10 results on '"Elvis, M"'
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2. “Comets” orbiting a black hole
- Author
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Maiolino, R., primary, Risaliti, G., additional, Salvati, M., additional, Pietrini, P., additional, Torricelli-Ciamponi, G., additional, Elvis, M., additional, Fabbiano, G., additional, Braito, V., additional, and Reeves, J., additional
- Published
- 2010
- Full Text
- View/download PDF
3. A non-hydrodynamical model for acceleration of line-driven winds in active galactic nuclei
- Author
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Risaliti, G., primary and Elvis, M., additional
- Published
- 2010
- Full Text
- View/download PDF
4. Ultraluminous X-ray sources out toz~ 0.3 in the COSMOS field
- Author
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Mainieri, V., primary, Vignali, C., additional, Merloni, A., additional, Civano, F., additional, Puccetti, S., additional, Brusa, M., additional, Gilli, R., additional, Bolzonella, M., additional, Comastri, A., additional, Zamorani, G., additional, Aller, M., additional, Carollo, M., additional, Scarlata, C., additional, Elvis, M., additional, Aldcroft, T. L., additional, Cappelluti, N., additional, Fabbiano, G., additional, Finoguenov, A., additional, Fiore, F., additional, Fruscione, A., additional, Koekemoer, A. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Lilly, S., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Bongiorno, A., additional, Caputi, K., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Mignoli, M., additional, Pello, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Capak, P., additional, Ilbert, O., additional, Impey, C., additional, Salvato, M., additional, Scoville, N., additional, Taniguchi, Y., additional, and Trump, J., additional
- Published
- 2010
- Full Text
- View/download PDF
5. The X-ray to optical-UV luminosity ratio of X-ray selected type 1 AGN in XMM-COSMOS
- Author
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Lusso, E., primary, Comastri, A., additional, Vignali, C., additional, Zamorani, G., additional, Brusa, M., additional, Gilli, R., additional, Iwasawa, K., additional, Salvato, M., additional, Civano, F., additional, Elvis, M., additional, Merloni, A., additional, Bongiorno, A., additional, Trump, J. R., additional, Koekemoer, A. M., additional, Schinnerer, E., additional, Le Floc'h, E., additional, Cappelluti, N., additional, Jahnke, K., additional, Sargent, M., additional, Silverman, J., additional, Mainieri, V., additional, Fiore, F., additional, Bolzonella, M., additional, Le Fèvre, O., additional, Garilli, B., additional, Iovino, A., additional, Kneib, J. P., additional, Lamareille, F., additional, Lilly, S., additional, Mignoli, M., additional, Scodeggio, M., additional, and Vergani, D., additional
- Published
- 2010
- Full Text
- View/download PDF
6. The XMM-Newtonwide-field survey in the COSMOS field***
- Author
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Cappelluti, N., Brusa, M., Hasinger, G., Comastri, A., Zamorani, G., Finoguenov, A., Gilli, R., Puccetti, S., Miyaji, T., Salvato, M., Vignali, C., Aldcroft, T., Böhringer, H., Brunner, H., Civano, F., Elvis, M., Fiore, F., Fruscione, A., Griffiths, R. E., Guzzo, L., Iovino, A., Koekemoer, A. M., Mainieri, V., Scoville, N. Z., Shopbell, P., Silverman, J., Urry, C. M., Cappelluti, N., Brusa, M., Hasinger, G., Comastri, A., Zamorani, G., Finoguenov, A., Gilli, R., Puccetti, S., Miyaji, T., Salvato, M., Vignali, C., Aldcroft, T., Böhringer, H., Brunner, H., Civano, F., Elvis, M., Fiore, F., Fruscione, A., Griffiths, R. E., Guzzo, L., Iovino, A., Koekemoer, A. M., Mainieri, V., Scoville, N. Z., Shopbell, P., Silverman, J., and Urry, C. M.
- Abstract
Context. The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey XMM-COSMOS a powerful tool to detect AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg2of the COSMOS area. It consists of 55 XMM-Newtonpointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg2.
- Published
- 2009
- Full Text
- View/download PDF
7. The faint X-ray source population near 3C 295
- Author
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D'Elia, V., Fiore, F., Elvis, M., Cappi, M., Mathur, S., Mazzotta, P., Falco, E., Cocchia, F., D'Elia, V., Fiore, F., Elvis, M., Cappi, M., Mathur, S., Mazzotta, P., Falco, E., and Cocchia, F.
- Abstract
We present a statistical analysis of the Chandraobservation of the source field around the 3C 295 galaxy cluster ($z=0.46$) to search for clustering of X-ray sources. We applied three different methods of analysis, all suggesting a strong clustering in the field on scales of a few arcmin. In particular 1) the $\log\,N{-}\log\,S$computed separately for the four ACIS-I chips reveals that there is a significant ($3.2 \sigma$in the 0.5-2 keV, $3.3 \sigma$in the 2-10 keV and $4.0 \sigma$in the 0.5-10 keV band) excess of sources to the North-North East and a void to the South of the central cluster; 2) the two point, two-dimensional Kolmogorov-Smirnov (KS) test, shows the probability that the sources are uniformly distributed is only a few percent; 3) a strong spatial correlation emerges from the study of the angular correlation function of the field: the angular correlation function (ACF) shows a clear signal on scales of $0.5\div 5$arcmin, correlation angle in the 0.5-7 keV band $\theta_0=8.5^{+6.5}_{-4.5}$, 90% confidence limit (assuming a power law ACF with slope $\gamma=1.8$). This correlation angle is 2 times higher than that of a sample of 8 ACIS-I field at the $2.5 \sigma$confidence level. The above scales translate to 0.2$\div$2 Mpc at the cluster redshift, higher than the typical cluster core radius, and more similar to the size of a “filament” of the large scale structure.
- Published
- 2004
- Full Text
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8. The XMM-Newton Serendipitous Survey*
- Author
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Watson, M. G., Auguères, J.-L., Ballet, J., Barcons, X., Barret, D., Boer, M., Boller, Th., Bromage, G. E., Brunner, H., Carrera, F. J., Cropper, M. S., Denby, M., Ehle, M., Elvis, M., Fabian, A. C., Freyberg, M. J., Guillout, P., Hameury, J.-M., Hasinger, G., Hinshaw, D. A., Maccacaro, T., Mason, K. O., McMahon, R. G., Michel, L., Mirioni, L., Mittaz, J. P., Motch, C., Olive, J.-F., Osborne, J. P., Page, C. G., Pakull, M., Perry, B. H., Pierre, M., Pietsch, W., Pye, J. P., Read, A. M., Roberts, T. P., Rosen, S. R., Sauvageot, J.-L., Schwope, A. D., Sekiguchi, K., Stewart, G. C., Stewart, I., Valtchanov, I., Ward, M. J., Warwick, R. S., West, R. G., White, N. E., Worrall, D. M., Watson, M. G., Auguères, J.-L., Ballet, J., Barcons, X., Barret, D., Boer, M., Boller, Th., Bromage, G. E., Brunner, H., Carrera, F. J., Cropper, M. S., Denby, M., Ehle, M., Elvis, M., Fabian, A. C., Freyberg, M. J., Guillout, P., Hameury, J.-M., Hasinger, G., Hinshaw, D. A., Maccacaro, T., Mason, K. O., McMahon, R. G., Michel, L., Mirioni, L., Mittaz, J. P., Motch, C., Olive, J.-F., Osborne, J. P., Page, C. G., Pakull, M., Perry, B. H., Pierre, M., Pietsch, W., Pye, J. P., Read, A. M., Roberts, T. P., Rosen, S. R., Sauvageot, J.-L., Schwope, A. D., Sekiguchi, K., Stewart, G. C., Stewart, I., Valtchanov, I., Ward, M. J., Warwick, R. S., West, R. G., White, N. E., and Worrall, D. M.
- Abstract
This paper describes the performance of XMM-Newtonfor serendipitous surveys and summarises the scope and potential of the XMM-NewtonSerendipitous Survey. The role of the Survey Science Centre (SSC) in the XMM-Newtonproject is outlined. The SSC's follow-up and identification programme for the XMM-Newtonserendipitous survey is described together with the presentation of some of the first results.
- Published
- 2001
- Full Text
- View/download PDF
9. Black hole accretion and host galaxies of obscured quasars in XMM-COSMOS⋆
- Author
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Mainieri, V., Bongiorno, A., Merloni, A., Aller, M., Carollo, M., Iwasawa, K., Koekemoer, A. M., Mignoli, M., Silverman, J. D., Bolzonella, M., Brusa, M., Comastri, A., Gilli, R., Halliday, C., Ilbert, O., Lusso, E., Salvato, M., Vignali, C., Zamorani, G., Contini, T., Kneib, J.-P., Le Fèvre, O., Lilly, S., Renzini, A., Scodeggio, M., Balestra, I., Bardelli, S., Caputi, K., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Nair, P., Pello, R., Peng, Y., Perez Montero, E., Pozzetti, L., Ricciardelli, E., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Aussel, H., Capak, P., Cappelluti, N., Elvis, M., Fiore, F., Hasinger, G., Impey, C., Le Floc’h, E., Scoville, N., Taniguchi, Y., and Trump, J.
- Abstract
Aims.We explore the connection between black hole growth at the center of obscured quasars selected from the XMM-COSMOS survey and the physical properties of their host galaxies. We study a bolometric regime ( ⟨ Lbol⟩ = 8 × 1045erg s-1) where several theoretical models invoke major galaxy mergers as the main fueling channel for black hole accretion.
- Published
- 2011
- Full Text
- View/download PDF
10. Ultraluminous X-ray sources out to z~ 0.3 in the COSMOS field
- Author
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Mainieri, V., Vignali, C., Merloni, A., Civano, F., Puccetti, S., Brusa, M., Gilli, R., Bolzonella, M., Comastri, A., Zamorani, G., Aller, M., Carollo, M., Scarlata, C., Elvis, M., Aldcroft, T. L., Cappelluti, N., Fabbiano, G., Finoguenov, A., Fiore, F., Fruscione, A., Koekemoer, A. M., Contini, T., Kneib, J.-P., Le Fèvre, O., Lilly, S., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Capak, P., Ilbert, O., Impey, C., Salvato, M., Scoville, N., Taniguchi, Y., and Trump, J.
- Abstract
Context. Using Chandra observations we identified a sample of seven off-nuclear X-ray sources in the redshift range z= 0.072–0.283, located within optically bright galaxies in the COSMOS Survey. All of them, if associated with their closest bright galaxy, would have L[0.5–7 keV] >1039erg s-1and therefore can be classified as ultraluminous X-ray sources (ULXs). Aims. Using the multi-wavelength coverage available in the COSMOS field, we studied the properties of the host galaxies of these ULXs. In detail, we derived their star formation rate from Hαmeasurements and their stellar masses using SED fitting techniques with the aim to compute the probability to have an off-nuclear source based on the host galaxy properties. We divided the host galaxies in different morphological classes with the available ACS/HST imaging.Methods. We selected off-nuclear candidates with the following criteria: 1) the distance between the X-ray and the optical centroid has to be larger than 0.9´´, larger than 1.8 times the radius of the Chandra positional error circle and smaller than the Petrosian radius of the host galaxy; 2) the optical counterpart is a bright galaxy (RAB<22); 3) the redshift of the counterpart is lower than z= 0.3; 4) the source has been observed in at least one Chandra pointing at an off-axis angle smaller than 5´; 5) the X-ray positional error is smaller than 0.8´´. We verified each candidate super-imposing the X-ray contours on the optical/IR images. We expect less than one misidentified AGN due to astrometric errors and on average 1.3 serendipitous background source matches.Results. We find that our ULXs candidates are located in regions of the SFR versus ${\rm M}_\star$plane where one or more off-nuclear detectable sources are expected. From a morphological analysis of the ACS imaging and the use of rest-frame colours, we find that our ULXs are hosted both in late and early type galaxies. Finally, we find that the fraction of galaxies hosting a ULX ranges from ≈0.5% to ≈0.2% going from $L_{0.5{-}2~{\rm keV}}$= 3 × 1039erg s-1to $L_{0.5{-}2~{\rm keV}}$= 2 × 1040erg s-1.
- Published
- 2010
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