Skip to main content
Open Access Publications from the University of California

Cross-correlation of cmb polarization lensing with high-z submillimeter herschel-atlas galaxies

  • Author(s): Faúndez, MA;
  • Arnold, K;
  • Baccigalupi, C;
  • Barron, D;
  • Beck, D;
  • Bianchini, F;
  • Boettger, D;
  • Borrill, J;
  • Carron, J;
  • Cheung, K;
  • Chinone, Y;
  • Bouhargani, HE;
  • Elleflot, T;
  • Errard, J;
  • Fabbian, G;
  • Feng, C;
  • Galitzki, N;
  • Goeckner-Wald, N;
  • Hasegawa, M;
  • Hazumi, M;
  • Howe, L;
  • Kaneko, D;
  • Katayama, N;
  • Keating, B;
  • Krachmalnicoff, N;
  • Kusaka, A;
  • Lee, AT;
  • Leon, D;
  • Linder, E;
  • Lowry, LN;
  • Matsuda, F;
  • Minami, Y;
  • Navaroli, M;
  • Nishino, H;
  • Pham, ATP;
  • Poletti, D;
  • Puglisi, G;
  • Reichardt, CL;
  • Sherwin, BD;
  • Silva-Feaver, M;
  • Stompor, R;
  • Suzuki, A;
  • Tajima, O;
  • Takakura, S;
  • Takatori, S;
  • Teply, GP;
  • Tsai, C;
  • Vergès, C
  • et al.

We report a 4.8σ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the Polarbear experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of b=5.76\pm 1.25, corresponding to a host halo mass log10(Mh M⊙. =13.5+0.2-0.3 of at an effective redshift of z ∼ 2 from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the submillimeter galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extragalactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments.

Main Content
For improved accessibility of PDF content, download the file to your device.
Current View