5 Conclusions
We have presented the SZE image of the Phoenix galaxy
cluster at z = 0.597 taken by ALMA in Band 3. The SZE is
imaged at 5 resolution (or 23 h−1 kpc) within 200 h−1 kpc
from the central AGN with a peak S/N exceeding 11. Combined with the Chandra X-ray image, the ALMA SZE data
further allow for non-parametric deprojection of electron
temperature, density, and entropy. Our method can minimize contamination by the central AGN and the X-ray
absorbing gas within the cluster, both of which largely affect
the X-ray spectrum.
We find no significant asymmetry or disturbance in the
SZE image within the current measurement errors. The
detected signal shows much higher central concentration
than other distant clusters and agrees well with the average
pressure profile of local cool-core clusters. Unlike in typical clusters at any redshift, the gas temperature drops by at
least a factor of 5 toward the center. In the inner 20 h−1 kpc,
we identify the presence of ∼6 × 1011 M cool gas with
kT ∼ 3 keV, the amount of which corresponds to ∼20%
of the stellar mass in the central galaxy. The low entropy
(∼10 keV cm2 ) and the short cooling time (∼0.1 Gyr) of
this gas further corroborates that radiative cooling is hardly
suppressed between kT ∼ 16 keV and kT ∼ 3 keV. Taken
together, our results imply that the gas is cooling efficiently
and nearly isobarically down to the inner 20 h−1 kpc in the
Phoenix cluster.
Acknowledgments
We thank the anonymous referee and Luca Di Mascolo for their
helpful comments. This paper makes use of the following ALMA
data: ADS/JAO.ALMA#2015.1.00894.S. The scientific results of
this paper are based in part on data obtained from the Chandra
Data Archive: ObsID 13401, 16135, 16545, 19581, 19582, 19583,
20630, 20631, 20634, 20635, 20636, and 20797. ALMA is a
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