Dark Energy Survey Year 1 Results: Constraining Baryonic Physics in the Universe. (arXiv:2007.15026v1 [astro-ph.CO])

Dark Energy Survey Year 1 Results: Constraining Baryonic Physics in the Universe. (arXiv:2007.15026v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Huang_H/0/1/0/all/0/1">Hung-Jin Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eifler_T/0/1/0/all/0/1">Tim Eifler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandelbaum_R/0/1/0/all/0/1">Rachel Mandelbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernstein_G/0/1/0/all/0/1">Gary M. Bernstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_A/0/1/0/all/0/1">Anqi Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_A/0/1/0/all/0/1">Ami Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">Juan Garc&#xed;a-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huterer_D/0/1/0/all/0/1">Dragan Huterer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krause_E/0/1/0/all/0/1">Elisabeth Krause</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozo_E/0/1/0/all/0/1">Eduardo Rozo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Singh_S/0/1/0/all/0/1">Sukhdeep Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bridle_S/0/1/0/all/0/1">Sarah Bridle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeRose_J/0/1/0/all/0/1">Joseph DeRose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elvin_Pole_J/0/1/0/all/0/1">Jack Elvin-Pole</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_X/0/1/0/all/0/1">Xiao Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Friedrich_O/0/1/0/all/0/1">Oliver Friedrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gatti_M/0/1/0/all/0/1">Marco Gatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaztanaga_E/0/1/0/all/0/1">Enrique Gaztanaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruen_D/0/1/0/all/0/1">Daniel Gruen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartley_W/0/1/0/all/0/1">Will Hartley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoyle_B/0/1/0/all/0/1">Ben Hoyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jarvis_M/0/1/0/all/0/1">Mike Jarvis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacCrann_N/0/1/0/all/0/1">Niall MacCrann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rau_M/0/1/0/all/0/1">Markus Rau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miranda_V/0/1/0/all/0/1">Vivian Miranda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prat_J/0/1/0/all/0/1">Judit Prat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_C/0/1/0/all/0/1">Carles S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Samuroff_S/0/1/0/all/0/1">Simon Samuroff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Troxel_M/0/1/0/all/0/1">Michael Troxel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zuntz_J/0/1/0/all/0/1">Joe Zuntz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">Tim Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguena_M/0/1/0/all/0/1">Michel Aguena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">James Annis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">Santiago Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_M/0/1/0/all/0/1">Matthew Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">Emmanuel Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">David Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">David Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">Aurelio Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">Matias Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">Jorge Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castander_F/0/1/0/all/0/1">Francisco Javier Castander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">Luiz da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">Juan De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_J/0/1/0/all/0/1">J&#xf6;rg Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">Peter Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_S/0/1/0/all/0/1">Spencer Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaugher_B/0/1/0/all/0/1">Brenna Flaugher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fosalba_P/0/1/0/all/0/1">Pablo Fosalba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">Josh Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruendl_R/0/1/0/all/0/1">Robert Gruendl</a>, et al. (26 additional authors not shown)

Measurements of large-scale structure are interpreted using theoretical
predictions for the matter distribution, including potential impacts of
baryonic physics. We constrain the feedback strength of baryons jointly with
cosmology using weak lensing and galaxy clustering observables (3$times$2pt)
of Dark Energy Survey (DES) Year 1 data in combination with external
information from baryon acoustic oscillations (BAO) and Planck cosmic microwave
background polarization. Our baryon modeling is informed by a set of
hydrodynamical simulations that span a variety of baryon scenarios; we span
this space via a Principal Component (PC) analysis of the summary statistics
extracted from these simulations. We show that at the level of DES Y1
constraining power, one PC is sufficient to describe the variation of baryonic
effects in the observables, and the first PC amplitude ($Q_1$) generally
reflects the strength of baryon feedback. With the upper limit of $Q_1$ prior
being bound by the Illustris feedback scenarios, we reach $sim 20%$
improvement in the constraint of $S_8=sigma_8(Omega_{rm
m}/0.3)^{0.5}=0.788^{+0.018}_{-0.021}$ compared to the original DES
3$times$2pt analysis. This gain is driven by the inclusion of small-scale
cosmic shear information down to 2.5$arcmin$, which was excluded in previous
DES analyses that did not model baryonic physics. We obtain
$S_8=0.781^{+0.014}_{-0.015}$ for the combined DES Y1+Planck EE+BAO analysis
with a non-informative $Q_1$ prior. In terms of the baryon constraints, we
measure $Q_1=1.14^{+2.20}_{-2.80}$ for DES Y1 only and
$Q_1=1.42^{+1.63}_{-1.48}$ for DESY1+Planck EE+BAO, allowing us to exclude one
of the most extreme AGN feedback hydrodynamical scenario at more than $2
sigma$.

Measurements of large-scale structure are interpreted using theoretical
predictions for the matter distribution, including potential impacts of
baryonic physics. We constrain the feedback strength of baryons jointly with
cosmology using weak lensing and galaxy clustering observables (3$times$2pt)
of Dark Energy Survey (DES) Year 1 data in combination with external
information from baryon acoustic oscillations (BAO) and Planck cosmic microwave
background polarization. Our baryon modeling is informed by a set of
hydrodynamical simulations that span a variety of baryon scenarios; we span
this space via a Principal Component (PC) analysis of the summary statistics
extracted from these simulations. We show that at the level of DES Y1
constraining power, one PC is sufficient to describe the variation of baryonic
effects in the observables, and the first PC amplitude ($Q_1$) generally
reflects the strength of baryon feedback. With the upper limit of $Q_1$ prior
being bound by the Illustris feedback scenarios, we reach $sim 20%$
improvement in the constraint of $S_8=sigma_8(Omega_{rm
m}/0.3)^{0.5}=0.788^{+0.018}_{-0.021}$ compared to the original DES
3$times$2pt analysis. This gain is driven by the inclusion of small-scale
cosmic shear information down to 2.5$arcmin$, which was excluded in previous
DES analyses that did not model baryonic physics. We obtain
$S_8=0.781^{+0.014}_{-0.015}$ for the combined DES Y1+Planck EE+BAO analysis
with a non-informative $Q_1$ prior. In terms of the baryon constraints, we
measure $Q_1=1.14^{+2.20}_{-2.80}$ for DES Y1 only and
$Q_1=1.42^{+1.63}_{-1.48}$ for DESY1+Planck EE+BAO, allowing us to exclude one
of the most extreme AGN feedback hydrodynamical scenario at more than $2
sigma$.

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