Please use this identifier to cite or link to this item:
Title: The XXL Survey XLIV. Sunyaev-Zel’dovich mapping of a low-mass cluster at z ∼ 1: a multi-wavelength approach
Authors: Ricci, C.
Adam, R.
Eckert, D.
Ade, P.
André, P.
Andrianasolo, A.
Altieri, B.
Aussel, H.
Beelen, A.
Benoist, C.
Benoit, A.
Berta, S.
Bideaud, A.
Birkinshaw, M.
Bourrion, O.
Boutigny, D.
Bremer, M.
Calvo, M.
Cappi, A.
Chiappetti, L.
Catalano, A.
De Petris, M.
Désert, F. X.
Doyle, S.
Driessen, E. F. C.
Faccioli, L.
Ferrari, C.
Fotopoulou, S.
Gastaldello, F.
Giles, P.
Gómez, A.
Goupy, J.
Hahn, O.
Horellou, C.
Kéruzoré, F.
Koulouridis, E.
Kramer, C.
Ladjelate, B.
Lagache, G.
Leclercq, S.
Lestrade, J. F.
Marcías Pérez, J. F.
Maughan, B.
Maurogordato, S.
Mauskopf, P.
Monfardini, A.
Pacaud, F.
Perotto, L.
Pierre, M.
Pisano, G.
Pompei, E.
Ponthieu, N.
Revéret, V.
Ritacco, A.
Romero, C.
Roussel, H.
Ruppin, F.
Sánchez Portal, M.
Schuster, K.
Sereno, M.
Shu, S.
Slievers, A.
Tucker, C.
Umetsu, K.
Keywords: Techniques: high angular resolution;Galaxies: clusters: individual: XLSSC 102;Galaxies: cluster: intracluester medium;X-rays: galaxies: clusters
Issue Date: 13-Oct-2020
Publisher: EDP Sciences
DOI: 10.1051/0004-6361/201937249
Published version:
Citation: Astronomy and Astrophysics 642: A126(2020)
Abstract: High-mass clusters at low redshifts have been intensively studied at various wavelengths. However, while more distant objects at lower masses constitute the bulk population of future surveys, their physical state remain poorly explored to date. In this paper, we present resolved observations of the Sunyaev-Zel’dovich (SZ) effect, obtained with the NIKA2 camera, towards the cluster of galaxies XLSSC 102, a relatively low-mass system (M500 ∼ 2 × 1014 M⊙) at z = 0.97 detected from the XXL survey. We combine NIKA2 SZ data, XMM-Newton X-ray data, and Megacam optical data to explore, respectively, the spatial distribution of the gas electron pressure, the gas density, and the galaxies themselves. We find significant offsets between the X-ray peak, the SZ peak, the brightest cluster galaxy, and the peak of galaxy density. Additionally, the galaxy distribution and the gas present elongated morphologies. This is interpreted as the sign of a recent major merging event, which induced a local boost of the gas pressure towards the north of XLSSC 102 and stripped the gas out of the galaxy group. The NIKA2 data are also combined with XXL data to construct the thermodynamic profiles of XLSSC 102, obtaining relatively tight constraints up to about ∼r500, and revealing properties that are typical of disturbed systems. We also explore the impact of the cluster centre definition and the implication of local pressure substructure on the recovered profiles. Finally, we derive the global properties of XLSSC 102 and compare them to those of high-mass-and-low-redshift systems, finding no strong evidence for non-standard evolution. We also use scaling relations to obtain alternative mass estimates from our profiles. The variation between these different mass estimates reflects the difficulty to accurately measure the mass of low-mass clusters at z ∼ 1, especially with low signal-to-noise ratio data and for a disturbed system. However, it also highlights the strength of resolved SZ observations alone and in combination with survey-like X-ray data. This is promising for the study of high redshift clusters from the combination of eROSITA and high resolution SZ instruments and will complement the new generation of optical surveys from facilities such as LSST and Euclid.
Description: Based on observations carried out under project number 179-17 and 094-18, with the NIKA2 camera at the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.
E-ISSN: 1432-0746
ISSN: 0004-6361
Appears in Collections:(CAB) Artículos

Files in This Item:
File Description SizeFormat 
The XXL survey XLIV.pdf10,31 MBAdobe PDFThumbnail

This item is licensed under a Creative Commons License Creative Commons