Chandra Observations of the Planck ESZ Sample: A Re-Examination of Masses and Mass Proxies. (arXiv:2103.07545v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Andrade_Santos_F/0/1/0/all/0/1">Felipe Andrade-Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pratt_G/0/1/0/all/0/1">Gabriel W. Pratt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melin_J/0/1/0/all/0/1">Jean-Baptiste Melin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_M/0/1/0/all/0/1">Monique Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_C/0/1/0/all/0/1">Christine Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">William R. Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pointecouteau_E/0/1/0/all/0/1">Etienne Pointecouteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartalucci_I/0/1/0/all/0/1">Iacopo Bartalucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vikhlinin_A/0/1/0/all/0/1">Alexey Vikhlinin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murray_S/0/1/0/all/0/1">Stephen S. Murray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mazzotta_P/0/1/0/all/0/1">Pasquale Mazzotta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borgani_S/0/1/0/all/0/1">Stefano Borgani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lovisari_L/0/1/0/all/0/1">Lorenzo Lovisari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">Reinout J. van Weeren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph P. Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+David_L/0/1/0/all/0/1">Laurence P. David</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giacintucci_S/0/1/0/all/0/1">Simona Giacintucci</a>
Using Chandra observations, we derive the $Y_{rm X}$ proxy and associated
total mass measurement, $M_{500}^{rm Y_X}$, for 147 clusters with $z leq
0.35$ from the Planck Early Sunyaev-Zel’dovich catalog, and for 80 clusters
with $z leq 0.30$ from an X-ray flux-limited sample. We re-extract the Planck
$Y_{rm SZ}$ measurements and obtain the corresponding mass proxy,
$M_{500}^{rm SZ}$, from the full Planck mission maps, minimizing the Malmquist
bias due to observational scatter. The masses re-extracted using the more
precise X-ray position and characteristic size agree with the published PSZ2
values, but yield a significant reduction in the scatter (by a factor of two)
in the $M_{500}^{rm SZ}$-$M_{500}^{rm X}$ relation. The slope is
$0.93pm0.03$, and the median ratio, $M_{500}^{rm SZ}/M_{500}^{rm X}=
0.91pm0.01$, is within the expectations from known X-ray calibration
systematics. The $Y_{rm SZ}/Y_{rm X}$ ratio is $0.88pm0.02$, in good
agreement with predictions from cluster structure, and implying a low level of
clumpiness. In agreement with the findings of the Planck Collaboration, the
slope of the $Y_{rm SZ}$-$D_{rm A}^{-2} Y_{X}$ flux relation is significantly
less than unity ($0.89pm0.01$). Using extensive simulations, we show that this
result is not due to selection effects, intrinsic scatter, or covariance
between quantities. We demonstrate analytically that changing the $Y_{rm
SZ}$-$Y_{X}$ relation from apparent flux to intrinsic properties results in a
best-fit slope that is closer to unity and increases the dispersion about the
relation. The redistribution resulting from this transformation implies that
the best fit parameters of the $M_{500}^{rm SZ}$-$M_{500}^{rm X}$ relation
will be sample-dependent.
Using Chandra observations, we derive the $Y_{rm X}$ proxy and associated
total mass measurement, $M_{500}^{rm Y_X}$, for 147 clusters with $z leq
0.35$ from the Planck Early Sunyaev-Zel’dovich catalog, and for 80 clusters
with $z leq 0.30$ from an X-ray flux-limited sample. We re-extract the Planck
$Y_{rm SZ}$ measurements and obtain the corresponding mass proxy,
$M_{500}^{rm SZ}$, from the full Planck mission maps, minimizing the Malmquist
bias due to observational scatter. The masses re-extracted using the more
precise X-ray position and characteristic size agree with the published PSZ2
values, but yield a significant reduction in the scatter (by a factor of two)
in the $M_{500}^{rm SZ}$-$M_{500}^{rm X}$ relation. The slope is
$0.93pm0.03$, and the median ratio, $M_{500}^{rm SZ}/M_{500}^{rm X}=
0.91pm0.01$, is within the expectations from known X-ray calibration
systematics. The $Y_{rm SZ}/Y_{rm X}$ ratio is $0.88pm0.02$, in good
agreement with predictions from cluster structure, and implying a low level of
clumpiness. In agreement with the findings of the Planck Collaboration, the
slope of the $Y_{rm SZ}$-$D_{rm A}^{-2} Y_{X}$ flux relation is significantly
less than unity ($0.89pm0.01$). Using extensive simulations, we show that this
result is not due to selection effects, intrinsic scatter, or covariance
between quantities. We demonstrate analytically that changing the $Y_{rm
SZ}$-$Y_{X}$ relation from apparent flux to intrinsic properties results in a
best-fit slope that is closer to unity and increases the dispersion about the
relation. The redistribution resulting from this transformation implies that
the best fit parameters of the $M_{500}^{rm SZ}$-$M_{500}^{rm X}$ relation
will be sample-dependent.
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