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1,897 results on '"Moran, C. A."'

1. First Constraints on the Epoch of Reionization Using the non-Gaussianity of the Kinematic Sunyaev-Zel{'}dovich Effect from the South Pole Telescope and {\it Herschel}-SPIRE Observations

Author

Raghunathan, S., Ade, P. A. R., Anderson, A. J., Ansarinejad, B., Archipley, M., Austermann, J. E., Balkenhol, L., Beall, J. A., Benabed, K., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Bock, J., Bouchet, F. R., Bryant, L., Camphuis, E., Carlstrom, J. E., Cecil, T. W., Chang, C. L., Chaubal, P., Chiang, H. C., Chichura, P. M., Chou, T. -L., Citron, R., Coerver, A., Crawford, T. M., Crites, A. T., Cukierman, A., Daley, C., Dibert, K. R., Dobbs, M. A., Doussot, A., Dutcher, D., Everett, W., Feng, C., Ferguson, K. R., Fichman, K., Foster, A., Galli, S., Gallicchio, J., Gambrel, A. E., Gardner, R. W., Ge, F., George, E. M., Goeckner-Wald, N., Gualtieri, R., Guidi, F., Guns, S., Gupta, N., de Haan, T., Halverson, N. W., Hivon, E., Holder, G. P., Holzapfel, W. L., Hood, J. C., Hrubes, J. D., Hryciuk, A., Huang, N., Hubmayr, J., Irwin, K. D., Kéruzoré, F., Khalife, A. R., Knox, L., Korman, M., Kornoelje, K., Kuo, C. -L., Lee, A. T., Levy, K., Li, D., Lowitz, A. E., Lu, C., Maniyar, A., Martsen, E. S., McMahon, J. J., Menanteau, F., Millea, M., Montgomery, J., Moran, C. Corbett, Nakato, Y., Natoli, T., Nibarger, J. P., Noble, G. I., Novosad, V., Omori, Y., Padin, S., Pan, Z., Paschos, P., Patil, S., Phadke, K. A., Prabhu, K., Pryke, C., Quan, W., Rahimi, M., Rahlin, A., Reichardt, C. L., Rouble, M., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Schiappucci, E., Sievers, C., Smecher, G., Sobrin, J. A., Stark, A. A., Stephen, J., Suzuki, A., Tandoi, C., Thompson, K. L., Thorne, B., Trendafilova, C., Tucker, C., Umilta, C., Veach, T., Vieira, J. D., Viero, M. P., Wan, Y., Wang, G., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Young, M. R., Zebrowski, J. A., and Zemcov, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report results from an analysis aimed at detecting the trispectrum of the kinematic Sunyaev-Zel{'}dovich (kSZ) effect by combining data from the South Pole Telescope (SPT) and {\it Herschel}-SPIRE experiments over a 100 ${\rm deg}^{2}$ field. The SPT observations combine data from the previous and current surveys, namely SPTpol and SPT-3G, to achieve depths of 4.5, 3, and 16 $\mu {\rm K-arcmin}$ in bands centered at 95, 150, and 220 GHz. For SPIRE, we include data from the 600 and 857 GHz bands. We reconstruct the velocity-induced large-scale correlation of the small-scale kSZ signal with a quadratic estimator that uses two cosmic microwave background (CMB) temperature maps, constructed by optimally combining data from all the frequency bands. We reject the null hypothesis of a zero trispectrum at $10.3\sigma$ level. However, the measured trispectrum contains contributions from both the kSZ and other undesired components, such as CMB lensing and astrophysical foregrounds, with kSZ being sub-dominant. We use the \textsc{Agora} simulations to estimate the expected signal from CMB lensing and astrophysical foregrounds. After accounting for the contributions from CMB lensing and foreground signals, we do not detect an excess kSZ-only trispectrum and use this non-detection to set constraints on reionization. By applying a prior based on observations of the Gunn-Peterson trough, we obtain an upper limit on the duration of reionization of $\Delta z_{\rm re, 50} < 4.5$ (95\% C.L). We find these constraints are fairly robust to foregrounds assumptions. This trispectrum measurement is independent of, but consistent with, {\it Planck}'s optical depth measurement. This result is the first constraint on the epoch of reionization using the non-Gaussian nature of the kSZ signal., Comment: 15 pages, 5 figures (3 in main text and 2 in Appendix); Accepted for publication in PRL; Some texts have been moved to Appendix; Minor change in Fig. 2 to include nomalization; Data products and plotting scripts can be downloaded from https://github.com/sriniraghunathan/kSZ_4pt_SPT_SPIRE

Published
2024

2. SPT Clusters with DES and HST Weak Lensing. II. Cosmological Constraints from the Abundance of Massive Halos

Author

Bocquet, S., Grandis, S., Bleem, L. E., Klein, M., Mohr, J. J., Schrabback, T., Abbott, T. M. C., Ade, P. A. R., Aguena, M., Alarcon, A., Allam, S., Allen, S. W., Alves, O., Amon, A., Anderson, A. J., Annis, J., Ansarinejad, B., Austermann, J. E., Avila, S., Bacon, D., Bayliss, M., Beall, J. A., Bechtol, K., Becker, M. R., Bender, A. N., Benson, B. A., Bernstein, G. M., Bhargava, S., Bianchini, F., Brodwin, M., Brooks, D., Bryant, L., Campos, A., Canning, R. E. A., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C. L., Chang, C., Chaubal, P., Chen, R., Chiang, H. C., Choi, A., Chou, T-L., Citron, R., Moran, C. Corbett, Cordero, J., Costanzi, M., Crawford, T. M., Crites, A. T., da Costa, L. N., Pereira, M. E. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., de Haan, T., Diehl, H. T., Dobbs, M. A., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Everett, W., Ferrero, I., Ferté, A., Flores, A. M., Frieman, J., Gallicchio, J., García-Bellido, J., Gatti, M., George, E. M., Giannini, G., Gladders, M. D., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Halverson, N. W., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Huang, N., Hubmayr, J., Huff, E. M., Huterer, D., Irwin, K. D., James, D. J., Jarvis, M., Khullar, G., Kim, K., Knox, L., Kraft, R., Krause, E., Kuehn, K., Kuropatkin, N., Kéruzoré, F., Lahav, O., Lee, A. T., Leget, P. -F., Li, D., Lin, H., Lowitz, A., MacCrann, N., Mahler, G., Mantz, A., Marshall, J. L., McCullough, J., McDonald, M., McMahon, J. J., Mena-Fernández, J., Menanteau, F., Meyer, S. S., Miquel, R., Montgomery, J., Myles, J., Natoli, T., Navarro-Alsina, A., Nibarger, J. P., Noble, G. I., Novosad, V., Ogando, R. L. C., Omori, Y., Padin, S., Pandey, S., Paschos, P., Patil, S., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Pryke, C., Raveri, M., Reichardt, C. L., Roberson, J., Rollins, R. P., Romero, C., Roodman, A., Ruhl, J. E., Rykoff, E. S., Saliwanchik, B. R., Salvati, L., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Saro, A., Schaffer, K. K., Secco, L. F., Sevilla-Noarbe, I., Sharon, K., Sheldon, E., Shin, T., Sievers, C., Smecher, G., Smith, M., Somboonpanyakul, T., Sommer, M., Stalder, B., Stark, A. A., Stephen, J., Strazzullo, V., Suchyta, E., Tarle, G., To, C., Troxel, M. A., Tucker, C., Tutusaus, I., Varga, T. N., Veach, T., Vieira, J. D., Vikhlinin, A., von der Linden, A., Wang, G., Weaverdyck, N., Weller, J., Whitehorn, N., Wu, W. L. K., Yanny, B., Yefremenko, V., Yin, B., Young, M., Zebrowski, J. A., Zhang, Y., Zohren, H., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel'dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range $0.25-1.78$ over a total sky area of 5,200 deg$^2$. We use DES Year 3 weak-lensing data for 688 clusters with redshifts $z<0.95$ and HST weak-lensing data for 39 clusters with $0.6

Published
2024

3. Galaxy Clusters Discovered via the Thermal Sunyaev-Zel'dovich Effect in the 500-square-degree SPTpol Survey

Author

Bleem, L. E., Klein, M., Abbott, T. M. C., Ade, P. A. R., Aguena, M., Alves, O., Anderson, A. J., Andrade-Oliveira, F., Ansarinejad, B., Archipley, M., Ashby, M. L. N., Austermann, J. E., Bacon, D., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bocquet, S., Brooks, D., Burke, D. L., Calzadilla, M., Carlstrom, J. E., Rosell, A. Carnero, Carretero, J., Chang, C. L., Chaubal, P., Chiang, H. C., Chou, T-L., Citron, R., Moran, C. Corbett, Costanzi, M., Crawford, T. M., Crites, A. T., da Costa, L. N., de Haan, T., De Vicente, J., Desai, S., Dobbs, M. A., Doel, P., Everett, W., Ferrero, I., Flaugher, B., Floyd, B., Friedel, D., Frieman, J., Gallicchio, J., Garc'ia-Bellido, J., Gatti, M., George, E. M., Giannini, G., Grandis, S., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Halverson, N. W., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Mena-Fernández, J., James, D. J., Kéruzoré, F., Knox, L., Kuehn, K., Lahav, O., Lee, A. T., Lee, S., Li, D., Lowitz, A., Marshal, J. L., McDonald, M., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mohr, J. J., Montgomery, J., Myles, J., Natoli, T., Nibarger, J. P., Noble, G. I., Novosad, V., Ogando, R. L. C., Padin, S., Patil, S., Pereira, M. E. S., Pieres, A., Malag'on, A. A. Plazas, Pryke, C., Reichardt, C. L., Rodr'iguez-Monroy, M., Romer, A. K., Ruhl, J. E., Saliwanchik, B. R., Salvati, L., Sanchez, E., Saro, A., Schaffer, K. K., Schrabback, T., Sevilla-Noarbe, I., Sievers, C., Smecher, G., Smith, M., Somboonpanyakul, T., Stalder, B., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Tucker, C., Veach, T., Vieira, J. D., Vincenzi, M., Wang, G., Weller, J., Whitehorn, N., Wiseman, P., Wu, W. L. K., Yefremenko, V., Zebrowski, J. A., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present a catalog of 689 galaxy cluster candidates detected at significance $\xi>4$ via their thermal Sunyaev-Zel'dovich (SZ) effect signature in 95 and 150 GHz data from the 500-square-degree SPTpol survey. We use optical and infrared data from the Dark Energy Camera and the Wide-field Infrared Survey Explorer (WISE) and \spitzer \ satellites, to confirm 544 of these candidates as clusters with $\sim94\%$ purity. The sample has an approximately redshift-independent mass threshold at redshift $z>0.25$ and spans $1.5 \times 10^{14} < M_{500c} < 9.1 \times 10^{14}$ $M_\odot/h_{70}$ \ and $0.031$. We use external radio data from the Sydney University Molonglo Sky Survey (SUMSS) to estimate contamination to the SZ signal from synchrotron sources. The contamination reduces the recovered $\xi$ by a median value of 0.032, or $\sim0.8\%$ of the $\xi=4$ threshold value, and $\sim7\%$ of candidates have a predicted contamination greater than $\Delta \xi = 1$. With the exception of a small number of systems $(<1\%)$, an analysis of clusters detected in single-frequency 95 and 150 GHz data shows no significant contamination of the SZ signal by emission from dusty or synchrotron sources. This cluster sample will be a key component in upcoming astrophysical and cosmological analyses of clusters. The SPTpol millimeter-wave maps and associated data products used to produce this sample are available at https://pole.uchicago.edu/public/data/sptpol_500d_clusters/index.html, and the NASA LAMBDA website. An interactive sky server with the SPTpol maps and Dark Energy Survey data release 2 images is also available at NCSA https://skyviewer.ncsa.illinois.edu., Comment: Matches version accepted by OJA. 19 pages + references, 14 figures, cluster candidate table provided in Appendix. Data products available at https://pole.uchicago.edu/public/data/sptpol_500d_clusters/index.html and an interactive sky server at https://skyviewer.ncsa.illinois.edu

Published
2023
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4. Treatment of Obesity with Thyroid hormones in Europe. Data from the THESIS* Collaboration

Author

Galofré, J. C., Díez, J. J., Attanasio, R., Nagy, E. V., Negro, R., Papini, E., Perros, P., Žarković, M., Akarsu, E., Alevizaki, M., Ayvaz, G., Bednarczuk, T., Beleslin, B. N., Berta, E., Bodor, M., Borissova, A. M., Boyanov, M., Buffet, C., Burlacu, M. C., Dobnig, H., Fadeyev, V., Field, B. C. T., Fliers, E., Führer, D., Hakala, T., Jiskra, J., Kopp, P., Krebs, M., Kršek, M., Kužma, M., Lantz, M., Lazúrová, I., Leenhardt, L., Luchytskiy, V., Puga, F. M., McGowan, A., Metso, S., Moran, C., Morgunova, T., Niculescu, D. A., Perić, B., Planck, T., Poiana, C., Robenshtok, E., Rosselet, P. O., Ruchala, M., Riis, K. R., Shepelkevich, A., Tronko, M., Unuane, D., Vardarli, I., Visser, W. E., Vryonidou, M., Younes, Y. R., and Hegedüs, L.

Published
2024
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5. Pattern Recognition of Pupillary Reflex Dynamics to Isoluminescent RGB Chromatic Stimuli

Author

Belen-Luna, J. C., González-Morán, C. O., Lima-Gómez, V., Suaste-Gómez, E., Hartmanis, Juris, Founding Editor, van Leeuwen, Jan, Series Editor, Hutchison, David, Editorial Board Member, Kanade, Takeo, Editorial Board Member, Kittler, Josef, Editorial Board Member, Kleinberg, Jon M., Editorial Board Member, Kobsa, Alfred, Series Editor, Mattern, Friedemann, Editorial Board Member, Mitchell, John C., Editorial Board Member, Naor, Moni, Editorial Board Member, Nierstrasz, Oscar, Series Editor, Pandu Rangan, C., Editorial Board Member, Sudan, Madhu, Series Editor, Terzopoulos, Demetri, Editorial Board Member, Tygar, Doug, Editorial Board Member, Weikum, Gerhard, Series Editor, Vardi, Moshe Y, Series Editor, Goos, Gerhard, Founding Editor, Bertino, Elisa, Editorial Board Member, Gao, Wen, Editorial Board Member, Steffen, Bernhard, Editorial Board Member, Yung, Moti, Editorial Board Member, Woeginger, Gerhard, Editorial Board Member, Mezura-Montes, Efrén, editor, Acosta-Mesa, Héctor Gabriel, editor, Carrasco-Ochoa, Jesús Ariel, editor, Martínez-Trinidad, José Francisco, editor, and Olvera-López, José Arturo, editor

Published
2024
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6. Simultaneous Millimeter-wave, Gamma-ray, and Optical Monitoring of the Blazar PKS 2326-502 During a Flaring State

Author

Hood II, J. C., Simpson, A., McDaniel, A., Foster, A., Ade, P. A. R., Ajello, M., Anderson, A. J., Austermann, J. E., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Chou, T-L., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gupta, N., Halverson, N. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Madejski, G., Malkan, M., McMahon, J. J., Meyer, S. S., Montgomery, J., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Sievers, C., Smecher, G., Stark, A. A., Tucker, C., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Zebrowski, J. A., and Zhang, L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

Including millimeter-wave (mm-wave) data in multi-wavelength studies of the variability of active galactic nuclei (AGN) can provide insights into AGN physics that are not easily accessible at other wavelengths. We demonstrate in this work the potential of cosmic microwave background (CMB) telescopes to provide long-term, high-cadence mm-wave AGN monitoring over large fractions of sky. We report on a pilot study using data from the SPTpol instrument on the South Pole Telescope (SPT), which was designed to observe the CMB at arcminute and larger angular scales. Between 2013 and 2016, SPTpol was used primarily to observe a single 500 deg^2 field, covering the entire field several times per day with detectors sensitive to radiation in bands centered at 95 and 150 GHz. We use SPT 150 GHz observations to create AGN light curves, and we compare these mm-wave light curves to those at other wavelengths, in particular gamma-ray and optical. In this Letter, we focus on a single source, PKS 2326-502, which has extensive, day-timescale monitoring data in gamma-ray, optical, and now mm-wave between 2013 and 2016. We find PKS 2326-502 to be in a flaring state in the first two years of this monitoring, and we present a search for evidence of correlated variability between mm-wave, optical R band, and gamma-ray observations. This pilot study is paving the way for AGN monitoring with current and upcoming CMB experiments such as SPT-3G, Simons Observatory, and CMB-S4, including multi-wavelength studies with facilities such as VRO-LSST., Comment: 9 pages, 3 figures, accepted to Astrophysical Journal Letters

Published
2023
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7. Simultaneous Millimeter-wave, Gamma-Ray, and Optical Monitoring of the Blazar PKS 2326-502 during a Flaring State

Author

Hood, JC, Simpson, A, McDaniel, A, Foster, A, Ade, PAR, Ajello, M, Anderson, AJ, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Chou, T-L, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gupta, N, Halverson, NW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Madejski, G, Malkan, M, McMahon, JJ, Meyer, SS, Montgomery, J, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Tucker, C, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, Yefremenko, V, Zebrowski, JA, and Zhang, L

Subjects
Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

Abstract Including millimeter-wave data in multiwavelength studies of the variability of active galactic nuclei (AGN) can provide insights into AGN physics that are not easily accessible at other wavelengths. We demonstrate in this work the potential of cosmic microwave background (CMB) telescopes to provide long-term, high-cadence millimeter-wave AGN monitoring over large fractions of sky. We report on a pilot study using data from the SPTpol instrument on the South Pole Telescope (SPT), which was designed to observe the CMB at arcminute and larger angular scales. Between 2013 and 2016, SPTpol was used primarily to observe a single 500 deg2 field, covering the entire field several times per day with detectors sensitive to radiation in bands centered at 95 and 150 GHz. We use SPT 150 GHz observations to create AGN light curves, and we compare these millimeter-wave light curves to those at other wavelengths, in particular γ-ray and optical. In this Letter, we focus on a single source, PKS 2326-502, which has extensive, day-timescale monitoring data in gamma-ray, optical, and now millimeter-wave between 2013 and 2016. We find PKS 2326-502 to be in a flaring state in the first 2 yr of this monitoring, and we present a search for evidence of correlated variability between millimeter-wave, optical R-band, and γ-ray observations. This pilot study is paving the way for AGN monitoring with current and upcoming CMB experiments such as SPT-3G, Simons Observatory, and CMB-S4, including multiwavelength studies with facilities such as Vera C. Rubin Observatories Large Synoptic Survey Telescope.

Published
2023

8. Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope

Author

Chichura, P. M., Foster, A., Patel, C., Ossa-Jaen, N., Ade, P. A. R., Ahmed, Z., Anderson, A. J., Archipley, M., Austermann, J. E., Avva, J. S., Balkenhol, L., Barry, P. S., Thakur, R. Basu, Beall, J. A., Benabed, K., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Bouchet, F. R., Bryant, L., Byrum, K., Carlstrom, J. E., Carter, F. W., Cecil, T. W., Chang, C. L., Chaubal, P., Chen, G., Chiang, H. C., Cho, H. -M., Chou, T-L., Citron, R., Cliche, J. -F., Crawford, T. M., Crites, A. T., Cukierman, A., Daley, C. M., Denison, E. V., Dibert, K., Ding, J., Dobbs, M. A., Dutcher, D., Everett, W., Feng, C., Ferguson, K. R., Fu, J., Galli, S., Gallicchio, J., Gambrel, A. E., Gardner, R. W., George, E. M., Goeckner-Wald, N., Gualtieri, R., Guns, S., Gupta, N., Guyser, R., de Haan, T., Halverson, N. W., Harke-Hosemann, A. H., Harrington, N. L., Henning, J. W., Hilton, G. C., Hivon, E., Holder, G. P., Holzapfel, W. L., Hood, J. C., Howe, D., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Jeong, O. B., Jonas, M., Jones, A., Khaire, T. S., Knox, L., Kofman, A. M., Korman, M., Kubik, D. L., Kuhlmann, S., Kuo, C. -L., Lee, A. T., Leitch, E. M., Li, D., Lowitz, A., Lu, C., Marrone, D. P., McMahon, J. J., Meyer, S. S., Michalik, D., Millea, M., Mocanu, L. M., Montgomery, J., Moran, C. Corbett, Nadolski, A., Natoli, T., Nguyen, H., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Pan, Z., Paschos, P., Patil, S., Pearson, J., Phadke, K. A., Posada, C. M., Prabhu, K., Pryke, C., Quan, W., Rahlin, A., Reichardt, C. L., Riebel, D., Riedel, B., Rouble, M., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Schiappucci, E., Shirokoff, E., Sievers, C., Smecher, G., Sobrin, J. A., Springmann, A., Stark, A. A., Stephen, J., Story, K. T., Suzuki, A., Tandoi, C., Thompson, K. L., Thorne, B., Tucker, C., Umilta, C., Vale, L. R., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Yoon, K. W., and Young, M. R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two $\sim270$ deg$^2$ sky regions near the ecliptic plane, each observed with the SPTpol camera $\sim100$ times over one month. We subtract the mean of all maps of a given field, removing static sky signal, and then average the mean-subtracted maps at known asteroid locations. We detect three asteroids$\text{ -- }$(324) Bamberga, (13) Egeria, and (22) Kalliope$\text{ -- }$with signal-to-noise ratios (S/N) of 11.2, 10.4, and 6.1, respectively, at 2.0 mm (150 GHz); we also detect (324) Bamberga with S/N of 4.1 at 3.2 mm (95 GHz). We place constraints on these asteroids' effective emissivities, brightness temperatures, and light curve modulation amplitude. Our flux density measurements of (324) Bamberga and (13) Egeria roughly agree with predictions, while our measurements of (22) Kalliope suggest lower flux, corresponding to effective emissivities of $0.66 \pm 0.11$ at 2.0 mm and $<0.47$ at 3.2mm. We predict the asteroids detectable in other SPT datasets and find good agreement with detections of (772) Tanete and (1093) Freda in recent data from the SPT-3G camera, which has $\sim10 \times$ the mapping speed of SPTpol. This work is the first focused analysis of asteroids in data from CMB surveys, and it demonstrates we can repurpose historic and future datasets for asteroid studies. Future SPT measurements can help constrain the distribution of surface properties over a larger asteroid population., Comment: 21 pages, 9 figures

Published
2022
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9. Effect of Aerobic Exercise in Chinese Adult Individuals at Risk for Type 2 Diabetes Mellitus (T2DM) with Low Salivary Amylase Gene (AMY1) Copy Number Variation

Author

Zhang X, Moran C, Wang R, and Zhou Y

Subjects
salivary amylase gene, copy number variation, blood glucose, insulin, Specialties of internal medicine, RC581-951
Abstract

Xinming Zhang,1,&ast; Colin Moran,2,&ast; Ruiyuan Wang,3 Yue Zhou3 1School of Sport Science, Nantong University, Nantong City, Jiangsu Province, People’s Republic of China; 2School of Health Sciences and Sport, University of Stirling, Stirling, Scotland, The United Kingdom; 3School of Sport Science, Beijing Sport University, Beijing City, People’s Republic of China&ast;These authors contributed equally to this workCorrespondence: Xinming Zhang, Nantong University, No. 9 Seyuan Road, Nantong, Jiangsu Province, People’s Republic of China, Tel +86 15901080090, Email smile-carrie@hotmail.comPurpose: Type 2 Diabetes mellitus (T2DM) has become a life-threatening health problem around the world. Studies have confirmed that aerobic exercise can prevent the risk of T2DM. Furthermore, recent research showed that salivary amylase gene (AMY1) copy number variation (CNV) could be one of the genetic factors that increased the risk of T2DM. To provide more evidence on how AMY1 CNV and exercise is correlated with the risk of T2DM, we designed this study to show the differences in postprandial carbohydrate metabolism between people with different AMY1 copy numbers, and how aerobic exercise can influence this process.Participants and Methods: Sixteen participants without cardiovascular disease were chosen, 8 with AMY1 CNV≥ 6 (High CNV group, HCNV), and 8 with AMY1 CNV ≤ 2 (Low CNV group, LCNV). All participants were Chinese, Han nationality, 18 to 40 years old, with fasting blood glucose lower than 6.1 mmol/L and normal blood pressure levels. They were asked to visit the laboratory in fasting state and drink a cup of solution with 75 grams of edible carbohydrate (glucose or starch). After carbohydrate intake, blood samples were taken at certain times at rest or after aerobic exercise. Blood glucose levels were tested with a portable blood glucose monitor, and insulin levels were tested with the enzyme-linked immunosorbent assay (ELISA).Results: The LCNV group had significantly higher resting insulin levels and homeostatic model assessment of insulin resistance (HOMA-IR) than the HCNV group. Compared to the HCNV group, postprandial blood glucose levels and insulin levels were insensitive to starch intake in the LCNV group. However, this difference disappeared after aerobic exercise was added as an intervention.Conclusion: Lower AMY1 CNV could be associated with higher risk of T2DM and complex carbohydrate metabolism disorder, while aerobic exercise can reduce the risk by increasing the carbohydrate utilization rate.Keywords: salivary amylase gene, copy number variation, blood glucose, insulin

Published
2023

10. Impact of primary kidney disease on the effects of empagliflozin in patients with chronic kidney disease: secondary analyses of the EMPA-KIDNEY trial

Author

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11. Effects of empagliflozin on progression of chronic kidney disease: a prespecified secondary analysis from the empa-kidney trial

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Staplin, N, Haynes, R, Judge, PK, Wanner, C, Green, JB, Emberson, J, Preiss, D, Mayne, KJ, Ng, SYA, Sammons, E, Zhu, D, Hill, M, Stevens, W, Wallendszus, K, Brenner, S, Cheung, AK, Liu, ZH, Li, J, Hooi, LS, Liu, WJ, Kadowaki, T, Nangaku, M, Levin, A, Cherney, D, Maggioni, AP, Pontremoli, R, Deo, R, Goto, S, Rossello, X, Tuttle, KR, Steubl, D, Petrini, M, Seidi, S, Landray, MJ, Baigent, C, Herrington, WG, Abat, S, Abd Rahman, R, Abdul Cader, R, Abdul Hafidz, MI, Abdul Wahab, MZ, Abdullah, NK, Abdul-Samad, T, Abe, M, Abraham, N, Acheampong, S, Achiri, P, Acosta, JA, Adeleke, A, Adell, V, Adewuyi-Dalton, R, Adnan, N, Africano, A, Agharazii, M, Aguilar, F, Aguilera, A, Ahmad, M, Ahmad, MK, Ahmad, NA, Ahmad, NH, Ahmad, NI, Ahmad Miswan, N, Ahmad Rosdi, H, Ahmed, I, Ahmed, S, Aiello, J, Aitken, A, AitSadi, R, Aker, S, Akimoto, S, Akinfolarin, A, Akram, S, Alberici, F, Albert, C, Aldrich, L, Alegata, M, Alexander, L, Alfaress, S, Alhadj Ali, M, Ali, A, Alicic, R, Aliu, A, Almaraz, R, 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S, Mafham, M, Magee, J, Mah, DY, Mahabadi, V, Maiguma, M, Makita, Y, Makos, G, Manco, L, Mangiacapra, R, Manley, J, Mann, P, Mano, S, Marcotte, G, Maris, J, Mark, P, Markau, S, Markovic, M, Marshall, C, Martin, M, Martinez, C, Martinez, S, Martins, G, Maruyama, K, Maruyama, S, Marx, K, Maselli, A, Masengu, A, Maskill, A, Masumoto, S, Masutani, K, Matsumoto, M, Matsunaga, T, Matsuoka, N, Matsushita, M, Matthews, M, Matthias, S, Matvienko, E, Maurer, M, Maxwell, P, Mazlan, N, Mazlan, SA, Mbuyisa, A, McCafferty, K, McCarroll, F, McCarthy, T, McClary-Wright, C, McCray, K, McDermott, P, McDonald, C, McDougall, R, McHaffie, E, McIntosh, K, McKinley, T, McLaughlin, S, McLean, N, McNeil, L, Measor, A, Meek, J, Mehta, A, Mehta, R, Melandri, M, Mené, P, Meng, T, Menne, J, Merritt, K, Merscher, S, Meshykhi, C, Messa, P, Messinger, L, Miftari, N, Miller, R, Miller, Y, Miller-Hodges, E, Minatoguchi, M, Miners, M, Minutolo, R, Mita, T, Miura, Y, Miyaji, M, Miyamoto, S, Miyatsuka, T, Miyazaki, M, Miyazawa, I, Mizumachi, R, Mizuno, M, Moffat, S, Mohamad Nor, FS, Mohamad Zaini, SN, Mohamed Affandi, FA, Mohandas, C, Mohd, R, Mohd Fauzi, NA, Mohd Sharif, NH, Mohd Yusoff, Y, Moist, L, Moncada, A, Montasser, M, Moon, A, Moran, C, Morgan, N, Moriarty, J, Morig, G, Morinaga, H, Morino, K, Morisaki, T, Morishita, Y, Morlok, S, Morris, A, Morris, F, Mostafa, S, Mostefai, Y, Motegi, M, Motherwell, N, Motta, D, Mottl, A, Moys, R, Mozaffari, S, Muir, J, Mulhern, J, Mulligan, S, Munakata, Y, Murakami, C, Murakoshi, M, Murawska, A, Murphy, K, Murphy, L, Murray, S, Murtagh, H, Musa, MA, Mushahar, L, Mustafa, R, Mustafar, R, Muto, M, Nadar, E, Nagano, R, Nagasawa, T, Nagashima, E, Nagasu, H, Nagelberg, S, Nair, H, Nakagawa, Y, Nakahara, M, Nakamura, J, Nakamura, R, Nakamura, T, Nakaoka, M, Nakashima, E, Nakata, J, Nakata, M, Nakatani, S, Nakatsuka, A, Nakayama, Y, Nakhoul, G, Naverrete, G, Navivala, A, Nazeer, I, Negrea, L, Nethaji, C, Newman, E, Ng, TJ, Ngu, LLS, Nimbkar, T, Nishi, H, Nishi, M, Nishi, S, Nishida, Y, Nishiyama, A, Niu, J, Niu, P, Nobili, G, Nohara, N, Nojima, I, Nolan, J, Nosseir, H, Nozawa, M, Nunn, M, Nunokawa, S, Oda, M, Oe, M, Oe, Y, Ogane, K, Ogawa, W, Ogihara, T, Oguchi, G, Ohsugi, M, Oishi, K, Okada, Y, Okajyo, J, Okamoto, S, Okamura, K, Olufuwa, O, Oluyombo, R, Omata, A, Omori, Y, Ong, LM, Ong, YC, Onyema, J, Oomatia, A, Oommen, A, Oremus, R, Orimo, Y, Ortalda, V, Osaki, Y, Osawa, Y, Osmond Foster, J, O'Sullivan, A, Otani, T, Othman, N, Otomo, S, O'Toole, J, Owen, L, Ozawa, T, Padiyar, A, Page, N, Pajak, S, Paliege, A, Pandey, A, Pandey, R, Pariani, H, Park, J, Parrigon, M, Passauer, J, Patecki, M, Patel, M, Patel, R, Patel, T, Patel, Z, Paul, R, Paulsen, L, Pavone, L, Peixoto, A, Peji, J, Peng, BC, Peng, K, Pennino, L, Pereira, E, Perez, E, Pergola, P, Pesce, F, Pessolano, G, Petchey, W, Petr, EJ, Pfab, T, Phelan, P, Phillips, R, Phillips, T, Phipps, M, Piccinni, G, Pickett, T, Pickworth, S, Piemontese, M, Pinto, D, Piper, J, Plummer-Morgan, J, Poehler, D, Polese, L, Poma, V, Postal, A, Pötz, C, Power, A, Pradhan, N, Pradhan, R, Preiss, E, Preston, K, Prib, N, Price, L, Provenzano, C, Pugay, C, Pulido, R, Putz, F, Qiao, Y, Quartagno, R, Quashie-Akponeware, M, Rabara, R, Rabasa-Lhoret, R, Radhakrishnan, D, Radley, M, Raff, R, Raguwaran, S, Rahbari-Oskoui, F, Rahman, M, Rahmat, K, Ramadoss, S, Ramanaidu, S, Ramasamy, S, Ramli, R, Ramli, S, Ramsey, T, Rankin, A, Rashidi, A, Raymond, L, Razali, WAFA, Read, K, Reiner, H, Reisler, A, Reith, C, Renner, J, Rettenmaier, B, Richmond, L, Rijos, D, Rivera, R, Rivers, V, Robinson, H, Rocco, M, Rodriguez-Bachiller, I, Rodriquez, R, Roesch, C, Roesch, J, Rogers, J, Rohnstock, M, Rolfsmeier, S, Roman, M, Romo, A, Rosati, A, Rosenberg, S, Ross, T, Roura, M, Roussel, M, Rovner, S, Roy, S, Rucker, S, Rump, L, Ruocco, M, Ruse, S, Russo, F, Russo, M, Ryder, M, Sabarai, A, Saccà, C, Sachson, R, Sadler, E, Safiee, NS, Sahani, M, Saillant, A, Saini, J, Saito, C, Saito, S, Sakaguchi, K, Sakai, M, Salim, H, Salviani, C, Sampson, A, Samson, F, Sandercock, P, Sanguila, S, Santorelli, G, Santoro, D, Sarabu, N, Saram, T, Sardell, R, Sasajima, H, Sasaki, T, Satko, S, Sato, A, Sato, D, Sato, H, Sato, J, Sato, T, Sato, Y, Satoh, M, Sawada, K, Schanz, M, Scheidemantel, F, Schemmelmann, M, Schettler, E, Schettler, V, Schlieper, GR, Schmidt, C, Schmidt, G, Schmidt, U, Schmidt-Gurtler, H, Schmude, M, Schneider, A, Schneider, I, Schneider-Danwitz, C, Schomig, M, Schramm, T, Schreiber, A, Schricker, S, Schroppel, B, Schulte-Kemna, L, Schulz, E, Schumacher, B, Schuster, A, Schwab, A, Scolari, F, Scott, A, Seeger, W, Segal, M, Seifert, L, Seifert, M, Sekiya, M, Sellars, R, Seman, MR, Shah, S, Shainberg, L, Shanmuganathan, M, Shao, F, Sharma, K, Sharpe, C, Sheikh-Ali, M, Sheldon, J, Shenton, C, Shepherd, A, Shepperd, M, Sheridan, R, Sheriff, Z, Shibata, Y, Shigehara, T, Shikata, K, Shimamura, K, Shimano, H, Shimizu, Y, Shimoda, H, Shin, K, Shivashankar, G, Shojima, N, Silva, R, Sim, CSB, Simmons, K, Sinha, S, Sitter, T, Sivanandam, S, Skipper, M, Sloan, K, Sloan, L, Smith, R, Smyth, J, Sobande, T, Sobata, M, Somalanka, S, Song, X, Sonntag, F, Sood, B, Sor, SY, Soufer, J, Sparks, H, Spatoliatore, G, Spinola, T, Squyres, S, Srivastava, A, Stanfield, J, Staylor, K, Steele, A, Steen, O, Steffl, D, Stegbauer, J, Stellbrink, C, Stellbrink, E, Stevenson, A, Stewart-Ray, V, Stickley, J, Stoffler, D, Stratmann, B, Streitenberger, S, Strutz, F, Stubbs, J, Stumpf, J, Suazo, N, Suchinda, P, Suckling, R, Sudin, A, Sugamori, K, Sugawara, H, Sugawara, K, Sugimoto, D, Sugiyama, H, Sugiyama, T, Sullivan, M, Sumi, M, Suresh, N, Sutton, D, Suzuki, H, Suzuki, R, Suzuki, Y, Swanson, E, Swift, P, Syed, S, Szerlip, H, Taal, M, Taddeo, M, Tailor, C, Tajima, K, Takagi, M, Takahashi, K, Takahashi, M, Takahashi, T, Takahira, E, Takai, T, Takaoka, M, Takeoka, J, Takesada, A, Takezawa, M, Talbot, M, Taliercio, J, Talsania, T, Tamori, Y, Tamura, R, Tamura, Y, Tan, CHH, Tan, EZZ, Tanabe, A, Tanabe, K, Tanaka, A, Tanaka, N, Tang, S, Tang, Z, Tanigaki, K, Tarlac, M, Tatsuzawa, A, Tay, JF, Tay, LL, Taylor, J, Taylor, K, Te, A, Tenbusch, L, Teng, KS, Terakawa, A, Terry, J, Tham, ZD, Tholl, S, Thomas, G, Thong, KM, Tietjen, D, Timadjer, A, Tindall, H, Tipper, S, Tobin, K, Toda, N, Tokuyama, A, Tolibas, M, Tomita, A, Tomita, T, Tomlinson, J, Tonks, L, Topf, J, Topping, S, Torp, A, Torres, A, Totaro, F, Toth, P, Toyonaga, Y, Tripodi, F, Trivedi, K, Tropman, E, Tschope, D, Tse, J, Tsuji, K, Tsunekawa, S, Tsunoda, R, Tucky, B, Tufail, S, Tuffaha, A, Turan, E, Turner, H, Turner, J, Turner, M, Tye, YL, Tyler, A, Tyler, J, Uchi, H, Uchida, H, Uchida, T, Udagawa, T, Ueda, S, Ueda, Y, Ueki, K, Ugni, S, Ugwu, E, Umeno, R, Unekawa, C, Uozumi, K, Urquia, K, Valleteau, A, Valletta, C, van Erp, R, Vanhoy, C, Varad, V, Varma, R, Varughese, A, Vasquez, P, Vasseur, A, Veelken, R, Velagapudi, C, Verdel, K, Vettoretti, S, Vezzoli, G, Vielhauer, V, Viera, R, Vilar, E, Villaruel, S, Vinall, L, Vinathan, J, Visnjic, M, Voigt, E, von-Eynatten, M, Vourvou, M, Wada, J, Wada, T, Wada, Y, Wakayama, K, Wakita, Y, Walters, T, Wan Mohamad, WH, Wang, L, Wang, W, Wang, X, Wang, Y, Wanninayake, S, Watada, H, Watanabe, K, Watanabe, M, Waterfall, H, Watkins, D, Watson, S, Weaving, L, Weber, B, Webley, Y, Webster, A, Webster, M, Weetman, M, Wei, W, Weihprecht, H, Weiland, L, Weinmann-Menke, J, Weinreich, T, Wendt, R, Weng, Y, Whalen, M, Whalley, G, Wheatley, R, Wheeler, A, Wheeler, J, Whelton, P, White, K, Whitmore, B, Whittaker, S, Wiebel, J, Wiley, J, Wilkinson, L, Willett, M, Williams, A, Williams, E, Williams, K, Williams, T, Wilson, A, Wilson, P, Wincott, L, Wines, E, Winkelmann, B, Winkler, M, Winter-Goodwin, B, Witczak, J, Wittes, J, Wittmann, M, Wolf, G, Wolf, L, Wolfling, R, Wong, C, Wong, E, Wong, HS, Wong, LW, Wong, YH, Wonnacott, A, Wood, A, Wood, L, Woodhouse, H, Wooding, N, Woodman, A, Wren, K, Wu, J, Wu, P, Xia, S, Xiao, H, Xiao, X, Xie, Y, Xu, C, Xu, Y, Xue, H, Yahaya, H, Yalamanchili, H, Yamada, A, Yamada, N, Yamagata, K, Yamaguchi, M, Yamaji, Y, Yamamoto, A, Yamamoto, S, Yamamoto, T, Yamanaka, A, Yamano, T, Yamanouchi, Y, Yamasaki, N, Yamasaki, Y, Yamashita, C, Yamauchi, T, Yan, Q, Yanagisawa, E, Yang, F, Yang, L, Yano, S, Yao, S, Yao, Y, Yarlagadda, S, Yasuda, Y, Yiu, V, Yokoyama, T, Yoshida, S, Yoshidome, E, Yoshikawa, H, Young, A, Young, T, Yousif, V, Yu, H, Yu, Y, Yuasa, K, Yusof, N, Zalunardo, N, Zander, B, Zani, R, Zappulo, F, Zayed, M, Zemann, B, Zettergren, P, Zhang, H, Zhang, L, Zhang, N, Zhang, X, Zhao, J, Zhao, L, Zhao, S, Zhao, Z, Zhong, H, Zhou, N, Zhou, S, Zhu, L, Zhu, S, Zietz, M, Zippo, M, Zirino, F, and Zulkipli, FH

Published
2024
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12. Optimal Cosmic Microwave Background Lensing Reconstruction and Parameter Estimation with SPTpol Data

Author

Millea, M, Daley, CM, Chou, T-L, Anderes, E, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Goeckner-Wald, N, Guns, S, Gupta, N, Halverson, NW, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Thorne, B, Tucker, C, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We perform the first simultaneous Bayesian parameter inference and optimal reconstruction of the gravitational lensing of the cosmic microwave background (CMB), using 100 deg2 of polarization observations from the SPTpol receiver on the South Pole Telescope. These data reach noise levels as low as 5.8 µK arcmin in polarization, which are low enough that the typically used quadratic estimator (QE) technique for analyzing CMB lensing is significantly suboptimal. Conversely, the Bayesian procedure extracts all lensing information from the data and is optimal at any noise level. We infer the amplitude of the gravitational lensing potential to be A f =0.949\,\pm \,0.122 using the Bayesian pipeline, consistent with our QE pipeline result, but with 17% smaller error bars. The Bayesian analysis also provides a simple way to account for systematic uncertainties, performing a similar job as frequentist "bias hardening"or linear bias correction, and reducing the systematic uncertainty on A f due to polarization calibration from almost half of the statistical error to effectively zero. Finally, we jointly constrain A f along with A L, the amplitude of lensing-like effects on the CMB power spectra, demonstrating that the Bayesian method can be used to easily infer parameters both from an optimal lensing reconstruction and from the delensed CMB, while exactly accounting for the correlation between the two. These results demonstrate the feasibility of the Bayesian approach on real data, and pave the way for future analysis of deep CMB polarization measurements with SPT-3G, Simons Observatory, and CMB-S4, where improvements relative to the QE can reach 1.5 times tighter constraints on A f and seven times lower effective lensing reconstruction noise.

Published
2021

13. Optimal CMB Lensing Reconstruction and Parameter Estimation with SPTpol Data

Author

Millea, M., Daley, C. M., Chou, T-L., Anderes, E., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Goeckner-Wald, N., Guns, S., Gupta, N., Halverson, N. W., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., McMahon, J. J., Meyer, S. S., Mocanu, L. M., Montgomery, J., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Sievers, C., Smecher, G., Stark, A. A., Thorne, B., Tucker, C., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform the first simultaneous Bayesian parameter inference and optimal reconstruction of the gravitational lensing of the cosmic microwave background (CMB), using 100 deg$^2$ of polarization observations from the SPTpol receiver on the South Pole Telescope. These data reach noise levels as low as 5.8 $\mu$K-arcmin in polarization, which are low enough that the typically used quadratic estimator (QE) technique for analyzing CMB lensing is significantly sub-optimal. Conversely, the Bayesian procedure extracts all lensing information from the data and is optimal at any noise level. We infer the amplitude of the gravitational lensing potential to be $A_\phi\,{=}\,0.949\,{\pm}\,0.122$ using the Bayesian pipeline, consistent with our QE pipeline result, but with 17\% smaller error bars. The Bayesian analysis also provides a simple way to account for systematic uncertainties, performing a similar job as frequentist "bias hardening," and reducing the systematic uncertainty on $A_\phi$ due to polarization calibration from almost half of the statistical error to effectively zero. Finally, we jointly constrain $A_\phi$ along with $A_{\rm L}$, the amplitude of lensing-like effects on the CMB power spectra, demonstrating that the Bayesian method can be used to easily infer parameters both from an optimal lensing reconstruction and from the delensed CMB, while exactly accounting for the correlation between the two. These results demonstrate the feasibility of the Bayesian approach on real data, and pave the way for future analysis of deep CMB polarization measurements with SPT-3G, Simons Observatory, and CMB-S4, where improvements relative to the QE can reach 1.5 times tighter constraints on $A_\phi$ and 7 times lower effective lensing reconstruction noise., Comment: 27 pages, 14 figures, accompanying software package available at https://cosmicmar.com/CMBLensing.jl

Published
2020
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14. A Demonstration of Improved Constraints on Primordial Gravitational Waves with Delensing

Author

BICEP/Keck, Collaborations, SPTpol, Ade, P. A. R., Ahmed, Z., Amiri, M., Anderson, A. J., Austermann, J. E., Avva, J. S., Barkats, D., Thakur, R. Basu, Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bischoff, C. A., Bleem, L. E., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Carlstrom, J. E., Chang, C. L., Cheshire IV, J. R., Chiang, H. C., Chou, T-L., Citron, R., Connors, J., Moran, C. Corbett, Cornelison, J., Crawford, T. M., Crites, A. T., Crumrine, M., Cukierman, A., de Haan, T., Dierickx, M., Dobbs, M. A., Duband, L., Everett, W., Fatigoni, S., Filippini, J. P., Fliescher, S., Gallicchio, J., George, E. M., Germaine, T. St., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Gupta, N., Hall, G., Halpern, M., Halverson, N. W., Harrison, S., Henderson, S., Henning, J. W., Hildebrandt, S. R., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Knox, L., Kovac, J. M., Kuo, C. L., Lau, K., Lee, A. T., Leitch, E. M., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Megerian, K. G., Meyer, S. S., Millea, M., Mocanu, L. M., Moncelsi, L., Montgomery, J., Nadolski, A., Namikawa, T., Natoli, T., Netterfield, C. B., Nguyen, H. T., Nibarger, J. P., Noble, G., Novosad, V., O'Brient, R., Ogburn IV, R. W., Omori, Y., Padin, S., Palladino, S., Patil, S., Prouve, T., Pryke, C., Racine, B., Reichardt, C. L., Reintsema, C. D., Richter, S., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Sievers, C., Smecher, G., Soliman, A., Stark, A. A., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umiltà, C., Veach, T., Vieira, J. D., Vieregg, A. G., Wandui, A., Wang, G., Weber, A. C., Whitehorn, N., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yefremenko, V., Yoon, K. W., Young, E., Yu, C., Zeng, L., and Zhang, C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck data set collected through 2014 using the same parametric foreground modelling as in the previous analysis. From simulations, we find that the uncertainty on $r$ is reduced by $\sim10\%$, from $\sigma(r)$= 0.024 to 0.022, which can be compared with a $\sim26\%$ reduction obtained when using a perfect lensing template. Applying the technique to the real data, the constraint on $r$ is improved from $r_{0.05} < 0.090$ to $r_{0.05} < 0.082$ (95\% C.L.). This is the first demonstration of improvement in an $r$ constraint through delensing., Comment: 23 pages, 11 figures; match published version

Published
2020
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15. Searching for Anisotropic Cosmic Birefringence with Polarization Data from SPTpol

Author

Bianchini, F., Wu, W. L. K., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Balkenhol, L., Baxter, E., Beall, J. A., Bender, A. N., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Chou, T. L., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Meyer, S. S., Millea, M., Mocanu, L. M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Sievers, C., Simard, G., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

We present a search for anisotropic cosmic birefringence in 500 deg$^2$ of southern sky observed at 150 GHz with the SPTpol camera on the South Pole Telescope. We reconstruct a map of cosmic polarization rotation anisotropies using higher-order correlations between the observed cosmic microwave background (CMB) $E$ and $B$ fields. We then measure the angular power spectrum of this map, which is found to be consistent with zero. The non-detection is translated into an upper limit on the amplitude of the scale-invariant cosmic rotation power spectrum, $L(L+1)C_L^{\alpha\alpha}/2\pi < 0.10 \times 10^{-4}$ rad$^2$ (0.033 deg$^2$, 95% C.L.). This upper limit can be used to place constraints on the strength of primordial magnetic fields, $B_{1 \rm Mpc} < 17 {\rm nG} $ (95% C.L.), and on the coupling constant of the Chern-Simons electromagnetic term $g_{a\gamma} < 4.0 \times 10^{-2}/H_I $ (95% C.L.), where $H_I$ is the inflationary Hubble scale. For the first time, we also cross-correlate the CMB temperature fluctuations with the reconstructed rotation angle map, a signal expected to be non-vanishing in certain theoretical scenarios, and find no detectable signal. We perform a suite of systematics and consistency checks and find no evidence for contamination., Comment: 17 pages, 7 figures - new subsection on non-Gaussian foregrounds, conclusions unchanged - updated to match published version on PRD

Published
2020
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16. An Improved Measurement of the Secondary Cosmic Microwave Background Anisotropies from the SPT-SZ + SPTpol Surveys

Author

Reichardt, C. L., Patil, S., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Baxter, E., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Chou, T. L., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Luong-Van, D., McMahon, J. J., Mehl, J., Meyer, S. S., Millea, M., Mocanu, L. M., Mohr, J. J., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Pryke, C., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Shirokoff, E., Sievers, C., Smecher, G., Spieler, H. G., Staniszewski, Z., Stark, A. A., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Williamson, R., Wu, W. L. K., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report new measurements of millimeter-wave power spectra in the angular multipole range $2000 \le \ell \le 11,000$ (angular scales $5^\prime \gtrsim \theta \gtrsim 1^\prime$). By adding 95 and 150\,GHz data from the low-noise 500 deg$^2$ SPTpol survey to the SPT-SZ three-frequency 2540 deg$^2$ survey, we substantially reduce the uncertainties in these bands. These power spectra include contributions from the primary cosmic microwave background, cosmic infrared background, radio galaxies, and thermal and kinematic Sunyaev-Zel'dovich (SZ) effects. The data favor a thermal SZ (tSZ) power at 143\,GHz of $D^{\rm tSZ}_{3000} = 3.42 \pm 0.54~ \mu {\rm K}^2$ and a kinematic SZ (kSZ) power of $D^{\rm kSZ}_{3000} = 3.0 \pm 1.0~ \mu {\rm K}^2$. This is the first measurement of kSZ power at $\ge 3\,\sigma$. We study the implications of the measured kSZ power for the epoch of reionization, finding the duration of reionization to be $\Delta z_{re} = 1.0^{+1.6}_{-0.7}$ ($\Delta z_{re}< 4.1$ at 95% confidence), when combined with our previously published tSZ bispectrum measurement., Comment: Submitted to ApJ, 16 pages. (revised portions of the introduction and description of bandpower estimation)

Published
2020
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17. Constraints on Cosmological Parameters from the 500 deg$^2$ SPTpol Lensing Power Spectrum

Author

Bianchini, F., Wu, W. L. K., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Meyer, S. S., Millea, M., Mocanu, L. M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Sievers, C., Simard, G., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg$^2$ SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat $\Lambda$CDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO) as well as primary CMB spectra from Planck and SPTpol. The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analysed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the CMB lensing data alone provide a 4\% constraint on $\sigma_8\Omega_m^{0.25} = 0.0593 \pm 0.025$.. Jointly fitting with BAO data, we find $\sigma_8=0.779 \pm 0.023$, $\Omega_m = 0.368^{+0.032}_{-0.037}$, and $H_0 = 72.0^{+2.1}_{-2.5}\,\text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1} $, up to $2\,\sigma$ away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat $\Lambda$CDM model. The SPTpol lensing spectrum constrains the spatial curvature to be $\Omega_K = -0.0007 \pm 0.0025$ and the sum of the neutrino masses to be $\sum m_{\nu} < 0.23$ eV at 95\% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the $S/N$ of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement., Comment: 16 pages, 8 figures, 3 tables, updated to match the version published on ApJ

Published
2019
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18. Measurements of B-mode Polarization of the Cosmic Microwave Background from 500 Square Degrees of SPTpol Data

Author

Sayre, J. T., Reichardt, C. L., Henning, J. W., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Harrington, N., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., McMahon, J. J., Meyer, S. S., Mocanu, L. M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Padin, S., Patil, S., Pryke, C., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Sievers, C., Smecher, G., Stark, A. A., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report a B-mode power spectrum measurement from the cosmic microwave background (CMB) polarization anisotropy observations made using the SPTpol instrument on the South Pole Telescope. This work uses 500 deg$^2$ of SPTpol data, a five-fold increase over the last SPTpol B-mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: $52 < \ell < 2301$. Data from both 95 and 150 GHz are used, allowing for three cross-spectra: 95 GHz x 95 GHz, 95 GHz x 150 GHz, and 150 GHz x 150 GHz. B-mode power is detected at very high significance; we find $P(BB < 0) = 5.8 \times 10^{-71}$, corresponding to a $18.1 \sigma$ detection of power. An upper limit is set on the tensor-to-scalar ratio, $r < 0.44$ at 95% confidence (the expected $1 \sigma$ constraint on $r$ given the measurement uncertainties is 0.22). We find the measured B-mode power is consistent with the Planck best-fit $\Lambda$CDM model predictions. Scaling the predicted lensing B-mode power in this model by a factor Alens, the data prefer Alens = $1.17 \pm 0.13$. These data are currently the most precise measurements of B-mode power at $\ell > 320$., Comment: 16 pages, 4 figures, Submitted to PRD

Published
2019
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19. The SPTpol Extended Cluster Survey

Author

Bleem, L. E., Bocquet, S., Stalder, B., Gladders, M. D., Ade, P. A. R., Allen, S. W., Anderson, A. J., Annis, J., Ashby, M. L. N., Austermann, J. E., Avila, S., Avva, J. S., Bayliss, M., Beall, J. A., Bechtol, K., Bender, A. N., Benson, B. A., Bertin, E., Bianchini, F., Blake, C., Brodwin, M., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. Corbett, Costanzi, M., Crawford, T. M., Crites, A. T., da Costa, L. N., de Haan, T., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Eifler, T. F., Everett, W., Flaugher, B., Floyd, B., Frieman, J., Gallicchio, J., García-Bellido, J., George, E. M., Gerdes, D. W., Gilbert, A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., Halverson, N. W., Harrington, N., Henning, J. W., Heymans, C., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., James, D. J., Jeltema, T., Joudaki, S., Khullar, G., Klein, M., Knox, L., Kuropatkin, N., Lee, A. T., Li, D., Lidman, C., Lowitz, A., MacCrann, N., Mahler, G., Maia, M. A. G., Marshall, J. L., McDonald, M., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Padin, S., Palmese, A., Parkinson, D., Patil, S., Paz-Chinchón, F., Plazas, A. A., Pryke, C., Ramachandra, N. S., Reichardt, C. L., González, J. D. Remolina, Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Saliwanchik, B. R., Sanchez, E., Saro, A., Sayre, J. T., Schaffer, K. K., Schrabback, T., Serrano, S., Sharon, K., Sievers, C., Smecher, G., Smith, M., Soares-Santos, M., Stark, A. A., Story, K. T., Suchyta, E., Tarle, G., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Weller, J., Whitehorn, N., Wu, W. L. K., Yefremenko, V., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the observations and resultant galaxy cluster catalog from the 2770 deg$^2$ SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect, and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete followup we have confirmed as clusters 244 of 266 candidates at a detection significance $\xi \ge 5$ and an additional 204 systems at $4<\xi<5$. The confirmed sample has a median mass of $M_{500c} \sim {4.4 \times 10^{14} M_\odot h_{70}^{-1}}$, a median redshift of $z=0.49$, and we have identified 44 strong gravitational lenses in the sample thus far. Radio data are used to characterize contamination to the SZ signal; the median contamination for confirmed clusters is predicted to be $\sim$1% of the SZ signal at the $\xi>4$ threshold, and $<4\%$ of clusters have a predicted contamination $>10\% $ of their measured SZ flux. We associate SZ-selected clusters, from both SPT-ECS and the SPT-SZ survey, with clusters from the DES redMaPPer sample, and find an offset distribution between the SZ center and central galaxy in general agreement with previous work, though with a larger fraction of clusters with significant offsets. Adopting a fixed Planck-like cosmology, we measure the optical richness-to-SZ-mass ($\lambda-M$) relation and find it to be 28% shallower than that from a weak-lensing analysis of the DES data---a difference significant at the 4 $\sigma$ level---with the relations intersecting at $\lambda=60$ . The SPT-ECS cluster sample will be particularly useful for studying the evolution of massive clusters and, in combination with DES lensing observations and the SPT-SZ cluster sample, will be an important component of future cosmological analyses., Comment: 49 pages, 14 figures, 10 tables. Minor changes to match accepted version in ApJS

Published
2019
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22. Galaxy Clusters Selected via the Sunyaev-Zel'dovich Effect in the SPTpol 100-Square-Degree Survey

Author

Huang, N., Bleem, L. E., Stalder, B., Ade, P. A. R., Allen, S. W., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bocquet, S., Brodwin, M., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Floyd, B., Gallicchio, J., George, E. M., Gilbert, A., Gladders, M. D., Guns, S., Gupta, N., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Hubmayr, J., Irwin, K. D., Khullar, G., Knox, L., Lee, A. T., Li, D., Lowitz, A., McDonald, M., McMahon, J. J., Meyer, S. S., Mocanu, L. M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Saro, A., Sayre, J. T., Schaffer, K. K., Sharon, K., Sievers, C., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev-Zel'dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional 2 galaxy clusters are confirmed using the overdensity of near-infrared galaxies only, and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift of $z \geq 1.0$, with a maximum confirmed redshift of $z_{\rm{max}} = 1.38 \pm 0.10$. We expect this catalog to contain every galaxy cluster with $M_{500c} > 2.6 \times 10^{14} M_\odot h^{-1}_{70}$ and $z > 0.25$ in the survey area. The mass threshold is approximately constant above $z = 0.25$, and the complete catalog has a median mass of approximately $ M_{500c} = 2.7 \times 10^{14} M_\odot h^{-1}_{70}$. Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 $\mu$K-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass., Comment: 21 pages, 7 figures, associated data available at http://pole.uchicago.edu/public/data/sptsz-clusters. V2 was accepted to the AJ, and includes minor changes requested by the reviewer

Published
2019
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23. A Detection of CMB-Cluster Lensing using Polarization Data from SPTpol

Author

Raghunathan, S., Patil, S., Baxter, E., Benson, B. A., Bleem, L. E., Crawford, T. M., Holder, G. P., McClintock, T., Reichardt, C. L., Varga, T. N., Whitehorn, N., Ade, P. A. R., Allam, S., Anderson, A. J., Austermann, J. E., Avila, S., Avva, J. S., Bacon, D., Beall, J. A., Bender, A. N., Bianchini, F., Bocquet, S., Brooks, D., Burke, D. L., Carlstrom, J. E., Carretero, J., Castander, F. J., Chang, C. L., Chiang, H. C., Citron, R., Costanzi, M., Crites, A. T., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Doel, P., Everett, S., Evrard, A. E., Feng, C., Flaugher, B., Fosalba, P., Frieman, J., Gallicchio, J., García-Bellido, J., Gaztanaga, E., George, E. M., Giannantonio, T., Gilbert, A., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., de Haan, T., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Jeltema, T., Kind, M. Carrasco, Knox, L., Kuropatkin, N., Lahav, O., Lee, A. T., Li, D., Lima, M., Lowitz, A., Maia, M. A. G., Marshall, J. L., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Montgomery, J., Moran, C. Corbett, Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Rapetti, D., Romer, A. K., Roodman, A., Rosell, A. Carnero, Rozo, E., Ruhl, J. E., Rykoff, E. S., Saliwanchik, B. R., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sievers, C., Smecher, G., Smith, M., Soares-Santos, M., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, C., Vanderlinde, K., Veach, T., De Vicente, J., Vieira, J. D., Vikram, V., Wang, G., Wu, W. L. K., Yefremenko, V., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes $Q/U$ map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500 deg$^{2}$ survey at the locations of roughly 18,000 clusters with richness $\lambda \ge 10$ from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at $4.8\sigma$. The mean stacked mass of the selected sample is found to be $(1.43 \pm 0.4)\ \times 10^{14}\ {\rm M_{\odot}}$ which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements., Comment: 10 pages, 3 figures, 1 table; typos fixed; accepted for publication in PRL

Published
2019
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24. Fractional Polarisation of Extragalactic Sources in the 500-square-degree SPTpol Survey

Author

Gupta, N., Reichardt, C. L., Ade, P. A. R., Anderson, A. J., Archipley, M., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Feng, C., Gallicchio, J., George, E. M., Gilbert, A., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hou, Z., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Luong-Van, D., Marrone, D. P., Manzotti, A., McMahon, J. J., Meyer, S. S., Millea, M., Mocanu, L. M., Mohr, J. J., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G. I., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Shirokoff, E., Sievers, C., Smecher, G., Staniszewski, Z., Stark, A. A., Story, K. T., Switzer, E. R., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Williamson, R., Wu, W. L. K., Yefremenko, V., and Zhang, L.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the polarisation properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg$^2$ survey. We estimate the polarised power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarised power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarisation fraction $\langle p^2 \rangle= [8.9\pm1.1] \times 10^{-4}$ at 95 GHz and $[6.9\pm1.1] \times 10^{-4}$ at 150~GHz for the full sample. This is consistent with the values obtained for a sub-sample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of $\langle p^2 \rangle_{\rm 95}<16.9 \times 10^{-3}$ and $\langle p^2 \rangle_{\rm 150}<2.6 \times 10^{-3}$. We find no evidence that the polarisation fraction depends on the source flux or observing frequency. The 1-$\sigma$ upper limit on measured mean squared polarisation fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarisation power spectra out to at least $\ell\lesssim5700$ ($\ell\lesssim4700$) and $\ell\lesssim5300$ ($\ell\lesssim3600$), respectively at 95 (150) GHz., Comment: 10 pages, 5 figures

Published
2019
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25. A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg$^2$ of SPTpol Temperature and Polarization Data

Author

Wu, W. L. K., Mocanu, L. M., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hou, Z., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Meyer, S. S., Millea, M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G. I., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Sievers, C., Simard, G., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a measurement of the cosmic microwave background (CMB) lensing potential using 500 deg$^2$ of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles $L \lesssim 250$, using a quadratic estimator on a combination of CMB temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of $100< L < 2000$ from sets of temperature-only, polarization-only, and minimum-variance estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit $\Lambda$CDM model to the $\textit{Planck}$ 2015 TT+lowP+lensing dataset. For the minimum-variance estimator, we find $A_{\rm{MV}} = 0.944 \pm 0.058{\rm (Stat.)}\pm0.025{\rm (Sys.)}$; restricting to only polarization data, we find $A_{\rm{POL}} = 0.906 \pm 0.090 {\rm (Stat.)} \pm 0.040 {\rm (Sys.)}$. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1 $\sigma$), and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination., Comment: 18 pages, 8 figures; updated to match published version

Published
2019
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26. Measurements of B-mode polarization of the cosmic microwave background from 500 square degrees of SPTpol data

Author

Sayre, JT, Reichardt, CL, Henning, JW, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract

We report a B-mode power spectrum measurement from the cosmic microwave background (CMB) polarization anisotropy observations made using the SPTpol instrument on the South Pole Telescope. This work uses 500 deg2 of SPTpol data, a five-fold increase over the last SPTpol B-mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52< 320.

Published
2020

27. The SPTpol Extended Cluster Survey

Author

Bleem, LE, Bocquet, S, Stalder, B, Gladders, MD, Ade, PAR, Allen, SW, Anderson, AJ, Annis, J, Ashby, MLN, Austermann, JE, Avila, S, Avva, JS, Bayliss, M, Beall, JA, Bechtol, K, Bender, AN, Benson, BA, Bertin, E, Bianchini, F, Blake, C, Brodwin, M, Brooks, D, Buckley-Geer, E, Burke, DL, Carlstrom, JE, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Costanzi, M, Crawford, TM, Crites, AT, da Costa, LN, de Haan, T, De Vicente, J, Desai, S, Diehl, HT, Dietrich, JP, Dobbs, MA, Eifler, TF, Everett, W, Flaugher, B, Floyd, B, Frieman, J, Gallicchio, J, García-Bellido, J, George, EM, Gerdes, DW, Gilbert, A, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, N, Gutierrez, G, Halverson, NW, Harrington, N, Henning, JW, Heymans, C, Holder, GP, Hollowood, DL, Holzapfel, WL, Honscheid, K, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, James, DJ, Jeltema, T, Joudaki, S, Khullar, G, Klein, M, Knox, L, Kuropatkin, N, Lee, AT, Li, D, Lidman, C, Lowitz, A, MacCrann, N, Mahler, G, Maia, MAG, Marshall, JL, McDonald, M, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miquel, R, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Padin, S, and Palmese, A

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

We describe the observations and resultant galaxy cluster catalog from the 2770 deg2 SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance ξ ≥ 5 and an additional 204 systems at 4 < ξ < 5. The confirmed sample has a median mass of M500c ~ 4.4 ´ 1014 M☉ h70 -1 and a median redshift of z = 0.49, and we have identified 44 strong gravitational lenses in the sample thus far. Radio data are used to characterize contamination to the SZ signal; the median contamination for confirmed clusters is predicted to be ∼1% of the SZ signal at the ξ > 4 threshold, and 10% of their measured SZ flux. We associate SZ-selected clusters, from both SPT-ECS and the SPT-SZ survey, with clusters from the DES redMaPPer sample, and we find an offset distribution between the SZ center and central galaxy in general agreement with previous work, though with a larger fraction of clusters with significant offsets. Adopting a fixed Planck-like cosmology, we measure the optical richness-SZ mass (l - M) relation and find it to be 28% shallower than that from a weak-lensing analysis of the DES data-a difference significant at the 4σ level-with the relations intersecting at λ = 60. The SPT-ECS cluster sample will be particularly useful for studying the evolution of massive clusters and, in combination with DES lensing observations and the SPT-SZ cluster sample, will be an important component of future cosmological analyses.

Published
2020

28. Galaxy Clusters Selected via the Sunyaev–Zel’dovich Effect in the SPTpol 100-square-degree Survey

Author

Huang, N, Bleem, LE, Stalder, B, Ade, PAR, Allen, SW, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Floyd, B, Gallicchio, J, George, EM, Gilbert, A, Gladders, MD, Guns, S, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Hubmayr, J, Irwin, KD, Khullar, G, Knox, L, Lee, AT, Li, D, Lowitz, A, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Sharon, K, 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

Subjects
Space Sciences, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract

We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev-Zel'dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional two galaxy clusters are confirmed using the overdensity of near-infrared galaxies only and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift z ≥ 1.0, with a maximum confirmed redshift of zmax = 1.38 ± 0.10. We expect this catalog to contain every galaxy cluster with M500c = 2.6 ×1014M⊙ h70-1 and z > 0.25 in the survey area. The mass threshold is approximately constant above z = 0.25, and the complete catalog has a median mass of approximately M500c = 2.7 ×1014M⊙ h70-1. Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 μK-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass.

Published
2020

29. Constraints on Cosmological Parameters from the 500 deg2 SPTPOL Lensing Power Spectrum

Author

Bianchini, F, Wu, WLK, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Sievers, C, Simard, G, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, and Yefremenko, V

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol. The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on. Jointly fitting with BAO data, we find away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.

Published
2020

30. Fractional Polarisation of Extragalactic Sources in the 500-square-degree SPTpol Survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
Astronomical Sciences, Physical Sciences, polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈p2〉= [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

31. Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Corbett Moran, C, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈p2〉= [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

32. Detection of CMB-Cluster Lensing using Polarization Data from SPTpol

Author

Raghunathan, S, Patil, S, Baxter, E, Benson, BA, Bleem, LE, Crawford, TM, Holder, GP, McClintock, T, Reichardt, CL, Varga, TN, Whitehorn, N, Ade, PAR, Allam, S, Anderson, AJ, Austermann, JE, Avila, S, Avva, JS, Bacon, D, Beall, JA, Bender, AN, Bianchini, F, Bocquet, S, Brooks, D, Burke, DL, Carlstrom, JE, Carretero, J, Castander, FJ, Chang, CL, Chiang, HC, Citron, R, Costanzi, M, Crites, AT, da Costa, LN, Desai, S, Diehl, HT, Dietrich, JP, Dobbs, MA, Doel, P, Everett, S, Evrard, AE, Feng, C, Flaugher, B, Fosalba, P, Frieman, J, Gallicchio, J, García-Bellido, J, Gaztanaga, E, George, EM, Giannantonio, T, Gilbert, A, Gruendl, RA, Gschwend, J, Gupta, N, Gutierrez, G, de Haan, T, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Hollowood, DL, Holzapfel, WL, Honscheid, K, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Jeltema, T, Kind, M Carrasco, Knox, L, Kuropatkin, N, Lahav, O, Lee, AT, Li, D, Lima, M, Lowitz, A, Maia, MAG, Marshall, JL, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miquel, R, Mocanu, LM, Mohr, JJ, Montgomery, J, Moran, C Corbett, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Ogando, RLC, Padin, S, Plazas, AA, Pryke, C, Rapetti, D, Romer, AK, Roodman, A, Rosell, A Carnero, and Rozo, E

Subjects
Astronomical Sciences, Physical Sciences, SPTpol and DES Collaboration, astro-ph.CO, Mathematical Sciences, Engineering, General Physics, Mathematical sciences, Physical sciences
Abstract

We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes QU map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500  deg^{2} survey at the locations of roughly 18 000 clusters with richness λ≥10 from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at 4.8σ. The mean stacked mass of the selected sample is found to be (1.43±0.40)×10^{14}M_{⊙} which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements.

Published
2019

33. A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data

Author

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

Subjects
Particle and High Energy Physics, Physical Sciences, cosmology: cosmic background radiation, large-scale structure of the universe, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present a measurement of the cosmic microwave background lensing potential using 500 deg2 of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles L ≲ 250, using a quadratic estimator on a combination of cosmic microwave background temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of 100 < L < 2000 from sets of temperature-only (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

Published
2019

35. The effects of metallicity and cooling physics on fragmentation: implications on direct-collapse black hole formation

Author

Moran, C. Corbett, Grudić, M. Y., and Hopkins, P. F.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

A promising supermassive black hole seed formation channel is that of direct collapse from primordial gas clouds. We perform a suite of 3D hydrodynamics simulations of an isolated turbulent gas cloud to investigate conditions conducive to forming massive black hole seeds via direct collapse, probing the impact of cloud metallicity, gas temperature floor and cooling physics on cloud fragmentation. We find there is no threshold in metallicity which produces a sharp drop in fragmentation. When molecular cooling is not present, metallicity has little effect on fragmentation. When molecular cooling is present, fragmentation is suppressed by at most $\sim 25\%$, with the greatest suppression seen at metallicities below $2\%$ solar. A gas temperature floor $\sim 10^{4}$K produces the largest drop in fragmentation of any parameter choice, reducing fragmentation by $\sim 60\%$. At metallicities below $2\%$ solar or at temperatures $\sim 10^{3}$K we see a reduction in fragmentation $\sim 20-25 \%$. For a cloud of metallicity $2\%$ solar above and a temperature below $10^3$K, the detailed choices of temperature floor, metallicity, and cooling physics have little impact on fragmentation., Comment: 5 pages, 4 figures, submitted to MNRAS

Published
2018

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

Author

Henning, J. W., Sayre, J. T., Reichardt, C. L., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Beall, J. A., Bender, A. N., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Cho, H-M., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Halverson, N. W., Harrington, N., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hoover, S., Hou, Z., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Keisler, R., Knox, L., Lee, A. T., Leitch, E. M., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Meyer, S. S., Mocanu, L., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Novosad, V., Padin, S., Pryke, C., Ruhl, J. E., Saliwanchik, B. R., Schaffer, K. K., Sievers, C., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., and Yefremenko, V.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present measurements of the $E$-mode polarization angular auto-power spectrum ($EE$) and temperature-$E$-mode cross-power spectrum ($TE$) of the cosmic microwave background (CMB) using 150 GHz data from three seasons of SPTpol observations. We report the power spectra over the spherical harmonic multipole range $50 < \ell \leq 8000$, and detect nine acoustic peaks in the $EE$ spectrum with high signal-to-noise ratio. These measurements are the most sensitive to date of the $EE$ and $TE$ power spectra at $\ell > 1050$ and $\ell > 1475$, respectively. The observations cover 500 deg$^2$, a fivefold increase in area compared to previous SPTpol analyses, which increases our sensitivity to the photon diffusion damping tail of the CMB power spectra enabling tighter constraints on \LCDM model extensions. After masking all sources with unpolarized flux $>50$ mJy we place a 95% confidence upper limit on residual polarized point-source power of $D_\ell = \ell(\ell+1)C_\ell/2\pi <0.107\,\mu{\rm K}^2$ at $\ell=3000$, suggesting that the $EE$ damping tail dominates foregrounds to at least $\ell = 4050$ with modest source masking. We find that the SPTpol dataset is in mild tension with the $\Lambda CDM$ model ($2.1\,\sigma$), and different data splits prefer parameter values that differ at the $\sim 1\,\sigma$ level. When fitting SPTpol data at $\ell < 1000$ we find cosmological parameter constraints consistent with those for $Planck$ temperature. Including SPTpol data at $\ell > 1000$ results in a preference for a higher value of the expansion rate ($H_0 = 71.3 \pm 2.1\,\mbox{km}\,s^{-1}\mbox{Mpc}^{-1}$ ) and a lower value for present-day density fluctuations ($\sigma_8 = 0.77 \pm 0.02$)., Comment: Updated to match version accepted to ApJ. 34 pages, 17 figures, 6 tables

Published
2017
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37. 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, C Corbett, 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

Subjects
Astronomical Sciences, Physical Sciences, cosmic background radiation, cosmological parameters, cosmology: observations, polarization, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present measurements of the E-mode polarization angular auto-power spectrum (EE) and temperature-E-mode cross-power spectrum (TE) of the cosmic microwave background (CMB) using 150 GHz data from three seasons of SPTpol observations. We report the power spectra over the spherical harmonic multipole range 50 < ℓ ≤ 8000 and detect nine acoustic peaks in the EE spectrum with high signal-to-noise ratio. These measurements are the most sensitive to date of the EE and TE power spectra at ℓ > 1050 and ℓ > 1475, respectively. The observations cover 500 , a fivefold increase in area compared to previous SPTpol analyses, which increases our sensitivity to the photon diffusion damping tail of the CMB power spectra enabling tighter constraints on ΛCDM model extensions. After masking all sources with unpolarized flux mJy, we place a 95% confidence upper limit on residual polarized point-source power of at Dℓ = ℓ(ℓ+1)ℓℓ/2π < 0.107 μK2 at ℓ = 3000, suggesting that the EE damping tail dominates foregrounds to at least ℓ= 4050 with modest source masking. We find that the SPTpol data set is in mild tension with the ΛCDM model (2.1 δ), and different data splits prefer parameter values that differ at the ∼ 1 δ level. When fitting SPTpol data at ℓ < 1000, we find cosmological parameter constraints consistent with those for Planck temperature. Including SPTpol data at ℓ> 1000 results in a preference for a higher value of the expansion rate (H071.3 ± 2.1 Km s-1 Mpc-1) and a lower value for present-day density fluctuations (δ8 =0.77 ±0.02).

Published
2018

40. P615 Clinical efficacy of accelerated 4-weekly vs. Conventional 8-weekly ustekinumab dosing in Inflammatory Bowel Disease: A single centre experience

Author

Lloyd, A, primary, Quarry, S, additional, Sugrue, K, additional, Gleeson, S, additional, O'Sullivan, G, additional, O'Sullivan, C, additional, Forde, G, additional, Doyle, M, additional, Moran, C, additional, Mcdonald, C, additional, Sheehan, D, additional, Buckley, M, additional, Iacucci, M, additional, and McCarthy, J, additional

Published
2024
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41. Mindfulness-Based Interventions in Cancer Survivors: A Systematic Review of Participants’ Adherence to Home Practice

Author

Baydoun M, Moran C, McLennan A, Piedalue KAL, Oberoi D, and Carlson LE

Subjects
oncology, mindfulness, adherence, distress, complementary therapy, Medicine (General), R5-920
Abstract

Mohamad Baydoun,1 Chelsea Moran,2 Andrew McLennan,1 Katherine-Ann L Piedalue,1 Devesh Oberoi,1 Linda E Carlson1 1Cumming School of Medicine, Department of Psychosocial Oncology, University of Calgary, Calgary, Canada; 2Department of Psychology, University of Calgary, Calgary, CanadaCorrespondence: Linda E CarlsonDepartment of Psychosocial Oncology, Cancer Control Alberta – Holy Cross Site, 2202 2nd St. SW, Calgary, Alberta, CanadaT2S 3C1 Tel +1 403-355-3207Email l.carlson@ucalgary.caBackground: Although mindfulness-based interventions (MBIs) have demonstrated efficacy for alleviating psychological distress in cancer survivors, little is known about the extent to which participants adhere to assigned home practice. The purpose of this systematic review was to summarize and appraise the literature on rates and correlates of adherence to mindfulness home practice among cancer survivors.Methods: Four databases (PubMed, Psychology and Behavioral Sciences, PsycInfo, and CINAHL) were searched for studies published before October 15, 2020. Articles were included if they evaluated the benefits of an MBI program for adults with cancer.Results: Twenty-one studies (N=1811 participants) meeting the inclusion criteria were identified (randomized controlled trials (n=13), non-randomized controlled designs (n=2), single-group studies (n=6)). The pooled adherence rate for participants’ home practice was 60% of the assigned amount, which equated to 27 min per day during the intervention period. There was some evidence for a relationship between home practice of mindfulness techniques and improvements in mood, stress, anxiety, depression, and fear of cancer recurrence (correlation coefficients ranged from 0.33 to 0.67). Factors including marital status, mood disturbance at baseline, intervention modality, and personality traits were evaluated in relation to adherence to home practice, but the current literature was inadequate to evaluate whether a relationship exists.Conclusion: Adherence to mindfulness home practice among cancer survivors is suboptimal, and most of the correlates of adherence studied to date are non-modifiable. More research is warranted to scrutinize the role of home practice in mindfulness-based interventions, including assessment of modifiable factors influencing adherence to improve benefits for this population.Keywords: oncology, mindfulness, adherence, distress, complementary therapy

Published
2021

42. Globular Cluster Formation in the Virgo Cluster

Author

Moran, C. Corbett, Teyssier, R., and Lake, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Metal poor globular clusters (MPGCs) are a unique probe of the early universe, in particular the reionization era. Systems of globular clusters in galaxy clusters are particularly interesting as it is in the progenitors of galaxy clusters that the earliest reionizing sources first formed. Although the exact physical origin of globular clusters is still debated, it is generally admitted that globular clusters form in early, rare dark matter peaks (Moore et al. 2006; Boley et al. 2009). We provide a fully numerical analysis of the Virgo cluster globular cluster system by identifying the present day globular cluster system with exactly such early, rare dark matter peaks. A popular hypothesis is that that the observed truncation of blue metal poor globular cluster formation is due to reionization (Spitler et al. 2012; Boley et al. 2009; Brodie & Strader 2006); adopting this view, constraining the formation epoch of MPGCs provides a complementary constraint on the epoch of reionization. By analyzing both the line of sight velocity dispersion and the surface density distribution of the present day distribution we are able to constrain the redshift and mass of the dark matter peaks. We find and quantify a dependence on the chosen line of sight of these quantities, whose strength varies with redshift, and coupled with star formation efficiency arguments find a best fitting formation mass and redshift of $\simeq 5 \times 10^8 \rm{M}_\odot$ and $z\simeq 9$. We predict $\simeq 300$ intracluster MPGCs in the Virgo cluster. Our results confirm the techniques pioneered by Moore et al. (2006) when applied to the the Virgo cluster and extend and refine the analytic results of Spitler et al. (2012) numerically., Comment: 13 Pages, 13 Figures, submitted to MNRAS

Published
2014
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43. DarkLight: A Search for Dark Forces at the Jefferson Laboratory Free-Electron Laser Facility

Author

Balewski, J., Bernauer, J., Bertozzi, W., Bessuille, J., Buck, B., Cowan, R., Dow, K., Epstein, C., Fisher, P., Gilad, S., Ihloff, E., Kahn, Y., Kelleher, A., Kelsey, J., Milner, R., Moran, C., Ou, L., Russell, R., Schmookler, B., Thaler, J., Tschalär, C., Vidal, C., Winnebeck, A., Benson, S., Gould, C., Biallas, G., Boyce, J. R., Coleman, J., Douglas, D., Ent, R., Evtushenko, P., Fenker, H. C., Gubeli, J., Hannon, F., Huang, J., Jordan, K., Legg, R., Marchlik, M., Moore, W., Neil, G., Shinn, M., Tennant, C., Walker, R., Williams, G., Zhang, S., Freytsis, M., Fiorito, R., O'Shea, P., Alarcon, R., Dipert, R., Ovanesyan, G., Gunter, T., Kalantarians, N., Kohl, M., Albayrak, I., Carmignotto, M., Horn, T., Gunarathne, D. S., Martoff, C. J., Olvitt, D. L., Surrow, B., Lia, X., Beck, R., Schmitz, R., Walther, D., Brinkmann, K., and Zaunig, H.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

We give a short overview of the DarkLight detector concept which is designed to search for a heavy photon A' with a mass in the range 10 MeV/c^2 < m(A') < 90 MeV/c^2 and which decays to lepton pairs. We describe the intended operating environment, the Jefferson Laboratory free electon laser, and a way to extend DarkLight's reach using A' --> invisible decays., Comment: 8 pages, 4 figures, contributed to the Community Summer Study 2013 "Snowmass on the Mississippi" in the New, Light, Weakly Coupled Particles (NLWCP) subgroup of the Intensity Frontier

Published
2013

46. Six detached white-dwarf close binaries

Author

Morales-Rueda, L., Marsh, T. R., Maxted, P. F. L., Nelemans, G., Karl, C., Napiwotzki, R., and Moran, C. K. J.

Subjects
Astrophysics
Abstract

We determine the orbits of four double degenerate systems (DDs), composed of two white dwarfs, and of two white dwarf -- M dwarf binaries. The four DDs, WD1022+050, WD1428+373, WD1824+040, and WD2032+188, show orbital periods of 1.157155(5) d, 1.15674(2) d, 6.26602(6) d and 5.0846(3) d respectively. These periods combined with estimates for the masses of the brighter component, based on their effective temperatures, allow us to constrain the masses of the unseen companions. We estimate that the upper limit for the contribution of the unseen companions to the total luminosity in the four DDs ranges between 10 and 20 per cent. In the case of the two white dwarf - M dwarf binaries, WD1042-690 and WD2009+622, we calculate the orbital parameters by fitting simultaneously the absorption line from the white dwarf and the emission core from the M-dwarf. Their orbital periods are 0.337083(1) d and 0.741226(2) d respectively. We find signatures of irradiation on the inner face of WD2009+622's companion. We calculate the masses of both components from the gravitational redshift and the mass-radius relationship for white dwarfs and find masses of 0.75 -- 0.78 Msun and 0.61 -- 0.64 Msun for WD1042-690 and WD2009+622 respectively. This indicates that the stars probably reached the asymptotic giant branch in their evolution before entering a common envelope phase. These two white dwarf - M dwarf binaries will become cataclysmic variables, although not within a Hubble time, with orbital periods below the period gap., Comment: 16 pages, 9 figures. Accepted for publication in MNRAS

Published
2005
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47. The systemic velocities of four long-period cataclysmic variable stars

Author

North, R. C., Marsh, T. R., Kolb, U., Dhillon, V. S., and Moran, C. K. J.

Subjects
Astrophysics
Abstract

Although a large number of orbital periods of cataclysmic variable stars (CVs) have been measured, comparison of period and luminosity distributions with evolutionary theory is affected by strong selection effects. A test has been discovered which is independent of these selection effects and is based upon the kinematics of CVs (Kolb & Stehle, 1996). If the standard models of evolution are correct then long-period (P_orb > 5 hrs) CVs should be typically less than 1.5 Gyr old, and their line-of-sight velocity dispersion ($\sigma_\gamma$) should be small. We present results from a pilot study which indicate that this postulate is indeed true. Four long-period dwarf novae (EM Cyg, V426 Oph, SS Cyg and AH Her) were observed over a complete orbit, in order that accurate radial velocities be obtained. We find values of -1.7, 5.4, 15.4 and 1.8 km/s with uncertainties of order 3 km/s, referred to the dynamical Local Standard of Rest (LSR), leading to a dispersion of ~ 8 km/s. Calculation of a 95 per cent confidence interval gives the result 4 < \sigma_\gamma < 28 km/s compared to a prediction of 15 km/s. We also have an improved determination of mass donor spectral type, K_2 and q for the four systems., Comment: To appear in MNRAS

Published
2002
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48. The mass ratio distribution of short period double degenerate stars

Author

Maxted, P. F. L., Marsh, T. R., and Moran, C. K. J.

Subjects
Astrophysics
Abstract

Short period double degenerates (DDs) are close white dwarf - white dwarf binary stars which are the result of the evolution of interacting binary stars. We present the first definitive measurements of the mass ratio for two DDs, WD0136+768 and WD1204+450, and an improved measurement of the mass ratio for WD0957-666. We compare the properties of the 6 known DDs with measured mass ratios to the predictions of various theoretical models. We confirm the result that standard models for the formation of DDs do not predict sufficient DDs with mass ratios near 1. We also show that the observed difference in cooling ages between white dwarfs in DDs is a useful constraint on the initial mass ratio of the binary. A more careful analysis of the properties of the white dwarf pair WD1704+481.2 leads us to conclude that the brighter white dwarf is older than its fainter companion. This is the opposite of the usual case for DDs and is caused by the more massive white dwarf being smaller and cooling faster. The mass ratio in the sense (mass of younger star)/(mass of older star) is then 1.43+-0.06 rather than the value 0.70+-0.03 given previously., Comment: Accepted for publication in MNRAS

Published
2002
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50. Radial velocity measurements of white dwarfs

Author

Maxted, P. F. L., Marsh, T. R., and Moran, C. K. J.

Subjects
Astrophysics
Abstract

We present 594 radial velocity measurements for 71 white dwarfs obtained during our search for binary white dwarfs and not reported elsewhere. We identify three excellent candidate binaries, which require further observations to confirm our preliminary estimates for their orbital periods, and one other good candidate. We investigate whether our data support the existence of a population of single, low mass (<~0.5 solar masses) white dwarfs (LMWDs). These stars are difficult to explain in standard models of stellar evolution. We find that a model with a mixed single/binary population is at least ~20 times more likely to explain our data than a pure binary population. This result depends on assumed period distributions for binary LMWDs, assumed companion masses and several other factors. Therefore, the evidence in favour of the existence of a population of single LMWDs is not sufficient, in our opinion, to firmly establish the existence of such a population, but does suggest that extended observations of LMWDs to obtain a more convincing result would be worthwhile ., Comment: 14 pages, 4 Figures. Accepted for publication in MNRAS. Added Institution

Published
2000
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