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834 results on '"Leitch, E. M."'

151. The South Pole Telescope

Author

SPT Collaboration, Ruhl, J. E., Ade, P. A. R., Carlstrom, J. E., Cho, H. M., Crawford, T., Dobbs, M., Greer, C. H., Halverson, N. W., Holzapfel, W. L., Lantin, T. M., Lee, A. T., Leong, J., Leitch, E. M., Lu, W., Lueker, M., Mehl, J., Meyer, S. S., Mohr, J. J., Padin, S., Plagge, T., Pryke, C., Schwan, D., Sharp, M. K., Runyan, M. C., Spieler, H., Staniszewski, Z., and Stark, A. A.

Subjects
Astrophysics
Abstract

A new 10 meter diameter telescope is being constructed for deployment at the NSF South Pole research station. The telescope is designed for conducting large-area millimeter and sub-millimeter wave surveys of faint, low contrast emission, as required to map primary and secondary anisotropies in the cosmic microwave background. To achieve the required sensitivity and resolution, the telescope design employs an off-axis primary with a 10m diameter clear aperture. The full aperture and the associated optics will have a combined surface accuracy of better than 20 microns rms to allow precision operation in the submillimeter atmospheric windows. The telescope will be surrounded with a large reflecting ground screen to reduce sensitivity to thermal emission from the ground and local interference. The optics of the telescope will support a square degree field of view at 2mm wavelength and will feed a new 1000-element micro-lithographed planar bolometric array with superconducting transition-edge sensors and frequency-multiplexed readouts. The first key project will be to conduct a survey over approximately 4000 degrees for galaxy clusters using the Sunyaev-Zel'dovich Effect. This survey should find many thousands of clusters with a mass selection criteria that is remarkably uniform with redshift. Armed with redshifts obtained from optical and infrared follow-up observations, it is expected that the survey will enable significant constraints to be placed on the equation of state of the dark energy., Comment: Written prior to SPIE conference, June 21-25, 2004. 19 pages, 13 figures. Also available (with higher resolution figures) at http://spt.uchicago.edu/

Published
2004
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152. Polarization Observations with the Cosmic Background Imager

Author

Readhead, A. C. S., Myers, S. T., Pearson, T. J., Sievers, J. L., Mason, B. S., Contaldi, C. R., Bond, J. R., Bustos, R., Altamirano, P., Achermann, C., Bronfman, L., Carlstrom, J. E., Cartwright, J. K., Casassus, S., Dickinson, C., Holzapfel, W. L., Kovac, J. M., Leitch, E. M., May, J., Padin, S., Pogosyan, D., Pospieszalski, M., Pryke, C., Reeves, R., Shepherd, M. C., and Torres, S.

Subjects
Astrophysics
Abstract

Polarization observations of the cosmic microwave background with the Cosmic Background Imager from September 2002 to May 2004 provide a significant detection of the E-mode polarization and reveal an angular power spectrum of polarized emission showing peaks and valleys that are shifted in phase by half a cycle relative to those of the total intensity spectrum. This key agreement between the phase of the observed polarization spectrum and that predicted based on the total intensity spectrum provides support for the standard model of cosmology, in which dark matter and dark energy are the dominant constituents, the geometry is close to flat, and primordial density fluctuations are predominantly adiabatic with a matter power spectrum commensurate with inflationary cosmological models., Comment: 28 pages including 11 color figures (reduced in quality for astro-ph). Version 2 includes supplementary material (window functions etc.) and matches the published paper

Published
2004
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153. Scientific optimization of a ground-based CMB polarization experiment

Author

Bowden, M., Taylor, A. N., Ganga, K. M., Ade, P. A. R., Bock, J. J., Cahill, G., Carlstrom, J. E., Church, S. E., Gear, W. K., Hinderks, J. R., Hu, W., Keating, B. G., Kovac, J., Lange, A . E., Leitch, E. M., Mallie, O. E., Melhuish, S. J., Murphy, J. A., Piccirillo, L., Pryke, C., Rusholme, B. A., O'Sullivan, C., and Thompson, K.

Subjects
Astrophysics
Abstract

We investigate the science goals achievable with the upcoming generation of ground-based Cosmic Microwave Background polarization experiments and calculate the optimal sky coverage for such an experiment including the effects of foregrounds. We find that with current technology an E-mode measurement will be sample-limited, while a B-mode measurement will be detector-noise-limited. We conclude that a 300 sq deg survey is an optimal compromise for a two-year experiment to measure both E and B-modes, and that ground-based polarization experiments can make an important contribution to B-mode surveys. Focusing on one particular experiment, QUaD, a proposed bolometric polarimeter operating from the South Pole, we find that a ground-based experiment can make a high significance measurement of the acoustic peaks in the E-mode spectrum, and will be able to detect the gravitational lensing signal in the B-mode spectrum. Such an experiment could also directly detect the gravitational wave component of the B-mode spectrum if the amplitude of the signal is close to current upper limits. We also investigate how a ground-based experiment can improve constraints on the cosmological parameters. We estimate that by combining two years of QUaD data with the four-year WMAP data, an optimized ground-based polarization experiment can improve constraints on cosmological parameters by a factor of two. If the foreground contamination can be reduced, the measurement of the tensor-to-scalar ratio can be improved by up to a factor of six over that obtainable from WMAP alone., Comment: 17 pages, 11 figures replaced with version accepted by MNRAS

Published
2003
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154. Status of CMB Polarization Measurements from DASI and Other Experiments

Author

Carlstrom, J. E., Kovac, J., Leitch, E. M., and Pryke, C.

Subjects
Astrophysics
Abstract

We review the current status and future plans for polarization measurements of the cosmic microwave background radiation, as well as the cosmology these measurements will address. After a long period of increasingly sensitive upper limits, the DASI experiment has detected the E-mode polarization and both the DASI and WMAP experiments have detected the TE correlation. These detections provide confirmation of the standard model of adiabatic primordial density fluctuations consistent with inflationary models. The WMAP TE correlation on large angular scales provides direct evidence of significant reionization at higher redshifts than had previously been supposed. These detections mark the beginning of a new era in CMB measurements and the rich cosmology that can be gleaned from them., Comment: 22 pages, 9 figures; To be published in the proceedings of "The Cosmic Microwave Background and its Polarization", New Astronomy Reviews, (eds. S. Hanany and K.A. Olive)

Published
2003
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155. Detection of Polarization in the Cosmic Microwave Background using DASI

Author

Kovac, J., Leitch, E. M., Pryke, C., Carlstrom, J. E., Halverson, N. W., and Holzapfel, W. L.

Subjects
Astrophysics
Abstract

We report the detection of polarized anisotropy in the Cosmic Microwave Background radiation with the Degree Angular Scale Interferometer (DASI), located at the Amundsen-Scott South Pole research station. Observations in all four Stokes parameters were obtained within two 3.4 FWHM fields separated by one hour in Right Ascension. The fields were selected from the subset of fields observed with DASI in 2000 in which no point sources were detected and are located in regions of low Galactic synchrotron and dust emission. The temperature angular power spectrum is consistent with previous measurements and its measured frequency spectral index is -0.01 (-0.16 -- 0.14 at 68% confidence), where 0 corresponds to a 2.73 K Planck spectrum. The power spectrum of the detected polarization is consistent with theoretical predictions based on the interpretation of CMB anisotropy as arising from primordial scalar adiabatic fluctuations. Specifically, E-mode polarization is detected at high confidence (4.9 sigma). Assuming a shape for the power spectrum consistent with previous temperature measurements, the level found for the E-mode polarization is 0.80 (0.56 -- 1.10), where the predicted level given previous temperature data is 0.9 -- 1.1. At 95% confidence, an upper limit of 0.59 is set to the level of B-mode polarization with the same shape and normalization as the E-mode spectrum. The TE correlation of the temperature and E-mode polarization is detected at 95% confidence, and also found to be consistent with predictions. These results provide strong validation of the underlying theoretical framework for the origin of CMB anisotropy and lend confidence to the values of the cosmological parameters that have been derived from CMB measurements., Comment: 20 pages, 6 figures

Published
2002
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156. Measuring Polarization with DASI

Author

Leitch, E. M., Kovac, J. M., Pryke, C., Reddall, B., Sandberg, E. S., Dragovan, M., Carlstrom, J. E., Halverson, N. W., and Holzapfel, W. L.

Subjects
Astrophysics
Abstract

We describe an experiment to measure the polarization of the Cosmic Microwave Background (CMB) with the Degree Angular Scale Interferometer (DASI), a compact microwave interferometer optimized to detect CMB anisotropy at multipoles 140 to 900. The telescope has operated at the Amundsen-Scott South Pole research station since 2000 January. The telescope was retrofit as a polarimeter during the 2000--2001 austral summer, and throughout the 2001 and 2002 austral winters has made observations of the CMB with sensitivity to all four Stokes parameters. The telescope performance has been extensively characterized through observations of artificial sources, the Moon, and polarized and unpolarized Galactic sources. In 271 days of observation, DASI has differenced the CMB fluctuations in two fields to an rms noise level of 2.8 uK., Comment: 12 pages, 9 figures, submitted to the Astrophysical Journal

Published
2002
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157. The Anisotropy of the Microwave Background to l = 3500: Deep Field Observations with the Cosmic Background Imager

Author

Mason, B. S., Pearson, T. J., Readhead, A. C. S., Shepherd, M. C., Sievers, J. L., Udomprasert, P. S., Cartwright, J. K., Farmer, A. J., Padin, S., Myers, S. T., Bond, J. R., Contaldi, C. R., Pen, U. -L., Prunet, S., Pogosyan, D., Carlstrom, J. E., Kovac, J., Leitch, E. M., Pryke, C., Halverson, N. W., Holzapfel, W. L., Altamirano, P., Bronfman, L., Casassus, S., May, J., and Joy, M.

Subjects
Astrophysics
Abstract

We report measurements of anisotropy in the cosmic microwave background radiation over the multipole range l ~ 200 - 3500 with the Cosmic Background Imager based on deep observations of three fields. These results confirm the drop in power with increasing l first reported in earlier measurements with this instrument, and extend the observations of this decline in power out to l \~ 2000. The decline in power is consistent with the predicted damping of primary anisotropies. At larger multipoles, l = 2000 - 3500, the power is 3.1 sigma greater than standard models for intrinsic microwave background anisotropy in this multipole range, and 3.5 sigma greater than zero. This excess power is not consistent with expected levels of residual radio source contamination but, for sigma_8 >~ 1, is consistent with predicted levels due to a secondary Sunyaev-Zeldovich anisotropy. Further observations are necessary to confirm the level of this excess and, if confirmed, determine its origin., Comment: Accepted by The Astrophysical Journal; 15 pages including 7 color figures. Additional information at http://www.astro.caltech.edu/~tjp/CBI/

Published
2002
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158. The Anisotropy of the Microwave Background to l = 3500: Mosaic Observations with the Cosmic Background Imager

Author

Pearson, T. J., Mason, B. S., Readhead, A. C. S., Shepherd, M. C., Sievers, J. L., Udomprasert, P. S., Cartwright, J. K., Farmer, A. J., Padin, S., Myers, S. T., Bond, J. R., Contaldi, C. R., Pen, U. -L., Prunet, S., Pogosyan, D., Carlstrom, J. E., Kovac, J., Leitch, E. M., Pryke, C., Halverson, N. W., Holzapfel, W. L., Altamirano, P., Bronfman, L., Casassus, S., May, J., and Joy, M.

Subjects
Astrophysics
Abstract

Using the Cosmic Background Imager, a 13-element interferometer array operating in the 26-36 GHz frequency band, we have observed 40 sq deg of sky in three pairs of fields, each ~ 145 x 165 arcmin, using overlapping pointings (mosaicing). We present images and power spectra of the cosmic microwave background radiation in these mosaic fields. We remove ground radiation and other low-level contaminating signals by differencing matched observations of the fields in each pair. The primary foreground contamination is due to point sources (radio galaxies and quasars). We have subtracted the strongest sources from the data using higher-resolution measurements, and we have projected out the response to other sources of known position in the power-spectrum analysis. The images show features on scales ~ 6 - 15 arcmin, corresponding to masses ~ (5 - 80)*10^{14} Msun at the surface of last scattering, which are likely to be the seeds of clusters of galaxies. The power spectrum estimates have a resolution Delta-l = 200 and are consistent with earlier results in the multipole range l <~ 1000. The power spectrum is detected with high signal-to-noise ratio in the range 300 <~ l <~ 1700. For 1700 <~ l <~ 3000 the observations are consistent with the results from more sensitive CBI deep-field observations. The results agree with the extrapolation of cosmological models fitted to observations at lower l, and show the predicted drop at high l (the "damping tail")., Comment: Accepted by The Astrophysical Journal; 16 pages including 17 color figures. Additional information at http://www.astro.caltech.edu/~tjp/CBI/

Published
2002
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159. SPT-3G: A Multichroic Receiver for the South Pole Telescope

Author

Anderson, A. J., Ade, P. A. R., Ahmed, Z., Austermann, J. E., Avva, J. S., Barry, P. S., Thakur, R. Basu, Bender, A. N., Benson, B. A., Bleem, L. E., Byrum, K., Carlstrom, J. E., Carter, F. W., Cecil, T., Chang, C. L., Cho, H. M., Cliche, J. F., Crawford, T. M., Cukierman, A., Denison, E. V., de Haan, T., Ding, J., Dobbs, M. A., Dutcher, D., Everett, W., Foster, A., Gannon, R. N., Gilbert, A., Groh, J. C., Halverson, N. W., Harke-Hosemann, A. H., Harrington, N. L., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Huang, N., Irwin, K. D., Jeong, O. B., Jonas, M., Khaire, T., Knox, L., Kofman, A. M., Korman, M., Kubik, D., Kuhlmann, S., Kuklev, N., Kuo, C. L., Lee, A. T., Leitch, E. M., Lowitz, A. E., Meyer, S. S., Michalik, D., Montgomery, J., Nadolski, A., Natoli, T., Nguyen, H., Noble, G. I., Novosad, V., Padin, S., Pan, Z., Pearson, J., Posada, C. M., Rahlin, A., Reichardt, C. L., Ruhl, J. E., Saunders, L. J., Sayre, J. T., Shirley, I., Shirokoff, E., Smecher, G., Sobrin, J. A., Stark, A. A., Story, K. T., Suzuki, A., Tang, Q. Y., Thompson, K. L., Tucker, C., Vale, L. R., Vanderlinde, K., Vieira, J. D., Wang, G., Whitehorn, N., Yefremenko, V., Yoon, K. W., and Young, M. R.

Published
2018
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160. Cosmological Parameter Extraction from the First Season of Observations with DASI

Author

Pryke, C., Halverson, N. W., Leitch, E. M., Kovac, J., Carlstrom, J. E., Holzapfel, W. L., and Dragovan, M.

Subjects
Astrophysics
Abstract

The Degree Angular Scale Interferometer (\dasi) has measured the power spectrum of the Cosmic Microwave Background anisotropy over the range of spherical harmonic multipoles 1000.45 and 0.0<=tau_c<=0.4, we find that the total density of the Universe Omega_tot=1.04+/-0.06, and the spectral index of the initial scalar fluctuations n_s=1.01+0.08-0.06, in accordance with the predictions of inflationary theory. In addition we find that the physical density of baryons Omega_b.h^2=0.022+0.004-0.003, and the physical density of cold dark matter Omega_cdm.h^2=0.14+/-0.04. This value of Omega_b.h^2 is consistent with that derived from measurements of the primordial abundance ratios of the light elements combined with big bang nucleosynthesis theory. Using the result of the HST Key Project h=0.72+/-0.08 we find that Omega_t=1.00+/-0.04, the matter density Omega_m=0.40+/-0.15, and the vacuum energy density Omega_lambda=0.60+/-0.15. (All 68% confidence limits.), Comment: 7 pages, 4 figures, minor changes in response to referee comments

Published
2001
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161. Experiment Design and First Season Observations with the Degree Angular Scale Interferometer

Author

Leitch, E. M., Pryke, C., Halverson, N. W., Kovac, J., Davidson, G., LaRoque, S., Schartman, E., Yamasaki, J., Carlstrom, J. E., Holzapfel, W. L., Dragovan, M., Cartwright, J. K., Mason, B. S., Padin, S., Pearson, T. J., Shepherd, M. C., and Readhead, A. C. S.

Subjects
Astrophysics
Abstract

We describe the instrumentation, experiment design and data reduction for the first season of observations with the Degree Angular Scale Interferometer (DASI), a compact microwave interferometer designed to measure anisotropy in the Cosmic Microwave Background (CMB) on degree and sub-degree scales (l=100--900). The telescope was deployed at the Amundsen-Scott South Pole research station during the 1999--2000 austral summer and conducted observations of the CMB throughout the following austral winter. In its first season of observations, DASI has mapped CMB fluctuations in 32 fields, each 3.4 deg across, with high sensitivity., Comment: 10 pages, 6 figures, minor changes in response to referee comments

Published
2001
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162. DASI First Results: A Measurement of the Cosmic Microwave Background Angular Power Spectrum

Author

Halverson, N. W., Leitch, E. M., Pryke, C., Kovac, J., Carlstrom, J. E., Holzapfel, W. L., Dragovan, M., Cartwright, J. K., Mason, B. S., Padin, S., Pearson, T. J., Shepherd, M. C., and Readhead, A. C. S.

Subjects
Astrophysics
Abstract

We present measurements of anisotropy in the Cosmic Microwave Background (CMB) from the first season of observations with the Degree Angular Scale Interferometer (DASI). The instrument was deployed at the South Pole in the austral summer 1999--2000, and made observations throughout the following austral winter. We have measured the angular power spectrum of the CMB in the range 100

Published
2001
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163. First Intrinsic Anisotropy Observations with the Cosmic Background Imager

Author

Padin, S., Cartwright, J. K., Mason, B. S., Pearson, T. J., Readhead, A. C. S., Shepherd, M. C., Sievers, J., Udomprasert, P. S., Holzapfel, W. L., Myers, S. T., Carlstrom, J. E., Leitch, E. M., Joy, M., Bronfman, L., and May, J.

Subjects
Astrophysics
Abstract

We present the first results of observations of the intrinsic anisotropy of the cosmic microwave background radiation with the Cosmic Background Imager from a site at 5080 m altitude in northern Chile. Our observations show a sharp decrease in C_l in the range l=400 - 1500. The broadband amplitudes we have measured are deltaT(band) = 58.7 (-6.3, +7.7) microK for l = 603 (-166, +180) and 29.7 (-4.2, +4.8) microK for l = 1190 (-224, +261), where these are half-power widths in l. Such a decrease in power at high l is one of the fundamental predictions of the standard cosmological model, and these are the first observations which cover a broad enough l range to show this decrease in a single experiment. The C_l we have measured enable us to place limits on the density parameter, Omega(tot) <= 0.4 or $Omega(tot) >= 0.7 (90% confidence)., Comment: 5 pages including 2 figures. Corrected an error in the comparison with Boomerang and Maxima

Published
2000
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164. A Sunyaev-Zel'dovich Effect Survey for High Redshift Clusters

Author

Mohr, J. J., Carlstrom, J. E., Holder, G. P., Holzapfel, W. L., Joy, M. K., Leitch, E. M., and Reese, E. D.

Subjects
Astrophysics
Abstract

Interferometric observations of the Sunyaev-Zel'dovich Effect (SZE) toward clusters of galaxies provide sensitive cosmological probes. We present results from 1 cm observations (at BIMA and OVRO) of a large, intermediate redshift cluster sample. In addition, we describe a proposed, higher sensitivity array which will enable us to survey large portions of the sky. Simulated observations indicate that we will be able to survey one square degree of sky per month to sufficient depth that we will detect all galaxy clusters more massive than 2x10^{14} h^{-1}_{50}M_\odot, regardless of their redshift. We describe the cluster yield and resulting cosmological constraints from such a survey., Comment: 7 pages, 6 figures, latex, contribution to VLT Opening Symposium

Published
1999
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165. A Measurement of Anisotropy in the Cosmic Microwave Background on 7-22 Arcminute Scales

Author

Leitch, E. M., Readhead, A. C. S., Pearson, T. J., Myers, S. T., Gulkis, S., and Lawrence, C. R.

Subjects
Astrophysics
Abstract

We report a measurement of anisotropy in the cosmic microwave background radiation (CMBR) on 7-22 arcminute scales. Observations of 36 fields near the North Celestial Pole (NCP) were made at 31.7 and 14.5 GHz, using the 5.5-meter and 40-meter telescopes at the Owens Valley Radio Observatory (OVRO) from 1993 to 1996. Multi-epoch VLA observations at 8.5 and 15 GHz allow removal of discrete source contamination. After point-source subtraction, we detect significant structure, which we identify with emission from a combination of a steep-spectrum foreground and the CMBR. The foreground component is found to correlate with IRAS 100 micron dust emission. Lack of H-alpha emission near the NCP suggests that this foreground is either high-temperature thermal bremsstrahlung (T_e ~ 10^6 K), flat-spectrum synchrotron or an exotic component of dust emission. On the basis of low-frequency maps of the NCP, we can restrict the spectral index of the foreground to beta >= -2.2. Although the foreground signal dominates at 14.5 GHz, the extracted CMBR component contributes 88\% of the variance at 31.7 GHz, yielding an rms fluctuation amplitude of 82^{+12.1}_{-9.1} microKelvin, including 4.3% calibration uncertainty and 12% sample variance (68% confidence). The equivalent broadband amplitude is dT_{l_e} = 59^{+8.6}_{-6.5} microKelvin at l_e = 589. This measurement, when combined with small angular-scale upper limits obtained at the OVRO, indicates that the CMBR angular power spectrum decreases between l ~ 600 and l ~ 2000 and is consistent with flat cosmological models., Comment: Revisions to match the published version, ApJ, 532: 37-56. Latex, emulateapj.sty, 22 pages, 21 Postscript figures

Published
1998

166. An Anomalous Component of Galactic Emission

Author

Leitch, E. M., Readhead, A. C. S., Pearson, T. J., and Myers, S. T.

Subjects
Astrophysics
Abstract

We present results from microwave background observations at the Owens Valley Radio Observatory. These observations, at 14.5 and 32 GHz, are designed to detect intrinsic anisotropy on scales of 7'. After point source removal, we detect significant emission with temperature spectral index beta ~ -2 towards the North Celestial Pole (NCP). Comparison of our data with the IRAS 100 micron map of the same fields reveals a strong correlation between this emission and the infrared dust emission. From the lack of detectable H-alpha emission, we conclude that the signals are consistent either with flat-spectrum synchrotron radiation, or with free-free emission from T_e ~ 10^6 K gas, probably associated with a large HI feature known as the NCP Loop. Assuming beta = -2.2, our data indicate a conversion T_f/I_(100 micron) = 0.075*nu(GHz)^-2.2 K/(MJy/sr). The detection of such a component suggests that we should be cautious in any assumptions made regarding foregrounds when designing experiments to map the microwave background radiation., Comment: 6 pages, Latex, 3 Postscript figures, uses aas2pp4.sty

Published
1997
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167. Measurements of the Sunyaev-Zeldovich Effect in the Nearby Clusters A478, A2142 and A2256

Author

Myers, S. T., Baker, J. E., Readhead, A. C. S., Leitch, E. M., and Herbig, T.

Subjects
Astrophysics
Abstract

This paper reports the measurement of the Sunyaev-Zeldovich effect (SZE) in the nearby clusters A478, A2142 and A2256 at 32 GHz. These clusters are part of a complete X-ray flux limited sample, which includes the previously measured Coma cluster. We find surface baryonic mass densities for the hot IGM within the 7.35' FWHM Gaussian beam of the OVRO 5.5-m telescope projected on the cluster centers. This is used to place lower limits on the ratio of the SZE determined baryonic mass to the gravitational binding mass. When combined with available X-ray models, the data from these three clusters and Coma yields a sample average value for the Hubble constant of 54 +/- 14 km/s/Mpc., Comment: 54 pages, 4 postscript figures, uses aaspp4.sty. To appear in the Astrophysical Journal, also available at ftp://dept.physics.upenn.edu/pub/myers/szepaper.ps.gz

Published
1997
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168. Optical Observations of the Binary Millisecond Pulsars J2145-0750 and J0034-0534

Author

Bell, J. F., Kulkarni, S. R., Bailes, M., Leitch, E. M., and Lyne, A. G.

Subjects
Astrophysics
Abstract

We report on optical observations of the low-mass binary millisecond pulsar systems J0034-0534 and J2145-0750. A faint (I=23.5) object was found to be coincident with the timing position of PSR J2145-0750. While a galaxy or distant main-sequence star cannot be ruled out, its magnitude is consistent with an ancient white dwarf, as expected from evolutionary models. For PSR J0034-0534 no objects were detected to a limiting magnitude of R=25.0, suggesting that the white dwarf in this system is cold. Using white dwarf cooling models, the limit on the magnitude of the PSR J0034-0534 companion suggests that at birth the pulsar in this system may have rotated with a period as short as 0.6 ms. These observations provide further evidence that the magnetic fields of millisecond pulsars do not decay on time scales shorter than 1 Gyr., Comment: 6 pages, uuencoded, gz -9 compressed postscript, accepted by ApJL

Published
1995
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169. BICEP/Keck. XVII. Line-of-sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors

Author

Ade, P. A. R., primary, Ahmed, Z., additional, Amiri, M., additional, Barkats, D., additional, Thakur, R. Basu, additional, Bischoff, C. A., additional, Beck, D., additional, Bock, J. J., additional, Boenish, H., additional, Bullock, E., additional, Buza, V., additional, IV, J. R. Cheshire, additional, Connors, J., additional, Cornelison, J., additional, Crumrine, M., additional, Cukierman, A., additional, Denison, E. V., additional, Dierickx, M., additional, Duband, L., additional, Eiben, M., additional, Fatigoni, S., additional, Filippini, J. P., additional, Fliescher, S., additional, Giannakopoulos, C., additional, Goeckner-Wald, N., additional, Goldfinger, D. C., additional, Grayson, J., additional, Grimes, P., additional, Hall, G., additional, Halal, G., additional, Halpern, M., additional, Hand, E., additional, Harrison, S., additional, Henderson, S., additional, Hildebrandt, S. R., additional, Hubmayr, J., additional, Hui, H., additional, Irwin, K. D., additional, Kang, J., additional, Karkare, K. S., additional, Karpel, E., additional, Kefeli, S., additional, Kernasovskiy, S. A., additional, Kovac, J. M., additional, Kuo, C. L., additional, Lau, K., additional, Leitch, E. M., additional, Lennox, A., additional, Megerian, K. G., additional, Minutolo, L., additional, Moncelsi, L., additional, Nakato, Y., additional, Namikawa, T., additional, Nguyen, H. T., additional, O’Brient, R., additional, IV, R. W. Ogburn, additional, Palladino, S., additional, Petroff, M., additional, Prouve, T., additional, Pryke, C., additional, Racine, B., additional, Reintsema, C. D., additional, Richter, S., additional, Schillaci, A., additional, Schwarz, R., additional, Schmitt, B. L., additional, Sheehy, C. D., additional, Singari, B., additional, Soliman, A., additional, Germaine, T. St., additional, Steinbach, B., additional, Sudiwala, R. V., additional, Teply, G. P., additional, Thompson, K. L., additional, Tolan, J. E., additional, Tucker, C., additional, Turner, A. D., additional, Umiltà, C., additional, Vergès, C., additional, Vieregg, A. G., additional, Wandui, A., additional, Weber, A. C., additional, Wiebe, D. V., additional, Willmert, J., additional, Wong, C. L., additional, Wu, W. L. K., additional, Yang, H., additional, Yoon, K. W., additional, Young, E., additional, Yu, C., additional, Zeng, L., additional, Zhang, C., additional, and Zhang, S., additional

Published
2023
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170. BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

Author

Ade, P. A. R., primary, Ahmed, Z., additional, Amiri, M., additional, Barkats, D., additional, Thakur, R. Basu, additional, Bischoff, C. A., additional, Beck, D., additional, Bock, J. J., additional, Boenish, H., additional, Bullock, E., additional, Buza, V., additional, Cheshire, J. R., additional, Clark, S. E., additional, Connors, J., additional, Cornelison, J., additional, Crumrine, M., additional, Cukierman, A., additional, Denison, E. V., additional, Dierickx, M., additional, Duband, L., additional, Eiben, M., additional, Fatigoni, S., additional, Filippini, J. P., additional, Fliescher, S., additional, Giannakopoulos, C., additional, Goeckner-Wald, N., additional, Goldfinger, D. C., additional, Grayson, J., additional, Grimes, P., additional, Hall, G., additional, Halal, G., additional, Halpern, M., additional, Hand, E., additional, Harrison, S., additional, Henderson, S., additional, Hildebrandt, S. R., additional, Hubmayr, J., additional, Hui, H., additional, Irwin, K. D., additional, Kang, J., additional, Karkare, K. S., additional, Karpel, E., additional, Kefeli, S., additional, Kernasovskiy, S. A., additional, Kovac, J. M., additional, Kuo, C. L., additional, Lau, K., additional, Leitch, E. M., additional, Lennox, A., additional, Megerian, K. G., additional, Minutolo, L., additional, Moncelsi, L., additional, Nakato, Y., additional, Namikawa, T., additional, Nguyen, H. T., additional, O’Brient, R., additional, IV, R. W. Ogburn, additional, Palladino, S., additional, Petroff, M. A., additional, Prouve, T., additional, Pryke, C., additional, Racine, B., additional, Reintsema, C. D., additional, Richter, S., additional, Schillaci, A., additional, Schwarz, R., additional, Schmitt, B. L., additional, Sheehy, C. D., additional, Singari, B., additional, Soliman, A., additional, Germaine, T. St., additional, Steinbach, B., additional, Sudiwala, R. V., additional, Teply, G. P., additional, Thompson, K. L., additional, Tolan, J. E., additional, Tucker, C., additional, Turner, A. D., additional, Umiltà, C., additional, Vergès, C., additional, Vieregg, A. G., additional, Wandui, A., additional, Weber, A. C., additional, Wiebe, D. V., additional, Willmert, J., additional, Wong, C. L., additional, Wu, W. L. K., additional, Yang, H., additional, Yoon, K. W., additional, Young, E., additional, Yu, C., additional, Zeng, L., additional, Zhang, C., additional, and Zhang, S., additional

Published
2023
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171. BICEP / Keck XVII: Line of Sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors

Author

Keck Collaboration, Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J. R., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E. V., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Fliescher, S., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P., Halal, G., Hall, G., Halpern, M., Hand, E., Harrison, S., Henderson, S., Hildebrandt, S. R., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Singari, B., Soliman, A., Germaine, T. St, Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umilta, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), BICEP/Keck, Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present estimates of line-of-sight distortion fields derived from the 95 GHz and 150 GHz data taken by BICEP2, BICEP3, and Keck Array up to the 2018 observing season, leading to cosmological constraints and a study of instrumental and astrophysical systematics. Cosmological constraints are derived from three of the distortion fields concerning gravitational lensing from large-scale structure, polarization rotation from magnetic fields or an axion-like field, and the screening effect of patchy reionization. We measure an amplitude of the lensing power spectrum $A_L^{\phi\phi}=0.95 \pm 0.20$. We constrain polarization rotation, expressed as the coupling constant of a Chern-Simons electromagnetic term $g_{a\gamma} \leq 2.6 \times 10^{-2}/H_I$, where $H_I$ is the inflationary Hubble parameter, and an amplitude of primordial magnetic fields smoothed over 1 Mpc $B_{1\text{Mpc}} \leq 6.6 \;\text{nG}$ at 95 GHz. We constrain the root mean square of optical-depth fluctuations in a simple "crinkly surface" model of patchy reionization, finding $A^\tau, Comment: 34 pages, 19 figures, accepted for publication in The Astrophysical Journal

Published
2023

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

Author

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

Published
2022
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173. BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

Author

Keck Collaboration, Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J. R., Clark, S. E., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E. V., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Fliescher, S., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P., Halal, G., Hall, G., Halpern, M., Hand, E., Harrison, S., Henderson, S., Hildebrandt, S. R., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Singari, B., Soliman, A., Germaine, T. St, Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umilta, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and BICEP/Keck

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H I) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H I is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H I emission into distinct velocity components and detect dust polarization correlated with the local Galactic H I but not with the H I associated with Magellanic Stream I. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H I morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the H I morphology template correlates in B modes at a $\sim$10-65$\%$ level over the multipole range $20 < \ell < 200$ with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be $β= 1.54 \pm 0.13$. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H I. Finally, we explore the morphological parameter space in the H I-based filamentary model., 27 pages, 12 figures

Published
2023

175. Bicep/Keck XV: The Bicep3 Cosmic Microwave Background Polarimeter and the First Three-year Data Set

Author

Ade, P. A. R., primary, Ahmed, Z., additional, Amiri, M., additional, Barkats, D., additional, Thakur, R. Basu, additional, Bischoff, C. A., additional, Beck, D., additional, Bock, J. J., additional, Boenish, H., additional, Bullock, E., additional, Buza, V., additional, Cheshire IV, J. R., additional, Connors, J., additional, Cornelison, J., additional, Crumrine, M., additional, Cukierman, A., additional, Denison, E. V., additional, Dierickx, M., additional, Duband, L., additional, Eiben, M., additional, Fatigoni, S., additional, Filippini, J. P., additional, Fliescher, S., additional, Goeckner-Wald, N., additional, Goldfinger, D. C., additional, Grayson, J., additional, Grimes, P., additional, Hall, G., additional, Halal, G., additional, Halpern, M., additional, Hand, E., additional, Harrison, S., additional, Henderson, S., additional, Hildebrandt, S. R., additional, Hilton, G. C., additional, Hubmayr, J., additional, Hui, H., additional, Irwin, K. D., additional, Kang, J., additional, Karkare, K. S., additional, Karpel, E., additional, Kefeli, S., additional, Kernasovskiy, S. A., additional, Kovac, J. M., additional, Kuo, C. L., additional, Lau, K., additional, Leitch, E. M., additional, Lennox, A., additional, Megerian, K. G., additional, Minutolo, L., additional, Moncelsi, L., additional, Nakato, Y., additional, Namikawa, T., additional, Nguyen, H. T., additional, O’Brient, R., additional, Ogburn IV, R. W., additional, Palladino, S., additional, Prouve, T., additional, Pryke, C., additional, Racine, B., additional, Reintsema, C. D., additional, Richter, S., additional, Schillaci, A., additional, Schwarz, R., additional, Schmitt, B. L., additional, Sheehy, C. D., additional, Soliman, A., additional, Germaine, T. St., additional, Steinbach, B., additional, Sudiwala, R. V., additional, Teply, G. P., additional, Thompson, K. L., additional, Tolan, J. E., additional, Tucker, C., additional, Turner, A. D., additional, Umiltà, C., additional, Vergès, C., additional, Vieregg, A. G., additional, Wandui, A., additional, Weber, A. C., additional, Wiebe, D. V., additional, Willmert, J., additional, Wong, C. L., additional, Wu, W. L. K., additional, Yang, H., additional, Yoon, K. W., additional, Young, E., additional, Yu, C., additional, Zeng, L., additional, Zhang, C., additional, and Zhang, S., additional

Published
2022
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176. The 10 Meter South Pole Telescope

Author

Carlstrom, J. E., Ade, P. A. R., Aird, K. A., Benson, B. A., Bleem, L. E., Busetti, S., Chang, C. L., Chauvin, E., Cho, H.-M., Crawford, T. M., Crites, A. T., Dobbs, M. A., Halverson, N. W., Heimsath, S., Holzapfel, W. L., Hrubes, J. D., Joy, M., Keisler, R., Lanting, T. M., Lee, A. T., Leitch, E. M., Leong, J., Lu, W., Lueker, M., Luong-Van, D., McMahon, J. J., Mehl, J., Meyer, S. S., Mohr, J. J., Montroy, T. E., Padin, S., Plagge, T., Pryke, C., Ruhl, J. E., Schaffer, K. K., Schwan, D., Shirokoff, E., Spieler, H. G., Staniszewski, Z., Stark, A. A., Tucker, C., Vanderlinde, K., Vieira, J. D., and Williamson, R.

Published
2011
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177. The Design and Integrated Performance of SPT-3G

Author

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

Published
2022
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178. BICEP / Keck XIII: Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

Author

Keck Collaboration, Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J. R., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E. V., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Fliescher, S., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P., Halal, G., Hall, G., Halpern, M., Hand, E., Harrison, S., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Soliman, A., Germaine, T. St, Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A., Umilta, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present results from an analysis of all data taken by the BICEP2, Keck Array and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz data set. The $Q/U$ maps now reach depths of 2.8, 2.8 and 8.8 $\mu{\mathrm K}_{cmb}$ arcmin at 95, 150 and 220 GHz respectively over an effective area of $\approx 600$ square degrees at 95 GHz and $\approx 400$ square degrees at 150 & 220 GHz. The 220 GHz maps now achieve a signal-to-noise on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-$\Lambda$CDM+$r$+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint $r_{0.05}, Comment: 22 pages, 24 figures, as published in PRL, data and figures available for download at http://bicepkeck.org

Published
2021

179. Detection of Galactic and Extragalactic Millimeter-wavelength Transient Sources with SPT-3G

Author

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

Published
2021
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180. BICEP/Keck XII: Constraints on axionlike polarization oscillations in the cosmic microwave background

Author

Keck Collaboration, Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J. R., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Dierickx, M., Duband, L., Fatigoni, S., Filippini, J. P., Fliescher, S., Goeckner-Wald, N., Grayson, J., Hall, G., Halpern, M., Harrison, S., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Soliman, A., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Teply, G., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umilta, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and BICEP/Keck

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), background: model, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, axion: parameter space, dark matter: direct detection, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), cosmic rays, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Experiments in gravity, beam: polarization, Astrophysics::Instrumentation and Methods for Astrophysics, coupling constant, oscillation, BICEP, sensitivity, polarization: monitoring, photon axion: coupling, cosmic background radiation: temperature, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], axion-like particles, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, S029AXI, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. A local axion field induces an all-sky, temporally sinusoidal rotation of CMB polarization. A CMB polarimeter can thus function as a direct-detection experiment for axion-like dark matter. We develop techniques to extract an oscillation signal. Many elements of the method are generic to CMB polarimetry experiments and can be adapted for other datasets. As a first demonstration, we process data from the 2012 observing season to set upper limits on the axion-photon coupling constant in the mass range $10^{-21}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to months. We find no statistically significant deviations from the background model. For periods larger than $24~\mathrm{hr}$ (mass $m < 4.8 \times 10^{-20}~\mathrm{eV}$), the median 95%-confidence upper limit is equivalent to a rotation amplitude of $0.68^\circ$, which constrains the axion-photon coupling constant to $g_{����} < \left ( 1.1 \times 10^{-11}~\mathrm{GeV}^{-1} \right ) m/\left (10^{-21}~\mathrm{eV} \right )$, if axion-like particles constitute all of the dark matter. The constraints can be improved substantially with data already collected by the BICEP series of experiments. Current and future CMB polarimetry experiments are expected to achieve sufficient sensitivity to rule out unexplored regions of the axion parameter space., 25 pages, 6 figures, 2 tables

Published
2021

181. SPT-3G: a next-generation cosmic microwave background polarization experiment on the South Pole telescope

Author

MIT Kavli Institute for Astrophysics and Space Research, Benson, B. A., Ade, P. A. R., Ahmed, Z., Allen, S. W., Arnold, K., Austermann, J. E., Bender, A. N., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. M., Cliche, J. F., Crawford, T. M., Cukierman, A., de Haan, T., Dobbs, M. A., Dutcher, D., Everett, W., Gilbert, A., Halverson, N. W., Hanson, D., Harrington, N. L., Hattori, K., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Irwin, K. D., Keisler, R., Knox, L., Kubik, D., Kuo, C. L., Lee, A. T., Leitch, E. M., Li, D., McDonald, M., Meyer, S. S., Montgomery, J., Myers, M., Natoli, T., Nguyen, H., Novosad, V., Padin, S., Pan, Z., Pearson, J., Reichardt, C., Ruhl, J. E., Saliwanchik, B. R., Simard, G., Smecher, G., Sayre, J. T., Shirokoff, E., Stark, A. A., Story, K., Suzuki, A., Thompson, K. L., Tucker, C., Vanderlinde, K., Vieira, J. D., Vikhlinin, A., Wang, G., Yefremenko, V., Yoon, K. W., MIT Kavli Institute for Astrophysics and Space Research, Benson, B. A., Ade, P. A. R., Ahmed, Z., Allen, S. W., Arnold, K., Austermann, J. E., Bender, A. N., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. M., Cliche, J. F., Crawford, T. M., Cukierman, A., de Haan, T., Dobbs, M. A., Dutcher, D., Everett, W., Gilbert, A., Halverson, N. W., Hanson, D., Harrington, N. L., Hattori, K., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Irwin, K. D., Keisler, R., Knox, L., Kubik, D., Kuo, C. L., Lee, A. T., Leitch, E. M., Li, D., McDonald, M., Meyer, S. S., Montgomery, J., Myers, M., Natoli, T., Nguyen, H., Novosad, V., Padin, S., Pan, Z., Pearson, J., Reichardt, C., Ruhl, J. E., Saliwanchik, B. R., Simard, G., Smecher, G., Sayre, J. T., Shirokoff, E., Stark, A. A., Story, K., Suzuki, A., Thompson, K. L., Tucker, C., Vanderlinde, K., Vieira, J. D., Vikhlinin, A., Wang, G., Yefremenko, V., and Yoon, K. W.

Abstract

© 2014 SPIE. We describe the design of a new polarization sensitive receiver, spt-3g, for the 10-meter South Pole Telescope (spt). The spt-3g receiver will deliver a factor of ∼20 improvement in mapping speed over the current receiver, spt-pol. The sensitivity of the spt-3g receiver will enable the advance from statistical detection of B-mode polarization anisotropy power to high signal-to-noise measurements of the individual modes, i.e., maps. This will lead to precise (∼0.06 eV) constraints on the sum of neutrino masses with the potential to directly address the neutrino mass hierarchy. It will allow a separation of the lensing and inflationary B-mode power spectra, improving constraints on the amplitude and shape of the primordial signal, either through spt-3g data alone or in combination with bicep2/keck, which is observing the same area of sky. The measurement of small-scale temperature anisotropy will provide new constraints on the epoch of reionization. Additional science from the spt-3g survey will be significantly enhanced by the synergy with the ongoing optical Dark Energy Survey (des), including: a 1% constraint on the bias of optical tracers of large-scale structure, a measurement of the differential Doppler signal from pairs of galaxy clusters that will test General Relativity on ∼200Mpc scales, and improved cosmological constraints from the abundance of clusters of galaxies.

Published
2021

182. Self-Calibration of BICEP1 Three-Year Data and Constraints on Astrophysical Polarization Rotation

Author

Kaufman, J. P, Miller, N. J, Shimon, M, Barkats, D, Bischoff, C, Buder, I, Keating, B. G, Kovac, J. M, Ade, P. A. R, Aikin, R, Battle, J. O, Bierman, E. M, Bock, J. J, Chiang, H. C, Dowell, C. D, Duband, L, Filippini, J, Hivon, E. F, Holzapfel, W. L, Hristov, V. V, Jones, W. C, Kernasovskiy, S. S, Kuo, C. L, Leitch, E. M, and Mason, P. V

Subjects
Astrophysics
Abstract

Cosmic microwave background (CMB) polarimeters aspire to measure the faint B-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence, rotation of the polarization of the CMB arising from parity-violating physics, which would produce nonzero expectation values for the CMB's temperature to B-mode correlation (TB) and E-mode to B-mode correlation (EB) spectra. However, instrumental systematic effects can also cause these TB and EB correlations to be nonzero. In particular, an overall miscalibration of the polarization orientation of the detectors produces TB and EB spectra which are degenerate with isotropic cosmological birefringence, while also introducing a small but predictable bias on the BB spectrum. We find that BICEP1 three-year spectra, which use our standard calibration of detector polarization angles from a dielectric sheet, are consistent with a polarization rotation of alpha = −2.77deg +/- 0.86deg (statistical) +/- 1.3deg (systematic). We have revised the estimate of systematic error on the polarization rotation angle from the two-year analysis by comparing multiple calibration methods. We also account for the (negligible) impact of measured beam systematic effects. We investigate the polarization rotation for the BICEP1 100 GHz and 150 GHz bands separately to investigate theoretical models that produce frequency-dependent cosmic birefringence. We find no evidence in the data supporting either of these models or Faraday rotation of the CMB polarization by the Milky Way galaxy's magnetic field. If we assume that there is no cosmic birefringence, we can use the TB and EB spectra to calibrate detector polarization orientations, thus reducing bias of the cosmological B-mode spectrum from leaked E-modes due to possible polarization orientation miscalibration. After applying this "self-calibration" process, we find that the upper limit on the tensor-to-scalar ratio decreases slightly, from r < 0.70 to r < 0.65 at 95% confidence.

Published
2014
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183. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author

Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., Zhou Y., Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., and Zhou Y.

Abstract

POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.

Published
2020

184. A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies

Author

McDonald, M., Bayliss, M., Benson, B. A., Foley, R. J., Ruel, J., Sullivan, P., Veilleux, S., Aird, K. A., Ashby, M. L. N., Bautz, M., Bazin, G., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., de Haan, T., Desai, S., Dobbs, M. A., Dudley, J. P., Egami, E., Forman, W. R., Garmire, G. P., George, E. M., Gladders, M. D., Gonzalez, A. H., Halverson, N. W., Harrington, N. L., High, F. W., Holder, G. P., Holzapfel, W. L., Hoover, S., Hrubes, J. D., Jones, C., Joy, M., Keisler, R., Knox, L., Lee, A. T., Leitch, E. M., Liu, J., Lueker, M., Luong-Van, D., Mantz, A., Marrone, D. P., McMahon, J. J., Mehl, J., Meyer, S. S., Miller, E. D., Mocanu, L., Mohr, J. J., Montroy, T. E., Murray, S. S., Natoli, T., Padin, S., Plagge, T., Pryke, C., Rawle, T. D., Reichardt, C. L., Rest, A., Rex, M., Ruhl, J. E., Saliwanchik, B. R., Saro, A., Sayre, J. T., Schaffer, K. K., Shaw, L., Shirokoff, E., Simcoe, R., Song, J., Spieler, H. G., Stalder, B., Staniszewski, Z., Stark, A. A., Story, K., Stubbs, C. W., Šuhada, R., van Engelen, A., Vanderlinde, K., Vieira, J. D., Vikhlinin, A., Williamson, R., Zahn, O., and Zenteno, A.

Published
2012
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185. Scientific Verification of Faraday Rotation Modulators: Detection of Diffuse Polarized Galactic Emission

Author

Moyerman, S, Bierman, E, Ade, P. A. R, Aiken, R, Barkats, D, Bischoff, C, Bock, J. J, Chiang, H. C, Dowell, C. D, Duband, L, Hivon, E. F, Holzapel, W. L, Hristov, V. V, Jones, W. C, Kaufman, J, Keating, B. G, Kovac, J. M, Kuo, C. L, Leitch, E. M, Mason, P. V, Matsumura, T, Nguyen, H. T, Ponthieu, N, Pryke, C, and Wollack, E

Subjects
Astrophysics
Abstract

The design and performance of a wide bandwidth linear polarization-modulator based on the Faraday effect is described. Faraday Rotation Modulators (FRMs) are solid-state polarization switches that are capable of modulation up to approx 10 kHz. Six FRMs were utilized during the 2006 observing season in the Background Imaging of Cosmic Extragalactic Polarization (BICEP) experiment; three FRMs were used at each of BICEP fs 100 and 150 GHz frequency bands. The technology was verified through high signal-to-noise detection of Galactic polarization using two of the six FRMs during four observing runs in 2006. The features exhibit strong agreement with BICEP fs measurements of the Galaxy using non-FRM pixels and with the Galactic polarization models. This marks the first detection of high signal-to-noise mm-wave celestial polarization using fast, active optical modulation. The performance of the FRMs during periods when they were not modulated was also analyzed and compared to results from BICEP fs 43 pixels without FRMs.

Published
2012

186. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author

Chinone, Y, primary, Adachi, S, additional, Ade, PAR, additional, Aguilar, M, additional, Akiba, Y, additional, Arnold, K, additional, Baccigalupi, C, additional, Barron, D, additional, Beck, D, additional, Beckman, S, additional, Bianchini, F, additional, Boettger, D, additional, Borrill, J, additional, ElBouhargani, H, additional, Carron, J, additional, Chapman, S, additional, Cheung, K, additional, Crowley, K, additional, Cukierman, A, additional, Dünner, R, additional, Dobbs, M, additional, Ducout, A, additional, Elleflot, T, additional, Errard, J, additional, Fabbian, G, additional, Feeney, S M, additional, Feng, C, additional, Fujino, T, additional, Galitzki, N, additional, Gilbert, A, additional, Goeckner-Wald, N, additional, Groh, J, additional, Groh, J C, additional, Hall, G, additional, Halverson, N, additional, Hamada, T, additional, Hasegawa, M, additional, Hazumi, M, additional, Hill, C A, additional, Howe, L, additional, Inoue, Y, additional, Jaehnig, G, additional, Jaffe, A H, additional, Jeong, O, additional, LeJeune, M, additional, Kaneko, D, additional, Katayama, N, additional, Keating, B, additional, Keskitalo, R, additional, Kikuchi, S, additional, Kisner, T, additional, Krachmalnicoff, N, additional, Kusaka, A, additional, Lee, A T, additional, Leitch, E M, additional, Leon, D, additional, Linder, E, additional, Lowry, L N, additional, Mangu, A, additional, Matsuda, F, additional, Matsumura, T, additional, Minami, Y, additional, Montgomery, J, additional, Navaroli, M, additional, Nishino, H, additional, Paar, H, additional, Peloton, J, additional, Pham, ATP, additional, Poletti, D, additional, Puglisi, G, additional, Reichardt, C L, additional, Richards, P L, additional, Ross, C, additional, Segawa, Y, additional, Sherwin, B D, additional, Silva-Feaver, M, additional, Siritanasak, P, additional, Stebor, N, additional, Stompor, R, additional, Suzuki, A, additional, Tajima, O, additional, Takakura, S, additional, Takatori, S, additional, Tanabe, D, additional, Teply, G P, additional, Tomaru, T, additional, Tsai, C, additional, Tucker, C, additional, Verges, C, additional, Westbrook, B, additional, Whitehorn, N, additional, Zahn, A, additional, and Zhou, Y, additional

Published
2020
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187. The QUIET Instrument

Author

Gaier, T, Kangaslahti, P, Lawrence, C. R, Leitch, E. M, and Wollack, E. J

Subjects
Astronomy
Abstract

The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the Cosmic Microwave Background, targeting the imprint of inflationary gravitational waves at large angular scales ( approx 1 deg.) . Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters which form the focal planes use a highly compact design based on High Electron Mobility Transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 micro Ks(exp 1/2)) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 micro Ks(exp 1/2) at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01 (QUIET Collaboration 2012) The two arrays together cover multipoles in the range l approximately equals 25-975 . These are the largest HEMT-ba.sed arrays deployed to date. This article describes the design, calibration, performance of, and sources of systematic error for the instrument

Published
2012

188. On-Sky Performance of the SPT-3G Frequency-Domain Multiplexed Readout

Author

Bender, A. N., primary, Anderson, A. J., additional, Avva, J. S., additional, Ade, P. A. R., additional, Ahmed, Z., additional, Barry, P. S., additional, Basu Thakur, R., additional, Benson, B. A., additional, Bryant, L., additional, Byrum, K., additional, Carlstrom, J. E., additional, Carter, F. W., additional, Cecil, T. W., additional, Chang, C. L., additional, Cho, H.-M., additional, Cliche, J. F., additional, Cukierman, A., additional, de Haan, T., additional, Denison, E. V., additional, Ding, J., additional, Dobbs, M. A., additional, Dutcher, D., additional, Everett, W., additional, Ferguson, K. R., additional, Foster, A., additional, Fu, J., additional, Gallicchio, J., additional, Gambrel, A. E., additional, Gardner, R. W., additional, Gilbert, A., additional, Groh, J. C., additional, Guns, S., additional, Guyser, R., additional, Halverson, N. W., additional, Harke-Hosemann, A. H., additional, Harrington, N. L., additional, Henning, J. W., additional, Hilton, G. C., additional, Holzapfel, W. L., additional, Howe, D., additional, Huang, N., additional, Irwin, K. D., additional, Jeong, O. B., additional, Jonas, M., additional, Jones, A., additional, Khaire, T. S., additional, Kofman, A. M., additional, Korman, M., additional, Kubik, D. L., additional, Kuhlmann, S., additional, Kuo, C.-L., additional, Lee, A. T., additional, Leitch, E. M., additional, Lowitz, A. E., additional, Meyer, S. S., additional, Michalik, D., additional, Montgomery, J., additional, Nadolski, A., additional, Natoli, T., additional, Nguyen, H., additional, Noble, G. I., additional, Novosad, V., additional, Padin, S., additional, Pan, Z., additional, Paschos, P., additional, Pearson, J., additional, Posada, C. M., additional, Quan, W., additional, Rahlin, A., additional, Riebel, D., additional, Ruhl, J. E., additional, Sayre, J. T., additional, Shirokoff, E., additional, Smecher, G., additional, Sobrin, J. A., additional, Stark, A. A., additional, Stephen, J., additional, Story, K. T., additional, Suzuki, A., additional, Thompson, K. L., additional, Tucker, C., additional, Vale, L. R., additional, Vanderlinde, K., additional, Vieira, J. D., additional, Wang, G., additional, Whitehorn, N., additional, Yefremenko, V., additional, Yoon, K. W., additional, and Young, M. R., additional

Published
2019
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189. Improved polarization calibration of the BICEP3 CMB polarimeter at the South Pole

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Cornelison, J., Vergès, C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Basu Thakur, R., Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire, J. R., Connors, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Look, K., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'brient, R., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., St. Germaine, T., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.

Published
2022
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190. Thermal testing for cryogenic CMB instrument optical design

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Goldfinger, D. C., Ade, P.A.R., Ahmed, Z., Amiri, M., Barkats, D., Basu Thakur, R., Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Prouvé, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Smith, A. G., St. Germaine, T., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.

Published
2022
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191. Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

Author

Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garc��a-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., S��nchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., Zuntz, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and SPT

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, FOS: Physical sciences, Context (language use), Field (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, Galaxy, Cosmology, South Pole Telescope, 0103 physical sciences, Dark energy, astro-ph.CO, LENTES GRAVITACIONAIS, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat $\Lambda$CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields $S_{8}\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3} = 0.782^{+0.019}_{-0.025}$ and $\Omega_{\rm m}=0.260^{+0.029}_{-0.019}$. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat $\Lambda$CDM models. Combining constraints from all six two-point functions yields $S_{8}=0.776^{+0.014}_{-0.021}$ and $\Omega_{\rm m}= 0.271^{+0.022}_{-0.016}$. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis., Comment: 20 pages, 7 figures

Published
2019

194. Performance of Al–Mn Transition-Edge Sensor Bolometers in SPT-3G

Author

Anderson, A. J., primary, Ade, P. A. R., additional, Ahmed, Z., additional, Avva, J. S., additional, Barry, P. S., additional, Thakur, R. Basu, additional, Bender, A. N., additional, Benson, B. A., additional, Bryant, L., additional, Byrum, K., additional, Carlstrom, J. E., additional, Carter, F. W., additional, Cecil, T. W., additional, Chang, C. L., additional, Cho, H.-M., additional, Cliche, J. F., additional, Cukierman, A., additional, de Haan, T., additional, Denison, E. V., additional, Ding, J., additional, Dobbs, M. A., additional, Dutcher, D., additional, Everett, W., additional, Ferguson, K. R., additional, Foster, A., additional, Fu, J., additional, Gallicchio, J., additional, Gambrel, A. E., additional, Gardner, R. W., additional, Gilbert, A., additional, Groh, J. C., additional, Guns, S. T., additional, Guyser, R., additional, Halverson, N. W., additional, Harke-Hosemann, A. H., additional, Harrington, N. L., additional, Henning, J. W., additional, Hilton, G. C., additional, Holzapfel, W. L., additional, Howe, D., additional, Huang, N., additional, Irwin, K. D., additional, Jeong, O. B., additional, Jonas, M., additional, Jones, A., additional, Khaire, T. S., additional, Kofman, A. M., additional, Korman, M., additional, Kubik, D. L., additional, Kuhlmann, S., additional, Kuo, C.-L., additional, Lee, A. T., additional, Leitch, E. M., additional, Lowitz, A. E., additional, Meyer, S. S., additional, Michalik, D., additional, Montgomery, J., additional, Nadolski, A., additional, Natoli, T., additional, Nguyen, H., additional, Noble, G. I., additional, Novosad, V., additional, Padin, S., additional, Pan, Z., additional, Paschos, P., additional, Pearson, J., additional, Posada, C. M., additional, Quan, W., additional, Rahlin, A., additional, Riebel, D., additional, Ruhl, J. E., additional, Sayre, J. T., additional, Shirokoff, E., additional, Smecher, G., additional, Sobrin, J. A., additional, Stark, A. A., additional, Stephen, J., additional, Story, K. T., additional, Suzuki, A., additional, Thompson, K. L., additional, Tucker, C., additional, Vale, L. R., additional, Vanderlinde, K., additional, Vieira, J. D., additional, Wang, G., additional, Whitehorn, N., additional, Yefremenko, V., additional, Yoon, K. W., additional, and Young, M. R., additional

Published
2019
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195. The C-Band All-Sky Survey (C-BASS): constraining diffuse Galactic radio emission in the North Celestial Pole region

Author

Dickinson, C, primary, Barr, A, primary, Chiang, H C, primary, Copley, C, primary, Grumitt, R D P, primary, Harper, S E, primary, Heilgendorff, H M, primary, Jew, L R P, primary, Jonas, J L, primary, Jones, Michael E, primary, Leahy, J P, primary, Leech, J, primary, Leitch, E M, primary, Muchovej, S J C, primary, Pearson, T J, primary, Peel, M W, primary, Readhead, A C S, primary, Sievers, J, primary, Stevenson, M A, primary, and Taylor, Angela C, primary

Published
2019
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196. A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of POLARBEAR Data

Author

The POLARBEAR Collaboration: Ade, P. A. R., Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, D., Bianchini, F., Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Crowley, K., Cukierman, Ari, Dunner, R., Dobbs, M., Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feeney, S. M., Feng, C., Fujino, Takuro, Galitzki, Nicholas, Gilbert, A., Goeckner-Wald, Neil, Groh, J. C., Hall, G., Halverson, Nils W., Hamada, T., Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaehnig, G., Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Le Jeune, M., Lee, Adrian T., Leitch, E. M., Leon, David, Linder, E., Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Minami, Y., Montgomery, J., Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Pham, A. T. P., Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Richards, P. L., Ross, Colin, Segawa, Y., Sherwin, B. D., Silva-Feaver, M., Siritanasak, Praween, Stebor, N., Stompor, R., Suzuki, Aritoki, Tajima, Osamu, Takakura, S., Takatori, Sayuri, Tanabe, D., Teply, Grant P., Tomaru, T., Tucker, C., Whitehorn, N., Zahn, A., 秋葉, 祥希, 茅根, 裕司, 長谷川, 雅也, 羽澄, 昌史, 井上, 優貴, 片山, 伸彦, 松村, 知岳, 西野, 玄記, 鈴木, 有春, 田島, 治, The POLARBEAR Collaboration: Ade, P. A. R., Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, D., Bianchini, F., Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Crowley, K., Cukierman, Ari, Dunner, R., Dobbs, M., Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feeney, S. M., Feng, C., Fujino, Takuro, Galitzki, Nicholas, Gilbert, A., Goeckner-Wald, Neil, Groh, J. C., Hall, G., Halverson, Nils W., Hamada, T., Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaehnig, G., Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Le Jeune, M., Lee, Adrian T., Leitch, E. M., Leon, David, Linder, E., Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Minami, Y., Montgomery, J., Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Pham, A. T. P., Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Richards, P. L., Ross, Colin, Segawa, Y., Sherwin, B. D., Silva-Feaver, M., Siritanasak, Praween, Stebor, N., Stompor, R., Suzuki, Aritoki, Tajima, Osamu, Takakura, S., Takatori, Sayuri, Tanabe, D., Teply, Grant P., Tomaru, T., Tucker, C., Whitehorn, N., Zahn, A., 秋葉, 祥希, 茅根, 裕司, 長谷川, 雅也, 羽澄, 昌史, 井上, 優貴, 片山, 伸彦, 松村, 知岳, 西野, 玄記, 鈴木, 有春, and 田島, 治

Abstract

著者人数: 81名, Accepted: 2017-09-20

Published
2018

197. Cosmological lensing ratios with DES Y1, SPT and Planck

Author

Prat, J., Baxter, E. J., Shin, T., Sánchez, C., Chang, C., Jain, B., Miquel, R., Alarcon, A., Bacon, D., Bernstein, G. M., Cawthon, R., Crawford, T. M., Davis, C., De Vicente, J., Dodelson, S., Eifler, T. F., Friedrich, O., Gatti, M., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Jarvis, M., Krause, E., MacCrann, N., Mawdsley, B., Nicola, A., Omori, Y., Pujol, A., Rau, M. M., Reichardt, C. L., Samuroff, S., Sheldon, E., Troxel, M. A., Vielzeuf, P., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bleem, L. E., Brooks, D., Burke, D. L., Carlstrom, J. E., Kind, M. Carrasco, Carretero, J., Chang, C. L., Cho, H-M., Chown, R., Crites, A. T., Cunha, C. E., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Doel, P., Everett, W. B., Evrard, A. E., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., de Haan, T., Halverson, N. W., Harrington, N. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Knox, L., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A. T., Leitch, E. M., Lima, M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miller, C. J., Mocanu, L. M., Mohr, J. J., Natoli, T., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Zahn, O., Prat, J., Baxter, E. J., Shin, T., Sánchez, C., Chang, C., Jain, B., Miquel, R., Alarcon, A., Bacon, D., Bernstein, G. M., Cawthon, R., Crawford, T. M., Davis, C., De Vicente, J., Dodelson, S., Eifler, T. F., Friedrich, O., Gatti, M., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Jarvis, M., Krause, E., MacCrann, N., Mawdsley, B., Nicola, A., Omori, Y., Pujol, A., Rau, M. M., Reichardt, C. L., Samuroff, S., Sheldon, E., Troxel, M. A., Vielzeuf, P., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bleem, L. E., Brooks, D., Burke, D. L., Carlstrom, J. E., Kind, M. Carrasco, Carretero, J., Chang, C. L., Cho, H-M., Chown, R., Crites, A. T., Cunha, C. E., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Doel, P., Everett, W. B., Evrard, A. E., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., de Haan, T., Halverson, N. W., Harrington, N. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Knox, L., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A. T., Leitch, E. M., Lima, M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miller, C. J., Mocanu, L. M., Mohr, J. J., Natoli, T., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., and Zahn, O.

Abstract

Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise down to small angular scales, even where directly modeling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance $\Lambda$CDM model, we find a best fit lensing ratio amplitude of $A = 1.1 \pm 0.1$. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation., Comment: 17 pages, 11 figures

Published
2018
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198. Dark Energy Survey Year 1 Results: Cross-correlation between DES Y1 galaxy weak lensing and SPT+Planck CMB weak lensing

Author

Omori, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., Bleem, L. E., Cawthon, R., Choi, A., Chown, R., Crawford, T. M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T. F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M. M., Reichardt, C. L., Rozo, E., Samuroff, S., Sánchez, C., Secco, L. F., Sheldon, E., Simard, G., Troxel, M. A., Vielzeuf, P., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., George, E. M., Gruendl, R. A., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hollowood, D. L., Honscheid, K., Holzapfel, W. L., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A. T., Leitch, E. M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Mocanu, L. M., Mohr, J. J., Natoli, T., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schaffer, K. K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Wu, W. L. K., Zahn, O., Omori, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., Bleem, L. E., Cawthon, R., Choi, A., Chown, R., Crawford, T. M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T. F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M. M., Reichardt, C. L., Rozo, E., Samuroff, S., Sánchez, C., Secco, L. F., Sheldon, E., Simard, G., Troxel, M. A., Vielzeuf, P., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., George, E. M., Gruendl, R. A., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hollowood, D. L., Honscheid, K., Holzapfel, W. L., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A. T., Leitch, E. M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Mocanu, L. M., Mohr, J. J., Natoli, T., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schaffer, K. K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Wu, W. L. K., and Zahn, O.

Abstract

We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one (Y1) data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg$^{2}$. With the combined measurements from four source galaxy redshift bins, we reject the hypothesis of no lensing with a significance of $10.8\sigma$. When employing angular scale cuts, this significance is reduced to $6.8\sigma$, which remains the highest signal-to-noise measurement of its kind to date. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial $\Lambda$CDM model, finding $A = 0.99 \pm 0.17$. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the $\Lambda$CDM model, we obtain the marginalized constraints of $\Omega_{\rm m}=0.261^{+0.070}_{-0.051}$ and $S_{8}\equiv \sigma_{8}\sqrt{\Omega_{\rm m}/0.3} = 0.660^{+0.085}_{-0.100}$. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT and Planck data., Comment: 15 pages, 6 figures

Published
2018
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199. Dark Energy Survey Year 1 Results: Joint Analysis of Galaxy Clustering, Galaxy Lensing, and CMB Lensing Two-point Functions

Author

Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., and Zuntz, J.

Abstract

We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat $\Lambda$CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields $S_{8}\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3} = 0.782^{+0.019}_{-0.025}$ and $\Omega_{\rm m}=0.260^{+0.029}_{-0.019}$. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat $\Lambda$CDM models. Combining constraints from all six two-point functions yields $S_{8}=0.776^{+0.014}_{-0.021}$ and $\Omega_{\rm m}= 0.271^{+0.022}_{-0.016}$. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis., Comment: 20 pages, 7 figures

Published
2018
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200. Year two instrument status of the SPT-3G cosmic microwave background receiver

Author

Bender, A. N., Ade, P. A. R., Ahmed, Z., Anderson, A. J., Avva, J. S., Aylor, K., Barry, P. S., Thakur, R. Basu, Benson, B. A., Bleem, L. S., Bocquet, S., Byrum, K., Carlstrom, J. E., Carter, F. W., Cecil, T. W., Chang, C. L., Cho, H. -M., Cliche, J. F., Crawford, T. M., Cukierman, A., de Haan, T., Denison, E. V., Ding, J., Dobbs, M. A., Dodelson, S., Dutcher, D., Everett, W., Foster, A., Gallicchio, J., Gilbert, A., Groh, J. C., Guns, S. T., Halverson, N. W., Harke-Hosemann, A. H., Harrington, N. L., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Huang, N., 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., Lowitz, A. E., Meyer, S. S., Michalik, D., Montgomery, J., Nadolski, A., Natoli, T., Nguyen, H., Noble, G. I., Novosad, V., Padin, S., Pan, Z., Pearson, J., Posada, C. M., Quan, W., Raghunathan, S., Rahlin, A., Reichardt, C. L., Ruhl, J. E., Sayre, J. T., Shirokoff, E., Smecher, G., Sobrin, J. A., Stark, A. A., Story, K. T., Suzuki, A., Thompson, K. L., Tucker, C., Vale, L. R., Vanderlinde, K., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Yoon, K. W., Young, M. R., Bender, A. N., Ade, P. A. R., Ahmed, Z., Anderson, A. J., Avva, J. S., Aylor, K., Barry, P. S., Thakur, R. Basu, Benson, B. A., Bleem, L. S., Bocquet, S., Byrum, K., Carlstrom, J. E., Carter, F. W., Cecil, T. W., Chang, C. L., Cho, H. -M., Cliche, J. F., Crawford, T. M., Cukierman, A., de Haan, T., Denison, E. V., Ding, J., Dobbs, M. A., Dodelson, S., Dutcher, D., Everett, W., Foster, A., Gallicchio, J., Gilbert, A., Groh, J. C., Guns, S. T., Halverson, N. W., Harke-Hosemann, A. H., Harrington, N. L., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Huang, N., 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., Lowitz, A. E., Meyer, S. S., Michalik, D., Montgomery, J., Nadolski, A., Natoli, T., Nguyen, H., Noble, G. I., Novosad, V., Padin, S., Pan, Z., Pearson, J., Posada, C. M., Quan, W., Raghunathan, S., Rahlin, A., Reichardt, C. L., Ruhl, J. E., Sayre, J. T., Shirokoff, E., Smecher, G., Sobrin, J. A., Stark, A. A., Story, K. T., Suzuki, A., Thompson, K. L., Tucker, C., Vale, L. R., Vanderlinde, K., Vieira, J. D., Wang, G., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Yoon, K. W., and Young, M. R.

Abstract

The South Pole Telescope (SPT) is a millimeter-wavelength telescope designed for high-precision measurements of the cosmic microwave background (CMB). The SPT measures both the temperature and polarization of the CMB with a large aperture, resulting in high resolution maps sensitive to signals across a wide range of angular scales on the sky. With these data, the SPT has the potential to make a broad range of cosmological measurements. These include constraining the effect of massive neutrinos on large-scale structure formation as well as cleaning galactic and cosmological foregrounds from CMB polarization data in future searches for inflationary gravitational waves. The SPT began observing in January 2017 with a new receiver (SPT-3G) containing $\sim$16,000 polarization-sensitive transition-edge sensor bolometers. Several key technology developments have enabled this large-format focal plane, including advances in detectors, readout electronics, and large millimeter-wavelength optics. We discuss the implementation of these technologies in the SPT-3G receiver as well as the challenges they presented. In late 2017 the implementations of all three of these technologies were modified to optimize total performance. Here, we present the current instrument status of the SPT-3G receiver., Comment: 21 pages, 9 Figures, Presented at SPIE Astronomical Telescopes + Instrumentation 2018

Published
2018
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