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1. The XXL Survey: First Results and Future

Author

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, A, 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. S, Coupon, J, Delhaize, J, Delvecchio, I, Democles, J, Desai, Sh, 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, Ch, Lavoie, S, Le Fevre, J.-P, Lieu, M, Kilbinger, M, Marulli, F, Mantz, A, McGee, S, Melin, J.-B, Melnyk, O, Moscardini, L, Novak, M, Piconcelli, E, Poggianti, B, Pomarede, D, Pompei, E, Ponman, T, Ramos Ceja, M. E, Rana, P, Rapetti, D, Raychaudhury, S, Ricci, M, Rottgering, H, Sahlen, M, Sauvageot, J.-L, Schimd, C, Sereno, M, Smith, G. P, 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, M, Kalfountzou, E, Kay, S, La Franca, F, Okabe, N, Muzzin, A, Rettura, A, Ricci, F, Ridl, J, Risaliti, G, Takizawa, M, Thomas, P, and Truong, N

Subjects
Astrophysics
Abstract

The XXL survey currently covers two 25 deg2 patches with XMM observations of approximately 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(zeta less than 2) cluster, (zeta less than 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-lambda 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 zeta greater than1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.

Published
2017
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3. changing-look AGN NGC 1566 in quiescence with XMM-Newton: a nuclear starburst and an AGN competing in power?

Author

Tomás, L, Matzeu, G A, Jiménez Bailón, E, Kalfountzou, E, Santos-Lleó, M, Parker, M L, Ballo, L, Loiseau, N, Ehle, M, Rodríguez-Pascual, P, and González-Riestra, R

Subjects
SEYFERT galaxies, ACTIVE galactic nuclei, X-ray imaging, GALACTIC evolution, SOFT X rays, STAR formation, IONIZED gases, STARBURSTS
Abstract

Star formation accretion on to the super massive black holes (SMBHs) and feedback processes link the evolution of galaxies with their SMBHs. X-ray observations in the imaging and spectral regime have revealed to be an important tool to study the connection between nuclear activity and circumnuclear star formation in nearby active galactic nuclei (AGN). X-ray spectral diagnostics can lead to disentangle, which is the ionization mechanism in the central kiloparsecs of nearby AGN. In this paper, we investigate, by means of XMM-Newton observations, the nuclear X-ray emission of the changing-look AGN NGC 1566 during its quiescent state. European Photon Imaging Camera (EPIC) soft X-ray images show an extended arm-like morphology. A detailed analysis of the high-resolution Reflection Grating Spectrometer (RGS) and medium resolution EPIC spectra shows that the material concentrated in the central kiloparsecs region is not in the photoionization-dominated regime while the presence of collisionally ionized plasma is needed to explain the observed spectral features. In the inner region (∼1.5 kpc), the brightness of the collisionally ionized gas is comparable to the brightness of the photoionized gas: the inner region hosts a luminous starburst whose ionized gas shows up bright in the X-rays when the AGN is in quiescence. [ABSTRACT FROM AUTHOR]

Published
2022
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4. The Largest X-ray Selected Sample of z>3 AGNs: C-COSMOS & ChaMP

Author

Kalfountzou, E., Civano, F., Elvis, M., Trichas, M., and Green, P.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra C-COSMOS and ChaMP surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGN, over a wide range of rest frame 2-10 keV luminosities logL_{X}=43.3 - 46.0 erg s^{-1}. X-ray hardness rates show that ~39% of the sources are highly obscured, N_{H}>10^{22} cm^{-2}, in agreement with the ~37% of type-2 AGN found in our sample based on their optical classification. For ~26% of objects have mismatched optical and X-ray classifications. Using the 1/V_{max} method, we confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGN (N=27) at z > 4, it is found that both source number counts in the 0.5 -2 keV band and comoving space density are consistent with the expectation of a luminosity dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGN shows a constant ratio between the two types at z > 3. Our results for both AGN types at these redshifts are consistent with the expectations of LDDE model., Comment: 20 pages, 11 figures. Accepted to MNRAS

Published
2014

5. A high-velocity component to the complex absorption in IRAS 13349+2438.

Author

Parker, M L, Matzeu, G A, Guainazzi, M, Kalfountzou, E, Miniutti, G, Santos-Lleó, M, and Schartel, N

Subjects
ACTIVE galactic nuclei, ACTIVE galaxies, SEYFERT galaxies, SPACE telescopes, ARTIFICIAL satellites, STAR formation
Abstract

We present an analysis of XMM–Newton spectra of the low-redshift quasar IRAS 13349+2438. The Reflection Grating Spectrometer spectrum shows a large number of absorption lines from two zones of warm absorption, with velocities of ∼−600 km s−1, as noted by previous authors. Additionally, we find robust evidence from multiple Lyα absorption lines for a previously undiscovered ultrafast zone of absorption, with an outflow velocity of −0.13 ± 0.01 c. The warm absorbers and ultrafast outflow have similar mass outflow rates, around $$40{{\ \rm per\ cent}}$$ of the Eddington accretion rate, but the kinetic power is dominated by the high-velocity gas that has a power of $${\sim }4{{\ \rm per\ cent}}$$ of the Eddington luminosity.d [ABSTRACT FROM AUTHOR]

Published
2018
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6. EFOSC2 Spectroscopy of SWIRE-CDFS Galaxies

Author

Kalfountzou, E., Trichas, M., Rowan-Robinson, M., Clements, D., Babbedge, T., and Seiradakis, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the optical spectra of a sample of 34 SWIRE-CDFS sources observed with EFOSC2 on the ESO 3.6m Telescope. We have used the spectra and spectroscopic redshifts to validate our photometric redshift codes and SED template fitting methods. 12 of our sources are Infrared Luminous Galaxies. Of these, five belong to the class of ULIRGs and one to the class of HLIRGs with evidence of both an AGN and starburst component contributing to their extreme infrared luminosity for 3, starburst contributing for 1 and AGN contributing for 2 of them., 14 pages, 11 figures, 4 tables, accepted for publication in MNRAS

Published
2010

7. Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power.

Author

Kalfountzou, E., Stevens, J. A., Jarvis, M. J., Hardcastle, M. J., Wilner, D., Elvis, M., Page, M. J., Trichas, M., and Smith, D. J. B.

Subjects
*STELLAR mass, *ACTIVE galactic nuclei, *GALAXY formation, *RADIO jets (Astrophysics), *STELLAR luminosity function, *STAR formation
Abstract

Several studies support the existence of a link between the active galactic nucleus (AGN) and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1, which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that (1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, (2) the RLQs show an SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radioAGNtriggering is linked to star formation triggering, and (3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power. [ABSTRACT FROM AUTHOR]

Published
2017
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8. The largest X-ray-selected sample of z > 3 AGNs: C-COSMOS and ChaMP.

Author

Kalfountzou, E., Civano, F., Elvis, M., Trichas, M., and Green, P.

Subjects
*GALACTIC redshift, *ACTIVE galactic nuclei, *STELLAR evolution, *CLASSIFICATION, *LUMINOSITY distance, *STELLAR luminosity function
Abstract

We present results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra Cosmological Evolution Survey and Chandra Multi-wavelength Project surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame 2-10 keV luminosities log LX = 43.3-46.0 erg s-1. X-ray hardness rates show that ~39 per cent of the sources are highly obscured, NH > 1022 cm-2, in agreement with the ~37 per cent of type-2 AGNs found in our sample based on their optical classification. For ~26 per cent of objects have mismatched optical and X-ray classifications. Utilizing the 1/Vmax method, we confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both source number counts in the 0.5-2 keV band and comoving space density are consistent with the expectation of a luminosity-dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGNs shows a constant ratio between the two types at z > 3. Our results for both AGN types at these redshifts are consistent with the expectations of LDDE model. [ABSTRACT FROM AUTHOR]

Published
2014
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9. Herschel-ATLAS★: far-infrared properties of radio-loud and radio-quiet quasars.

Author

Kalfountzou, E., Stevens, J. A., Jarvis, M. J., Hardcastle, M. J., Smith, D. J. B., Bourne, N., Dunne, L., Ibar, E., Eales, S., Ivison, R. J., Maddox, S., Smith, M. W. L., Valiante, E., and de Zotti, G.

Subjects
*INFRARED radiation, *QUASARS, *RADIO waves, *STATISTICAL correlation, *LUMINOSITY, *RADIO jets (Astrophysics)
Abstract

We have constructed a sample of radio-loud and radio-quiet quasars from the Faint Images Radio Sky at Twenty-one centimetres and the Sloan Digital Sky Survey Data Release 7, over the Herschel-ATLAS Phase 1 area (9h, 12h and $14{^{h}_{.}}5$). Using a stacking analysis, we find a significant correlation between the far-infrared (FIR) luminosity and 1.4-GHz luminosity for radio-loud quasars. Partial correlation analysis confirms the intrinsic correlation after removing the redshift contribution, while for radio-quiet quasars, no partial correlation is found. Using a single-temperature grey-body model, we find a general trend of lower dust temperatures in case of radio-loud quasars compared to radio-quiet quasars. Also, radio-loud quasars are found to have almost constant mean values of dust mass along redshift and optical luminosity bins. In addition, we find that radio-loud quasars at lower optical luminosities tend to have on average higher FIR and 250-μm luminosity with respect to radio-quiet quasars with the same optical luminosites. Even if we use a two-temperature grey-body model to describe the FIR data, the FIR luminosity excess remains at lower optical luminosities. These results suggest that powerful radio jets are associated with star formation especially at lower accretion rates. [ABSTRACT FROM AUTHOR]

Published
2014
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10. Star formation in high-redshift quasars: excess [O ii] emission in the radio-loud population.

Author

Kalfountzou, E., Jarvis, M. J., Bonfield, D. G., and Hardcastle, M. J.

Subjects
*STAR formation, *REDSHIFT, *QUASARS, *STELLAR luminosity function
Abstract

ABSTRACT We investigate the [O ii] emission-line properties of 18 508 quasars at z < 1.6 drawn from the Sloan Digital Sky Survey (SDSS) quasar sample. The quasar sample has been separated into 1692 radio-loud and 16 816 radio-quiet quasars (hereafter RLQs and RQQs) matched in both redshift and i′-band absolute magnitude. We use the [O ii]λ3726 + 3729 line as an indicator of star formation. Based on these measurements we find evidence that star formation activity is higher in the RLQ population. The mean equivalent widths (EW) for [O ii] are EW([O ii])RL = 7.80 ± 0.30 Å and EW([O ii])RQ = 4.77 ± 0.06 Å for the RLQ and RQQ samples, respectively. The mean [O ii] luminosities are log10[ L([O ii])RL/W] = 34.31 ± 0.01 and log10[ L([O ii])RQ/W] = 34.192 ± 0.004 for the samples of RLQs and RQQs, respectively. Finally, to overcome possible biases in the EW measurements due to the continuum emission below the [O ii] line being contaminated by young stars in the host galaxy, we use the ratio of the [O ii] luminosity to rest-frame i′-band luminosity; in this case, we find for the RLQs log10[ L([O ii])RL/ Lopt] = −3.89 ± 0.01 and log10[ L([O ii])RQ/ Lopt] = −4.011 ± 0.004 for RQQs. However the results depend upon the optical luminosity of the quasar. RLQs and RQQs with the same high optical luminosity log10( Lopt/W) > 38.6 tend to have the same level of [O ii] emission. On the other hand, at lower optical luminosities log10( Lopt/W) < 38.6, there is a clear [O ii] emission excess for the RLQs. As an additional check of our results we use the [O iii] emission line as a tracer of the bolometric accretion luminosity, instead of the i′-band absolute magnitude, and we obtain similar results. Radio jets appear to be the main reason for the [O ii] emission excess in the case of RLQs. In contrast, we suggest active galactic nuclei feedback ensures that the two populations acquire the same [O ii] emission at higher optical luminosities. [ABSTRACT FROM AUTHOR]

Published
2012
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11. EFOSC2 spectroscopy of SWIRE-CDFS galaxies.

Author

Kalfountzou, E., Trichas, M., Rowan-Robinson, M., Clements, D., Babbedge, T., and Seiradakis, J. H.

Subjects
*SPECTRUM analysis, *OPTICAL spectroscopy, *FAINT Object Camera, *REDSHIFT, *ACTIVE galactic nuclei, *SPECTRAL energy distribution
Abstract

ABSTRACT We present the optical spectra of a sample of 34 Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE)- Chandra Deep Field South (CDFS) sources observed with the European Southern Observatory (ESO) Faint Object Spectrograph and Camera (EFOSC2) on the ESO 3.6-m telescope. We have used the spectra and spectroscopic redshifts to validate our photometric redshift codes and spectral energy distribution (SED) template fitting methods. 12 of our sources are infrared luminous galaxies. Of these, five belong to the class of ultraluminous infrared galaxies (ULIRGs) and one to the class of hyperluminous infrared galaxies (HLIRGs), with evidence of both an active galactic nucleus and a starburst component contributing to their extreme infrared luminosity for three, a starburst contributing for one and AGN contributing for two of them. [ABSTRACT FROM AUTHOR]

Published
2011
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12. The XXL survey: first results and future

Author

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., Brun, A. Le, 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. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., 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, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Bologna (OABO), University of Michigan [Ann Arbor], University of Michigan System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Anglo-Australian Observatory (AAO), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), University of Liverpool, National Astronomical Observatory of Japan (NAOJ), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Thessaloniki], Aristotle University of Thessaloniki, Argelander-Institut für Astronomie (AlfA), University of Zagreb, NASA Goddard Space Flight Center (GSFC), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, University of Victoria [Canada] (UVIC), Istanbul University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Physics [Oxford], University of Oxford [Oxford], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Indian Institute of Technology [Hyderabad] (IIT Hyderabad), University of Geneva [Switzerland], Uppsala University, INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), The University of Western Australia (UWA), University of Bologna, University of Chicago, University of Birmingham [Birmingham], CEA, DSM, SPP, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Padova (OAPD), European Southern Observatory (ESO), Lund University [Lund], University of Colorado [Boulder], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Yamagata University, Victoria University of Wellington, Roma Tre University, Hiroshima University, York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Sussex, Università degli Studi di Roma Tor Vergata [Roma], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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.S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., 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, Ch., Lavoie, S., Le Fevre, J.-P., Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., Mcgee, S., Melin, J.-B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ramos Ceja, M.E., Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlen, M., Sauvageot, J.-L., Schimd, C., Sereno, M., Smith, G.P., 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, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Corasaniti, P. S., Desai, S. h., Jones, C. h., Le Fevre, J. P., Maruili, F., Melin, J. B., Ramos Ceja, M. E., Sauvageot, J. L., Smith, G. P., Johnston Hollitt, M., LA FRANCA, Fabio, Ricci, Federica, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, Université de Genève = University of Geneva (UNIGE), Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, University of Bologna/Università di Bologna, Universiteit Leiden, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, X-ray: general, FOS: Physical sciences, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, XXL survey, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], clusters: general [galaxies], cosmological parameter, X-ray:general, cosmological parameters, general [X-ray], QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract

The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016

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