The XXL survey: First results and future

Pierre, M.; Adami, C.; Birkinshaw, M.; Chiappetti, L.; Ettori, S.; Evrard, A.; Faccioli, L.; Gastaldello, F.; Giles, P.; Horellou, C.; Iovino, A.; Koulouridis, E.; Lidman, C.; Le Brun, A.; Maughan, B.; Maurogordato, S.; McCarthy, I.; Miyazaki, S.; Pacaud, F.; Paltani, S.; Plionis, M.; Reiprich, T.; Sadibekova, T.; Smolcic, V.; Snowden, S.; Surdej, J.; Tsirou, M.; Vignali, C.; Willis, J.; Alis, S.; Altieri, B.; Baran, N.; Benoist, C.; Bongiorno, A.; Bremer, M.; Butler, A.; Cappi, A.; Caretta, C.; Ciliegi, P.; Clerc, N.; Corasaniti, P.; Coupon, J.; Delhaize, J.; Delvecchio, I.; Democles, J.; Desai, S.; Devriendt, J.; Dubois, Y.; Eckert, D.; Elyiv, A.; Farahi, A.; Ferraril, C.; Fotopoulou, S.; Forman, W.; Georgantopoulos, I.; Guglielmo, V.; Huynh, M.; Jerlin, N.; Jones, C.; Lavoie, S.; Le Fevre, J.; Lieu, M.; Kilbinger, M.; MaruIli, F.; Mantz, A.; McGee, S.; Melin, J.; Melnyk, O.; Moscardini, L.; Novak, M.; Piconcelli, E.; Poggianti, B.; Pomarede, D.; Pompei, E.; Ponman, T.; Ramos Ceja, M.; Rana, P.; Rapetti, D.; Raychaudhury, S.; Ricci, M.; Rottgering, H.; Sahlen, M.; Sauvageot, J.; Schimd, C.; Sereno, M.; Smith, G.; Umetsu, K.; Valageas, P.; Valotti, A.; Valtchanov, I.; Veropalumbo, A.; Ascaso, B.; Barnes, D.; De Petris, M.; Durret, F.; Donahue, M.; Ithana, M.; Jarvis, M.; Johnston-Hollitt, Melanie

doi:10.1002/asna.201713352

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Authors

Pierre, M.

Adami, C.

Birkinshaw, M.

Chiappetti, L.

Ettori, S.

Evrard, A.

Faccioli, L.

Gastaldello, F.

Giles, P.

Horellou, C.

Iovino, A.

Koulouridis, E.

Lidman, C.

Le Brun, A.

Maughan, B.

Maurogordato, S.

McCarthy, I.

Miyazaki, S.

Pacaud, F.

Paltani, S.

Plionis, M.

Reiprich, T.

Sadibekova, T.

Smolcic, V.

Snowden, S.

Surdej, J.

Tsirou, M.

Vignali, C.

Willis, J.

Alis, S.

Altieri, B.

Baran, N.

Benoist, C.

Bongiorno, A.

Bremer, M.

Butler, A.

Cappi, A.

Caretta, C.

Ciliegi, P.

Clerc, N.

Corasaniti, P.

Coupon, J.

Delhaize, J.

Delvecchio, I.

Democles, J.

Desai, S.

Devriendt, J.

Dubois, Y.

Eckert, D.

Elyiv, A.

Farahi, A.

Ferraril, C.

Fotopoulou, S.

Forman, W.

Georgantopoulos, I.

Guglielmo, V.

Huynh, M.

Jerlin, N.

Jones, C.

Lavoie, S.

Le Fevre, J.

Lieu, M.

Kilbinger, M.

MaruIli, F.

Mantz, A.

McGee, S.

Melin, J.

Melnyk, O.

Moscardini, L.

Novak, M.

Piconcelli, E.

Poggianti, B.

Pomarede, D.

Pompei, E.

Ponman, T.

Ramos Ceja, M.

Rana, P.

Rapetti, D.

Raychaudhury, S.

Ricci, M.

Rottgering, H.

Sahlen, M.

Sauvageot, J.

Schimd, C.

Sereno, M.

Smith, G.

Umetsu, K.

Valageas, P.

Valotti, A.

Valtchanov, I.

Veropalumbo, A.

Ascaso, B.

Barnes, D.

De Petris, M.

Durret, F.

Donahue, M.

Ithana, M.

Jarvis, M.

Johnston-Hollitt, Melanie

Date

2017

Type

Journal Article

Metadata

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Citation

Pierre, M. and Adami, C. and Birkinshaw, M. and Chiappetti, L. and Ettori, S. and Evrard, A. and Faccioli, L. et al. 2017. The XXL survey: First results and future. Astronomische Nachrichten. 338 (2-3): pp. 334-341.

Source Title

Astronomische Nachrichten

DOI

10.1002/asna.201713352

ISSN

0004-6337

School

Curtin Institute of Radio Astronomy (Physics)

URI

http://hdl.handle.net/20.500.11937/73060

Collection

Curtin Research Publications

Abstract

© 2017 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim The XXL survey currently covers two 25 deg2patches with XMM observations of ~10 ks. We summarize the scientific results associated with the first release of the XXL dataset, which occurred in mid-2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z < 2) cluster, (z < 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-? observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters, and the X-ray background. In particular, it will offer a unique opportunity to pinpoint the z > 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.