244 results on '"A, Bongiorno"'
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2. MAMBO: An empirical galaxy and AGN mock catalogue for the exploitation of future surveys.
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López-López, X., Bolzonella, M., Pozzetti, L., Salvato, M., Bisigello, L., Feltre, A., López, I. E., Viitanen, A., Allevato, V., Bongiorno, A., Girelli, G., Buchner, J., Charlot, S., Ricci, F., Schreiber, C., and Zamorani, G.
- Subjects
ACTIVE galactic nuclei ,ACTIVE galaxies ,STELLAR mass ,DARK matter ,DISTRIBUTION (Probability theory) - Abstract
Context. Current and future large surveys will produce unprecedented amounts of data. Realistic simulations have become essential for the design and development of these surveys, as well as for the interpretation of the results. Aims. We present MAMBO, a flexible and efficient workflow to build empirical galaxy and active galactic nucleus (AGN) mock catalogues that reproduce the physical and observational properties of these sources. Methods. We started with simulated dark matter (DM) haloes, to preserve the link with the cosmic web, and we populated them with galaxies and AGN using abundance matching techniques. We followed an empirical methodology, using stellar mass functions, host galaxy AGN mass functions, and AGN accretion rate distribution functions studied at different redshifts to assign, among other properties, stellar masses, the fraction of quenched galaxies, or the AGN activity (demography, obscuration, multiwavelength emission, etc.). Results. As a proof test, we applied the method to a Millennium DM lightcone of 3.14 deg2 up to a redshift of z = 10 and down to stellar masses of ℳ ≳ 1075 M
⊙ . We show that the AGN population from the mock lightcone presented here reproduces with good accuracy various observables, such as state-of-the-art luminosity functions in the X-ray up to z~7 and in the ultraviolet up to z~5, optical/near-infrared colour-colour diagrams, and narrow emission line diagnostic diagrams. Finally, we demonstrate how this catalogue can be used to make useful predictions for large surveys. Using Euclid as a case example, we compute, among other forecasts, the expected surface densities of galaxies and AGN detectable in the Euclid HE band. We find that Euclid might observe (on HE only) about 107 and 8 × 107 type 1 and 2 AGN, respectively, and 2 × 109 galaxies at the end of its 14 679 deg2 Wide survey, in good agreement with other published forecasts. [ABSTRACT FROM AUTHOR]- Published
- 2024
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3. X-ray polarization measurement of the gold standard of radio-quiet active galactic nuclei: NGC 1068
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Marin, F., primary, Marinucci, A., additional, Laurenti, M., additional, Kim, D.E., additional, Barnouin, T., additional, Di Marco, A., additional, Ursini, F., additional, Bianchi, S., additional, Ravi, S., additional, Marshall, H.L., additional, Matt, G., additional, Chen, C.-T., additional, Gianolli, V.E., additional, Ingram, A., additional, Middei, R., additional, Maksym, W.P., additional, Panagiotou, C., additional, Podgorny, J., additional, Puccetti, S., additional, Ratheesh, A., additional, Tombesi, F., additional, Agudo, I., additional, Antonelli, L.A., additional, Bachetti, M., additional, Baldini, L., additional, Baumgartner, W., additional, Bellazzini, R., additional, Bongiorno, S., additional, Bonino, R., additional, Brez, A., additional, Bucciantini, N., additional, Capitanio, F., additional, Castellano, S., additional, Cavazzuti, E., additional, Ciprini, S., additional, Costa, E., additional, De Rosa, A., additional, Del Monte, E., additional, Di Gesu, L., additional, Di Lalla, N., additional, Donnarumma, I., additional, Doroshenko, V., additional, Dovčiak, M., additional, Ehlert, S., additional, Enoto, T., additional, Evangelista, Y., additional, Fabiani, S., additional, Ferrazzoli, R., additional, Garcia, J., additional, Gunji, S., additional, Heyl, J., additional, Iwakiri, W., additional, Jorstad, S., additional, Kaaret, P., additional, Karas, V., additional, Kislat, F., additional, Kitaguchi, T., additional, Kolodziejczak, J., additional, Krawczynski, H., additional, La Monaca, F., additional, Latronico, L., additional, Liodakis, I., additional, Madejski, G., additional, Maldera, S., additional, Manfreda, A., additional, Marscher, A., additional, Massaro, F., additional, Mitsuishi, I., additional, Mizuno, T., additional, Muleri, F., additional, Negro, M., additional, Ng, S., additional, O'Dell, S., additional, Omodei, N., additional, Oppedisano, C., additional, Papitto, A., additional, Pavlov, G., additional, Perri, M., additional, Pesce-Rollins, M., additional, Petrucci, P.-O., additional, Pilia, M., additional, Possenti, A., additional, Poutanen, J., additional, Ramsey, B., additional, Rankin, J., additional, Roberts, O., additional, Romani, R., additional, Sgrò, C., additional, Slane, P., additional, Soffitta, P., additional, Spandre, G., additional, Swartz, D., additional, Tamagawa, T., additional, Tavecchio, F., additional, Taverna, R., additional, Tawara, Y., additional, Tennant, A., additional, Thomas, N., additional, Trois, A., additional, Tsygankov, S., additional, Turolla, R., additional, Vink, J., additional, Weisskopf, M., additional, Wu, K., additional, Xie, F., additional, and Zane, S., additional
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- 2024
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4. MUSE view of PDS 456: Kiloparsec-scale wind, extended ionized gas, and close environment
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Travascio, A., primary, Piconcelli, E., additional, Bischetti, M., additional, Cresci, G., additional, Feruglio, C., additional, Perna, M., additional, Vietri, G., additional, Carniani, S., additional, Cantalupo, S., additional, Cicone, C., additional, Ginolfi, M., additional, Venturi, G., additional, Zubovas, K., additional, Bongiorno, A., additional, Brusa, M., additional, Luminari, A., additional, Mainieri, V., additional, Marconi, A., additional, Menci, N., additional, Nardini, E., additional, Pensabene, A., additional, Ramos Almeida, C., additional, Tombesi, F., additional, Vignali, C., additional, Zappacosta, L., additional, and Fiore, F., additional
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- 2024
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5. Discovery of a variable energy-dependent X-ray polarization in the accreting neutron star GX 5−1
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Fabiani, Sergio, primary, Capitanio, Fiamma, additional, Iaria, Rosario, additional, Poutanen, Juri, additional, Gnarini, Andrea, additional, Ursini, Francesco, additional, Farinelli, Ruben, additional, Bobrikova, Anna, additional, Steiner, James F., additional, Svoboda, Jiri, additional, Anitra, Alessio, additional, Baglio, Maria C., additional, Carotenuto, Francesco, additional, Del Santo, Melania, additional, Ferrigno, Carlo, additional, Lewis, Fraser, additional, Russell, David M., additional, Russell, Thomas D., additional, van den Eijnden, Jakob, additional, Cocchi, Massimo, additional, Di Marco, Alessandro, additional, La Monaca, Fabio, additional, Liu, Kuan, additional, Rankin, John, additional, Weisskopf, Martin C., additional, Xie, Fei, additional, Bianchi, Stefano, additional, Burderi, Luciano, additional, Di Salvo, Tiziana, additional, Egron, Elise, additional, Illiano, Giulia, additional, Kaaret, Philip, additional, Matt, Giorgio, additional, Mikušincová, Romana, additional, Muleri, Fabio, additional, Papitto, Alessandro, additional, Agudo, Iván, additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bongiorno, Stephen D., additional, Bonino, Raffaella, additional, Brez, Alessandro, additional, Bucciantini, Niccolò, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, Costa, Enrico, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Gesu, Laura, additional, Di Lalla, Niccolò, additional, Donnarumma, Immacolata, additional, Doroshenko, Victor, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Ferrazzoli, Riccardo, additional, Garcia, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Heyl, Jeremy, additional, Iwakiri, Wataru, additional, Jorstad, Svetlana G., additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, Latronico, Luca, additional, Liodakis, Ioannis, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Marscher, Alan P., additional, Marshall, Herman L., additional, Massaro, Francesco, additional, Mitsuishi, Ikuyuki, additional, Mizuno, Tsunefumi, additional, Negro, Michela, additional, Ng, Chi-Yung, additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Petrucci, Pierre-Olivier, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Puccetti, Simonetta, additional, Ramsey, Brian D., additional, Ratheesh, Ajay, additional, Roberts, Oliver J., additional, Romani, Roger W., additional, Sgrò, Carmelo, additional, Slane, Patrick, additional, Soffitta, Paolo, additional, Spandre, Gloria, additional, Swartz, Douglas A., additional, Tamagawa, Toru, additional, Tavecchio, Fabrizio, additional, Taverna, Roberto, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Tombesi, Francesco, additional, Trois, Alessio, additional, Tsygankov, Sergey S., additional, Turolla, Roberto, additional, Vink, Jacco, additional, Wu, Kinwah, additional, and Zane, Silvia, additional
- Published
- 2024
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6. Tracing the rise of supermassive black holes: A panchromatic search for faint, unobscured quasars at z > 6 with COSMOS-Web and other surveys
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Andika, Irham T., primary, Jahnke, Knud, additional, Onoue, Masafusa, additional, Silverman, John D., additional, Fitriana, Itsna K., additional, Bongiorno, Angela, additional, Brinch, Malte, additional, Casey, Caitlin M., additional, Faisst, Andreas, additional, Gillman, Steven, additional, Gozaliasl, Ghassem, additional, Hayward, Christopher C., additional, Hirschmann, Michaela, additional, Kocevski, Dale, additional, Koekemoer, Anton M., additional, Kokorev, Vasily, additional, Lambrides, Erini, additional, Lee, Minju M., additional, Michael Rich, R., additional, Trakhtenbrot, Benny, additional, Megan Urry, C., additional, Wilkins, Stephen M., additional, and Vijayan, Aswin P., additional
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- 2024
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7. Magnetic field properties inside the jet of Mrk 421
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Kim, Dawoon E., primary, Di Gesu, Laura, additional, Liodakis, Ioannis, additional, Marscher, Alan P., additional, Jorstad, Svetlana G., additional, Middei, Riccardo, additional, Marshall, Herman L., additional, Pacciani, Luigi, additional, Agudo, Iván, additional, Tavecchio, Fabrizio, additional, Cibrario, Nicoló, additional, Tugliani, Stefano, additional, Bonino, Raffaella, additional, Negro, Michela, additional, Puccetti, Simonetta, additional, Tombesi, Francesco, additional, Costa, Enrico, additional, Donnarumma, Immacolata, additional, Soffitta, Paolo, additional, Mizuno, Tsunefumi, additional, Fukazawa, Yasushi, additional, Kawabata, Koji S., additional, Nakaoka, Tatsuya, additional, Uemura, Makoto, additional, Imazawa, Ryo, additional, Sasada, Mahito, additional, Akitaya, Hiroshi, additional, Josè Aceituno, Francisco, additional, Bonnoli, Giacomo, additional, Casanova, Vìctor, additional, Myserlis, Ioannis, additional, Sievers, Albrecht, additional, Angelakis, Emmanouil, additional, Kraus, Alexander, additional, Yeon Cheong, Whee, additional, Jeong, Hyeon-Woo, additional, Kang, Sincheol, additional, Kim, Sang-Hyun, additional, Lee, Sang-Sung, additional, Agìs-Gonzàlez, Beatriz, additional, Sota, Alfredo, additional, Escudero, Juan, additional, Gurwell, Mark, additional, Keating, Garrett K., additional, Rao, Ramprasad, additional, Kouch, Pouya M., additional, Lindfors, Elina, additional, Bourbah, Ioakeim G., additional, Kiehlmann, Sebastian, additional, Kontopodis, Evangelos, additional, Mandarakas, Nikos, additional, Romanopoulos, Stylianos, additional, Skalidis, Raphael, additional, Vervelaki, Anna, additional, Savchenko, Sergey S., additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bianchi, Stefano, additional, Bongiorno, Stephen D., additional, Brez, Alessandro, additional, Bucciantini, Niccoló, additional, Capitanio, Fiamma, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Lalla, Niccoló, additional, Di Marco, Alessandro, additional, Doroshenko, Victor, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Fabiani, Sergio, additional, Ferrazzoli, Riccardo, additional, Garcia, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Heyl, Jeremy, additional, Iwakiri, Wataru, additional, Kaaret, Philip, additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, La Monaca, Fabio, additional, Latronico, Luca, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Massaro, Francesco, additional, Matt, Giorgio, additional, Mitsuishi, Ikuyuki, additional, Muleri, Fabio, additional, Ng, C.-Y., additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Papitto, Alessandro, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Petrucci, Pierre-Olivier, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Poutanen, Juri, additional, Ramsey, Brian D., additional, Rankin, John, additional, Ratheesh, Ajay, additional, Roberts, Oliver, additional, Romani, Roger W., additional, Sgró, Carmelo, additional, Slane, Patrick, additional, Spandre, Gloria, additional, Swartz, Doug, additional, Tamagawa, Toru, additional, Taverna, Roberto, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Trois, Alessio, additional, Tsygankov, Sergey S., additional, Turolla, Roberto, additional, Vink, Jacco, additional, Weisskopf, Martin C., additional, Wu, Kinwah, additional, Xie, Fei, additional, and Zane, Silvia, additional
- Published
- 2024
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8. HYPerluminous quasars at the Epoch of ReionizatION (HYPERION). A new regime for the X-ray nuclear properties of the first quasars
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Zappacosta, L., primary, Piconcelli, E., additional, Fiore, F., additional, Saccheo, I., additional, Valiante, R., additional, Vignali, C., additional, Vito, F., additional, Volonteri, M., additional, Bischetti, M., additional, Comastri, A., additional, Done, C., additional, Elvis, M., additional, Giallongo, E., additional, La Franca, F., additional, Lanzuisi, G., additional, Laurenti, M., additional, Miniutti, G., additional, Bongiorno, A., additional, Brusa, M., additional, Civano, F., additional, Carniani, S., additional, D’Odorico, V., additional, Feruglio, C., additional, Gallerani, S., additional, Gilli, R., additional, Grazian, A., additional, Guainazzi, M., additional, Marinucci, A., additional, Menci, N., additional, Middei, R., additional, Nicastro, F., additional, Puccetti, S., additional, Tombesi, F., additional, Tortosa, A., additional, Testa, V., additional, Vietri, G., additional, Cristiani, S., additional, Haardt, F., additional, Maiolino, R., additional, Schneider, R., additional, Tripodi, R., additional, Vallini, L., additional, and Vanzella, E., additional
- Published
- 2023
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9. The VANDELS ESO public spectroscopic survey: The spectroscopic measurements catalogue
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Talia, M., primary, Schreiber, C., additional, Garilli, B., additional, Pentericci, L., additional, Pozzetti, L., additional, Zamorani, G., additional, Cullen, F., additional, Moresco, M., additional, Calabrò, A., additional, Castellano, M., additional, Fynbo, J. P. U., additional, Guaita, L., additional, Marchi, F., additional, Mascia, S., additional, McLure, R., additional, Mignoli, M., additional, Pompei, E., additional, Vanzella, E., additional, Bongiorno, A., additional, Vietri, G., additional, Amorín, R. O., additional, Bolzonella, M., additional, Carnall, A. C., additional, Cimatti, A., additional, Cresci, G., additional, Cristiani, S., additional, Cucciati, O., additional, Dunlop, J. S., additional, Fontanot, F., additional, Franzetti, P., additional, Gargiulo, A., additional, Hamadouche, M. L., additional, Hathi, N. P., additional, Hibon, P., additional, Iovino, A., additional, Koekemoer, A. M., additional, Mannucci, F., additional, McLeod, D. J., additional, and Saldana-Lopez, A., additional
- Published
- 2023
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10. Complex variations in X-ray polarization in the X-ray pulsar LS V +44 17/RX J0440.9+4431
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Doroshenko, Victor, primary, Poutanen, Juri, additional, Heyl, Jeremy, additional, Tsygankov, Sergey S., additional, Caiazzo, Ilaria, additional, Turolla, Roberto, additional, Veledina, Alexandra, additional, Weisskopf, Martin C., additional, Forsblom, Sofia V., additional, González-Caniulef, Denis, additional, Loktev, Vladislav, additional, Malacaria, Christian, additional, Mushtukov, Alexander A., additional, Suleimanov, Valery F., additional, Lutovinov, Alexander A., additional, Mereminskiy, Ilya A., additional, Molkov, Sergey V., additional, Salganik, Alexander, additional, Santangelo, Andrea, additional, Berdyugin, Andrei V., additional, Kravtsov, Vadim, additional, Nitindala, Anagha P., additional, Agudo, Iván, additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bianchi, Stefano, additional, Bongiorno, Stephen D., additional, Bonino, Raffaella, additional, Brez, Alessandro, additional, Bucciantini, Niccolò, additional, Capitanio, Fiamma, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, Costa, Enrico, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Gesu, Laura, additional, Di Lalla, Niccolò, additional, Di Marco, Alessandro, additional, Donnarumma, Immacolata, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Fabiani, Sergio, additional, Ferrazzoli, Riccardo, additional, García, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Iwakiri, Wataru, additional, Jorstad, Svetlana G., additional, Kaaret, Philip, additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, La Monaca, Fabio, additional, Latronico, Luca, additional, Liodakis, Ioannis, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Marscher, Alan P., additional, Marshall, Herman L., additional, Massaro, Francesco, additional, Matt, Giorgio, additional, Mitsuishi, Ikuyuki, additional, Mizuno, Tsunefumi, additional, Muleri, Fabio, additional, Negro, Michela, additional, Ng, Chi-Yung, additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Papitto, Alessandro, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Petrucci, Pierre-Olivier, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Puccetti, Simonetta, additional, Ramsey, Brian D., additional, Rankin, John, additional, Ratheesh, Ajay, additional, Roberts, Oliver J., additional, Romani, Roger W., additional, Sgrò, Carmelo, additional, Slane, Patrick, additional, Soffitta, Paolo, additional, Spandre, Gloria, additional, Swartz, Douglas A., additional, Tamagawa, Toru, additional, Tavecchio, Fabrizio, additional, Taverna, Roberto, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Tombesi, Francesco, additional, Trois, Alessio, additional, Vink, Jacco, additional, Wu, Kinwah, additional, Xie, Fei, additional, and Zane, Silvia, additional
- Published
- 2023
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11. Characterization of a metallic interconnect operated in stack during 40,000 hours in SOFC mode
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Piccardo Paolo, Spotorno Roberto, Bongiorno Valeria, Paravidino Daniele, Geipel Christian, Patrone Greta, and Valente Francesca
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Environmental sciences ,GE1-350 - Abstract
An SOFC stack operated for 40,000 hours has been dismantled offering the opportunity to characterize the metallic interconnect. The metal plate was carefully investigated to define the evolution of the surfaces exposed to the air and to the hydrogen electrodes respectively. The observations of the surfaces reveal the stability of the layers applied on top of the rib at the air side while in the bottom of the channels the protective coating (i.e., Co-Mn base spinel oxide) shows large crystals. The cross section allowed to highlight the formation of a rather homogeneous layer of thermal grown oxide between the metal and the coating. The average thickness of the TGO is around 11 μm. The hydrogen side shows a superficial alteration (due to the interaction with the water vapour) changing from the inlet to the outlet where it seems thinner as if the TGO further reacted by forming volatile compounds. The cross section observations confirmed the presence of a porous TGO with a rather high content of manganese in a Cr-Mn spinel oxide. Several spots testifies the zones of contact with the Ni base contacting layer. The cross section corresponding to such zones highlighted the Ni diffusion in the metal substrate.
- Published
- 2022
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12. Tracing the rise of supermassive black holes: A panchromatic search for faint, unobscured quasars at z ≳ 6 with COSMOS-Web and other surveys.
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Andika, Irham T., Jahnke, Knud, Onoue, Masafusa, Silverman, John D., Fitriana, Itsna K., Bongiorno, Angela, Brinch, Malte, Casey, Caitlin M., Faisst, Andreas, Gillman, Steven, Gozaliasl, Ghassem, Hayward, Christopher C., Hirschmann, Michaela, Kocevski, Dale, Koekemoer, Anton M., Kokorev, Vasily, Lambrides, Erini, Lee, Minju M., Michael Rich, Robert, and Trakhtenbrot, Benny
- Subjects
QUASARS ,SUPERMASSIVE black holes ,ACTIVE galactic nuclei ,MONTE Carlo method ,SPECTRAL energy distribution ,DWARF galaxies - Abstract
We report the identification of 64 new candidates of compact galaxies, potentially hosting faint quasars with bolometric luminosities of L
bol = 1043 –1046 erg s−1 , residing in the reionization epoch within the redshift range of 6 ≲ z ≲ 8. These candidates were selected by harnessing the rich multiband datasets provided by the emerging JWST-driven extragalactic surveys, focusing on COSMOS-Web, as well as JADES, UNCOVER, CEERS, and PRIMER. Our search strategy includes two stages: applying stringent photometric cuts to catalog-level data and detailed spectral energy distribution fitting. These techniques effectively isolate the quasar candidates while mitigating contamination from low-redshift interlopers, such as brown dwarfs and nearby galaxies. The selected candidates indicate physical traits compatible with low-luminosity active galactic nuclei, likely hosting ≈105 –107 M⊙ supermassive black holes (SMBHs) living in galaxies with stellar masses of ≈108 –1010 M⊙ . The SMBHs selected in this study, on average, exhibit an elevated mass compared to their hosts, with the mass ratio distribution slightly higher than those of galaxies in the local Universe. As with other high-z studies, this is at least in part due to the selection method for these quasars. An extensive Monte Carlo analysis provides compelling evidence that heavy black hole seeds from the direct collapse scenario appear to be the preferred pathway to mature this specific subset of SMBHs by z ≈ 7. Notably, most of the selected candidates might have emerged from seeds with masses of ∼105 M⊙ , assuming a thin disk accretion with an average Eddington ratio of fEdd = 0.6 ± 0.3 and a radiative efficiency of ϵ = 0.2 ± 0.1. This work underscores the significance of further spectroscopic observations, as the quasar candidates presented here offer exceptional opportunities to delve into the nature of the earliest galaxies and SMBHs that formed during cosmic infancy. [ABSTRACT FROM AUTHOR]- Published
- 2024
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13. X-ray polarimetry and spectroscopy of the neutron star low-mass X-ray binary GX 9+9: An in-depth study with IXPE and NuSTAR
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Ursini, F., primary, Farinelli, R., additional, Gnarini, A., additional, Poutanen, J., additional, Bianchi, S., additional, Capitanio, F., additional, Di Marco, A., additional, Fabiani, S., additional, La Monaca, F., additional, Malacaria, C., additional, Matt, G., additional, Mikušincová, R., additional, Cocchi, M., additional, Kaaret, P., additional, Kajava, J. J. E., additional, Pilia, M., additional, Zhang, W., additional, Agudo, I., additional, Antonelli, L. A., additional, Bachetti, M., additional, Baldini, L., additional, Baumgartner, W. H., additional, Bellazzini, R., additional, Bongiorno, S. D., additional, Bonino, R., additional, Brez, A., additional, Bucciantini, N., additional, Castellano, S., additional, Cavazzuti, E., additional, Chen, C.-T., additional, Ciprini, S., additional, Costa, E., additional, De Rosa, A., additional, Del Monte, E., additional, Di Gesu, L., additional, Di Lalla, N., additional, Donnarumma, I., additional, Doroshenko, V., additional, Dovčiak, M., additional, Ehlert, S. R., additional, Enoto, T., additional, Evangelista, Y., additional, Ferrazzoli, R., additional, Garcia, J. A., additional, Gunji, S., additional, Hayashida, K., additional, Heyl, J., additional, Iwakiri, W., additional, Jorstad, S. G., additional, Karas, V., additional, Kislat, F., additional, Kitaguchi, T., additional, Kolodziejczak, J. J., additional, Krawczynski, H., additional, Latronico, L., additional, Liodakis, I., additional, Maldera, S., additional, Manfreda, A., additional, Marin, F., additional, Marinucci, A., additional, Marscher, A. P., additional, Marshall, H. L., additional, Massaro, F., additional, Mitsuishi, I., additional, Mizuno, T., additional, Muleri, F., additional, Negro, M., additional, Ng, C.-Y., additional, O’Dell, S. L., additional, Omodei, N., additional, Oppedisano, C., additional, Papitto, A., additional, Pavlov, G. G., additional, Peirson, A. L., additional, Perri, M., additional, Pesce-Rollins, M., additional, Petrucci, P.-O., additional, Possenti, A., additional, Puccetti, S., additional, Ramsey, B. D., additional, Rankin, J., additional, Ratheesh, A., additional, Roberts, O. J., additional, Romani, R. W., additional, Sgrò, C., additional, Slane, P., additional, Soffitta, P., additional, Spandre, G., additional, Swartz, D. A., additional, Tamagawa, T., additional, Tavecchio, F., additional, Taverna, R., additional, Tawara, Y., additional, Tennant, A. F., additional, Thomas, N. E., additional, Tombesi, F., additional, Trois, A., additional, Tsygankov, S. S., additional, Turolla, R., additional, Vink, J., additional, Weisskopf, M. C., additional, Wu, K., additional, Xie, F., additional, and Zane, S., additional
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- 2023
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14. The ionizing photon production efficiency of bright z ∼ 2 − 5 galaxies
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Castellano, M., primary, Belfiori, D., additional, Pentericci, L., additional, Calabrò, A., additional, Mascia, S., additional, Napolitano, L., additional, Caro, F., additional, Charlot, S., additional, Chevallard, J., additional, Curtis Lake, E., additional, Talia, M., additional, Bongiorno, A., additional, Fontana, A., additional, Fynbo, J. P. U., additional, Garilli, B., additional, Guaita, L., additional, McLure, R. J., additional, Merlin, E., additional, Mignoli, M., additional, Moresco, M., additional, Pompei, E., additional, Pozzetti, L., additional, Saldana Lopez, A., additional, Saxena, A., additional, Santini, P., additional, Schaerer, D., additional, Schreiber, C., additional, Shapley, A. E., additional, Vanzella, E., additional, and Zamorani, G., additional
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- 2023
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15. A polarimetrically oriented X-ray stare at the accreting pulsar EXO 2030+375
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Malacaria, Christian, primary, Heyl, Jeremy, additional, Doroshenko, Victor, additional, Tsygankov, Sergey S., additional, Poutanen, Juri, additional, Forsblom, Sofia V., additional, Capitanio, Fiamma, additional, Di Marco, Alessandro, additional, Du, Yujia, additional, Ducci, Lorenzo, additional, La Monaca, Fabio, additional, Lutovinov, Alexander A., additional, Marshall, Herman L., additional, Mereminskiy, Ilya A., additional, Molkov, Sergey V., additional, Mushtukov, Alexander A., additional, Ng, Mason, additional, Petrucci, Pierre-Olivier, additional, Santangelo, Andrea, additional, Shtykovsky, Andrey E., additional, Suleimanov, Valery F., additional, Agudo, Iván, additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bianchi, Stefano, additional, Bongiorno, Stephen D., additional, Bonino, Raffaella, additional, Brez, Alessandro, additional, Bucciantini, Niccolò, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, Costa, Enrico, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Gesu, Laura, additional, Di Lalla, Niccolò, additional, Donnarumma, Immacolata, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Fabiani, Sergio, additional, Ferrazzoli, Riccardo, additional, Garcia, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Iwakiri, Wataru, additional, Jorstad, Svetlana G., additional, Kaaret, Philip, additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, Latronico, Luca, additional, Liodakis, Ioannis, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Marscher, Alan P., additional, Massaro, Francesco, additional, Matt, Giorgio, additional, Mitsuishi, Ikuyuki, additional, Mizuno, Tsunefumi, additional, Muleri, Fabio, additional, Negro, Michela, additional, Ng, Chi-Yung, additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Papitto, Alessandro, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Puccetti, Simonetta, additional, Ramsey, Brian D., additional, Rankin, John, additional, Ratheesh, Ajay, additional, Roberts, Oliver J., additional, Romani, Roger W., additional, Sgrò, Carmelo, additional, Slane, Patrick, additional, Soffitta, Paolo, additional, Spandre, Gloria, additional, Swartz, Douglas A., additional, Tamagawa, Toru, additional, Tavecchio, Fabrizio, additional, Taverna, Roberto, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Tombesi, Francesco, additional, Trois, Alessio, additional, Turolla, Roberto, additional, Vink, Jacco, additional, Weisskopf, Martin C., additional, Wu, Kinwah, additional, Xie, Fei, additional, and Zane, Silvia, additional
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- 2023
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16. X-ray pulsar GRO J1008−57 as an orthogonal rotator
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Tsygankov, Sergey S., primary, Doroshenko, Victor, additional, Mushtukov, Alexander A., additional, Poutanen, Juri, additional, Di Marco, Alessandro, additional, Heyl, Jeremy, additional, La Monaca, Fabio, additional, Forsblom, Sofia V., additional, Malacaria, Christian, additional, Marshall, Herman L., additional, Suleimanov, Valery F., additional, Svoboda, Jiri, additional, Taverna, Roberto, additional, Ursini, Francesco, additional, Agudo, Iván, additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bianchi, Stefano, additional, Bongiorno, Stephen D., additional, Bonino, Raffaella, additional, Brez, Alessandro, additional, Bucciantini, Niccolò, additional, Capitanio, Fiamma, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, Costa, Enrico, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Gesu, Laura, additional, Di Lalla, Niccolò, additional, Donnarumma, Immacolata, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Fabiani, Sergio, additional, Ferrazzoli, Riccardo, additional, Garcia, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Iwakiri, Wataru, additional, Jorstad, Svetlana G., additional, Kaaret, Philip, additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, Latronico, Luca, additional, Liodakis, Ioannis, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Marscher, Alan P., additional, Massaro, Francesco, additional, Matt, Giorgio, additional, Mitsuishi, Ikuyuki, additional, Mizuno, Tsunefumi, additional, Muleri, Fabio, additional, Negro, Michela, additional, Ng, Chi-Yung, additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Papitto, Alessandro, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Petrucci, Pierre-Olivier, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Puccetti, Simonetta, additional, Ramsey, Brian D., additional, Rankin, John, additional, Ratheesh, Ajay, additional, Roberts, Oliver J., additional, Romani, Roger W., additional, Sgrò, Carmelo, additional, Slane, Patrick, additional, Soffitta, Paolo, additional, Spandre, Gloria, additional, Swartz, Douglas A., additional, Tamagawa, Toru, additional, Tavecchio, Fabrizio, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Tombesi, Francesco, additional, Trois, Alessio, additional, Turolla, Roberto, additional, Vink, Jacco, additional, Weisskopf, Martin C., additional, Wu, Kinwah, additional, Xie, Fei, additional, and Zane, Silvia, additional
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- 2023
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17. Discovery of strongly variable X-ray polarization in the neutron star low-mass X-ray binary transient XTE J1701−462
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Cocchi, Massimo, primary, Gnarini, Andrea, additional, Fabiani, Sergio, additional, Ursini, Francesco, additional, Poutanen, Juri, additional, Capitanio, Fiamma, additional, Bobrikova, Anna, additional, Farinelli, Ruben, additional, Paizis, Adamantia, additional, Sidoli, Lara, additional, Veledina, Alexandra, additional, Bianchi, Stefano, additional, Di Marco, Alessandro, additional, Ingram, Adam, additional, Kajava, Jari J. E., additional, La Monaca, Fabio, additional, Matt, Giorgio, additional, Malacaria, Christian, additional, Mikušincová, Romana, additional, Rankin, John, additional, Zane, Silvia, additional, Agudo, Iván, additional, Antonelli, Lucio A., additional, Bachetti, Matteo, additional, Baldini, Luca, additional, Baumgartner, Wayne H., additional, Bellazzini, Ronaldo, additional, Bongiorno, Stephen D., additional, Bonino, Raffaella, additional, Brez, Alessandro, additional, Bucciantini, Niccolò, additional, Castellano, Simone, additional, Cavazzuti, Elisabetta, additional, Chen, Chien-Ting, additional, Ciprini, Stefano, additional, Costa, Enrico, additional, De Rosa, Alessandra, additional, Del Monte, Ettore, additional, Di Gesu, Laura, additional, Di Lalla, Niccolò, additional, Donnarumma, Immacolata, additional, Doroshenko, Victor, additional, Dovčiak, Michal, additional, Ehlert, Steven R., additional, Enoto, Teruaki, additional, Evangelista, Yuri, additional, Ferrazzoli, Riccardo, additional, Garcia, Javier A., additional, Gunji, Shuichi, additional, Hayashida, Kiyoshi, additional, Heyl, Jeremy, additional, Iwakiri, Wataru, additional, Jorstad, Svetlana G., additional, Kaaret, Philip, additional, Karas, Vladimir, additional, Kislat, Fabian, additional, Kitaguchi, Takao, additional, Kolodziejczak, Jeffery J., additional, Krawczynski, Henric, additional, Latronico, Luca, additional, Liodakis, Ioannis, additional, Maldera, Simone, additional, Manfreda, Alberto, additional, Marin, Frédéric, additional, Marinucci, Andrea, additional, Marscher, Alan P., additional, Marshall, Herman L., additional, Massaro, Francesco, additional, Mitsuishi, Ikuyuki, additional, Mizuno, Tsunefumi, additional, Muleri, Fabio, additional, Negro, Michela, additional, Ng, Chi-Yung, additional, O’Dell, Stephen L., additional, Omodei, Nicola, additional, Oppedisano, Chiara, additional, Papitto, Alessandro, additional, Pavlov, George G., additional, Peirson, Abel L., additional, Perri, Matteo, additional, Pesce-Rollins, Melissa, additional, Petrucci, Pierre-Olivier, additional, Pilia, Maura, additional, Possenti, Andrea, additional, Puccetti, Simonetta, additional, Ramsey, Brian D., additional, Ratheesh, Ajay, additional, Roberts, Oliver J., additional, Romani, Roger W., additional, Sgrò, Carmelo, additional, Slane, Patrick, additional, Soffitta, Paolo, additional, Spandre, Gloria, additional, Swartz, Douglas A., additional, Tamagawa, Toru, additional, Tavecchio, Fabrizio, additional, Taverna, Roberto, additional, Tawara, Yuzuru, additional, Tennant, Allyn F., additional, Thomas, Nicholas E., additional, Tombesi, Francesco, additional, Trois, Alessio, additional, Tsygankov, Sergey S., additional, Turolla, Roberto, additional, Vink, Jacco, additional, Weisskopf, Martin C., additional, Wu, Kinwah, additional, and Xie, Fei, additional
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- 2023
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18. The WISSH quasars project. XI. The mean spectral energy distribution and bolometric corrections of the most luminous quasars
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Saccheo, I., primary, Bongiorno, A., additional, Piconcelli, E., additional, Testa, V., additional, Bischetti, M., additional, Bisogni, S., additional, Bruni, G., additional, Cresci, G., additional, Feruglio, C., additional, Fiore, F., additional, Grazian, A., additional, Luminari, A., additional, Lusso, E., additional, Mainieri, V., additional, Maiolino, R., additional, Marconi, A., additional, Ricci, F., additional, Tombesi, F., additional, Travascio, A., additional, Vietri, G., additional, Vignali, C., additional, Zappacosta, L., additional, and La Franca, F., additional
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- 2022
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19. Mass assembly and active galactic nucleus activity at z ≳ 1.5 in the dense environment of XDCP J0044.0–2033
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Lepore, M., primary, Bongiorno, A., additional, Tozzi, P., additional, Travascio, A., additional, Zappacosta, L., additional, Merlin, E., additional, and Fassbender, R., additional
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- 2022
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20. The WISSH quasars project
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Vietri, G., primary, Misawa, T., additional, Piconcelli, E., additional, Franzetti, P., additional, Luminari, A., additional, Travascio, A., additional, Bischetti, M., additional, Bisogni, S., additional, Bongiorno, A., additional, Bruni, G., additional, Feruglio, C., additional, Giunta, A., additional, Nicastro, F., additional, Saccheo, I., additional, Testa, V., additional, Tombesi, F., additional, Vignali, C., additional, Zappacosta, L., additional, and Fiore, F., additional
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- 2022
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21. The faintest solar coronal hard X-rays observed with FOXSI
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Buitrago-Casas, Juan Camilo, primary, Glesener, Lindsay, additional, Christe, Steven, additional, Krucker, Säm, additional, Vievering, Juliana, additional, Athiray, P. S., additional, Musset, Sophie, additional, Davis, Lance, additional, Courtade, Sasha, additional, Dalton, Gregory, additional, Turin, Paul, additional, Turin, Zoe, additional, Ramsey, Brian, additional, Bongiorno, Stephen, additional, Ryan, Daniel, additional, Takahashi, Tadayuki, additional, Furukawa, Kento, additional, Watanabe, Shin, additional, Narukage, Noriyuki, additional, Ishikawa, Shin-nosuke, additional, Mitsuishi, Ikuyuki, additional, Hagino, Kouichi, additional, Shourt, Van, additional, Duncan, Jessie, additional, Zhang, Yixian, additional, and Bale, Stuart D., additional
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- 2022
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22. Capturing dual AGN activity and kiloparsec-scale outflows in IRAS 20210+1121
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Fabrizio Fiore, C. Vignali, Chiara Feruglio, Bernd Husemann, M. Bischetti, Enrico Piconcelli, C. Ramos Almeida, G. Vietri, Angela Bongiorno, F. G. Saturni, Sara Cazzoli, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Saturni, FRANCESCO GABRIELE, Vietri, Giustina, Piconcelli, Enrico, Christian, Vignali, Bischetti, Manuela, Bongiorno, Angela, Sara, Cazzoli, Feruglio, Chiara, Fiore, Fabrizio, Bernd, Husemann, Cristina Ramos, Almeida, ITA, Saturni F.G., Vietri G., Piconcelli E., Vignali C., Bischetti M., Bongiorno A., Cazzoli S., Feruglio C., Fiore F., Husemann B., and Almeida C.R.
- Subjects
Seyfert [Galaxies] ,Galaxies: Seyfert ,Active galactic nucleus ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,active [Galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,galaxies active ,Quasars: supermassive black holes ,FOS: Physical sciences ,Context (language use) ,Galaxies: groups: general ,quasars supermassive black holes ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxy merger ,galaxies groups general ,emission lines [Quasars] ,Astrophysics::Galaxy Astrophysics ,Physics ,Supermassive black hole ,Quasars: emission lines ,Star formation ,Quasars: emission line ,Astronomy and Astrophysics ,Galaxies: active ,Astrophysics - Astrophysics of Galaxies ,Galaxies: groups: individual: IRAS 20210+1121 ,Galaxy ,Accretion (astrophysics) ,Interstellar medium ,groups: general [Galaxies] ,groups: individual: IRAS 20210+1121 [Galaxies] ,Space and Planetary Science ,galaxies groups individual IRAS 20210+1121 ,Astrophysics of Galaxies (astro-ph.GA) ,galaxies Seyfert ,quasars emission line ,Astrophysics - Cosmology and Nongalactic Astrophysics ,supermassive black holes [Quasars] - Abstract
The most standard scenario for the evolution of massive galaxies across cosmic time assumes a correspondence based on the interplay between active galactic nuclei (AGN) feedback, which injects large amounts of energy into the host environment, and galaxy mergers, with their ability to trigger massive star formation events and accretion onto supermassive black holes. Interacting systems hosting AGN are useful laboratories for obtaining key insights into both phenomena. In this context, we present an analysis of the optical spectral properties of IRAS 20210+1121 (I20210), a merging system at z = 0.056. According to X-ray data, this object comprises two interacting galaxies, each hosting an obscured AGN. The optical spectra confirm the presence of AGN features in both galaxies. In particular, we are able to provide a Seyfert classification for I20210 North. The spectrum of I20120 South shows broad blueshifted components associated with the most intense emission lines that indicate the presence of an ionized outflow, for which we derive a maximum velocity of ∼2000 km s-1, an extension of ∼2 kpc, and a mass rate of ∼0.6 M⊙ yr-1. We also report the existence of an ionized nebular component with v ∼ 1000 km s-1 at ∼6.5 kpc southwards of I20210 South, which can be interpreted as disrupted gas ejected from the host galaxy by the action of the outflow. I20120 therefore exhibits a double obscured AGN, with one of them showing evidence of ongoing events for AGN-powered outflows. Future spatially resolved spectroscopy will allow for an accurate mapping of the gas kinematics in this AGN pair and evaluate the impact of the outflow on both the interstellar medium and the galaxy environment. © ESO 2021., GV, EP, CV, MB, CF and FF acknowledge support from PRIN MIUR project "Black Hole winds and the Baryon Life Cycle of Galaxies: the stone-guest at the galaxy evolution supper", contract #2017PH3WAT. GV also acknowledges financial support from Premiale 2015 MITic (PI: B. Garilli). CRA acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MCIU) under grant with reference RYC-2014-15779, from the European Union's Horizon 2020 research and innovation programme under Marie Skodowska-Curie grant agreement No 860744 (BiD4BESt), from the State Research Agency (AEI-MCINN) of the Spanish MCIU under grants "Feeding and feedback in active galaxies" with reference PID2019-106027GB-C42, "Feeding, feedback and obscuration in active galaxies" with reference AYA2016-76682-C3-2-P, and "Quantifying the impact of quasar feedback on galaxy evolution (QSOFEED)" with reference EUR2020-112266. CRA also acknowledges support from the Consejeria de Economia, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant with reference ProID2020010105 and from IAC project P/301404, financed by the Ministry of Science and Innovation, through the State Budget and by the Canary Islands Department of Economy, Knowledge and Employment, through the Regional Budget of the Autonomous Community. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
- Published
- 2021
23. The VANDELS survey: Global properties of CIII]λ1908 Å emitting star-forming galaxies at z ∼ 3
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Ross J. McLure, P. Hibon, Daniel Schaerer, G. Zamorani, M. Castellano, D. J. McLeod, Ricardo Amorín, A. C. Carnall, Laura Pentericci, M. Llerena, Margherita Talia, A. Saxena, Angela Bongiorno, Adriano Fontana, F. Mannucci, A. Calabrò, Enrique Perez-Montero, Fergus Cullen, F. Marchi, Nimish P. Hathi, European Commission, and Ministerio de Ciencia e Innovación (España)
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Physics ,Galaxies: abundances ,Galaxies: high-redshift ,abundances [Galaxies] ,Galaxies: evolution ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,Galaxies: formation ,evolution [Galaxies] ,formation [Galaxies] ,Galaxy ,galaxies [Ultraviolet] ,high-redshift [Galaxies] ,Space and Planetary Science ,Ultraviolet: galaxies ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Context. Strong nebular emission is ubiquitous in galaxies that contribute to cosmic reionization at redshift z ≳ 6. High-ionization UV metal lines, such as CIII]λ1908 Å, show high equivalent widths (EW) in these early galaxies, suggesting harder radiation fields at low metallicity than low-z galaxies of similar stellar mass. Understanding the physical properties driving the observed UV nebular line emission at high-z requires large and very deep spectroscopic surveys, which are now only accessible out to z ∼ 4. Aims. We study the mean properties of a large representative sample of 217 galaxies showing CIII] emission at 2, his work is based on data products from observations made with ESO Telescopes at La Silla Paranal Observatory under ESO program ID 194.A-2003 (PIs: Laura Pentericci and Ross McLure). MLl acknowledges support from the National Agency for Research and Development (ANID)/Scholarship Program/Doctorado Nacional/2019-21191036. RA acknowledges support from ANID FONDECYT Regular Grant 1202007. This work has made extensive use of Python packages astropy (Astropy Collaboration 2018), numpy (Harris et al. 2020), and Matplotlib (Hunter 2007)., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
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- 2022
24. The WISSH quasars project: XI. The mean spectral energy distribution and bolometric corrections of the most luminous quasars.
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Saccheo, I., Bongiorno, A., Piconcelli, E., Testa, V., Bischetti, M., Bisogni, S., Bruni, G., Cresci, G., Feruglio, C., Fiore, F., Grazian, A., Luminari, A., Lusso, E., Mainieri, V., Maiolino, R., Marconi, A., Ricci, F., Tombesi, F., Travascio, A., and Vietri, G.
- Subjects
- *
SPECTRAL energy distribution , *STELLAR luminosity function , *ACTIVE galactic nuclei , *QUASARS , *INTERSTELLAR medium - Abstract
Context. Hyperluminous quasi-stellar objects (QSOs) are ideal laboratories to investigate active galactic nucleus (AGN) feedback mechanisms. Their formidable energy release causes powerful winds at all scales, and thus the maximum feedback is expected. Aims. Our aim is to derive the mean spectral energy distribution (SED) of a sample of 85 WISE-SDSS selected hyperluminous (WISSH) quasars. Since the SED provides a direct way to investigate the AGN structure, our goal is to understand if quasars at the bright end of the luminosity function have peculiar properties compared to the bulk of the QSO population. Methods. We collected all the available photometry, from X-rays to the far-infrared (FIR); each WISSH quasar is observed in at least 12 different bands. We then built a mean intrinsic SED after correcting for the dust extinction, absorption and emission lines, and intergalactic medium absorption. We also derived bolometric, IR band, and monochromatic luminosities together with bolometric corrections at λ = 5100 Å and 3 μm. We define a new relation for the 3 μm bolometric correction. Results. We find that the mean SED of hyperluminous WISSH QSOs shows some differences compared to that of less luminous sources (i.e., a lower X-ray emission and a near- and mid-IR excess which can be explained assuming a larger dust contribution. WISSH QSOs have stronger emission from both warm (T ∼ 500 − 600 K) and very hot (T ≥ 1000 K) dust, the latter being responsible for shifting the typical dip of the AGN SED from 1.3 μm to 1.1 μm. We also derived the mean SEDs of two subsamples created based on their spectral features (presence of broad absorption lines and equivalent width of CIV line). We confirm that broad absorption lines (BALs) are X-ray weak and that they have a reddened UV-optical continuum. We also find that BALs tend to have stronger emission from the hot dust component. For sources with a weaker CIV line, our main result is the confirmation of their lower X-ray emission. By populating the LIR vs. z diagram proposed by Symeonidis & Page (MNRAS, 503, 3992), we found that ∼90% of WISSH QSOs with z ≥ 3.5 have their FIR emission dominated by star-forming activity. Conclusions. This analysis suggests that hyperluminous QSOs have a peculiar SED compared to less luminous objects. It is therefore critical to use SED templates constructed exclusively from very bright quasar samples (such as this one) when dealing with particularly luminous sources, such as high-redshift QSOs. [ABSTRACT FROM AUTHOR]
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- 2023
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25. Mass assembly and active galactic nucleus activity at z ≳ 1.5 in the dense environment of XDCP J0044.0–2033
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M. Lepore, A. Bongiorno, P. Tozzi, A. Travascio, L. Zappacosta, E. Merlin, and R. Fassbender
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Space and Planetary Science ,Astronomy and Astrophysics - Abstract
Context. XDCP J0044.0−2033 is the most massive galaxy cluster known at z > 1.5 and its core shows a high density of galaxies, which are experiencing mergers and hosting nuclear activity. Aims. We present a multi-wavelength study of a region of 24 kpc × 24 kpc located ∼157 kpc from the center of the cluster, for which we have photometric and spectroscopic observations. Our main goal is to investigate the environmental effects acting on the galaxies inhabiting this high-density region. Methods. We performed source identification and a photometric analysis on high-resolution Hubble Space Telescope (HST) images in the F105W, F140W, and F160W bands and a spectroscopic analysis of the near-infrared (NIR) KMOS data in H and YJ bands. In addition, we analyzed the deep Chandra ACIS-S X-ray exposure. Results. We find that the analyzed region hosts at least nine different sources –six of them confirmed to be cluster members within a narrow redshift range 1.5728 z Complex M and Complex N) at a projected distance of ∼13 kpc, which are undergoing merging on an estimated timescale of 10−30 Myr. One of the sources shows the presence of a broad Hα emission line and is classified as a Type-1 active galactic nucleus (AGN). This AGN is associated to an X-ray point-like source whose emission appears moderately obscured (with intrinsic absorption NH ∼ 1022 cm−2) and hosts a relatively massive black hole (BH) with a mass of MBH ∼ 107 M⊙, which is accreting with an Eddington ratio of ∼0.2. Conclusions. We conclude that the region analyzed here is consistent with being the formation site of a secondary brightest cluster galaxy (BCG). These findings, together with an in-depth analysis of the X-ray morphology of the cluster, suggest a merging scenario for the entire cluster, with two massive halos both harboring two rapidly evolving BCGs on the verge of being assembled. Our results are also consistent with the scenario in which the AGN phase in member galaxies is triggered by gas-rich mergers and plays a relevant role in the formation of the red sequence of elliptical galaxies observed in the center of local galaxy clusters.
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- 2022
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26. The WISSH quasars project: VIII. Outflows and metals in the circum-galactic medium around the hyper-luminous z ∼ 3.6 quasar J1538+08
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M. Bischetti, Sebastiano Cantalupo, F. Duras, Michele Ginolfi, Enrico Piconcelli, Fabrizio Fiore, Chiara Feruglio, A. Travascio, C. Vignali, G. Vietri, F. Arrigoni Battaia, Luca Zappacosta, Valentina D'Odorico, Angela Bongiorno, Travascio, A, Zappacosta, L, Cantalupo, S, Piconcelli, E, Arrigoni Battaia, F, Ginolfi, M, Bischetti, M, Vietri, G, Bongiorno, A, D'Odorico, V, Duras, F, Feruglio, C, Vignali, C, Fiore, F, Travascio, A., Zappacosta, Luca, Cantalupo, S., Piconcelli, Enrico, Arrigoni Battaia, F., Ginolfi, M., Bischetti, Manuela, Vietri, Giustina, Bongiorno, Angela, D'Odorico, Valentina, Duras, Federica, Feruglio, Chiara, Vignali, C., Fiore, Fabrizio, Travascio A., Zappacosta L., Cantalupo S., Piconcelli E., Arrigoni Battaia F., Ginolfi M., Bischetti M., Vietri G., Bongiorno A., D'Odorico V., Duras F., Feruglio C., Vignali C., Fiore F., ITA, DEU, and CHE
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quasars emission lines ,Astrophysics::High Energy Astrophysical Phenomena ,galaxies active ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,intergalactic medium ,quasars individual SDSS153830 ,55+085517 ,0 ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Intergalactic medium ,Physics ,Nebula ,active ,quasars: emission lines ,quasars: individual: SDSS 153830.55+085517.0 [galaxies] ,010308 nuclear & particles physics ,Quasars: individual: SDSS 153830.55+085517.0 ,Quasars: emission line ,Velocity dispersion ,Astronomy and Astrophysics ,Quasar ,Galaxies: active ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Intergalactic travel ,quasars emission line - Abstract
During the last years, Ly$\alpha$ nebulae have been routinely detected around high-z, radio-quiet quasars (RQQs) thanks to the advent of sensitive integral field spectrographs. Constraining the physical properties of the Ly$\alpha$ nebulae is crucial for a full understanding of the circum-galactic medium (CGM), which is a venue of feeding and feedback processes. The most luminous quasars are privileged test-beds to study these processes, given their large ionizing fluxes and dense CGM environments in which they are expected to be embedded. We aim at characterizing the rest-frame UV emission lines in the CGM around a hyper-luminous, broad emission line, RQQ at z~3.6, that exhibits powerful outflows at both nuclear and host galaxy scales. We analyze VLT/MUSE observations of the quasar J1538+08 and perform a search for extended UV emission lines to characterize its morphology, emissivity, kinematics and metal content. We report the discovery of a very luminous ($\sim2 \times10^{44}~erg~s^{-1}$), giant Ly$\alpha$ nebula and a likely associated extended CIV nebula. The Ly$\alpha$ nebula emission exhibits moderate blueshift compared with the quasar systemic redshift and large average velocity dispersion ($\sigma_{v}$ ~700 $km~s^{-1}$) across the nebula, while the CIV nebula shows $\sigma_{v}$~$350~km~s^{-1}$. The Ly$\alpha$ line profile exhibits a significant asymmetry towards negative velocity values at 20-30 kpc south of the quasar and is well parameterized by two Gaussian components: a narrow ($\sigma$~$470~km~s^{-1}$) systemic one plus a broad ($\sigma$~1200 $km~s^{-1}$), blueshifted (~1500 $km~s^{-1}$) one. Our analysis of the MUSE observation of J1538+08 reveals metal-enriched CGM around this hyper-luminous quasar and our detection of blueshifted emission in the line profile of the Ly$\alpha$ nebula suggests that powerful nuclear outflows can propagate through the CGM over tens of kpc., Comment: 14 pages, 16 figures, 2 tables. Accepted for publication in A&A Journal
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- 2020
27. Entomological and parasitological study on phlebotomine sandflies in central and northern Albania
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Velo E., Paparisto A., Bongiorno G., Di Muccio T., Khoury C., Bino S., Gramiccia M., Gradoni L., and Maroli M.
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phlebotomine sandfly ,feeding habit ,Leishmania ,PCR ,Albania ,Infectious and parasitic diseases ,RC109-216 - Abstract
An entomological survey was carried out in two districts of central (Kruje) and northern (Lezhe) Albania. Six collecting sites, showing a variety of diurnal resting sites, were monitored for adult sandflies from June through October 2002. Flies were collected with CDC miniature light traps, sticky traps and mechanical or hand aspirators in peridomestic sites, in bedrooms and inside cow barns, chicken coops and pigpens. All collecting sites monitored were found positive for sandflies. A total of 849 specimens were caught (29.2 % males) belonging to five Phlebotomus species. Phlebotomus neglectus (75.6 %) was the most abundant species followed by P. perfiliewi (14.4 %), P. papatasi (4.6 %), P. tobbi (3.6 %) and P. similis (1.8 %). The first adult of P. neglectus appeared on June 11 and the last one was collected on October 16. The highest density for this species was observed at the end of July. A total of 111 blood-fed females were caught from the two areas studied. P. neglectus was the only species found blood fed in Lezhe and the same species was prevalent (56.1 %) in Kruje followed by P. perfiliewi (30.3 %), P. tobbi (10.6 %); P. papatasi was represented by only two specimens. Blood meal origin was determined in 45/66 (68.2 %) of the females tested from Kruje district. P. neglectus was found fed on four hosts, showing the following feeding patterns: cow (71.4 %), dog (17.1 %), chicken (5.7 %) and human (5.7 %) ; P. perfiliewi was found fed on cow (80.0 %) and chicken (20.0 %), P. tobbi on cow (50.0 %), chicken (25.0 %) and dog (25.0 %). One specimen of P. papatasi was found fed on cow. When such prevalences were analysed by the available biomass for each host present at the collecting site, P. neglectus resulted to be an opportunistic feeder rather than exhibiting preferences for any specific animal. PCR analysis of 39 P. neglectus from the Lezhe district gave negative results for the presence of Leishmania DNA.
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- 2005
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28. The VANDELS survey: Global properties of CIII]λ1908 Å emitting star-forming galaxies at z ∼ 3
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Llerena, M., primary, Amorín, R., additional, Cullen, F., additional, Pentericci, L., additional, Calabrò, A., additional, McLure, R., additional, Carnall, A., additional, Pérez-Montero, E., additional, Marchi, F., additional, Bongiorno, A., additional, Castellano, M., additional, Fontana, A., additional, McLeod, D. J., additional, Talia, M., additional, Hathi, N. P., additional, Hibon, P., additional, Mannucci, F., additional, Saxena, A., additional, Schaerer, D., additional, and Zamorani, G., additional
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- 2022
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29. X-ray spectroscopic survey of highly accreting AGN
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Laurenti, M., primary, Piconcelli, E., additional, Zappacosta, L., additional, Tombesi, F., additional, Vignali, C., additional, Bianchi, S., additional, Marziani, P., additional, Vagnetti, F., additional, Bongiorno, A., additional, Bischetti, M., additional, del Olmo, A., additional, Lanzuisi, G., additional, Luminari, A., additional, Middei, R., additional, Perri, M., additional, Ricci, C., additional, and Vietri, G., additional
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- 2022
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30. Track insulation verification and measurement
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Bongiorno Jacopo and Mariscotti Andrea
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Engineering (General). Civil engineering (General) ,TA1-2040 - Abstract
Methods for the measurement of track insulation are reviewed pointing out minimum necessary conditions and practical aspects, as well as consistency and repeatability of results. Track configuration, need of electrical sectioning and use of external electrodes or conductive structure are key parameters to determine suitable methods.
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- 2018
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31. The faintest solar coronal hard X-rays observed with FOXSI
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Juan Camilo Buitrago-Casas, Lindsay Glesener, Steven Christe, Säm Krucker, Juliana Vievering, P. S. Athiray, Sophie Musset, Lance Davis, Sasha Courtade, Gregory Dalton, Paul Turin, Zoe Turin, Brian Ramsey, Stephen Bongiorno, Daniel Ryan, Tadayuki Takahashi, Kento Furukawa, Shin Watanabe, Noriyuki Narukage, Shin-nosuke Ishikawa, Ikuyuki Mitsuishi, Kouichi Hagino, Van Shourt, Jessie Duncan, Yixian Zhang, and Stuart D. Bale
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Context. Solar nanoflares are small impulsive events releasing magnetic energy in the corona. If nanoflares follow the same physics as their larger counterparts, they should emit hard X-rays (HXRs) but with a rather faint intensity. A copious and continuous presence of nanoflares would result in a sustained HXR emission. These nanoflares could deliver enormous amounts of energy into the solar corona, possibly accounting for its high temperatures. To date, there has not been any direct observation of such persistent HXRs from the quiescent Sun. However, the quiet-Sun HXR emission was constrained in 2010 using almost 12 days of quiescent solar off-pointing observations by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). These observations set 2σ upper limits at 3.4 × 10−2 photons s−1 cm−2 keV−1 and 9.5 × 10−4 photons s−1 cm−2 keV−1 for the 3–6 keV and 6–12 keV energy ranges, respectively. Aims. Observing faint HXR emission is challenging because it demands high sensitivity and dynamic range instruments. The Focusing Optics X-ray Solar Imager (FOXSI) sounding rocket experiment excels in these two attributes when compared with RHESSI. FOXSI completed its second and third successful flights (FOXSI-2 and -3) on December 11, 2014, and September 7, 2018, respectively. This paper aims to constrain the quiet-Sun emission in the 5–10 keV energy range using FOXSI-2 and -3 observations. Methods. To fully characterize the sensitivity of FOXSI, we assessed ghost ray backgrounds generated by sources outside of the field of view via a ray-tracing algorithm. We used a Bayesian approach to provide upper thresholds of quiet-Sun HXR emission and probability distributions for the expected flux when a quiet-Sun HXR source is assumed to exist. Results. We found a FOXSI-2 upper limit of 4.5 × 10−2 photons s−1 cm−2 keV−1 with a 2σ confidence level in the 5–10 keV energy range. This limit is the first-ever quiet-Sun upper threshold in HXR reported using ∼1 min observations during a period of high solar activity. RHESSI was unable to measure the quiet-Sun emission during active times due to its limited dynamic range. During the FOXSI-3 flight, the Sun exhibited a fairly quiet configuration, displaying only one aged nonflaring active region. Using the entire ∼6.5 min of FOXSI-3 data, we report a 2σ upper limit of ∼10−4 photons s−1 cm−2 keV−1 for the 5–10 keV energy range. Conclusions. The FOXSI-3 upper limits on quiet-Sun emission are similar to that previously reported, but FOXSI-3 achieved these results with only 5 min of observations or about 1/2600 less time than RHESSI. A possible future spacecraft using hard X-ray focusing optics like those in the FOXSI concept would allow enough observation time to constrain the current HXR quiet-Sun limits further, or perhaps even make direct detections. This is the first report of quiet-Sun HXR limits from FOXSI and the first science paper using FOXSI-3 observations.
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- 2022
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32. The IBISCO survey
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Zanchettin, M. V., primary, Feruglio, C., additional, Bischetti, M., additional, Malizia, A., additional, Molina, M., additional, Bongiorno, A., additional, Dadina, M., additional, Gruppioni, C., additional, Piconcelli, E., additional, Tombesi, F., additional, Travascio, A., additional, and Fiore, F., additional
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- 2021
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33. Capturing dual AGN activity and kiloparsec-scale outflows in IRAS 20210+1121
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Saturni, F. G., primary, Vietri, G., additional, Piconcelli, E., additional, Vignali, C., additional, Bischetti, M., additional, Bongiorno, A., additional, Cazzoli, S., additional, Feruglio, C., additional, Fiore, F., additional, Husemann, B., additional, and Ramos Almeida, C., additional
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- 2021
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34. The gentle monster PDS 456: Kiloparsec-scale molecular outflow and its implications for QSO feedback
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Marcella Brusa, M. Bischetti, Chiara Feruglio, Fabrizio Fiore, Luca Zappacosta, C. Vignali, Enrico Piconcelli, Giovanni Cresci, Alessandro Marconi, Emanuele Nardini, Vincenzo Mainieri, Angela Bongiorno, S. Carniani, Claudia Cicone, Roberto Maiolino, Maiolino, Roberto [0000-0002-4985-3819], Apollo - University of Cambridge Repository, Bischetti, Manuela, Piconcelli, Enrico, Feruglio, Chiara, Fiore, Fabrizio, Carniani, S., Brusa, M., Cicone, Claudia, Vignali, C., Bongiorno, Angela, Cresci, Giovanni, Mainieri, V., Maiolino, R., Marconi, Alessandro, Nardini, Emanuele, Zappacosta, Luca, Bischetti M., Piconcelli E., Feruglio C., Fiore F., Carniani S., Brusa M., Cicone C., Vignali C., Bongiorno A., Cresci G., Mainieri V., Maiolino R., Marconi A., Nardini E., Zappacosta L., ITA, GBR, DEU, Bischetti, M., Piconcelli, E., Feruglio, C., Fiore, F., Cicone, C., Bongiorno, A., Cresci, G., Marconi, A., Nardini, E., and Zappacosta, L.
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quasars individual PDS456 ,quasars emission lines ,quasars: individual: PDS 456 ,active [Galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,Continuum (design consultancy) ,galaxies: active ,galaxies active ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Luminosity ,Settore FIS/05 - Astronomia e Astrofisica ,0103 physical sciences ,Radiative transfer ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,galaxies: active, quasars: individual: PDS 456, galaxies: evolution, quasars: emission lines, techniques: imaging spectroscopy, techniques: interferometric, Astrophysics - Astrophysics of Galaxies ,010308 nuclear & particles physics ,imaging spectroscopy [Techniques] ,techniques imaging spectroscopy ,emission line [Quasars] ,Astronomy and Astrophysics ,evolution [Galaxies] ,individual: PDS 456 [Quasars] ,Astrophysics - Astrophysics of Galaxies ,galaxies evolution ,Interstellar medium ,quasars: emission lines ,Stars ,Radiation pressure ,13. Climate action ,Space and Planetary Science ,techniques interferometric ,techniques: imaging spectroscopy ,techniques: interferometric ,Astrophysics of Galaxies (astro-ph.GA) ,interferometric [Techniques] ,Outflow ,quasars emission line ,galaxies: evolution - Abstract
We report on the first ALMA observation of the CO(3$-$2) and rest-frame ~340 GHz continuum emission in PDS 456, which is the most luminous, radio-quiet QSO in the local Universe ($z$~0.18), with a bolometric luminosity $L_{\rm Bol}\sim10^{47}$ erg s$^{-1}$. ALMA angular resolution allowed us to map scales as small as ~700 pc. The molecular gas reservoir, traced by the core of the very bright CO(3$-$2) emission line, is distributed in a compact rotating disk, with size of ~1.3 kpc, seen close to face-on ($i$~25 deg). Fast CO(3$-$2) emission in the velocity range $v\in[-1000,+500]$ km s$^{-1}$ is also present. Specifically, we detect several blue-shifted clumps out to ~5 kpc from the nucleus, in addition to a compact ($R\lesssim1.2$ kpc), broad emission component. These components reveal a galaxy-wide molecular outflow, with a total mass $M_{\rm mol}^{\rm out}\sim2.5\times10^8$ $M_{\odot}$ and a mass outflow rate $\dot{M}_{\rm mol}\sim290$ $M_{\odot}$ yr$^{-1}$. The corresponding depletion time is ~8 Myr, shorter than the rate at which the molecular gas is converted into stars, indicating that the detected outflow is potentially able to quench star-formation in the host. The momentum flux of the molecular outflow normalised to the radiative momentum output (i.e. $L_{\rm Bol}/c$) is $\lesssim1$, comparable to that of the X-ray ultra-fast outflow (UFO) detected in PDS 456. This is at odds with the expectations for an energy-conserving expansion suggested for most of the large-scale outflows detected in low-luminosity AGN so far. We suggest three possible scenarios that may explain this observation: (i) in very luminous AGN such as our target the molecular gas phase is tracing only a fraction of the total outflowing mass; (ii) a small coupling between the shocked gas by the UFO and the host-galaxy ISM (iii) AGN radiation pressure may play an important role in driving the outflow., Accepted in A&A
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- 2019
35. Universal bolometric corrections for active galactic nuclei over seven luminosity decades
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Enrico Piconcelli, F. Duras, Francesca Onori, Fabrizio Fiore, Federica Ricci, Roberto Maiolino, Angela Bongiorno, F. La Franca, Stefano Bianchi, E. Sani, Elisabeta Lusso, Francesco Shankar, Raffaella Schneider, Alessandro Marconi, C. Vignali, 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), Duras, F., Bongiorno, A., Ricci, F., Piconcelli, E., Shankar, F., Lusso, E., Bianchi, S., Fiore, F., Maiolino, R., Marconi, A., Onori, F., Sani, E., Schneider, R., Vignali, C., La Franca, F., Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository
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Galaxies: fundamental parameters ,Active galactic nucleus ,Demographics ,quasars ,Population ,Quasars: supermassive black holes ,active ,Astrophysics ,01 natural sciences ,law.invention ,law ,galaxies ,evolution ,X-rays ,0103 physical sciences ,Bolometric correction ,education ,010303 astronomy & astrophysics ,Physics ,education.field_of_study ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Bolometer ,supermassive black holes ,Galaxies: evolution ,Astronomy and Astrophysics ,Galaxies: active ,Black hole physics ,Astrophysics - Astrophysics of Galaxies ,Accretion (astrophysics) ,Redshift ,X-rays: galaxies ,Black hole physicsGalaxies: activeGalaxies: evolutionGalaxies: fundamental parametersQuasars: supermassive black holesX-rays: galaxies ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Order of magnitude ,fundamental parameters - Abstract
The AGN bolometric correction is a key element to understand BH demographics and compute accurate BH accretion histories from AGN luminosities. However, current estimates still differ from each other by up to a factor of two to three, and rely on extrapolations at the lowest and highest luminosities. Here we revisit this fundamental issue presenting general hard X-ray ($K_{X}$) and optical ($K_{O}$) bolometric corrections, computed combining several AGN samples spanning the widest (about 7 dex) luminosity range ever used for this kind of studies. We analysed a total of $\sim 1000$ type 1 and type 2 AGN for which a dedicated SED-fitting has been carried out. We provide a bolometric correction separately for type 1 and type 2 AGN; the two bolometric corrections results to be in agreement in the overlapping luminosity range and therefore, for the first time, a universal bolometric correction for the whole AGN sample (both type 1 and type 2) has been computed. We found that $K_{X}$ is fairly constant at $log(L_{BOL}/L_{\odot}) < 11$, while it increases up to about one order of magnitude at $log(L_{BOL}/L_{\odot}) \sim 14.5$. A similar increasing trend has been observed when its dependence on either the Eddington ratio or the BH mass is considered, while no dependence on redshift up to $z\sim3.5$ has been found. On the contrary, the optical bolometric correction appears to be fairly constant (i.e. $K_{O} \sim 5$) whatever is the independent variable. We also verified that our bolometric corrections correctly predict the AGN bolometric luminosity functions. According to this analysis, our bolometric corrections can be applied to the whole AGN population in a wide range of luminosity and redshift., STFC ERC
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- 2020
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36. Capturing dual AGN activity and kiloparsec-scale outflows in IRAS 20210+1121
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European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Saturni, F. G., Vietri, G., Piconcelli, E., Vignali, C., Bischetti, M., Bongiorno, A., Cazzoli, S., Feruglio, C., Fiore, F., Husemann, B., Ramos Almeida, C., European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Saturni, F. G., Vietri, G., Piconcelli, E., Vignali, C., Bischetti, M., Bongiorno, A., Cazzoli, S., Feruglio, C., Fiore, F., Husemann, B., and Ramos Almeida, C.
- Abstract
The most standard scenario for the evolution of massive galaxies across cosmic time assumes a correspondence based on the interplay between active galactic nuclei (AGN) feedback, which injects large amounts of energy into the host environment, and galaxy mergers, with their ability to trigger massive star formation events and accretion onto supermassive black holes. Interacting systems hosting AGN are useful laboratories for obtaining key insights into both phenomena. In this context, we present an analysis of the optical spectral properties of IRAS 20210+1121 (I20210), a merging system at z = 0.056. According to X-ray data, this object comprises two interacting galaxies, each hosting an obscured AGN. The optical spectra confirm the presence of AGN features in both galaxies. In particular, we are able to provide a Seyfert classification for I20210 North. The spectrum of I20120 South shows broad blueshifted components associated with the most intense emission lines that indicate the presence of an ionized outflow, for which we derive a maximum velocity of ∼2000 km s-1, an extension of ∼2 kpc, and a mass rate of ∼0.6 M⊙ yr-1. We also report the existence of an ionized nebular component with v ∼ 1000 km s-1 at ∼6.5 kpc southwards of I20210 South, which can be interpreted as disrupted gas ejected from the host galaxy by the action of the outflow. I20120 therefore exhibits a double obscured AGN, with one of them showing evidence of ongoing events for AGN-powered outflows. Future spatially resolved spectroscopy will allow for an accurate mapping of the gas kinematics in this AGN pair and evaluate the impact of the outflow on both the interstellar medium and the galaxy environment. © ESO 2021.
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- 2021
37. The VANDELS ESO public spectroscopic survey
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Garilli, B., primary, McLure, R., additional, Pentericci, L., additional, Franzetti, P., additional, Gargiulo, A., additional, Carnall, A., additional, Cucciati, O., additional, Iovino, A., additional, Amorin, R., additional, Bolzonella, M., additional, Bongiorno, A., additional, Castellano, M., additional, Cimatti, A., additional, Cirasuolo, M., additional, Cullen, F., additional, Dunlop, J., additional, Elbaz, D., additional, Finkelstein, S., additional, Fontana, A., additional, Fontanot, F., additional, Fumana, M., additional, Guaita, L., additional, Hartley, W., additional, Jarvis, M., additional, Juneau, S., additional, Maccagni, D., additional, McLeod, D., additional, Nandra, K., additional, Pompei, E., additional, Pozzetti, L., additional, Scodeggio, M., additional, Talia, M., additional, Calabrò, A., additional, Cresci, G., additional, Fynbo, J. P. U., additional, Hathi, N. P., additional, Hibon, P., additional, Koekemoer, A. M., additional, Magliocchetti, M., additional, Salvato, M., additional, Vietri, G., additional, Zamorani, G., additional, Almaini, O., additional, Balestra, I., additional, Bardelli, S., additional, Begley, R., additional, Brammer, G., additional, Bell, E. F., additional, Bowler, R. A. A., additional, Brusa, M., additional, Buitrago, F., additional, Caputi, C., additional, Cassata, P., additional, Charlot, S., additional, Citro, A., additional, Cristiani, S., additional, Curtis-Lake, E., additional, Dickinson, M., additional, Fazio, G., additional, Ferguson, H. C., additional, Fiore, F., additional, Franco, M., additional, Georgakakis, A., additional, Giavalisco, M., additional, Grazian, A., additional, Hamadouche, M., additional, Jung, I., additional, Kim, S., additional, Khusanova, Y., additional, Le Fèvre, O., additional, Longhetti, M., additional, Lotz, J., additional, Mannucci, F., additional, Maltby, D., additional, Matsuoka, K., additional, Mendez-Hernandez, H., additional, Mendez-Abreu, J., additional, Mignoli, M., additional, Moresco, M., additional, Nonino, M., additional, Pannella, M., additional, Papovich, C., additional, Popesso, P., additional, Roberts-Borsani, G., additional, Rosario, D. J., additional, Saldana-Lopez, A., additional, Santini, P., additional, Saxena, A., additional, Schaerer, D., additional, Schreiber, C., additional, Stark, D., additional, Tasca, L. A. M., additional, Thomas, R., additional, Vanzella, E., additional, Wild, V., additional, Williams, C., additional, and Zucca, E., additional
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- 2021
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38. The WISSH quasars project
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Bischetti, M., primary, Feruglio, C., additional, Piconcelli, E., additional, Duras, F., additional, Pérez-Torres, M., additional, Herrero, R., additional, Venturi, G., additional, Carniani, S., additional, Bruni, G., additional, Gavignaud, I., additional, Testa, V., additional, Bongiorno, A., additional, Brusa, M., additional, Circosta, C., additional, Cresci, G., additional, D’Odorico, V., additional, Maiolino, R., additional, Marconi, A., additional, Mingozzi, M., additional, Pappalardo, C., additional, Perna, M., additional, Traianou, E., additional, Travascio, A., additional, Vietri, G., additional, Zappacosta, L., additional, and Fiore, F., additional
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- 2020
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39. SUPER
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Vietri, G., primary, Mainieri, V., additional, Kakkad, D., additional, Netzer, H., additional, Perna, M., additional, Circosta, C., additional, Harrison, C. M., additional, Zappacosta, L., additional, Husemann, B., additional, Padovani, P., additional, Bischetti, M., additional, Bongiorno, A., additional, Brusa, M., additional, Carniani, S., additional, Cicone, C., additional, Comastri, A., additional, Cresci, G., additional, Feruglio, C., additional, Fiore, F., additional, Lanzuisi, G., additional, Mannucci, F., additional, Marconi, A., additional, Piconcelli, E., additional, Puglisi, A., additional, Salvato, M., additional, Schramm, M., additional, Schulze, A., additional, Scholtz, J., additional, Vignali, C., additional, and Zamorani, G., additional
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- 2020
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40. The properties of He IIλ1640 emitters at z ∼ 2.5–5 from the VANDELS survey
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Saxena, A., primary, Pentericci, L., additional, Mirabelli, M., additional, Schaerer, D., additional, Schneider, R., additional, Cullen, F., additional, Amorin, R., additional, Bolzonella, M., additional, Bongiorno, A., additional, Carnall, A. C., additional, Castellano, M., additional, Cucciati, O., additional, Fontana, A., additional, Fynbo, J. P. U., additional, Garilli, B., additional, Gargiulo, A., additional, Guaita, L., additional, Hathi, N. P., additional, Hutchison, T. A., additional, Koekemoer, A. M., additional, Marchi, F., additional, McLeod, D. J., additional, McLure, R. J., additional, Papovich, C., additional, Pozzetti, L., additional, Talia, M., additional, and Zamorani, G., additional
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- 2020
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41. Universal bolometric corrections for active galactic nuclei over seven luminosity decades
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Duras, F., primary, Bongiorno, A., additional, Ricci, F., additional, Piconcelli, E., additional, Shankar, F., additional, Lusso, E., additional, Bianchi, S., additional, Fiore, F., additional, Maiolino, R., additional, Marconi, A., additional, Onori, F., additional, Sani, E., additional, Schneider, R., additional, Vignali, C., additional, and La Franca, F., additional
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- 2020
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42. The WISSH quasars project
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Travascio, A., primary, Zappacosta, L., additional, Cantalupo, S., additional, Piconcelli, E., additional, Arrigoni Battaia, F., additional, Ginolfi, M., additional, Bischetti, M., additional, Vietri, G., additional, Bongiorno, A., additional, D’Odorico, V., additional, Duras, F., additional, Feruglio, C., additional, Vignali, C., additional, and Fiore, F., additional
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- 2020
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43. The WISSH quasars project
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Zappacosta, L., primary, Piconcelli, E., additional, Giustini, M., additional, Vietri, G., additional, Duras, F., additional, Miniutti, G., additional, Bischetti, M., additional, Bongiorno, A., additional, Brusa, M., additional, Chiaberge, M., additional, Comastri, A., additional, Feruglio, C., additional, Luminari, A., additional, Marconi, A., additional, Ricci, C., additional, Vignali, C., additional, and Fiore, F., additional
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- 2020
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44. SUPER III. Broad Line Region properties of AGN at z
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Vietri, G., Mainieri, V., Kakkad, D., Netzer, H., Perna, M., Circosta, C., Harrison, C. M., Zappacosta, L., Husemann, B., Padovani, P., Bischetti, M, Bongiorno, A., Brusa, M., Carniani, S., Cicone, C., Comastri, A., Cresci, G., Feruglio, C., Fiore, F., Lanzuisi, G., Mannucci, F., Marconi, A., Piconcelli, E., Puglisi, A., Salvato, M., Schramm, M., Schulze, A., Scholtz, J., Vignali, C., Zamorani, G., Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Comunidad de Madrid, Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), Deutsche Forschungsgemeinschaft (DFG), and info:eu-repo/grantAgreement/SPAIN/MINECO/ICTI2013-2016/MDM-2017-0737
- Subjects
Quasars- Emission Lines ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Solar and Stellar Astrophysics ,Galaxies-Evolution ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxies. High-Redshift ,Supermassive Black Holes [Quasars] ,Galaxies-Active ,Astrophysics::Galaxy Astrophysics - Abstract
Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray-selected AGNs at redshift z ∼ 2 with high (∼2 kpc) spatial resolution, and to correlate them with the properties of their host galaxy and central black hole. The main aims of this paper are: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Methods. We analysed rest-frame optical and UV spectra of 21 Type-1 AGNs. We used Hα, Hβ, and MgII line profiles to estimate the masses of the black holes. We used the blueshift of the CIV line profile to trace the presence of winds in the BLR. Results. We find that the Hα and Hβ line widths are strongly correlated, as is the line continuum luminosity at 5100 Å with Hα line luminosity, resulting in a well-defined correlation between black hole masses estimated from Hα and Hβ. Using these lines, we estimate that the black hole masses for our objects are in the range Log (MBH/M⊙) = 8.4–10.8 and are accreting at λEdd = 0.04–1.3. Furthermore, we confirm the well-known finding that the CIV line width does not correlate with the Balmer lines and the peak of the line profile is blueshifted with respect to the [OIII]-based systemic redshift. These findings support the idea that the CIV line is tracing outflowing gas in the BLR for which we estimated velocities up to ∼4700 km s−1. We confirm the strong dependence of the BLR wind velocity on the UV-to-X-ray continuum slope, the bolometric luminosity, and Eddington ratio. We infer BLR mass outflow rates in the range 0.005–3 M⊙ yr−1, revealing a correlation with the bolometric luminosity consistent with that observed for ionised winds in the narrow line region (NLR), and X-ray winds detected in local AGNs, and kinetic power ∼10−7 − 10−4 × LBol. The coupling efficiencies predicted by AGN-feedback models are much higher than the values reported for the BLR winds in the SUPER sample; although it should be noted that only a fraction of the energy injected by the AGN into the surrounding medium is expected to become kinetic power in the outflow. Finally, we find an anti-correlation between the equivalent width of the [OIII] line and the CIV velocity shift, and a positive correlation between this latter parameter and [OIII] outflow velocity. These findings, for the first time in an unbiased sample of AGNs at z ∼ 2, support a scenario where BLR winds are connected to galaxy-scale detected outflows, and are therefore capable of affecting the gas in the NLR located at kiloparsec scale distances. We thank the anonymous referee for the useful comments that improved the paper. The scientific results reported in this article are based on observations collected at the European organisation for Astronomical Research in the Southern Hemisphere under ESO programs 196.A-0377 (SINFONI data) and LP175.A-0839 (zCOSMOS data), and SDSS. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This research project was supported by the DFG Cluster of Excellence “Origin and Structure of the Universe” (universe-cluster.de). G. V. acknowledges financial support from Premiale 2015 MITic (PI B. Garilli). G. C., M. Bi, C. F. and F. F. acknowledge support from PRIN MIUR project “Black Hole winds and the Baryon Life Cycle of Galaxies: the stone-guest at the galaxy evolution supper”, contract #2017PH3WAT. M. P. is supported by the Programa Atracción de Talento de la Comunidad de Madrid via grant 2018-T2/TIC-11715.. With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737) Peer review
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- 2020
45. Obscured AGN at 1.5 <z <3.0 from the zCOSMOS-deep Survey I. Properties of the emitting gas in the narrow-line region
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V. Mainieri, M. Bolzonella, Angela Bongiorno, E. Perez Montero, E. Zucca, Roberto Gilli, Simon J. Lilly, Anton M. Koekemoer, Christian Maier, Rongmon Bordoloi, V. Le Brun, Karina Caputi, M. Mignoli, G. Zamorani, Bianca Garilli, Andrea Cimatti, Cristian Vignali, Y. Peng, C. Diener, S. Bardelli, O. Le Fèvre, Anna Feltre, John D. Silverman, Francesco Calura, Istituto Nazionale di Astrofisica, European Research Council, National Key Research and Development Program (China), National Science Foundation (US), Astronomy, ITA, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
- Subjects
ACTIVE GALACTIC NUCLEI ,EMISSION-LINES ,Active galactic nucleus ,Radio galaxy ,Metallicity ,Astrophysics::High Energy Astrophysical Phenomena ,MASS-METALLICITY RELATION ,galaxies: active ,galaxies [x-rays] ,CHEMICAL EVOLUTION ,RADIO GALAXIES ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,LUMINOSITY RELATIONSHIP ,01 natural sciences ,formation [line] ,SUPERMASSIVE BLACK-HOLES ,emission lines [quasars] ,0103 physical sciences ,STAR-FORMING GALAXIES ,fundamental parameters [galaxies] ,Emission spectrum ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,evolution [galaxies] ,Physics ,Supermassive black hole ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,NEBULAR EMISSION ,Astronomy and Astrophysics ,galaxies: fundamental parameters ,Astrophysics - Astrophysics of Galaxies ,FUNDAMENTAL RELATION ,Galaxy ,Redshift ,quasars: emission lines ,X-rays: galaxies ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,active [galaxies] ,Microturbulence ,line: formation ,galaxies: evolution - Abstract
The physics and demographics of high-redshift obscured active galactic nuclei (AGN) is still scarcely investigated. New samples of such objects, selected with different techniques, can provide useful insights into their physical properties. Aims. With the goal to determine the properties of the gas in the emitting region of type 2 AGN, in particular, the gas metal content, we exploit predictions from photoionization models, including new parameterizations for the distance of gas distribution from the central source and internal microturbulence in the emitting clouds, to interpret rest-frame UV spectral data. Methods. We selected a sample of 90 obscured (type 2) AGN with 1.45 ≤ z ≤ 3.05 from the zCOSMOS-deep galaxy sample by 5σ detection of the high-ionization C iv λ1549 narrow emission line. This feature in a galaxy spectrum is often associated with nuclear activity, and the selection effectiveness has also been confirmed by diagnostic diagrams based on utraviolet (UV) emission-line ratios. We applied the same selection technique and collected a sample of 102 unobscured (type 1) AGN. Taking advantage of the large amount of multiband data available in the COSMOS field, we investigated the properties of the Civ-selected type 2 AGN, focusing on their host galaxies, X-ray emission, and UV emission lines. Finally, we investigated the physical properties of the ionized gas in the narrow-line region (NLR) of this type 2 AGN sample by combining the analysis of strong UV emission lines with predictions from photoionization models. Results. We find that in order to successfully reproduce the relative intensity of UV emission lines of the selected high-z type 2 AGN, two new ingredients in the photoionization models are fundamental: small inner radii of the NLR (≈90 pc for LAGN = 1045 erg s−1 ), and the internal dissipative microturbulence of the gas-emitting clouds (with vmicr ≈ 100 km s−1 ). With these modified models, we compute the gas-phase metallicity of the NLR, and our measurements indicate a statistically significant evolution of the metal content with redshift. Finally, we do not observe a strong relationship between the NLR gas metallicity and the stellar mass of the host galaxy in our Civ-selected type 2 AGN sample.© ESO 2019, We acknowledge financial support from the agreement ASI-INAF n. 2017-14-H.O. A.F. acknowledges support from the ERC via an Advanced Grant under grant agreement no. 321323-NEOGAL and no. 339659- MUSICOS. A.C. acknowledges the support from the grants PRIN-MIUR 2015 and ASI n.I/023/12/0 and ASI n.2018-23-HH.0. Y.P. acknowledges National Key R&D Program of China Grant 2016YFA0400702, and NSFC Grant No. 11773001 and 11721303.
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- 2019
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46. The WISSH quasars project: IX. Cold gas content and environment of luminous QSOs at z ∼ 2.4–4.7
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Centre National de la Recherche Scientifique (France), Max Planck Society, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, European Research Council, Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Comunidad de Madrid, Bischetti, Manuela, Feruglio, Chiara, Piconcelli, Enrico, Duras, F., Pérez-Torres, Miguel A., Herrero, R., Venturi, G., Carniani, Stefano, Bruni, G., Gavignaud, I., Testa, V., Bongiorno, A., Brusa, Marcella, Circosta, C., Cresci, G., D'Odorico, Valentina, Maiolino, Roberto, Marconi, A., Mingozzi, M., Pappalardo, C., Perna, M., Traianou, E., Travascio, A., Vietri, G., Zappacosta, Luca, Fiore, Fabricio, Centre National de la Recherche Scientifique (France), Max Planck Society, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, European Research Council, Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Comunidad de Madrid, Bischetti, Manuela, Feruglio, Chiara, Piconcelli, Enrico, Duras, F., Pérez-Torres, Miguel A., Herrero, R., Venturi, G., Carniani, Stefano, Bruni, G., Gavignaud, I., Testa, V., Bongiorno, A., Brusa, Marcella, Circosta, C., Cresci, G., D'Odorico, Valentina, Maiolino, Roberto, Marconi, A., Mingozzi, M., Pappalardo, C., Perna, M., Traianou, E., Travascio, A., Vietri, G., Zappacosta, Luca, and Fiore, Fabricio
- Abstract
Context. Sources at the brightest end of the quasi-stellar object (QSO) luminosity function, during the peak epoch in the history of star formation and black hole accretion (z ∼ 2-4, often referred to as "Cosmic noon") are privileged sites to study the cycle of feeding & feedback processes in massive galaxies. Aims. We aim to perform the first systematic study of cold gas properties in the most luminous QSOs, by characterising their host-galaxies and environment. These targets exhibit indeed widespread evidence of outflows at nuclear and galactic scales. Methods. We analyse ALMA, NOEMA and JVLA observations of the far-infrared continuum, CO and [CII] emission lines in eight QSOs (bolometric luminosity LBol ≳ 3 × 1047 erg s-1) from the WISE-SDSS selected hyper-luminous (WISSH) QSOs sample at z ∼ 2.4-4.7. Results. We report a 100% emission line detection rate and a 80% detection rate in continuum emission, and we find CO emission to be consistent with the steepest CO ladders observed so far. Sub-millimetre data reveal presence of (one or more) bright companion galaxies around ∼80% of WISSH QSOs, at projected distances of ∼6-130 kpc. We observe a variety of sizes for the molecular gas reservoirs (∼1.7-10 kpc), mostly associated with rotating disks with disturbed kinematics. WISSH QSOs typically show lower CO luminosity and higher star formation efficiency than infrared matched, z ∼ 0-3 main-sequence galaxies, implying that, given the observed SFR ∼170-1100 M⊙ yr-1, molecular gas is converted into stars in ≲ 50 Myr. Most targets show extreme dynamical to black-hole mass ratios Mdyn/MBH ∼ 3-10, two orders of magnitude smaller than local relations. The molecular gas fraction in the host-galaxies of WISSH is lower by a factor of ∼10-100 than in star forming galaxies with similar M∗. Conclusions. Our analysis reveals that hyper-luminous QSOs at Cosmic noon undergo an intense growth phase of both the central super-massive black hole and of the host-galaxy. These s
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- 2020
47. The WISSH quasars project: V. ALMA reveals the assembly of a giant galaxy around a z = 4.4 hyper-luminous QSO
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A. Travascio, Angela Bongiorno, Fabrizio Fiore, Rosa Valiante, Chiara Feruglio, Stefano Carniani, Raffaella Schneider, Luca Zappacosta, G. Vietri, Ciro Pappalardo, M. Bischetti, Alessandro Marconi, Enrico Piconcelli, F. Duras, Carniani, Stefano [0000-0002-6719-380X], Apollo - University of Cambridge Repository, Bischetti, M., Piconcelli, E., Feruglio, C., Duras, F., Bongiorno, A., Carniani, S., Marconi, A., Pappalardo, C., Schneider, R., Travascio, A., Valiante, R., Vietri, G., Zappacosta, L., Fiore, F., and ITA
- Subjects
QSOS ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,astro-ph.GA ,Continuum (design consultancy) ,FOS: Physical sciences ,Quasars: supermassive black holes ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,star formation [Galaxies] ,high-redshift [Galaxies] ,Settore FIS/05 - Astronomia e Astrofisica ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,10. No inequality ,010303 astronomy & astrophysics ,individual: SDSSJ101549.00+002020.03 [Quasars] ,Astrophysics::Galaxy Astrophysics ,Physics ,Galaxies: star formation ,Quasars: emission lines ,010308 nuclear & particles physics ,Galaxies: high-redshift ,Quasars: individual: SDSSJ101549.00+002020.03 ,Astronomy and Astrophysics ,Space and Planetary Science ,Quasar ,emission line [Quasars] ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Black hole ,13. Climate action ,Astrophysics of Galaxies (astro-ph.GA) ,astro-ph.CO ,Astrophysics::Earth and Planetary Astrophysics ,Order of magnitude ,supermassive black holes [Quasars] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present an ALMA high-resolution observation of the 840 um continuum and [CII] line emission in the WISE-SDSS selected hyper-luminous (WISSH) QSO J1015+0020 at z~4.4. Our analysis reveals an exceptional overdensity of [CII]-emitting companions with a very small (, Accepted
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- 2018
48. ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties
- Author
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Angela Bongiorno, Viola Allevato, Roberto Gilli, Alexis Finoguenov, Andrea Ferrara, Nico Cappelluti, Francesca Civano, Stefano Marchesi, Hyewon Suh, Francesco Shankar, Takamitsu Miyaji, A. Viitanen, Mara Salvato, ITA, USA, GBR, Allevato, V., Viitanen, A., Finoguenov, A., Civano, F., Suh, H., Shankar, F., Bongiorno, A., Ferrara, A., Gilli, R., Miyaji, T., Marchesi, S., Cappelluti, N., Salvato, M., Department of Physics, and Helsinki Institute of Physics
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Active galactic nucleus ,Stellar mass ,Astrophysics::High Energy Astrophysical Phenomena ,quasars ,Dark matter ,active ,POPULATION SYNTHESIS ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,dark matter ,STAR-FORMATION ,Luminosity ,SUPERMASSIVE BLACK-HOLES ,SATELLITE GALAXIES ,galaxies ,0103 physical sciences ,X-RAY AGN ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,REDSHIFT SURVEY ,Physics ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,115 Astronomy, Space science ,Redshift ,Galaxy ,COLD DARK-MATTER ,general ,Space and Planetary Science ,CROSS-CORRELATION ,large-scale structure of Universe ,STELLAR MASS ,Low Mass ,WIDE-FIELD SURVEY - Abstract
Aims.We perform clustering measurements of 800 X-ray selectedChandraCOSMOS Legacy (CCL) Type 2 active galactic nuclei (AGN) with known spectroscopic redshift to probe the halo mass dependence on AGN host galaxy properties, such as galaxy stellar massMstar, star formation rate (SFR), and specific black hole accretion rate (BHAR;λBHAR) in the redshift rangez = [0−3].Methods.We split the sample of AGN with known spectroscopic redshits according toMstar, SFR andλBHAR, while matching the distributions in terms of the other parameters, including redshift. We measured the projected two-point correlation functionwp(rp) and modeled the clustering signal, for the different subsamples, with the two-halo term to derive the large-scale biasband corresponding typical mass of the hosting halo.Results.We find no significant dependence of the large-scale bias and typical halo mass on galaxy stellar mass and specific BHAR for CCL Type 2 AGN at meanz ∼ 1, while a negative dependence on SFR is observed, i.e. lower SFR AGN reside in richer environment. Mock catalogs of AGN, matched to have the same X-ray luminosity, stellar mass,λBHAR, and SFR of CCL Type 2 AGN, almost reproduce the observedMstar − Mh,λBHAR − Mhand SFR–Mhrelations, when assuming a fraction of satellite AGNfAGNsat∼ 0.15. This corresponds to a ratio of the probabilities of satellite to central AGN of being activeQ ∼ 2. Mock matched normal galaxies follow a slightly steeperMstar − Mhrelation, in which low mass mock galaxies reside in less massive halos than mock AGN of similar mass. Moreover, matched mock normal galaxies are less biased than mock AGN with similar specific BHAR and SFR, at least forQ > 1.
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- 2019
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49. Triggering nuclear and galaxy activity in the Bullet cluster
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Puccetti, S., primary, Fiore, F., additional, Bongiorno, A., additional, Boutsia, K., additional, Fassbender, R., additional, and Verdugo, M., additional
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- 2020
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50. ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties
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Allevato, V., primary, Viitanen, A., additional, Finoguenov, A., additional, Civano, F., additional, Suh, H., additional, Shankar, F., additional, Bongiorno, A., additional, Ferrara, A., additional, Gilli, R., additional, Miyaji, T., additional, Marchesi, S., additional, Cappelluti, N., additional, and Salvato, M., additional
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- 2019
- Full Text
- View/download PDF
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