Unveiling the merger dynamics of the most massive MaDCoWS cluster at $z = 1.2$ from a multi-wavelength mapping of its intracluster medium properties. (arXiv:1911.00560v1 [astro-ph.CO])

Unveiling the merger dynamics of the most massive MaDCoWS cluster at $z = 1.2$ from a multi-wavelength mapping of its intracluster medium properties. (arXiv:1911.00560v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ruppin_F/0/1/0/all/0/1">F. Ruppin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDonald_M/0/1/0/all/0/1">M. McDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brodwin_M/0/1/0/all/0/1">M. Brodwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adam_R/0/1/0/all/0/1">R. Adam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">P. Ade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andre_P/0/1/0/all/0/1">P. André</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrianasolo_A/0/1/0/all/0/1">A. Andrianasolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_M/0/1/0/all/0/1">M. Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aussel_H/0/1/0/all/0/1">H. Aussel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartalucci_I/0/1/0/all/0/1">I. Bartalucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bautz_M/0/1/0/all/0/1">M. W. Bautz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beelen_A/0/1/0/all/0/1">A. Beelen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_A/0/1/0/all/0/1">A. Benoît</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bideaud_A/0/1/0/all/0/1">A. Bideaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrion_O/0/1/0/all/0/1">O. Bourrion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvo_M/0/1/0/all/0/1">M. Calvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catalano_A/0/1/0/all/0/1">A. Catalano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comis_B/0/1/0/all/0/1">B. Comis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decker_B/0/1/0/all/0/1">B. Decker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petris_M/0/1/0/all/0/1">M. De Petris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desert_F/0/1/0/all/0/1">F.-X. Désert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doyle_S/0/1/0/all/0/1">S. Doyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Driessen_E/0/1/0/all/0/1">E. F. C. Driessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisenhardt_P/0/1/0/all/0/1">P. R. M. Eisenhardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_A/0/1/0/all/0/1">A. Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_A/0/1/0/all/0/1">A. H. Gonzalez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goupy_J/0/1/0/all/0/1">J. Goupy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keruzore_F/0/1/0/all/0/1">F. Kéruzoré</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_C/0/1/0/all/0/1">C. Kramer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ladjelate_B/0/1/0/all/0/1">B. Ladjelate</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">G. Lagache</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leclercq_S/0/1/0/all/0/1">S. Leclercq</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lestrade_J/0/1/0/all/0/1">J.-F. Lestrade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macias_Perez_J/0/1/0/all/0/1">J.F. Macías-Pérez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mauskopf_P/0/1/0/all/0/1">P. Mauskopf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayet_F/0/1/0/all/0/1">F. Mayet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monfardini_A/0/1/0/all/0/1">A. Monfardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moravec_E/0/1/0/all/0/1">E. Moravec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perotto_L/0/1/0/all/0/1">L. Perotto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pisano_G/0/1/0/all/0/1">G. Pisano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pointecouteau_E/0/1/0/all/0/1">E. Pointecouteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponthieu_N/0/1/0/all/0/1">N. Ponthieu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pratt_G/0/1/0/all/0/1">G. W. Pratt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reveret_V/0/1/0/all/0/1">V. Revéret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ritacco_A/0/1/0/all/0/1">A. Ritacco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_C/0/1/0/all/0/1">C. Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roussel_H/0/1/0/all/0/1">H. Roussel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schuster_K/0/1/0/all/0/1">K. Schuster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shu_S/0/1/0/all/0/1">S. Shu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sievers_A/0/1/0/all/0/1">A. Sievers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanford_S/0/1/0/all/0/1">S. A. Stanford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stern_D/0/1/0/all/0/1">D. Stern</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tucker_C/0/1/0/all/0/1">C. Tucker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zylka_R/0/1/0/all/0/1">R. Zylka</a>

The characterization of the Intra-Cluster Medium (ICM) properties of
high-redshift galaxy clusters is fundamental to our understanding of
large-scale structure formation processes. We present the results of a
multi-wavelength analysis of the very massive cluster MOO J1142$+$1527 at a
redshift $z = 1.2$ discovered as part of the Massive and Distant Clusters of
WISE Survey (MaDCoWS). This analysis is based on high angular resolution
$Chandra$ X-ray and NIKA2 Sunyaev-Zel’dovich (SZ) data. Although the X-ray data
have only about 1700 counts, we are able to determine the ICM thermodynamic
radial profiles, namely temperature, entropy, and hydrostatic mass. These have
been obtained with unprecedented precision at this redshift and up to
$0.7R_{500}$, thanks to the combination of high-resolution X-ray and SZ data.
The comparison between the galaxy distribution mapped in infrared by $Spitzer$
and the morphological properties of the ICM derived from the combined analysis
of the $Chandra$ and NIKA2 data leads us to the conclusion that the cluster is
an on-going merger. We measure the hydrostatic mass profile of the cluster in
four angular sectors centered on the large-scale X-ray centroid. This allows us
to estimate a systematic uncertainty on the cluster total mass that
characterizes both the impact of the observed deviations from spherical
symmetry and of the core dynamics on the mass profile. We further combine the
X-ray and SZ data at the pixel level to obtain maps of the temperature and
entropy distributions averaged along the line of sight. We find a relatively
low entropy core at the position of the X-ray peak and high temperature regions
located on its south and west sides. The increase in ICM temperature at the
location of the SZ peak is expected given the merger dynamics. (abridged)

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