parameter estimator which fits multi-frequency models to the SPT 150 and $220\,$GHz bandpowers. We find an excellent fit to the measured bandpowers with a model that includes lensed primary CMB anisotropy, secondary thermal (tSZ) and kinetic (kSZ) Sunyaev-Zel'dovich anisotropies, unclustered synchrotron point sources, and clustered dusty point sources. In addition to measuring the power spectrum of dusty galaxies at high signal-to-noise, the data primarily constrain a linear combination of the kSZ and tSZ anisotropy contributions at $150\,$GHz and $\ell=3000$: $D^{tSZ}_{3000} + 0.5\,D^{kSZ}_{3000} = 4.5\pm 1.0 \,\mu{\rm K}^2$. The 95% confidence upper limits on secondary anisotropy power are $D^{tSZ}_{3000} < 5.3\,\mu{\rm K}^2$ and $D^{kSZ}_{3000} < 6.5\,\mu{\rm K}^2$. We also consider the potential correlation of dusty and tSZ sources, and find it incapable of relaxing the tSZ upper limit. These results increase the significance of the lower than expected tSZ amplitude previously determined from SPT power spectrum measurements. We find that models including non-thermal pressure support in groups and clusters predict tSZ power in better agreement with the SPT data. Combining the tSZ power measurement with primary CMB data halves the statistical uncertainty on $\sigma_8$. However, the preferred value of $\sigma_8$ varies significantly between tSZ models. Improved constraints on cosmological parameters from tSZ power spectrum measurements require continued progress in the modeling of the tSZ power.
Published: 2011

29. X-RAY PROPERTIES OF THE FIRST SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE

Author: Andersson, K, Benson, BA, Ade, PAR, Aird, KA, Armstrong, B, Bautz, M, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, Garmire, G, George, EM, Gladders, MD, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Yang, Y, Zahn, O, Zenteno, A, Andersson, K, Benson, BA, Ade, PAR, Aird, KA, Armstrong, B, Bautz, M, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, Garmire, G, George, EM, Gladders, MD, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Yang, Y, Zahn, O, and Zenteno, A
Abstract: We present results of X-ray observations of a sample of 15 clusters selected via their imprint on the cosmic microwave background (CMB) from the thermal Sunyaev-Zel'dovich (SZ) effect. These clusters are a subset of the first SZ-selected cluster catalog, obtained from observations of 178 deg^2 of sky surveyed by the South Pole Telescope. Using X-ray observations with Chandra and XMM-Newton, we estimate the temperature, T_X, and mass, M_g, of the intracluster medium (ICM) within r_500 for each cluster. From these, we calculate Y_X=M_g T_X and estimate the total cluster mass using a M_500-Y_X scaling relation measured from previous X-ray studies. The integrated Comptonization, Y_SZ, is derived from the SZ measurements, using additional information from the X-ray measured gas density profiles and a universal temperature profile. We calculate scaling relations between the X-ray and SZ observables, and find results generally consistent with other measurements and the expectations from simple self-similar behavior. Specifically, we fit a Y_SZ-Y_X relation and find a normalization of 0.82 +- 0.07, marginally consistent with the predicted ratio of Y_SZ/Y_X=0.91+-0.01 that would be expected from the density and temperature models used in this work. Using the Y_X derived mass estimates, we fit a Y_SZ-M_500 relation and find a slope consistent with the self-similar expectation of Y_SZ ~ M^5/3 with a normalization consistent with predictions from other X-ray studies. We compare the X-ray mass estimates to previously published SZ mass estimates derived from cosmological simulations of the SPT survey. We find that the SZ mass estimates are lower by a factor of 0.89+-0.06, which is within the ~15% systematic uncertainty quoted for the simulation-based SZ masses.
Published: 2011

30. SOUTH POLE TELESCOPE DETECTIONS OF THE PREVIOUSLY UNCONFIRMED PLANCK EARLY SUNYAEV-ZEL'DOVICH CLUSTERS IN THE SOUTHERN HEMISPHERE

Author: Story, K, Aird, KA, Andersson, K, Armstrong, R, Bazin, G, Benson, BA, Bleem, LE, Bonamente, M, Brodwin, M, Carlstrom, JE, Chang, CL, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zenteno, A, Story, K, Aird, KA, Andersson, K, Armstrong, R, Bazin, G, Benson, BA, Bleem, LE, Bonamente, M, Brodwin, M, Carlstrom, JE, Chang, CL, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, and Zenteno, A
Abstract: We present South Pole Telescope (SPT) observations of the five galaxy cluster candidates in the southern hemisphere which were reported as unconfirmed in the Planck Early Sunyaev-Zel'dovich (ESZ) sample. One cluster candidate, PLCKESZ G255.62-46.16, is located in the 2500-square-degree SPT SZ survey region and was reported previously as SPT-CL J0411-4819. For the remaining four candidates, which are located outside of the SPT SZ survey region, we performed short, dedicated SPT observations. Each of these four candidates was strongly detected in maps made from these observations, with signal-to-noise ratios ranging from 6.3 to 13.8. We have observed these four candidates on the Magellan-Baade telescope and used these data to estimate cluster redshifts from the red sequence. Resulting redshifts range from 0.24 to 0.46. We report measurements of Y_0.75', the integrated Comptonization within a 0.75' radius, for all five candidates. We also report X-ray luminosities calculated from ROSAT All-Sky Survey catalog counts, as well as optical and improved SZ coordinates for each candidate. The combination of SPT SZ measurements, optical red-sequence measurements, and X-ray luminosity estimates demonstrates that these five Planck ESZ cluster candidates do indeed correspond to real galaxy clusters with redshifts and observable properties consistent with the rest of the ESZ sample.
Published: 2011

31. A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE

Author: Keisler, R, Reichardt, CL, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Joy, M, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mohr, JJ, Montroy, TE, Natoli, T, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Keisler, R, Reichardt, CL, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dudley, J, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Joy, M, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Millea, M, Mohr, JJ, Montroy, TE, Natoli, T, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, van Engelen, A, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Abstract: We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) using data from the South Pole Telescope (SPT). The data consist of 790 square degrees of sky observed at 150 GHz during 2008 and 2009. Here we present the power spectrum over the multipole range 650 < ell < 3000, where it is dominated by primary CMB anisotropy. We combine this power spectrum with the power spectra from the seven-year Wilkinson Microwave Anisotropy Probe (WMAP) data release to constrain cosmological models. We find that the SPT and WMAP data are consistent with each other and, when combined, are well fit by a spatially flat, LCDM cosmological model. The SPT+WMAP constraint on the spectral index of scalar fluctuations is ns = 0.9663 +/- 0.0112. We detect, at ~5-sigma significance, the effect of gravitational lensing on the CMB power spectrum, and find its amplitude to be consistent with the LCDM cosmological model. We explore a number of extensions beyond the LCDM model. Each extension is tested independently, although there are degeneracies between some of the extension parameters. We constrain the tensor-to-scalar ratio to be r < 0.21 (95% CL) and constrain the running of the scalar spectral index to be dns/dlnk = -0.024 +/- 0.013. We strongly detect the effects of primordial helium and neutrinos on the CMB; a model without helium is rejected at 7.7-sigma, while a model without neutrinos is rejected at 7.5-sigma. The primordial helium abundance is measured to be Yp = 0.296 +/- 0.030, and the effective number of relativistic species is measured to be Neff = 3.85 +/- 0.62. The constraints on these models are strengthened when the CMB data are combined with measurements of the Hubble constant and the baryon acoustic oscillation feature. Notable improvements include ns = 0.9668 +/- 0.0093, r < 0.17 (95% CL), and Neff = 3.86 +/- 0.42. The SPT+WMAP data show...
Published: 2011

32. OPTICAL REDSHIFT AND RICHNESS ESTIMATES FOR GALAXY CLUSTERS SELECTED WITH THE SUNYAEV-ZEL'DOVICH EFFECT FROM 2008 SOUTH POLE TELESCOPE OBSERVATIONS

Author: High, FW, Stalder, B, Song, J, Ade, PAR, Aird, KA, Allam, SS, Armstrong, R, Barkhouse, WA, Benson, BA, Bertin, E, Bhattacharya, S, Bleem, LE, Brodwin, M, Buckley-Geer, EJ, Carlstrom, JE, Challis, P, Chang, CL, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, M, Halverson, NW, Hamuy, M, Hansen, SM, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Lee, AT, Leitch, EM, Lin, H, Lin, Y-T, Loehr, A, Lueker, M, Marrone, D, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Morell, N, Ngeow, C-C, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Smith, RC, Spieler, HG, Staniszewski, Z, Stark, AA, Stubbs, CW, Tucker, DL, Vanderlinde, K, Vieira, JD, Williamson, R, Wood-Vasey, WM, Yang, Y, Zahn, O, Zenteno, A, High, FW, Stalder, B, Song, J, Ade, PAR, Aird, KA, Allam, SS, Armstrong, R, Barkhouse, WA, Benson, BA, Bertin, E, Bhattacharya, S, Bleem, LE, Brodwin, M, Buckley-Geer, EJ, Carlstrom, JE, Challis, P, Chang, CL, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, M, Halverson, NW, Hamuy, M, Hansen, SM, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Lee, AT, Leitch, EM, Lin, H, Lin, Y-T, Loehr, A, Lueker, M, Marrone, D, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Morell, N, Ngeow, C-C, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Smith, RC, Spieler, HG, Staniszewski, Z, Stark, AA, Stubbs, CW, Tucker, DL, Vanderlinde, K, Vieira, JD, Williamson, R, Wood-Vasey, WM, Yang, Y, Zahn, O, and Zenteno, A
Abstract: We present redshifts and optical richness properties of 21 galaxy clusters uniformly selected by their Sunyaev-Zel'dovich signature. These clusters, plus an additional, unconfirmed candidate, were detected in a 178 square-degree area surveyed by the South Pole Telescope in 2008. Using griz imaging from the Blanco Cosmology Survey and from pointed Magellan telescope observations, as well as spectroscopy using Magellan facilities, we confirm the existence of clustered red-sequence galaxies, report red-sequence photometric redshifts, present spectroscopic redshifts for a subsample, and derive R_200 radii and M_200 masses from optical richness. The clusters span redshifts from 0.15 to greater than 1, with a median redshift of 0.74; three clusters are estimated to be at z > 1. Redshifts inferred from mean red-sequence colors exhibit 2% RMS scatter in sigma_z/(1+z) with respect to the spectroscopic subsample for z < 1. We show that M_200 cluster masses derived from optical richness correlate with masses derived from South Pole Telescope data and agree with previously derived scaling relations to within the uncertainties. Optical and infrared imaging is an efficient means of cluster identification and redshift estimation in large Sunyaev-Zel'dovich surveys, and exploiting the same data for richness measurements, as we have done, will be useful for constraining cluster masses and radii for large samples in cosmological analysis.
Published: 2010

33. EXTRAGALACTIC MILLIMETER-WAVE SOURCES IN SOUTH POLE TELESCOPE SURVEY DATA: SOURCE COUNTS, CATALOG, AND STATISTICS FOR AN 87 SQUARE-DEGREE FIELD

Author: Vieira, JD, Crawford, TM, Switzer, ER, Ade, PAR, Aird, KA, Ashby, MLN, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, George, EM, Gladders, M, Hall, NR, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Marrone, DP, McIntyre, V, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Vanderlinde, K, Walsh, W, Williamson, R, Yang, Y, Zahn, O, Zenteno, A, Vieira, JD, Crawford, TM, Switzer, ER, Ade, PAR, Aird, KA, Ashby, MLN, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, H-M, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, George, EM, Gladders, M, Hall, NR, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Marrone, DP, McIntyre, V, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Vanderlinde, K, Walsh, W, Williamson, R, Yang, Y, Zahn, O, and Zenteno, A
Abstract: We report the results of an 87 square-degree point-source survey centered at R.A. 5h30m, decl. -55 deg. taken with the South Pole Telescope (SPT) at 1.4 and 2.0 mm wavelengths with arc-minute resolution and milli-Jansky depth. Based on the ratio of flux in the two bands, we separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei (AGN) and one consistent with thermal emission from dust. We present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800 mJy at 2.0 mm. The 2.0 mm counts are dominated by synchrotron-dominated sources across our reported flux range; the 1.4 mm counts are dominated by synchroton-dominated sources above ~15 mJy and by dust-dominated sources below that flux level. We detect 141 synchrotron-dominated sources and 47 dust-dominated sources at S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z << 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite (IRAS). However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs. We argue that these sources represent the rarest and brightest members of the population commonly referred to as sub-millimeter galaxies (SMGs). Because these sources are selected at longer wavelengths than in typical SMG surveys, they are expected to have a higher mean redshift distribution and may provide a new window on galaxy formation in the early universe.
Published: 2010

34. MEASUREMENTS OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH THE SOUTH POLE TELESCOPE

Author: Lueker, M, Reichardt, CL, Schaffer, KK, Zahn, O, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, George, EM, Hall, NR, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, Williamson, R, Lueker, M, Reichardt, CL, Schaffer, KK, Zahn, O, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, George, EM, Hall, NR, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, and Williamson, R
Abstract: We report cosmic microwave background (CMB) power spectrum measurements from the first 100 sq. deg. field observed by the South Pole Telescope (SPT) at 150 and 220 GHz. On angular scales where the primary CMB anisotropy is dominant, ell ~< 3000, the SPT power spectrum is consistent with the standard LambdaCDM cosmology. On smaller scales, we see strong evidence for a point source contribution, consistent with a population of dusty, star-forming galaxies. After we mask bright point sources, anisotropy power on angular scales of 3000 < ell < 9500 is detected with a signal-to-noise > 50 at both frequencies. We combine the 150 and 220 GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at 2.6 sigma. At ell=3000, the SZ power in the subtracted bandpowers is 4.2 +/- 1.5 uK^2, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. This discrepancy may suggest that contemporary galaxy cluster models overestimate the thermal pressure of intracluster gas. Alternatively, this result can be interpreted as evidence for lower values of sigma8. When combined with an estimate of the kinetic SZ contribution, the measured SZ amplitude shifts sigma8 from the primary CMB anisotropy derived constraint of 0.794 +/- 0.028 down to 0.773 +/- 0.025. The uncertainty in the constraint on sigma8 from this analysis is dominated by uncertainties in the theoretical modeling required to predict the amplitude of the SZ power spectrum for a given set of cosmological parameters.
Published: 2010

35. ANGULAR POWER SPECTRA OF THE MILLIMETER-WAVELENGTH BACKGROUND LIGHT FROM DUSTY STAR-FORMING GALAXIES WITH THE SOUTH POLE TELESCOPE

Author: Hall, NR, Keisler, R, Knox, L, Reichardt, CL, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, De Haan, T, Dobbs, MA, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Lee, AT, Leitch, EM, Lueker, M, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Switzer, ER, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Hall, NR, Keisler, R, Knox, L, Reichardt, CL, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, De Haan, T, Dobbs, MA, George, EM, Halverson, NW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Lee, AT, Leitch, EM, Lueker, M, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Ruhl, JE, Schaffer, KK, Shaw, L, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Switzer, ER, Vanderlinde, K, Vieira, JD, Williamson, R, and Zahn, O
Abstract: We use data from the first 100 square-degree field observed by the South Pole Telescope (SPT) in 2008 to measure the angular power spectrum of temperature anisotropies contributed by the background of dusty star-forming galaxies (DSFGs) at millimeter wavelengths. From the auto and cross-correlation of 150 and 220 GHz SPT maps, we significantly detect both Poisson distributed and, for the first time at millimeter wavelengths, clustered components of power from a background of DSFGs. The spectral indices between 150 and 220 GHz of the Poisson and clustered components are found to be 3.86 +- 0.23 and 3.8 +- 1.3 respectively, implying a steep scaling of the dust emissivity index beta ~ 2. The Poisson and clustered power detected in SPT, BLAST (at 600, 860, and 1200 GHz), and Spitzer (1900 GHz) data can be understood in the context of a simple model in which all galaxies have the same graybody spectrum with dust emissivity index of beta = 2 and dust temperature T_d = 34 K. In this model, half of the 150 GHz background light comes from redshifts greater than 3.2. We also use the SPT data to place an upper limit on the amplitude of the kinetic Sunyaev-Zel'dovich power spectrum at l = 3000 of 13 uK^2 at 95% confidence.
Published: 2010

36. GALAXY CLUSTERS SELECTED WITH THE SUNYAEV-ZEL'DOVICH EFFECT FROM 2008 SOUTH POLE TELESCOPE OBSERVATIONS

Author: Vanderlinde, K, Crawford, TM, de Haan, T, Dudley, JP, Shaw, L, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, George, EM, Gladders, MD, Hall, NR, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Loehr, A, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Ngeow, C-C, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, van Engelen, A, Vieira, JD, Williamson, R, Yang, Y, Zahn, O, Zenteno, A, Vanderlinde, K, Crawford, TM, de Haan, T, Dudley, JP, Shaw, L, Ade, PAR, Aird, KA, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, George, EM, Gladders, MD, Hall, NR, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Loehr, A, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Ngeow, C-C, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, van Engelen, A, Vieira, JD, Williamson, R, Yang, Y, Zahn, O, and Zenteno, A
Abstract: We present a detection-significance-limited catalog of 21 Sunyaev-Zel'dovich selected galaxy clusters. These clusters, along with 1 unconfirmed candidate, were identified in 178 deg^2 of sky surveyed in 2008 by the South Pole Telescope to a depth of 18 uK-arcmin at 150 GHz. Optical imaging from the Blanco Cosmology Survey (BCS) and Magellan telescopes provided photometric (and in some cases spectroscopic) redshift estimates, with catalog redshifts ranging from z=0.15 to z>1, with a median z = 0.74. Of the 21 confirmed galaxy clusters, three were previously identified as Abell clusters, three were presented as SPT discoveries in Staniszewski et al, 2009, and three were first identified in a recent analysis of BCS data by Menanteau et al, 2010; the remaining 12 clusters are presented for the first time in this work. Simulated observations of the SPT fields predict the sample to be nearly 100% complete above a mass threshold of M_200 ~ 5x10^14 M_sun/h at z = 0.6. This completeness threshold pushes to lower mass with increasing redshift, dropping to ~4x10^14 M_sun/h at z=1. The size and redshift distribution of this catalog are in good agreement with expectations based on our current understanding of galaxy clusters and cosmology. In combination with other cosmological probes, we use the cluster catalog to improve estimates of cosmological parameters. Assuming a standard spatially flat wCDM cosmological model, the addition of our catalog to the WMAP 7-year analysis yields sigma_8 = 0.81 +- 0.09 and w = -1.07 +- 0.29, a ~50% improvement in precision on both parameters over WMAP7 alone.
Published: 2010

37. CMB-S4

Author: Collaboration, The CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zonca, Andrea, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11), Apollo - University of Cambridge Repository, Van Swinderen Institute for Particle Physics and G, Cosmic Frontier, Abazajian, K, Addison, G, Adshead, P, Ahmed, Z, Akerib, D, Ali, A, Allen, S, Alonso, D, Alvarez, M, Amin, M, Anderson, A, Arnold, K, Ashton, P, Baccigalupi, C, Bard, D, Barkats, D, Barron, D, Barry, P, Bartlett, J, Basu Thakur, R, Battaglia, N, Bean, R, Bebek, C, Bender, A, Benson, B, Bianchini, F, Bischoff, C, Bleem, L, Bock, J, Bocquet, S, Boddy, K, Richard Bond, J, Borrill, J, Bouchet, F, Brinckmann, T, Brown, M, Bryan, S, Buza, V, Byrum, K, Hervias Caimapo, C, Calabrese, E, Calafut, V, Caldwell, R, Carlstrom, J, Carron, J, Cecil, T, Challinor, A, Chang, C, Chinone, Y, Sherry Cho, H, Cooray, A, Coulton, W, Crawford, T, Crites, A, Cukierman, A, Cyr-Racine, F, De Haan, T, Delabrouille, J, Devlin, M, Di Valentino, E, Dierickx, M, Dobbs, M, Duff, S, Dvorkin, C, Eimer, J, Elleflot, T, Errard, J, Essinger-Hileman, T, Fabbian, G, Feng, C, Ferraro, S, Filippini, J, Flauger, R, Flaugher, B, Fraisse, A, Frolov, A, Galitzki, N, Gallardo, P, Galli, S, Ganga, K, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Green, D, Grin, D, Grohs, E, Gualtieri, R, Gudmundsson, J, Gullett, I, Gupta, N, Habib, S, Halpern, M, Halverson, N, Hanany, S, Harrington, K, Hasegawa, M, Hasselfield, M, Hazumi, M, Heitmann, K, Henderson, S, Hensley, B, Hill, C, Colin Hill, J, Hlozek, R, Patty Ho, S, Hoang, T, Holder, G, Holzapfel, W, Hood, J, Hubmayr, J, Huffenberger, K, Hui, H, Irwin, K, Jeong, O, Johnson, B, Jones, W, Hwan Kang, J, Karkare, K, Katayama, N, Keskitalo, R, Kisner, T, Knox, L, Koopman, B, Kosowsky, A, Kovac, J, Kovetz, E, Kuhlmann, S, Kuo, C, Kusaka, A, Lahteenmaki, A, Lawrence, C, Lee, A, Lewis, A, Li, D, Linder, E, Loverde, M, Lowitz, A, Lubin, P, Madhavacheril, M, Mantz, A, Marques, G, Matsuda, F, Mauskopf, P, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Melin, J, Menanteau, F, Meyers, J, Millea, M, Mohr, J, Moncelsi, L, Monzani, M, Mroczkowski, T, Mukherjee, S, Nagy, J, Namikawa, T, Nati, F, Natoli, T, Newburgh, L, Niemack, M, Nishino, H, Nord, B, Novosad, V, O'Brient, R, Padin, S, Palladino, S, Partridge, B, Petravick, D, Pierpaoli, E, Pogosian, L, Prabhu, K, Pryke, C, Puglisi, G, Racine, B, Rahlin, A, Sathyanarayana Rao, M, Raveri, M, Reichardt, C, Remazeilles, M, Rocha, G, Roe, N, Roy, A, Ruhl, J, Salatino, M, Saliwanchik, B, Schaan, E, Schillaci, A, Schmitt, B, Schmittfull, M, Scott, D, Sehgal, N, Shandera, S, Sherwin, B, Shirokoff, E, Simon, S, Slosar, A, Spergel, D, S, T, Staggs, S, Stark, A, Starkman, G, Stompor, R, Stoughton, C, Suzuki, A, Tajima, O, Teply, G, Thompson, K, Thorne, B, Timbie, P, Tomasi, M, Tristram, M, Tucker, G, Umilta, C, Van Engelen, A, Vavagiakis, E, Vieira, J, Vieregg, A, Wagoner, K, Wallisch, B, Wang, G, Watson, S, Westbrook, B, Whitehorn, N, Wollack, E, Kimmy Wu, W, Xu, Z, Eric Yang, H, Yasini, S, Yefremenko, V, Won Yoon, K, Young, E, Yu, C, Zonca, A, University of California Irvine, Johns Hopkins University, University of Illinois at Urbana-Champaign, SLAC National Accelerator Laboratory, University of California Berkeley, Stanford University, University of Oxford, Rice University, Fermi National Accelerator Laboratory, University of California San Diego, International School for Advanced Studies, Lawrence Berkeley National Laboratory, Harvard University, University of New Mexico, Argonne National Laboratory, Université Paris-Diderot, California Institute of Technology, Cornell University, University of Melbourne, University of Cincinnati, Ludwig Maximilian University of Munich, University of Toronto, UMR7095, Stony Brook University, University of Manchester, Arizona State University, Florida State University, Cardiff University, Dartmouth College, University of Geneva, University of Cambridge, The University of Tokyo, University of Groningen, University of Chicago, University of Pennsylvania, McGill University, National Institute of Standards and Technology, NASA Goddard Space Flight Center, University of Sussex, Princeton University, Simon Fraser University, National Institute for Nuclear Physics, Haverford College, Stockholm University, Case Western Reserve University, University of British Columbia, University of Colorado Boulder, University of Minnesota Twin Cities, University of Michigan, Ann Arbor, Simons Foundation, Columbia University, University of Virginia, University of California Davis, Yale University, University of Pittsburgh, Ben-Gurion University of the Negev, Department of Electronics and Nanoengineering, Jet Propulsion Laboratory, University of California Santa Barbara, Perimeter Institute for Theoretical Physics, Service d'Astrophysique CEA, European Southern Observatory, Washington University St. Louis, University of Milan - Bicocca, University of Southern California, Institute for Advanced Studies, Pennsylvania State University, Brookhaven National Laboratory, Kyoto University, University of Wisconsin-Madison, University of Milano, Université Paris-Saclay, Brown University, Syracuse University, University of California Los Angeles, Aalto-yliopisto, and Aalto University
Subjects: Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, CMB, Settore FIS/05, Space and Planetary Science, astro-ph.CO, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies and Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5��$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473
Published: 2022

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