Details

Autor(en) / Beteiligte

• Hou, Z.
• Aylor, K.
• Benson, B. A.
• Bleem, L. E.
• Carlstrom, J. E.
• Chang, C. L.
• Cho, H-M.
• Chown, R.
• Crawford, T. M.
• Crites, A. T.
• de Haan, T.
• Dobbs, M. A.
• Everett, W. B.
• Follin, B.
• George, E. M.
• Halverson, N. W.
• Harrington, N. L.
• Holder, G. P.
• Holzapfel, W. L.
• Hrubes, J. D.
• Keisler, R.
• Knox, L.
• Lee, A. T.
• Leitch, E. M.
• Luong-Van, D.
• Marrone, D. P.
• McMahon, J. J.
• Meyer, S. S.
• Millea, M.
• Mocanu, L. M.
• Mohr, J. J.
• Natoli, T.
• Omori, Y.
• Padin, S.
• Pryke, C.
• Reichardt, C. L.
• Ruhl, J. E.
• Sayre, J. T.
• Schaffer, K. K.
• Shirokoff, E.
• Staniszewski, Z.
• Stark, A. A.
• Story, K. T.
• Vanderlinde, K.
• Vieira, J. D.
• Williamson, R.

Titel

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

Ist Teil von

• The Astrophysical journal, 2018-01, Vol.853 (1), p.3

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2018

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• We study the consistency of 150 GHz data from the South Pole Telescope (SPT) and 143 GHz data from the Planck satellite over the patch of sky covered by the SPT-SZ survey. We first visually compare the maps and find that the residuals appear consistent with noise after accounting for differences in angular resolution and filtering. We then calculate (1) the cross-spectrum between two independent halves of SPT data, (2) the cross-spectrum between two independent halves of Planck data, and (3) the cross-spectrum between SPT and Planck data. We find that the three cross-spectra are well fit (PTE = 0.30) by the null hypothesis in which both experiments have measured the same sky map up to a single free calibration parameter-i.e., we find no evidence for systematic errors in either data set. As a by-product, we improve the precision of the SPT calibration by nearly an order of magnitude, from 2.6% to 0.3% in power. Finally, we compare all three cross-spectra to the full-sky Planck power spectrum and find marginal evidence for differences between the power spectra from the SPT-SZ footprint and the full sky. We model these differences as a power law in spherical harmonic multipole number. The best-fit value of this tilt is consistent among the three cross-spectra in the SPT-SZ footprint, implying that the source of this tilt is a sample variance fluctuation in the SPT-SZ region relative to the full sky. The consistency of cosmological parameters derived from these data sets is discussed in a companion paper.