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Your search keyword '"Smolcic, V."' showing total 13 results
Start Over Author "Smolcic, V." Topic cosmology and nongalactic astrophysics (astro-ph.co)
13 results on '"Smolcic, V."'

1. The COSMOS2015 Catalog: Exploring the 1

Author

Laigle, C, McCracken, H, Ilbert, O, Hsieh, B, Davidzon, I, Capak, P, Hasinger, G, Silverman, J, Pichon, C, Coupon, J, Aussel, H, Le Borgne, D, Caputi, K, Cassata, P, Chang, Y, Civano, F, Dunlop, J, Fynbo, J, Kartaltepe, J, Koekemoer, A, Le Fèvre, O, Le Floc’H, E, Leauthaud, A, Lilly, S, Lin, L, Marchesi, S, Milvang-Jensen, B, Salvato, M, Sanders, D, Scoville, N, Smolcic, V, Stockmann, M, Taniguchi, Y, Tasca, L, Toft, S, Vaccari, M, and Zabl, J

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the COSMOS2015 catalog which contains precise photometric redshifts and stellar masses for more than half a million objects over the 2deg$^{2}$ COSMOS field. Including new $YJHK_{\rm s}$ images from the UltraVISTA-DR2 survey, $Y$-band from Subaru/Hyper-Suprime-Cam and infrared data from the Spitzer Large Area Survey with the Hyper-Suprime-Cam Spitzer legacy program, this near-infrared-selected catalog is highly optimized for the study of galaxy evolution and environments in the early Universe. To maximise catalog completeness for bluer objects and at higher redshifts, objects have been detected on a $��^{2}$ sum of the $YJHK_{\rm s}$ and $z^{++}$ images. The catalog contains $\sim 6\times 10^5$ objects in the 1.5 deg$^{2}$ UltraVISTA-DR2 region, and $\sim 1.5\times 10^5$ objects are detected in the "ultra-deep stripes" (0.62 deg$^{2}$) at $K_{\rm s}\leq 24.7$ (3$��$, 3", AB magnitude). Through a comparison with the zCOSMOS-bright spectroscopic redshifts, we measure a photometric redshift precision of $��_{��z/(1+z_s)}$ = 0.007 and a catastrophic failure fraction of $��=0.5$%. At $3, Accepted for publication in ApJ

Published
2016
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2. On the occupation of X-ray selected galaxy groups by radio AGN since z=1.3

Author

Smolcic, V., Finoguenov, A., Zamorani, G., Schinnerer, E., Tanaka, M., Giodini, S., and Scoville, N.

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

Previous clustering analysis of low-power radio AGN has indicated that they preferentially live in massive groups. The X-ray surveys of the COSMOS field have achieved a sensitivity at which these groups are directly detected out to z=1.3. Making use of Chandra-, XMM- and VLA-COSMOS surveys we identify radio AGN members (10**23.6 < L_1.4GHz/(W/Hz) < 10**25) of galaxy groups (10**13.2 < M_200/M_sun < 10**14.4; 0.1, Comment: 5 pages, 4 figures, accepted for publication in MNRAS Letters

Published
2011

3. The Molecular Gas Content of z<0.1 Radio Galaxies: Linking the AGN Accretion Mode to Host Galaxy Properties

Author

Smolcic, V. and Riechers, D. A.

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

One of the main achievements in modern cosmology is the so-called `unified model', which successfully describes most classes of active galactic nuclei (AGN) within a single physical scheme. However, there is a particular class of radio-luminous AGN that presently cannot be explained within this framework -- the `low-excitation' radio AGN (LERAGN). Recently, a scenario has been put forward which predicts that LERAGN, and their regular `high-excitation' radio AGN (HERAGN) counterparts represent different (red sequence vs. green valley) phases of galaxy evolution. These different evolutionary states are also expected to be reflected in their host galaxy properties, in particular their cold gas content. To test this, here we present CO(1-0) observations toward a sample of 11 of these systems conducted with CARMA. Combining our observations with literature data, we derive molecular gas masses (or upper limits) for a complete, representative, sample of 21 z, 8 pages, 4 figures, 4 tables; accepted for publication in ApJ

Published
2011
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4. Radio galaxy feedback in X-ray selected groups from COSMOS: the effect on the ICM

Author

Giodini, S., Smolcic, V., Finoguenov, A., Boehringer, H., Birzan, L., Zamorani, G., Oklopcic, A., Pierini, D., Pratt, G. W., Schinnerer, E., Massey, R., Koekemoer, A. M., Salvato, M., Sanders, D. B., Kartaltepe, J. S., and Thompson, D.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We quantify the importance of the mechanical energy released by radio-galaxies inside galaxy groups. We use scaling relations to estimate the mechanical energy released by 16 radio-AGN located inside X-ray detected galaxy groups in the COSMOS field. By comparing this energy output to the host groups' gravitational binding energy, we find that radio galaxies produce sufficient energy to unbind a significant fraction of the intra-group medium. This unbinding effect is negligible in massive galaxy clusters with deeper potential wells. Our results correctly reproduce the breaking of self-similarity observed in the scaling relation between entropy and temperature for galaxy groups., Accepted for publication in the Astrophysical Journal. 12 Pages

Published
2010

5. The VLA-COSMOS Perspective on the IR-Radio Relation. I. New Constraints on Selection Biases and the Non-Evolution of the IR/Radio Properties of Star Forming and AGN Galaxies at Intermediate and High Redshift

Author

Sargent, Mark T., Schinnerer, E., Murphy, E., Aussel, H., Floc'h, E. Le, Frayer, D. T., Mart��nez-Sansigre, A., Oesch, P., Salvato, M., Smolcic, V., Zamorani, G., Brusa, M., Cappelluti, N., Carollo, C. M., Ilbert, O., Kartaltepe, J., Koekemoer, A. M., Lilly, S. J., Sanders, D. B., and Scoville, N. Z.

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

VLA 1.4 GHz (rms noise ~0.012 mJy) and MIPS 24 and 70 micron (rms noise ~0.02 and ~1.7 mJy, respectively) observations covering the 2 square degree COSMOS field are combined with an extensive multi-wavelength data set to study the evolution of the IR-radio relation at intermediate and high redshift. With ~4500 sources -- of which ~30% have spectroscopic redshifts -- the current sample is significantly larger than previous ones used for the same purpose. Both monochromatic IR/radio flux ratios (q24 & q70), as well as the ratio of the total IR and the 1.4 GHz luminosity (qTIR) are used as indicators for the IR/radio properties of star forming galaxies and AGN. Using a sample jointly selected at IR and radio wavelengths in order to reduce selection biases, we provide firm support for previous findings that the IR-radio relation remains unchanged out to at least z~1.4. Moreover, based on data from ~150 objects we also find that the local relation likely still holds at 2.5, Comment: 52 pages, 23 figures (11 at reduced resolution). Accepted for publication in ApJS

Published
2010

6. No Evolution in the IR-Radio Relation for IR-Luminous Galaxies at z<2 in the COSMOS Field

Author

Sargent, Mark T., Schinnerer, E., Murphy, E., Carilli, C. L., Helou, G., Aussel, H., Floc'h, E. Le, Frayer, D. T., Ilbert, O., Oesch, P., Salvato, M., Smolcic, V., Kartaltepe, J., and Sanders, D. B.

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

Previous observational studies of the infrared (IR)-radio relation out to high redshift employed any detectable star forming systems at a given redshift within the restricted area of cosmological survey fields. Consequently, the evolution inferred relies on a comparison between the average IR/radio properties of (i) very IR-luminous high-z sources and (ii) more heterogeneous low(er)-z samples that often lack the strongest IR emitters. In this report we consider populations of objects with comparable luminosities over the last 10 Gyr by taking advantage of deep IR (esp. Spitzer 24 micron) and VLA 1.4 GHz observations of the COSMOS field. Consistent with recent model predictions, both Ultra Luminous Infrared Galaxies (ULIRGs) and galaxies on the bright end of the evolving IR luminosity function do not display any change in their average IR/radio ratios out to z~2 when corrected for bias. Uncorrected data suggested ~0.3 dex of positive evolution., 9 pages, 4 figures. Accepted for publication in ApJL.

Published
2010
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7. The radio AGN population dichotomy: Green valley Seyferts versus red sequence low-excitation AGN

Author

Smolcic, V.

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

Radio outflows of active galactic nuclei (AGN) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently it has been suggested that the two major radio AGN populations -- the powerful high-excitation, and the weak low-excitation radio AGN (HERAGN and LERAGN, resp.) -- represent two earlier and later stages of massive galaxy build-up. To test this, here we make use of a local (0.04, Comment: 5 pages, 4 figures, 1 table, to appear in ApJL

Published
2009
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8. 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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9. A JVLA 10~degree^2 deep survey

Author

Jarvis, M, Bhatnagar, S, Bruggen, M, Ferrari, C, Heywood, I, Hardcastle, M, Murphy, E, Taylor, R, Smirnov, O, Simpson, C, Smolcic, V, Stil, J, and Heyden, K

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged)One of the fundamental challenges for astrophysics in the 21st century is finding a way to untangle the physical processes that govern galaxy formation and evolution. Given the importance and scope of this problem, the multi-wavelength astronomical community has used the past decade to build up a wealth of information over specific extragalactic deep fields to address key questions in galaxy formation and evolution. These fields generally cover at least 10square degrees to facilitate the investigation of the rarest, typically most massive, galaxies and AGN. Furthermore, such areal coverage allows the environments to be fully accounted for, thereby linking the single halo to the two-halo terms in the halo occupation distribution. Surveys at radio wavelengths have begun to lag behind those at other wavelengths, especially in this medium-deep survey tier. However, the survey speed offered by the JVLA means that we can now reach a point where we can begin to obtain commensurate data at radio wavelengths to those which already exists from the X-ray through to the far-infrared over ~10 square degrees. We therefore present the case for a 10 square degree survey to 1.5uJy at L-band in A or B Array, requiring ~4000 hours to provide census of star-formation and AGN-accretion activity in the Universe. For example, the observations will allow galaxies forming stars at 10Msolar/yr to be detected out to z~1 and luminous infrared galaxies (1000Msolar/yr to be found out to z~6. Furthermore, the survey area ensures that we will have enough cosmic volume to find these rare sources at all epochs. The bandwidth will allow us to determine the polarisation properties galaxies in the high-redshift Universe as a function of stellar mass, morphology and redshift., 18 pages, 6 figures. White Paper submitted to the call for Very Large Array Sky Surveys

10. HST/ACS Morphology of Lyman Alpha Emitters at Redshift 5.7 in the COSMOS Field

Author

Taniguchi, Y., Murayama, T., Scoville, N. Z., Sasaki, S. S., Nagao, T., Shioya, Y., Saito, T., Ideue, Y., Nakajima, A., Matsuoka, K., Sanders, D. B., Mobasher, B., Aussel, H., Capak, P., Salvato, M., Koekemoer, A., Carilli, C., Cimatti, A., Ellis, R. S., Bianca Garilli, Giavalisco, M., Ilbert, O., Impey, C. D., Kitzbichler, M. G., Le Fevre, O., Mccracken, H. J., Scarlata, C., Schinnerer, E., Smolcic, V., Tribiano, S., and Trump, J. R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present detailed morphological properties of Lyman alpha emitters (LAEs) at z~ 5.7 in the COSMOS field, based on {\it Hubble Space Telescope} Advanced Camera for Surveys (ACS) data. The ACS imaging in the F814W filter covered 85 LAEs of the 119 LAEs identified in the full two square degree field, and 47 LAEs of them are detected in the ACS images. Nearly half of them are spatially extended with a size larger than 0.15 arcsec (~0.88 kpc at z=5.7) up to 0.4 arcsec (~2.5 kpc at z=5.7). The others are nearly unresolved compact objects. Two LAEs show double-component structures, indicating interaction or merging of building components to form more massive galaxies. By stacking the ACS images of all the detected sources, we obtain a Sersic parameter of n~0.7 with a half-light radius of 0.13 arcsec (0.76 kpc), suggesting that the majority of ACS detected LAEs have not spheroidal-like but disk-like or irregular light profiles. Comparing ACS F814W magnitudes (I_814) with Subaru/Suprime-Cam magnitudes in the NB816, i', and z' bands, we find that the ACS imaging in the F814W band mainly probes UV continuum rather than Lyman alpha line emission. UV continuum sizes tend to be larger for LAEs with larger Ly\alpha emission regions as traced by the NB816 imaging. The non-detection of 38 LAEs in the ACS images is likely due to the fact that their surface brightness is even too low both in the UV continuum and Lyalpha emission. Estimating I_814 for the LAEs with ACS non-detection from the z' and NB816 magnitudes, we find that 16 of these are probably LAEs with a size larger than 0.15 arcsec in UV continuum. All these results suggest that our LAE sample contains systematically larger LAEs in UV continuum size than those previously studied at z~6., Comment: 71 pages, 18 figures. Accepted for pulication in ApJ. High resolution paper: http://cosmos.phys.sci.ehime-u.ac.jp/~murayama/COSMOS/cosmos-lae57-acs.pdf

11. Radio selection of the most distant galaxy clusters

Author

R. T. Coogan, Ivan Delvecchio, Veronica Strazzullo, A. Calabrò, David Elbaz, Eva Schinnerer, Mark Sargent, Vernesa Smolčić, R. Gobat, Emanuele Daddi, Tao Wang, Chiara Ferrari, Francesco Valentino, Daizhong Liu, J. Delhaize, Mladen Novak, Qiusheng Gu, Shuowen Jin, 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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)-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)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Daddi, E, Jin, S, Strazzullo, V, Sargent, Mt, Wang, T, Ferrari, C, Schinnerer, E, Smolcic, V, Calabro, A, Coogan, R, Delhaize, J, Delvecchio, I, Elbaz, D, Gobat, R, Gu, Q, Liu, D, Novak, M, Valentino, F, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, formation [galaxies], PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Cluster (physics), galaxies: formation, clusters: general [galaxies], NATURAL SCIENCES. Physics. Astronomy and Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, evolution [galaxies], QB, Physics, radio continuum: galaxies, 010308 nuclear & particles physics, Star formation, galaxies: clusters: general, galaxies: evolution, galaxies: formation, galaxies: high-redshift, radio continuum: galaxies, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, First generation, galaxies [radio continuum], Square degree, galaxies: clusters: general, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxie [radio continuum], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies]
Abstract

We show that the most distant X-ray detected cluster known to date, ClJ1001 at z=2.506, hosts a strong overdensity of radio sources. Six of them are individually detected (within 10") in deep 0.75" resolution VLA 3GHz imaging, with S(3GHz)>8uJy. Of the six, AGN likely affects the radio emission in two galaxies while star formation is the dominant source powering the remaining four. We searched for cluster candidates over the full COSMOS 2-square degree field using radio-detected 3GHz sources and looking for peaks in Sigma5 density maps. ClJ1001 is the strongest overdensity by far with >10sigma, with a simple z_phot>1.5 preselection. A cruder photometric rejection of z2.5. Samples of hundreds such high-redshift clusters could potentially constrain cosmological parameters and test cluster and galaxy formation models., ApJ Letters in press

Published
2017
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12. The Chandra COSMOS Legacy survey: optical/IR identifications

Author

Stephanie M. LaMassa, Takamitsu Miyaji, Vernesa Smolčić, Knud Jahnke, Hyewon Suh, Ezequiel Treister, Piero Ranalli, Kevin Schawinski, Benny Trakhtenbrot, Viola Allevato, C. Cardamone, Alexis Finoguenov, Mara Salvato, Clotilde Laigle, Alexander Karim, Günther Hasinger, G. Zamorani, S. Marchesi, Martin Elvis, Marcella Brusa, Nico Cappelluti, Cristian Vignali, Richard E. Griffiths, John D. Silverman, Giorgio Lanzuisi, Andrea Comastri, Eva Schinnerer, Roberto Gilli, C. M. Urry, Francesca Civano, ITA, USA, FRA, DEU, CHL, HRV, FIN, JPN, MEX, SWE, CHE, Marchesi, S., Civano, F., Elvis, M., Salvato, M., Brusa, M., Comastri, A., Gilli, R., Hasinger, G., Lanzuisi, G., Miyaji, T., Treister, E., Urry, C.M., Vignali, C., Zamorani, G., Allevato, V., Cappelluti, N., Cardamone, C., Finoguenov, A., Griffiths, R.E., Karim, A., Laigle, C., Lamassa, S.M., Jahnke, K., Ranalli, P., Schawinski, K., Schinnerer, E., Silverman, J.D., Smolcic, V., Suh, H., Trakhtenbrot, B., Urry, C. M., Griffiths, R. E., Lamassa, S. M., Silverman, J. D., and Department of Physics

Subjects
catalogs, cosmology: observations, galaxies: active, galaxies: evolution, surveys, X-rays: general, COMPTON-THICK AGN, catalog, Infrared, X-RAY SOURCES, Astrophysics, 01 natural sciences, Luminosity, general [X-rays], 010303 astronomy & astrophysics, Photometric redshift, Physics, observations [cosmology], PRIRODNE ZNANOSTI. Fizika, ROSAT DEEP SURVEY, active [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, WIDE-FIELD SURVEY, observation [cosmology], ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometry (optics), SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, STAR-FORMING GALAXIES, survey, evolution [galaxies], Astrophysics::Galaxy Astrophysics, EVOLUTION SURVEY COSMOS, Supermassive black hole, cosmology: observation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, NATURAL SCIENCES. Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MEDIUM-SENSITIVITY SURVEY
Abstract

We present the catalog of optical and infrared counterparts of the Chandra COSMOS-Legacy Survey, a 4.6 Ms Chandra program on the 2.2 square degrees of the COSMOS field, combination of 56 new overlapping observations obtained in Cycle 14 with the previous C-COSMOS survey. In this Paper we report the i, K, and 3.6 micron identifications of the 2273 X-ray point sources detected in the new Cycle 14 observations. We use the likelihood ratio technique to derive the association of optical/infrared (IR) counterparts for 97% of the X-ray sources. We also update the information for the 1743 sources detected in C-COSMOS, using new K and 3.6 micron information not available when the C-COSMOS analysis was performed. The final catalog contains 4016 X-ray sources, 97% of which have an optical/IR counterpart and a photometric redshift, while 54% of the sources have a spectroscopic redshift. The full catalog, including spectroscopic and photometric redshifts and optical and X-ray properties described here in detail, is available online. We study several X-ray to optical (X/O) properties: with our large statistics we put better constraints on the X/O flux ratio locus, finding a shift towards faint optical magnitudes in both soft and hard X-ray band. We confirm the existence of a correlation between X/O and the the 2-10 keV luminosity for Type 2 sources. We extend to low luminosities the analysis of the correlation between the fraction of obscured AGN and the hard band luminosity, finding a different behavior between the optically and X-ray classified obscured fraction., Comment: 28 pages, 14 figures, accepted to ApJ

Published
2016
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13. X-ray properties of radio-selected star forming galaxies in the Chandra-COSMOS survey

Author

I. Georgantopoulos, Eva Schinnerer, Piero Ranalli, Roberto Gilli, Andrea Comastri, Nico Cappelluti, Cristian Vignali, F. Civano, Vernesa Smolčić, Gianni Zamorani, Ranalli P., Comastri A., Zamorani G., Cappelluti N., Civano F., Georgantopoulos I., Gilli R., Schinnerer E., Smolcic V., and Vignali C.

Subjects
Brightness, Radio Continuum: Galaxie, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Sample (material), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, Luminosity, galaxies: high-redshift, 0103 physical sciences, 010303 astronomy & astrophysics, galaxies: fundamental parameter, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, starburst [galaxies], Astronomy and Astrophysics, X-rays: galaxies, radio continuum: galaxies, galaxies: fundamental parameters, galaxies: star formation, Galaxy, Redshift, NATURAL SCIENCES. Physics, PRIRODNE ZNANOSTI. Fizika, Space and Planetary Science, active [galaxies], Cosmos (category theory), distances and redshifts [galaxies], X-rays: galaxie, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

X-ray surveys contain sizable numbers of star forming galaxies, beyond the AGN which usually make the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multiwavelength properties. We aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. We build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008) according to their optical colours and observed with Chandra. A similarly selected control sample of AGN is also used for comparison. We review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star forming galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, tough it is likely explained by a bias arising from the radio selection. Finally, we discuss the X-ray number counts of star forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys., Comment: 15 pages, 7 figures, 3 tables

Published
2012

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