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SPT-3G D1: Maps of the millimeter-wave sky from 2019 and 2020 observations of the SPT-3G Main field

W. Quan, E. Camphuis, C. Daley, N. Huang, Y. Omori, F. Guidi, E. Anderes, A. J. Anderson, B. Ansarinejad, M. Archipley, L. Balkenhol, D. R. Barron, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, S. Bocquet, F. R. Bouchet, M. G. Campitiello, J. E. Carlstrom, J. Carron, C. L. Chang, P. M. Chichura, A. Chokshi, T. -L. Chou, A. Coerver, T. M. Crawford, T. de Haan, K. R. Dibert, M. A. Dobbs, M. Doohan, D. Dutcher, C. Feng, K. R. Ferguson, N. C. Ferree, K. Fichman, A. Foster, S. Galli, A. E. Gambrel, A. K. Gao, F. Ge, S. Guns, N. W. Halverson, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, A. Hryciuk, T. Jhaveri, F. Kéruzoré, A. R. Khalife, L. Knox, K. Kornoelje, C. -L. Kuo, K. Levy, Y. Li, A. E. Lowitz, C. Lu, G. P. Lynch, T. J. Maccarone, A. S. Maniyar, E. S. Martsen, F. Menanteau, M. Millea, J. Montgomery, Y. Nakato, T. Natoli, A. Ouellette, Z. Pan, P. Paschos, K. A. Phadke, A. W. Pollak, K. Prabhu, S. Raghunathan, M. Rahimi, A. Rahlin, C. L. Reichardt, M. Rouble, J. E. Ruhl, A. C. Silva Oliveira, A. Simpson, J. A. Sobrin, A. A. Stark, J. Stephen, C. Tandoi, C. Trendafilova, J. D. Vieira, A. G. Vieregg, A. Vitrier, Y. Wan, N. Whitehorn, W. L. K. Wu, M. R. Young, J. A. Zebrowski

Abstract

Maps of the sky in millimeter wavelengths contain rich information on cosmology through anisotropies of the cosmic microwave background (CMB). Creating multifrequency sky maps of anisotropies in the $I$, $Q$, and $U$ Stokes parameters is one of the first steps of CMB cosmology analyses. In this work, we describe the production and validation of a set of sky maps from the South Pole Telescope's third-generation camera, SPT-3G. The maps are from data taken in frequency bands centered at 95, 150, and 220 GHz and taken during the first two years, 2019 and 2020, of the SPT-3G Main survey, which covers $4\%$ of the sky. We applied high-pass filters to time series of individual detectors and binned the filtered time series samples into map pixels. After that, we calibrated and cleaned the maps to reduce known systematic errors. In addition, we searched for other systematic errors through null tests and mitigated a significant systematic error detected therein. The white noise levels of the full-depth maps of the $I$ Stokes parameter are $5.4$, $4.4$, and $16.2$ $\mathrm{μK}$-$\mathrm{arcmin}$ in the 95, 150, and 220 GHz bands, respectively, and $8.4$, $6.6$, and $25.8$ $\mathrm{μK}$-$\mathrm{arcmin}$ for $Q/U$. These maps are the deepest to date used for measurements of mid-to-high-$\ell$ primary temperature and $E$-mode polarization CMB anisotropies, and reconstructions of the CMB gravitational lensing potential. We make these maps and supporting data products publicly accessible.

SPT-3G D1: Maps of the millimeter-wave sky from 2019 and 2020 observations of the SPT-3G Main field

Abstract

Maps of the sky in millimeter wavelengths contain rich information on cosmology through anisotropies of the cosmic microwave background (CMB). Creating multifrequency sky maps of anisotropies in the , , and Stokes parameters is one of the first steps of CMB cosmology analyses. In this work, we describe the production and validation of a set of sky maps from the South Pole Telescope's third-generation camera, SPT-3G. The maps are from data taken in frequency bands centered at 95, 150, and 220 GHz and taken during the first two years, 2019 and 2020, of the SPT-3G Main survey, which covers of the sky. We applied high-pass filters to time series of individual detectors and binned the filtered time series samples into map pixels. After that, we calibrated and cleaned the maps to reduce known systematic errors. In addition, we searched for other systematic errors through null tests and mitigated a significant systematic error detected therein. The white noise levels of the full-depth maps of the Stokes parameter are , , and - in the 95, 150, and 220 GHz bands, respectively, and , , and - for . These maps are the deepest to date used for measurements of mid-to-high- primary temperature and -mode polarization CMB anisotropies, and reconstructions of the CMB gravitational lensing potential. We make these maps and supporting data products publicly accessible.
Paper Structure (50 sections, 32 equations, 25 figures, 6 tables)

This paper contains 50 sections, 32 equations, 25 figures, 6 tables.

Table of Contents

  1. Introduction
  2. Observations
  3. Field Observations
  4. Calibration Observations
  5. SPT-3G D1
  6. Mapmaking
  7. Filter-and-bin Method
  8. Filter-and-bin Parameters
  9. High-pass Filter Cutoff
  10. Masking in High-pass Filter
  11. Low-pass Filter
  12. Pointing
  13. Binning
  14. Other Pipelines
  15. Coadded Maps
  16. ...and 35 more sections

Figures (25)

  • Figure 1: The target uniform coverage region of the SPT-3G Main field (the light blue, approximately trapezoidal region) overlaid on top of the full-sky galactic dust map from Planck Public Data Release 3 (the background image) in the equatorial coordinate system and the Mollweide projection. The dust map is the Stokes $I$ map in the file COM_CompMap_IQU-thermaldust-gnilc-unires_2048_R3.00. fits downloaded from Planck Legacy Archive (https://pla.esac.esa.int/pla/).
  • Figure 2: The target uniform coverage region of the SPT-3G Main field and the footprint of each of the four subfields in a Lambert azimuthal equal-area projection (ZEA, a flat-sky projection, calabretta02). The subfields are the four shaded regions colored by the different hues. Three contours of constant right ascension ($\alpha$) and three contours of constant declination ($\delta$) are also shown.
  • Figure 3: The 2D $TT$ noise spectra in the 150 GHz band obtained from the four test mapmaking runs. The top left corner of each panel indicates the $\ell_{x,\,c}$ used in a particular mapmaking run. The color represents the logarithm of the noise power with an arbitrary normalization and is saturated in a large fraction of the bright region near the bottom left corner. The spherical harmonic coefficients are 0.0 in the gray region in each panel. This region is above the line $m \sim \ell\,\cos\,\delta_{\mathrm{low}}$, where $\delta_{\mathrm{low}}$ is the lowest declination covered by the SPT-3G Main field ($-40$ degrees). The high-$m$ modes in the gray region are concentrated near the equator of the spherical coordinates and have little overlap with the SPT-3G Main field. As a result, their spherical harmonic coefficients are practically zero.
  • Figure 4: The ratio of each 2D power spectrum shown in Figure \ref{['fig:noise_tt_alm_triangle']} to the power spectrum in the $\ell_{x,\,c}$ = 300 case along four constant-$\ell$ slices. Each panel shows the four ratios at a particular $\ell$, which is indicated in the upper right corner. The color of each ratio represents the spectrum used in the numerator. The denominator is the spectrum in the $\ell_{x,\,c}$ = 300 case for every ratio.
  • Figure 5: The first diagonal element of the weight map matrix associated with the 95 GHz full-field full coadd (top) and the cross section of the weight map along the contour of constant right ascension at $0^{\mathrm{h}}$ (bottom). The weight map is normalized to its maximum value. The contours of constant declination and those of constant right ascension in the top panel are the same as the ones shown in Figure \ref{['fig:survey_field_subdivision']}. In the bottom panel, each gray dashed cross section is the weight map associated with one subfield. The sum of the four gray cross sections is equal to the black cross section.
  • ...and 20 more figures