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Start Over Author "Brusa, M." Journal monthly notices of the royal astronomical society
49 results on '"Brusa, M."'

1. The X-ray invisible Universe. A look into the halos undetected by eROSITA

Author

Popesso, P, primary, Biviano, A, additional, Bulbul, E, additional, Merloni, A, additional, Comparat, J, additional, Clerc, N, additional, Igo, Z, additional, Liu, A, additional, Driver, S, additional, Salvato, M, additional, Brusa, M, additional, Bahar, Y E, additional, Malavasi, N, additional, Ghirardini, V, additional, Robotham, A, additional, Liske, J, additional, and Grandis, S, additional

Published
2023
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2. The X-ray invisible Universe. A look into the haloes undetected by eROSITA.

Author

Popesso, P, Biviano, A, Bulbul, E, Merloni, A, Comparat, J, Clerc, N, Igo, Z, Liu, A, Driver, S, Salvato, M, Brusa, M, Bahar, Y E, Malavasi, N, Ghirardini, V, Robotham, A, Liske, J, and Grandis, S

Subjects
GALACTIC halos, SURFACE brightness (Astronomy), ACTIVE galactic nuclei, X-rays, GAS distribution, X-ray detection, UNIVERSE
Abstract

The paper presents the analysis of optically selected GAMA groups and clusters in the SRG/eROSITA X-ray map of eROSITA Final Equatorial Depth Survey, in the halo mass range 1013−5 × 1014 M⊙ and at z < 0.2. All X-ray detections have a clear GAMA counterpart, but most of the GAMA groups in the halo mass range 1013−1014 M⊙ remain undetected. We compare the X-ray surface brightness profiles of the eROSITA detected groups with the mean stacked profile of the undetected low-mass haloes at fixed halo mass. Overall, we find that the undetected groups exhibit less concentrated X-ray surface brightness, dark matter, and galaxy distributions with respect to the X-ray-detected haloes. The mean gas mass fraction profiles are consistent in the two samples within 1.5σ, indicating that the gas follows the dark matter profile. The low-mass concentration and the magnitude gap indicate that these systems are young. They reside with a higher probability in filaments while X-ray-detected groups favour the nodes of the Cosmic Web. Because of the lower central emission, the undetected systems tend to be X-ray underluminous at fixed halo mass and to lie below the LX − M halo relation. Interestingly, the X-ray-detected systems inhabiting the nodes scatter the less around the relation, while those in filaments tend to lie below it. We do not observe any strong relationship between the system X-ray appearance and the active galactic nucleus (AGN) activity. We cannot exclude the role of the past AGN feedback in affecting the gas distribution over the halo lifetime. However, the data suggests that the observed differences might be related to the halo assembly bias. [ABSTRACT FROM AUTHOR]

Published
2024
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3. A new emulated Monte Carlo radiative transfer disc-wind model: X-Ray Accretion Disc-wind Emulator – xrade

Author

Matzeu, G A, primary, Lieu, M, additional, Costa, M T, additional, Reeves, J N, additional, Braito, V, additional, Dadina, M, additional, Nardini, E, additional, Boorman, P G, additional, Parker, M L, additional, Sim, S A, additional, Barret, D, additional, Kammoun, E, additional, Middei, R, additional, Giustini, M, additional, Brusa, M, additional, Cabrera, J Pérez, additional, and Marchesi, S, additional

Published
2022
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4. new emulated Monte Carlo radiative transfer disc-wind model: X-Ray Accretion Disc-wind Emulator – xrade.

Author

Matzeu, G A, Lieu, M, Costa, M T, Reeves, J N, Braito, V, Dadina, M, Nardini, E, Boorman, P G, Parker, M L, Sim, S A, Barret, D, Kammoun, E, Middei, R, Giustini, M, Brusa, M, Cabrera, J Pérez, and Marchesi, S

Subjects
RADIATIVE transfer, SUPERVISED learning, X-ray spectra, X-rays, ARTIFICIAL neural networks, ACCRETION (Astrophysics)
Abstract

We present a new X-Ray Accretion Disc-wind Emulator (xrade) based on the 2.5D Monte Carlo radiative transfer code that provides a physically motivated, self-consistent treatment of both absorption and emission from a disc wind by computing the local ionization state and velocity field within the flow. xrade is then implemented through a process that combines X-ray tracing with supervised machine learning. We develop a novel emulation method consisting in training, validating, and testing the simulated disc-wind spectra into a purposely built artificial neural network. The trained emulator can generate a single synthetic spectrum for a particular parameter set in a fraction of a second, in contrast to the few hours required by a standard Monte Carlo radiative transfer pipeline. The emulator does not suffer from interpolation issues with multidimensional spaces that are typically faced by traditional X-ray fitting packages such as xspec. xrade will be suitable to a wide number of sources across the black hole mass, ionizing luminosity, and accretion rate scales. As an example, we demonstrate the applicability of xrade to the physical interpretation of the X-ray spectra of the bright quasar PDS 456, which hosts the best-established accretion disc wind observed to date. We anticipate that our emulation method will be an indispensable tool for the development of high-resolution theoretical models, with the necessary flexibility to be optimized for the next generation microcalorimeters onboard future missions, like X-Ray Imaging and Spectroscopy Mission (XRISM)/Resolve and Athena /X-ray Integral Field Unit (X-IFU). This tool can also be implemented across a wide variety of X-ray spectral models and beyond. [ABSTRACT FROM AUTHOR]

Published
2022
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6. The role of galaxy mass on AGN emission: a view from the VANDELS survey

Author

Magliocchetti, M, primary, Pentericci, L, primary, Cirasuolo, M, primary, Zamorani, G, primary, Amorin, R, primary, Bongiorno, A, primary, Cimatti, A, primary, Fontana, A, primary, Garilli, B, primary, Gargiulo, A, primary, Hathi, N P, primary, McLeod, D J, primary, McLure, R J, primary, Brusa, M, primary, Saxena, A, primary, and Talia, M, primary

Published
2020
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7. Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Author

Comparat, J, primary, Merloni, A, additional, Salvato, M, additional, Nandra, K, additional, Boller, T, additional, Georgakakis, A, additional, Finoguenov, A, additional, Dwelly, T, additional, Buchner, J, additional, Del Moro, A, additional, Clerc, N, additional, Wang, Y, additional, Zhao, G, additional, Prada, F, additional, Yepes, G, additional, Brusa, M, additional, Krumpe, M, additional, and Liu, T, additional

Published
2019
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10. The VANDELS ESO public spectroscopic survey

Author

McLure, R J, primary, Pentericci, L, additional, Cimatti, A, additional, Dunlop, J S, additional, Elbaz, D, additional, Fontana, A, additional, Nandra, K, additional, Amorin, R, additional, Bolzonella, M, additional, Bongiorno, A, additional, Carnall, A C, additional, Castellano, M, additional, Cirasuolo, M, additional, Cucciati, O, additional, Cullen, F, additional, De Barros, S, additional, Finkelstein, S L, additional, Fontanot, F, additional, Franzetti, P, additional, Fumana, M, additional, Gargiulo, A, additional, Garilli, B, additional, Guaita, L, additional, Hartley, W G, additional, Iovino, A, additional, Jarvis, M J, additional, Juneau, S, additional, Karman, W, additional, Maccagni, D, additional, Marchi, F, additional, Mármol-Queraltó, E, additional, Pompei, E, additional, Pozzetti, L, additional, Scodeggio, M, additional, Sommariva, V, additional, Talia, M, additional, Almaini, O, additional, Balestra, I, additional, Bardelli, S, additional, Bell, E F, additional, Bourne, N, additional, Bowler, R A A, additional, Brusa, M, additional, Buitrago, F, additional, Caputi, K I, additional, Cassata, P, additional, Charlot, S, additional, Citro, A, additional, Cresci, G, additional, Cristiani, S, additional, Curtis-Lake, E, additional, Dickinson, M, additional, Fazio, G G, additional, Ferguson, H C, additional, Fiore, F, additional, Franco, M, additional, Fynbo, J P U, additional, Galametz, A, additional, Georgakakis, A, additional, Giavalisco, M, additional, Grazian, A, additional, Hathi, N P, additional, Jung, I, additional, Kim, S, additional, Koekemoer, A M, additional, Khusanova, Y, additional, Fèvre, O Le, additional, Lotz, J M, additional, Mannucci, F, additional, Maltby, D T, additional, Matsuoka, K, additional, McLeod, D J, additional, Mendez-Hernandez, H, additional, Mendez-Abreu, J, additional, Mignoli, M, additional, Moresco, M, additional, Mortlock, A, additional, Nonino, M, additional, Pannella, M, additional, Papovich, C, additional, Popesso, P, additional, Rosario, D P, additional, Salvato, M, additional, Santini, P, additional, Schaerer, D, additional, Schreiber, C, additional, Stark, D P, additional, Tasca, L A M, additional, Thomas, R, additional, Treu, T, additional, Vanzella, E, additional, Wild, V, additional, Williams, C C, additional, Zamorani, G, additional, and Zucca, E, additional

Published
2018
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11. ALMA view of a massive spheroid progenitor: a compact rotating core of molecular gas in an AGN host at z = 2.226

Author

Talia, M, primary, Pozzi, F, additional, Vallini, L, additional, Cimatti, A, additional, Cassata, P, additional, Fraternali, F, additional, Brusa, M, additional, Daddi, E, additional, Delvecchio, I, additional, Ibar, E, additional, Liuzzo, E, additional, Vignali, C, additional, Massardi, M, additional, Zamorani, G, additional, Gruppioni, C, additional, Renzini, A, additional, Mignoli, M, additional, Pozzetti, L, additional, and Rodighiero, G, additional

Published
2018
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12. A Statistical Relation between the X-ray Spectral Index and Eddington Ratio of Active Galactic Nuclei in Deep Surveys

Author

Brightman, M., Silverman, J. D., Mainieri, V., Schramm, M., Steinhardt, C., Kartaltepe, J., Sanders, D. B., Treister, E., Shemmer, O., Brandt, W. N., Brusa, M., Comastri, A., Ho, L. C., Lanzuisi, G., Lusso, E., Nandra, K., Salvato, M., Zamorani, G., Alexander, D. M., Bongiorno, A., Capak, P., Civano, F., Del, Moro A., Elvis, M., Hasinger, G., Ueda, Y., Matsuoka, K., Nagao, T., Akiyama, M., Doi, Akihiro, M. Brightman, J. D. Silverman, V. Mainieri, Y. Ueda, M. Schramm, K. Matsuoka, T. Nagao, C. Steinhardt, J. Kartaltepe, D. B. Sander, E. Treister, O. Shemmer, W. N. Brandt, M. Brusa, A. Comastri, L. C. Ho, G. Lanzuisi, E. Lusso, K. Nandra, M. Salvato, G. Zamorani, M. Akiyama, D. M. Alexander, A. Bongiorno, P. Capak, F. Civano, A. . Moro, A. Doi, M. Elvi, G. Hasinger, E. S. Laird, D. Master, M. Mignoli, K. Ohta, K. Schawinski, and Y. Taniguchi

Subjects
Accretion, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies. [X-rays], galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, emission lines [Quasars], accretion, accretion disc, quasars: general, Bolometric correction, Emission spectrum, Accretion discs, Galaxies: Active, Galaxies: Nuclei, Quasars: Emission lines, Quasars: General, X-rays: galaxies, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Supermassive black hole, Astronomy, general [Quasars], Astronomy and Astrophysics, Quasar, Space and Planetary Science, nuclei [Galaxies], Chandra Deep Field South, Spectral energy distribution, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, quasars: emission line, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 36名, Accepted: 2013-05-22, 資料番号: SA1004651000

Published
2013

15. AGN-enhanced outflows of low-ionization gas in star-forming galaxies at 1.7 < z < 4.6*

Author

Talia, M., primary, Brusa, M., additional, Cimatti, A., additional, Lemaux, B. C., additional, Amorin, R., additional, Bardelli, S., additional, Cassarà, L. P., additional, Cucciati, O., additional, Garilli, B., additional, Grazian, A., additional, Guaita, L., additional, Hathi, N. P., additional, Koekemoer, A., additional, Le Fèvre, O., additional, Maccagni, D., additional, Nakajima, K., additional, Pentericci, L., additional, Pforr, J., additional, Schaerer, D., additional, Vanzella, E., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2017
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17. SPIDERS: selection of spectroscopic targets using AGN candidates detected in all-sky X-ray surveys

Author

Dwelly, T., primary, Salvato, M., additional, Merloni, A., additional, Brusa, M., additional, Buchner, J., additional, Anderson, S. F., additional, Boller, Th., additional, Brandt, W. N., additional, Budavári, T., additional, Clerc, N., additional, Coffey, D., additional, Del Moro, A., additional, Georgakakis, A., additional, Green, P. J., additional, Jin, C., additional, Menzel, M.-L., additional, Myers, A. D., additional, Nandra, K., additional, Nichol, R. C., additional, Ridl, J., additional, Schwope, A. D., additional, and Simm, T., additional

Published
2017
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20. A spectroscopic survey of X-ray-selected AGNs in the northern XMM-XXL field

Author

Menzel, M.-L., primary, Merloni, A., additional, Georgakakis, A., additional, Salvato, M., additional, Aubourg, E., additional, Brandt, W. N., additional, Brusa, M., additional, Buchner, J., additional, Dwelly, T., additional, Nandra, K., additional, Pâris, I., additional, Petitjean, P., additional, and Schwope, A., additional

Published
2016
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21. A census of radio-selected AGNs on the COSMOS field and of their FIR properties.

Author

Magliocchetti, M., Popesso, P., Brusa, M., and Salvato, M.

Subjects
WAVELENGTHS, STAR formation, PROBABILITY theory, ACTIVE galactic nuclei, RADIO sources (Astronomy)
Abstract

We use the new catalogue by Laigle et al. to provide a full census of VLA-COSMOS radio sources. We identify 90 per cent of such sources and sub-divide them into active galactic nuclei (AGNs) and star-forming galaxies on the basis of their radio luminosity. The AGN sample is complete with respect to radio selection at all z ≲ 3.5. Out of 704 AGNs, 272 have a counterpart in the Herschel maps. By exploiting the better statistics of the new sample, we confirm the results of Magliocchetti et al.: the probability for a radio-selected AGN to be detected at far-infrared (FIR) wavelengths is both a function of radio luminosity and redshift, whereby powerful sources are more likely FIR emitters at earlier epochs. Such an emission is due to star-forming processes within the host galaxy. FIR emitters and non-FIR emitters only differentiate in the z ≲ 1 universe. At higher redshifts, they are indistinguishable from each other, as there is no difference between FIR-emitting AGNs and star-forming galaxies. Lastly, we focus on radio AGNs which show AGN emission at other wavelengths. We find that midinfrared (MIR) emission is mainly associated with ongoing star formation and with sources which are smaller, younger and more radio luminous than the average parent population. X-ray emitters instead preferentially appear in more massive and older galaxies. We can therefore envisage an evolutionary track whereby the first phase of a radio-active AGN and of its host galaxy is associated with MIR emission, while at later stages the source becomes only active at radio wavelengths and possibly also in the X-ray. [ABSTRACT FROM AUTHOR]

Published
2018
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23. Mapping the average AGN accretion rate in the SFR–M* plane for Herschel★-selected galaxies at 0 < z ≤ 2.5

Author

Delvecchio, I., primary, Lutz, D., additional, Berta, S., additional, Rosario, D. J., additional, Zamorani, G., additional, Pozzi, F., additional, Gruppioni, C., additional, Vignali, C., additional, Brusa, M., additional, Cimatti, A., additional, Clements, D. L., additional, Cooray, A., additional, Farrah, D., additional, Lanzuisi, G., additional, Oliver, S., additional, Rodighiero, G., additional, Santini, P., additional, and Symeonidis, M., additional

Published
2015
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24. X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

Author

Brusa, M., primary, Bongiorno, A., additional, Cresci, G., additional, Perna, M., additional, Marconi, A., additional, Mainieri, V., additional, Maiolino, R., additional, Salvato, M., additional, Lusso, E., additional, Santini, P., additional, Comastri, A., additional, Fiore, F., additional, Gilli, R., additional, Franca, F. La, additional, Lanzuisi, G., additional, Lutz, D., additional, Merloni, A., additional, Mignoli, M., additional, Onori, F., additional, Piconcelli, E., additional, Rosario, D., additional, Vignali, C., additional, and Zamorani, G., additional

Published
2014
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25. Detection of faint broad emission lines in type 2 AGN - I. Near-infrared observations and spectral fitting.

Author

Onori, F., La Franca, F., Ricci, F., Brusa, M., Sani, E., Maiolino, R., Bianchi, S., Bongiorno, A., Fiore, F., Marconi, A., and Vignali, C.

Subjects
EMISSION-line galaxies, NEAR infrared radiation, SPECTROSCOPIC imaging, ACTIVE galactic nuclei, IR spectrometers
Abstract

We present medium resolution near-infrared spectroscopic observations of 41 obscured and intermediate class active galactic nuclei (AGN; type 2, 1.9 and 1.8; AGN2) with redshift z ≲ 0.1, selected from the Swift/Burst Alert Telescope 70-month catalogue. The observations have been carried out in the framework of a systematic study of theAGN2near-infrared spectral properties and have been executed using Infrared Spectrometer And Array Camera/VLT, X-shooter/VLT and LUCI/LBT, reaching an average S/N ratio of ~30 per resolution element. For those objects observed with X-shooter, we also obtained simultaneous optical and UV spectroscopy. We have identified a component from the broad line region in 13 out of 41AGN2, with full width at half-maximum (FWHM) > 800 km s-1. We have verified that the detection of the broad line region components does not significantly depend on selection effects due to the quality of the spectra, the X-ray or near-infrared fluxes, the orientation angle of the host galaxy or the hydrogen column density measured in the X-ray band. The average broad line region components found in AGN2 has a significantly (a factor 2) smaller FWHMif compared with a control sample of type 1 AGN. [ABSTRACT FROM AUTHOR]

Published
2017
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27. The MBH-M* relation for X-ray-obscured, red QSOs at 1.2 < z < 2.6

Author

Bongiorno, A., primary, Maiolino, R., additional, Brusa, M., additional, Marconi, A., additional, Piconcelli, E., additional, Lamastra, A., additional, Cano-Díaz, M., additional, Schulze, A., additional, Magnelli, B., additional, Vignali, C., additional, Fiore, F., additional, Menci, N., additional, Cresci,  G., additional, La Franca, F., additional, and Merloni, A., additional

Published
2014
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28. Black hole accretion preferentially occurs in gas-rich galaxies*

Author

Vito, F., primary, Maiolino, R., additional, Santini, P., additional, Brusa, M., additional, Comastri, A., additional, Cresci, G., additional, Farrah, D., additional, Franceschini, A., additional, Gilli, R., additional, Granato, G. L., additional, Gruppioni, C., additional, Lutz, D., additional, Mannucci, F., additional, Pozzi, F., additional, Rosario, D. J., additional, Scott, D., additional, Viero, M., additional, and Vignali, C., additional

Published
2014
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29. Evidence for two modes of black hole accretion in massive galaxies at z∼2

Author

Rangel, C., primary, Nandra, K., additional, Barro, G., additional, Brightman, M., additional, Hsu, L., additional, Salvato, M., additional, Koekemoer, A. M., additional, Brusa, M., additional, Laird, E. S., additional, Trump, J. R., additional, Croton, D. J., additional, Koo, D. C., additional, Kocevski, D., additional, Donley, J. L., additional, Hathi, N. P., additional, Peth, M., additional, Faber, S. M., additional, Mozena, M., additional, Grogin, N. A., additional, Ferguson, H. C., additional, and Lai, K., additional

Published
2014
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30. The incidence of obscuration in active galactic nuclei

Author

Merloni, A., primary, Bongiorno, A., additional, Brusa, M., additional, Iwasawa, K., additional, Mainieri, V., additional, Magnelli, B., additional, Salvato, M., additional, Berta, S., additional, Cappelluti, N., additional, Comastri, A., additional, Fiore, F., additional, Gilli, R., additional, Koekemoer, A., additional, Le Floc'h, E., additional, Lusso, E., additional, Lutz, D., additional, Miyaji, T., additional, Pozzi, F., additional, Riguccini, L., additional, Rosario, D. J., additional, Silverman, J., additional, Symeonidis, M., additional, Treister, E., additional, Vignali, C., additional, and Zamorani, G., additional

Published
2013
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32. The Chandra-COSMOS survey – IV. X-ray spectra of the bright sample

Author

Lanzuisi, G., primary, Civano, F., additional, Elvis, M., additional, Salvato, M., additional, Hasinger, G., additional, Vignali, C., additional, Zamorani, G., additional, Aldcroft, T., additional, Brusa, M., additional, Comastri, A., additional, Fiore, F., additional, Fruscione, A., additional, Gilli, R., additional, Ho, L. C., additional, Mainieri, V., additional, Merloni, A., additional, and Siemiginowska, A., additional

Published
2013
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33. Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies

Author

Bongiorno, A., primary, Merloni, A., additional, Brusa, M., additional, Magnelli, B., additional, Salvato, M., additional, Mignoli, M., additional, Zamorani, G., additional, Fiore, F., additional, Rosario, D., additional, Mainieri, V., additional, Hao, H., additional, Comastri, A., additional, Vignali, C., additional, Balestra, I., additional, Bardelli, S., additional, Berta, S., additional, Civano, F., additional, Kampczyk, P., additional, Le Floc'h, E., additional, Lusso, E., additional, Lutz, D., additional, Pozzetti, L., additional, Pozzi, F., additional, Riguccini, L., additional, Shankar, F., additional, and Silverman, J., additional

Published
2012
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35. Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in theXMM-COSMOS survey

Author

Lusso, E., primary, Comastri, A., additional, Simmons, B. D., additional, Mignoli, M., additional, Zamorani, G., additional, Vignali, C., additional, Brusa, M., additional, Shankar, F., additional, Lutz, D., additional, Trump, J. R., additional, Maiolino, R., additional, Gilli, R., additional, Bolzonella, M., additional, Puccetti, S., additional, Salvato, M., additional, Impey, C. D., additional, Civano, F., additional, Elvis, M., additional, Mainieri, V., additional, Silverman, J. D., additional, Koekemoer, A. M., additional, Bongiorno, A., additional, Merloni, A., additional, Berta, S., additional, Le Floc'h, E., additional, Magnelli, B., additional, Pozzi, F., additional, and Riguccini, L., additional

Published
2012
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37. The HELLAS2XMM survey - XII. The infrared/submillimetre view of an X-ray selected type 2 quasar atz≈ 2

Author

Vignali, C., primary, Pozzi, F., additional, Fritz, J., additional, Comastri, A., additional, Gruppioni, C., additional, Bellocchi, E., additional, Fiore, F., additional, Brusa, M., additional, Maiolino, R., additional, Mignoli, M., additional, Franca, F. La, additional, Pozzetti, L., additional, Zamorani, G., additional, and Merloni, A., additional

Published
2009
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38. Mapping the average AGN accretion rate in the SFR-M* plane for Herschel-selected galaxies at 0 < z ≤ 2.5.

Author

Delvecchio, I., Lutz, D., Berta, S., Rosario, D. J., Zamorani, G., Pozzi, F., Gruppioni, C., Vignali, C., Brusa, M., Cimatti, A., Clements, D. L., Cooray, A., Farrah, D., Lanzuisi, G., Oliver, S., Rodighiero, G., Santini, P., and Symeonidis, M.

Subjects
ACCRETION (Astrophysics), STELLAR mass, STAR formation, STELLAR luminosity function, STELLAR evolution
Abstract

We study the relation of AGN accretion, star formation rate (SFR) and stellar mass (M*) using a sample of ≈8600 star-forming galaxies up to z = 2.5 selected with Herschel imaging in the GOODS and COSMOS fields. For each of them we derive SFR and M*, both corrected, when necessary, for emission from an active galactic nucleus (AGN), through the decomposition of their spectral energy distributions (SEDs). About 10 per cent of the sample are detected individually in Chandra observations of the fields. For the rest of the sample, we stack the X-ray maps to get average X-ray properties. After subtracting the X-ray luminosity expected from star formation and correcting for nuclear obscuration, we derive the average AGN accretion rate for both detected sources and stacks, as a function of M*, SFR and redshift. The average accretion rate correlates with SFR and with M*. The dependence on SFR becomes progressively more significant at z > 0.8. This may suggest that SFR is the original driver of these correlations. We find that average AGN accretion and star formation increase in a similar fashion with offset from the star-forming 'main-sequence'. Our interpretation is that accretion on to the central black hole and star formation broadly trace each other, irrespective of whether the galaxy is evolving steadily on the main-sequence or bursting. [ABSTRACT FROM AUTHOR]

Published
2015
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39. X-shooter reveals powerful outflows in z ~ 1.5 X-ray selected obscured quasi-stellar objects.

Author

Brusa, M., Bongiorno, A., Cresci, G., Perna, M., Marconi, A., Mainieri, V., Maiolino, R., Salvato, M., Lusso, E., Santini, P., Comastri, A., Fiore, F., Gilli, R., La Franca, F., Lanzuisi, G., Lutz, D., Merloni, A., Mignoli, M., Onori, F., and Piconcelli, E.

Subjects
*VERY large telescopes, *X-ray detection, *BIPOLAR outflows (Astrophysics), *ACTIVE galactic nuclei, *ASTRONOMICAL observations
Abstract

We present X-shooter at Very Large Telescope observations of a sample of 10 luminous, X-ray obscured quasi-stellar objects (QSOs) at z ~ 1.5 from the XMM-COSMOS survey, expected to be caught in the transitioning phase from starburst to active galactic nucleus (AGN)-dominated systems. The main selection criterion is X-ray detection at bright fluxes (LX 1044 erg s-1) coupled to red optical-to-near-infrared-to-mid-infrared colours. Thanks to its large wavelength coverage, X-shooter allowed us to determine accurate redshifts from the presence of multiple emission lines for five out of six targets for which we had only a photometric redshift estimate, with an 80 per cent success rate, significantly larger than what is observed in similar programs of spectroscopic follow-up of red QSOs. We report the detection of broad and shifted components in the [OIII] ƛƛ5007, 4959 complexes for six out of eight sources with these lines observable in regions free from strong atmospheric absorptions. The full width at half-maximum (FWHM) associated with the broad components are in the range FWHM ~ 900-1600 km s-1, larger than the average value observed in Sloan Digital Sky Survey type 2 AGN samples at similar observed [OIII] luminosity, but comparable to those observed for QSO/ultraluminous infrared galaxies systems for which the presence of kpc scale outflows has been revealed through integral field unit spectroscopy. Although the total outflow energetics (inferred under reasonable assumptions) may be consistent with winds accelerated by stellar processes, we favour an AGN origin for the outflows given the high outflow velocities observed (v > 1000 km s-1) and the presence of strong winds also in objects undetected in the far-infrared. [ABSTRACT FROM AUTHOR]

Published
2015
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40. The high-redshift (z > 3) active galactic nucleus population in the 4-Ms Chandra Deep Field-South.

Author

Vito, F., Vignali, C., Gilli, R., Comastri, A., Iwasawa, K., Brandt, W. N., Alexander, D. M., Brusa, M., Lehmer, B., Bauer, F. E., Schneider, D. P., Xue, Y. Q., and Luo, B.

Subjects
REDSHIFT, GALACTIC nuclei, ASTRONOMICAL surveys, X-rays, SIMULATION methods & models, COMPARATIVE studies, LUMINOSITY
Abstract

We present results from a spectral analysis of a sample of high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) in the 4-Ms Chandra Deep Field-South (CDF-S), the deepest X-ray survey to date. The sample is selected using the most recent spectroscopic and photometric information available in this field. It consists of 34 sources with median redshift z = 3.7, 80 median net counts in the 0.5-7 keV band and median rest-frame absorption-corrected luminosity L2-10keV ≈ 1.5 × 1044 erg s-1. Spectral analysis for the full sample is presented and the intrinsic column density distribution, corrected for observational biases using spectral simulations, is compared with the expectations of X-ray background (XRB) synthesis models. We find that ≈57 per cent of the sources are highly obscured (NH > 1023 cm-2). Source number counts in the 0.5-2 keV band down to flux F0.5-2 keV ≈ 4 × 10-17 erg s-1 cm-2 are also presented. Our results are consistent with a decline of the AGN space density at z > 3 and suggest that, at those redshifts, the AGN obscured fraction is in agreement with the expectations of XRB synthesis models. [ABSTRACT FROM AUTHOR]

Published
2013
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41. Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey.

Author

Lusso, E., Comastri, A., Simmons, B. D., Mignoli, M., Zamorani, G., Vignali, C., Brusa, M., Shankar, F., Lutz, D., Trump, J. R., Maiolino, R., Gilli, R., Bolzonella, M., Puccetti, S., Salvato, M., Impey, C. D., Civano, F., Elvis, M., Mainieri, V., and Silverman, J. D.

Subjects
ACTIVE galactic nuclei, SPECTRUM analysis, COSMOS satellites, X-ray astronomy, BOLOMETERS, REDSHIFT, WAVELENGTHS
Abstract

ABSTRACT Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) active galactic nuclei (AGN) from the XMM-Newton survey in the Cosmic Evolution Survey field are presented. The sample is composed of 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65 per cent of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83 and 52 per cent, respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high-quality multiwavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 and 160 μm) to the optical-ultraviolet allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol - Lbol relations derived in this work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. and Hopkins et al. Black hole (BH) masses and Eddington ratios are available for 170 Type-1 AGN, while BH masses for Type-2 AGN are computed for 481 objects using the BH mass-stellar mass relation and the morphological information. We confirm a trend between kbol and λEdd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, the Eddington ratio increases with redshift for all types of AGN at any given MBH, while no clear evolution with redshift is seen at any given Lbol. [ABSTRACT FROM AUTHOR]

Published
2012
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42. The HELLAS2XMM survey – XII. The infrared/submillimetre view of an X-ray selected type 2 quasar at z≈ 2.

Author

Vignali, C., Pozzi, F., Fritz, J., Comastri, A., Gruppioni, C., Bellocchi, E., Fiore, F., Brusa, M., Maiolino, R., Mignoli, M., Franca, F. La, Pozzetti, L., Zamorani, G., and Merloni, A.

Subjects
SUBMILLIMETER astronomy, BOLOMETERS, QUASARS, ACTIVE galactic nuclei, STAR formation
Abstract

We present multiwavelength observations (from optical to submillimetre, including Spitzer and Submillimetre Common-User Bolometer Array) of H2XMMJ 003357.2−120038 (also GD 158_19), an X-ray selected, luminous narrow-line (type 2) quasar at selected from the HELLAS2XMM survey. Its broad-band properties can be reasonably well modelled assuming three components: a stellar component to account for the optical and near-infrared (IR) emission; an active galactic nucleus (AGN) component (i.e. dust heated by an accreting active nucleus), dominant in the mid-IR, with an optical depth at 9.7 along the line of sight (close to the equatorial plane of the obscuring matter) of and a full covering angle of the reprocessing matter (torus) of 140° and a far-IR starburst component (i.e. dust heated by star formation) to reproduce the wide bump observed longward of 70 . The derived star formation rate is . The overall modelling indicates that GD 158_19 is a high-redshift X-ray luminous, obscured quasar with coeval powerful AGN activity and intense star formation. It is probably caught before the process of expelling the obscuring gas has started, thus quenching the star formation. [ABSTRACT FROM AUTHOR]

Published
2009
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43. The role of galaxy mass on AGN emission: a view from the VANDELS survey

Author

Ricardo Amorín, Adriana Gargiulo, D. J. McLeod, Angela Bongiorno, Laura Pentericci, Andrea Cimatti, Margherita Talia, G. Zamorani, Nimish P. Hathi, Ross J. McLure, Marcella Brusa, Adriano Fontana, Michele Cirasuolo, A. Saxena, M. Magliocchetti, B. Garilli, ITA, Magliocchetti M., Pentericci L., Cirasuolo M., Zamorani G., Amorin R., Bongiorno A., Cimatti A., Fontana A., Garilli B., Gargiulo A., Hathi N.P., McLeod D.J., McLure R.J., Brusa M., Saxena A., and Talia M.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radio continuum: galaxie, 01 natural sciences, Luminosity, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, COSMIC cancer database, Mass distribution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies: active, Astrophysics - Astrophysics of Galaxies, Galaxy, X-rays: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a comparative analysis of the properties of AGN emitting at radio and X-ray wavelengths. The study is performed on 907 X-ray AGN and 100 radio AGN selected on the CDFS and UDS fields and makes use of new and ancillary data available to the VANDELS collaboration. Our results indicate that the mass of the host galaxy is a fundamental quantity which determines the level of AGN activity at the various wavelengths. Indeed large stellar masses are found to be connected with AGN radio emission, as virtually all radio-active AGN reside within galaxies of M*>10^{10} Msun. Large stellar masses also seem to favour AGN activity in the X-ray, even though X-ray AGN present a mass distribution which is more spread out and with a non-negligible tail at M*, 18 pages, 18 figures, to appear on MNRAS

Published
2020

44. The environmental properties of radio-emitting AGN

Author

M. Magliocchetti, P. Popesso, Marcella Brusa, Mara Salvato, and Magliocchetti M., Popesso P., Brusa M., Salvato, M.

Subjects
Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Dark matter, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, dark matter, 0103 physical sciences, Satellite galaxy, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, radio continuum: galaxies, Physics, cosmology: observation, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Content (measure theory), Astrophysics::Earth and Planetary Astrophysics, large-scale structure of Universe
Abstract

We study the environmental properties of z10^{23.5} W Hz^{-1} sr^{-1}$ are twice more likely to be found in clusters with respect to fainter sources (~38% vs ~15%), just as radio-selected AGN with stellar masses $M*>10^{11} M_\odot$ are twice more likely to be found in overdense environments with respect to objects of lower mass (~24% vs ~11%). Comparisons with galaxy samples further suggest that radio-selected AGN of large stellar mass tend to avoid underdense environments more than normal galaxies with the same stellar content. Stellar masses also seem to determine the location of radio-active AGN within clusters: ~100% of the sources found as satellite galaxies have $M*10^{11} M_\odot$. No different location within the cluster is instead observed for AGN of various radio luminosities. Radio AGN which also emit in the MIR show a marked preference to be found as isolated galaxies (~70%) at variance with those also active in the X-ray which all seem to reside within overdensities. What emerges from our work is a scenario whereby physical processes on sub-pc and kpc scales (e.g. emission respectively related to the AGN and to star formation) are strongly interconnected with the large-scale environment of the AGN itself., 8 pages, 6 figures, to appear on MNRAS

Published
2018

45. A census of radio-selected AGNs on the COSMOS field and of their FIR properties

Author

Mara Salvato, P. Popesso, M. Magliocchetti, Marcella Brusa, Magliocchetti, M., Popesso, P., Brusa, M., and Salvato, M.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Luminous infrared galaxy, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Methods observational, Galaxies: activeGalaxies: evolutionGalaxies: starburstInfrared: galaxiesMethods: observationalRadio continuum: galaxies, Universe, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use the new catalogue by Laigle et al. (2016) to provide a full census of VLA-COSMOS radio sources. We identify 90% of such sources and sub-divide them into AGN and star-forming galaxies on the basis of their radio luminosity. The AGN sample is COMPLETE with respect to radio selection at all z, 15 pages, 17 figures, to appear in MNRAS

Published
2017

46. Detection of faint broad emission lines in type 2 AGN – I. Near-infrared observations and spectral fitting

Author

F. Onori, Roberto Maiolino, Fabrizio Fiore, F. La Franca, Stefano Bianchi, Angela Bongiorno, Federica Ricci, Cristian Vignali, Marcella Brusa, E. Sani, Alessandro Marconi, ITA, GBR, Onori, Francesca, LA FRANCA, Fabio, Ricci, Federica, Brusa, Marcella, Sani, E., Maiolino, Roberto, Bianchi, Stefano, Bongiorno, A., Fiore, Fabrizio, Marconi, Alessandro, Vignali, C., Maiolino, Roberto [0000-0002-4985-3819], Apollo - University of Cambridge Repository, Onori, F., La Franca, F., Ricci, F., Brusa, M., Maiolino, R., Bianchi, S., Fiore, F., and Marconi, A.

Subjects
Infrared: galaxie, Data products, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Infrared Processing and Analysis Center, infrared: galaxies, 0103 physical sciences, Emission spectrum, Spectral fitting, Hardware_REGISTER-TRANSFER-LEVELIMPLEMENTATION, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, Near-infrared spectroscopy, Quasars: emission line, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, galaxies: Seyfert, quasars: emission lines, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present medium resolution near-infrared spectroscopic observations of 41 obscured and intermediate class active galactic nuclei (AGN; type 2, 1.9 and 1.8; AGN2) with redshift z ≲ 0.1, selected from the $\textit{Swift}$/Burst Alert Telescope 70-month catalogue. The observations have been carried out in the framework of a systematic study of the AGN2 near-infrared spectral properties and have been executed using Infrared Spectrometer And Array Camera/VLT, X-shooter/VLT and LUCI/LBT, reaching an average S/N ratio of ∼30 per resolution element. For those objects observed with X-shooter, we also obtained simultaneous optical and UV spectroscopy. We have identified a component from the broad line region in 13 out of 41 AGN2, with full width at half-maximum (FWHM) > 800 km s$^{-1}$. We have verified that the detection of the broad line region components does not significantly depend on selection effects due to the quality of the spectra, the X-ray or near-infrared fluxes, the orientation angle of the host galaxy or the hydrogen column density measured in the X-ray band. The average broad line region components found in AGN2 has a significantly (a factor 2) smaller FWHM if compared with a control sample of type 1 AGN., This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge funding from PRIN/MIUR and PRIN/INAF. MB acknowledges support from the FP7 Career Integration Grant “eEASy” (CIG 321913).

Published
2016

47. The MBH-M* relation for X-ray-obscured, red QSOs at 1.2 < z < 2.6

Author

Benjamin Magnelli, Marcella Brusa, C. Vignali, Enrico Piconcelli, Andreas Schulze, A. Lamastra, Alessandro Marconi, F. La Franca, Nicola Menci, Roberto Maiolino, Fabrizio Fiore, M. Cano-Díaz, Andrea Merloni, Angela Bongiorno, Giovanni Cresci, Bongiorno, A, Maiolino, R, Brusa, M, Marconi, A, Piconcelli, E, Lamastra, A, Cano Díaz, M, Schulze, A, Magnelli, B, Vignali, C, Fiore, F, Menci, N, Cresci, G, LA FRANCA, Fabio, and Merloni, A.

Subjects
QSOS, Physics, Stellar mass, galaxies active, galaxies evolution, quasars emission lines, quasars supermassive black holes, cosmology observations, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics, Lambda, 01 natural sciences, Spectral line, Redshift, Virial theorem, Galaxy, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Line (formation)
Abstract

We present near-infrared spectra, obtained with SINFONI and XShooter observations at ESO VLT, of nine dusty, red QSOs at 1.2 10^{21} - 10^{22} cm^{-2}) and show a broad Ha component in the NIR spectra. We complement this sample with twelve additional sources taken from the literature with similar properties resulting in a total sample of 21 X-ray obscured, intermediate type (1.8-1.9), dusty reddened QSOs. From the broad Ha line we have computed the BH masses through the virial formula and derived Eddington ratios. Moreover, from optical/IR multi-component SED fitting we have derived the stellar mass of their host galaxies and their SFRs. We find that most of the sources in our sample are hosted in starburst and main sequence star-forming galaxies with Eddington ratios lambda>0.1. We find a strong trend with the BH mass i.e. less massive objects are scattered below and above the local relation while the most massive ones are mainly located above it. We also studied the evolution of these sources on the M_BH-M_star plane compared to a sample of optically blue type--1 QSOs and we find that obscured red QSOs show a ratio of M_BH to M_star that increases with redshift which is consistent with or slightly lower than what has been found for blue QSOs. These sources may represent the blow-out phase at the end of the rapid BH growth and immediately preceding the classical blue QSOs typically sampled in optical surveys. They in fact show evidence of outflows in the ionized gas component, but their BH has already fully formed.

Published
2014

48. A quasar–galaxy mixing diagram: quasar spectral energy distribution shapes in the optical to near-infrared

Author

Jonathan R. Trump, Brandon C. Kelly, Luis C. Ho, Giorgio Lanzuisi, Chris Impey, John D. Silverman, Knud Jahnke, Anton M. Koekemoer, Martin Elvis, Andrea Comastri, Heng Hao, Mara Salvato, Francesca Civano, Annalisa Celotti, Kevin Schawinski, Cristian Vignali, Gianni Zamorani, Andrea Merloni, Vincenzo Mainieri, C. Megan Urry, Marcella Brusa, Angela Bongiorno, Hao H., Elvis M., Bongiorno A., Zamorani G., Merloni A., Kelly B.C., Civano F., Celotti A., Ho L.C., Jahnke K., Comastri A., Trump J.R., Mainieri V., Salvato M., Brusa M., Impey C.D., Koekemoer A.M., Lanzuisi G., Vignali C., Silverman J.D., Urry C.M., and Schawinski K.

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Settore FIS/05 - Astronomia e Astrofisica, quasars: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Mixing (physics), 0105 earth and related environmental sciences, Physics, surveys - galaxies: evolution, Diagram, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Black hole, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, galaxies: evolution, SURVEYS
Abstract

We define a quasar-galaxy mixing diagram using the slopes of their spectral energy distributions (SEDs) from 1\mu m to 3000\AA\ and from 1\mu m to 3\mu m in the rest frame. The mixing diagram can easily distinguish among quasar-dominated, galaxy-dominated and reddening-dominated SED shapes. By studying the position of the 413 XMM selected Type 1 AGN in the wide-field "Cosmic Evolution Survey" (COSMOS) in the mixing diagram, we find that a combination of the Elvis et al. (1994, hereafter E94) quasar SED with various contributions from galaxy emission and some dust reddening is remarkably effective in describing the SED shape from 0.3-3\mu m for large ranges of redshift, luminosity, black hole mass and Eddington ratio of type 1 AGN. In particular, the location in the mixing diagram of the highest luminosity AGN is very close (within 1\sigma) to that of the E94 SED. The mixing diagram can also be used to estimate the host galaxy fraction and reddening in quasar. We also show examples of some outliers which might be AGN in different evolutionary stages compared to the majority of AGN in the quasar-host galaxy co-evolution cycle., Comment: 19 pages, 13 figures, 2 tables, accepted by MNRAS

Published
2013

49. The Chandra-COSMOS survey – IV. X-ray spectra of the bright sample

Author

Tom Aldcroft, G. Zamorani, Luis C. Ho, Martin Elvis, Aneta Siemiginowska, Marcella Brusa, Antonella Fruscione, Cristian Vignali, Fabrizio Fiore, Mara Salvato, Vincenzo Mainieri, Andrea Merloni, G. Hasinger, Giorgio Lanzuisi, Roberto Gilli, Andrea Comastri, Francesca Civano, Lanzuisi G., Civano F., Elvis M., Salvato M., Hasinger G., Vignali C., Zamorani G., Aldcroft T., Brusa M., Comastri A., Fiore F., Fruscione A., Gilli R., Ho L.C., Mainieri V., Merloni A., and Siemiginowska A.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, X-ray, GALAXIES: HIGH REDSHIFT, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Small sample, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Spectral line, X-rays: galaxies, Space and Planetary Science, Spectral analysis, galaxies: nuclei, X ray spectra, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Photometric redshift
Abstract

We present the X-ray spectral analysis of the 390 brightest extragalactic sources in the Chandra-COSMOS catalog, showing at least 70 net counts in the 0.5-7 keV band. This sample has a 100% completeness in optical-IR identification, with 75% of the sample having a spectroscopic redshift and 25% a photometric redshift. Our analysis allows us to accurately determine the intrinsic absorption, the broad band continuum shape ({\Gamma}) and intrinsic L(2-10) distributions, with an accuracy better than 30% on the spectral parameters for 95% of the sample. The sample is equally divided in type-1 (49.7%) and type-2 AGN (48.7%) plus few passive galaxies at low z. We found a significant difference in the distribution of {\Gamma} of type-1 and type-2, with small intrinsic dispersion, a weak correlation of {\Gamma} with L(2-10) and a large population (15% of the sample) of high luminosity, highly obscured (QSO2) sources. The distribution of the X ray/Optical flux ratio (Log(FX /Fi)) for type-1 is narrow (0 < X/O < 1), while type-2 are spread up to X/O = 2. The X/O correlates well with the amount of X-ray obscuration. Finally, a small sample of Compton thick candidates and peculiar sources is presented. In the appendix we discuss the comparison between Chandra and XMM-Newton spectra for 280 sources in common. We found a small systematic difference, with XMM-Newton spectra that tend to have softer power-laws and lower obscuration., Comment: 20 pages, 16 figures. Accepted for Pubblication in MNRAS, 2013 February 5

Published
2013

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