Journal
ASTRONOMY & ASTROPHYSICS
Volume 624, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201935159
Keywords
cosmology: observations; large-scale structure of Universe; cosmic background radiation; intergalactic medium
Categories
Funding
- Edinburgh School of Physics and Astronomy Career Development Summer Scholarship
- RSE Cormack Vacation Research Scholarship
- European Research Council [670193, 647112]
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- European Research Council (ERC) [647112] Funding Source: European Research Council (ERC)
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Observations of galaxies and galaxy clusters in the local universe can account for only similar to 10% of the total baryon content. Cosmological simulations predict that the missing baryons are spread throughout filamentary structures in the cosmic web, forming a low-density gas with temperatures of 10(5)-10(7)K. We search for this warm-hot intergalactic medium (WHIM) by stacking the Planck Compton y-parameter map of the thermal Sunyaev-Zel'dovich (tSZ) effect for 1 002 334 pairs of CMASS galaxies from the Sloan Digital Sky Survey. We model the contribution from the galaxy halo pairs assuming spherical symmetry, finding a residual tSZ signal at the 2.9 sigma level from a stacked filament of length 10.5 h(-1) Mpc with a Compton parameter magnitude y = (0.6 +/- 0.2)x 10(-8). We consider possible sources of contamination and conclude that bound gas in haloes may contribute only up to 20% of the measured filamentary signal. To estimate the filament gas properties we measure the gravitational lensing signal for the same sample of galaxy pairs; in combination with the tSZ signal, this yields an inferred gas density of rho(b) = (5.5 +/- 2.9) x (rho) over bar (b) with a temperature T = (2.7 +/- 1.7) x 10(6) K. This result is consistent with the predicted WHIM properties, and overall the filamentary gas can account for 11 +/- 7% of the total baryon content of the Universe. We also see evidence that the gas filament extends beyond the galaxy pair. Averaging over this longer baseline boosts the significance of the tSZ signal and increases the associated baryon content to 28 +/- 12% of the global value.
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