Browsing by Author "Giroletti, M."

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    Bubbles and outflows: The novel JWST/NIRSpec view of the z=1.59 obscured quasar XID2028
    (2023) Cresci, G.; Tozzi, G.; Perna, M.; Brusa, M.; Marconcini, C.; Marconi, A.; Carniani, S.; Brienza, M.; Giroletti, M.; Belfiore, F.; Ginolfi, M.; Mannucci, F.; Ulivi, L.; Scholtz, J.; Venturi, G.; Arribas, S.; Ubler, H.; D'Eugenio, F.; Mingozzi, M.; Balmaverde, B.; Capetti, A.; Parlanti, E.; Zana, T.
    Quasar feedback in the form of powerful outflows is invoked as a key mechanism to quench star formation in galaxies, although direct observational evidence is still scarce and debated. Here we present Early Release Science JWST NIRSpec IFU observations of the z = 1.59 prototypical obscured Active Galactic Nucleus (AGN) XID2028: This target represents a unique test case for studying quasar feedback at the peak epoch of AGN-galaxy co-evolution because extensive multi-wavelength coverage is available and a massive and extended outflow is detected in the ionised and molecular components. With the unprecedented sensitivity and spatial resolution of the JWST, the NIRSpec dataset reveals a wealth of structures in the ionised gas kinematics and morphology that were previously hidden in the seeing-limited ground-based data. In particular, we find evidence of an interaction between the interstellar medium of the galaxy and the quasar-driven outflow and radio jet that produces an expanding bubble from which the fast and extended wind detected in previous observations emerges. The new observations confirm the complex interplay between the AGN jet, wind and the interstellar medium of the host galaxy, highlighting the role of low-luminosity radio jets in AGN feedback. They also clearly show the new window that NIRSpec opens for detailed studies of feedback at high redshift.
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    Panning for gold, but finding helium: Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observations
    (2023) Agudo, I.; Amati, L.; An, T.; Bauer, F. E.; Benetti, S.; Bernardini, M. G.; Beswick, R.; Bhirombhakdi, K.; de Boer, T.; Branchesi, M.; Brennan, S. J.; Brocato, E.; Caballero-Garcia, M. D.; Cappellaro, E.; Castro Rodriguez, N.; Castro-Tirado, A. J.; Chambers, K. C.; Chassande-Mottin, E.; Chaty, S.; Chen, T. -W.; Coleiro, A.; Covino, S.; D'Ammando, F.; D'Avanzo, P.; D'Elia, V.; Fiore, A.; Floers, A.; Fraser, M.; Frey, S.; Frohmaier, C.; Fulton, M.; Galbany, L.; Gall, C.; Gao, H.; Garcia-Rojas, J.; Ghirlanda, G.; Giarratana, S.; Gillanders, J. H.; Giroletti, M.; Gompertz, B. P.; Gromadzki, M.; Heintz, K. E.; Hjorth, J.; Hu, Y. -D.; Huber, M. E.; Inkenhaag, A.; Izzo, L.; Jin, Z. P.; Jonker, P. G.; Kann, D. A.; Kool, E. C.; Kotak, R.; Leloudas, G.; Levan, A. J.; Lin, C. -C.; Lyman, J. D.; Magnier, E. A.; Maguire, K.; Mandel, I.; Marcote, B.; Sanchez, D. Mata; Mattila, S.; Melandri, A.; Michalowski, M. J.; Moldon, J.; Nicholl, M.; Guelbenzu, A. Nicuesa; Oates, S. R.; Onori, F.; Orienti, M.; Paladino, R.; Paragi, Z.; Perez-Torres, M.; Pian, E.; Pignata, G.; Piranomonte, S.; Quirola-Vasquez, J.; Ragosta, F.; Rau, A.; Ronchini, S.; Rossi, A.; Sanchez-Ramirez, R.; Salafia, O. S.; Schulze, S.; Smartt, S. J.; Smith, K. W.; Sollerman, J.; Srivastav, S.; Starling, R. L. C.; Steeghs, D.; Stevance, H. F.; Tanvir, N. R.; Testa, V.; Torres, M. A. P.; Valeev, A.; Vergani, S. D.; Vescovi, D.; Wainscost, R.; Watson, D.; Wiersema, K.; Wyrzykowski, L.; Yang, J.; Yang, S.; Young, D. R.
    We present the results from multi-wavelength observations of a transient discovered during an intensive follow-up campaign of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN 2019wxt, a young transient in a galaxy whose sky position (in the 80% GW contour) and distance (similar to SIM;150 Mpc) were plausibly compatible with the localisation uncertainty of the GW event. Initially, the transient's tightly constrained age, its relatively faint peak magnitude (M-i similar to -16.7 mag), and the r-band decline rate of similar to 1 mag per 5 days appeared suggestive of a compact binary merger. However, SN 2019wxt spectroscopically resembled a type Ib supernova, and analysis of the optical-near-infrared evolution rapidly led to the conclusion that while it could not be associated with S191213g, it nevertheless represented an extreme outcome of stellar evolution. By modelling the light curve, we estimated an ejecta mass of only similar to 0.1 M circle dot, with Ni-56 comprising similar to 20% of this. We were broadly able to reproduce its spectral evolution with a composition dominated by helium and oxygen, with trace amounts of calcium. We considered various progenitor channels that could give rise to the observed properties of SN 2019wxt and concluded that an ultra-stripped origin in a binary system is the most likely explanation. Disentangling genuine electromagnetic counterparts to GW events from transients such as SN 2019wxt soon after discovery is challenging: in a bid to characterise this level of contamination, we estimated the rate of events with a volumetric rate density comparable to that of SN 2019wxt and found that around one such event per week can occur within the typical GW localisation area of O4 alerts out to a luminosity distance of 500 Mpc, beyond which it would become fainter than the typical depth of current electromagnetic follow-up campaigns.
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    Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants
    (2023) Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Aloisio, R.; Crespo, N. Alvarez; Batista, R. Alves; Amati, L.; Amato, E.; Ambrosi, G.; Anguner, E. O.; Aramo, C.; Arcaro, C.; Armstrong, T.; Asano, K.; Ascasibar, Y.; Aschersleben, J.; Backes, M.; Baktash, A.; Balazs, C.; Balbo, M.; Ballet, J.; Larriva, A. Baquero; Martins, V. Barbosa; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Baxter, J. R.; Tjus, J. Becker; Benbow, W.; Bernardos-Martin, M. I.; Bernete, J.; Berti, A.; Bertucci, B.; Beshley, V.; Bhattacharjee, P.; Bhattacharyya, S.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Bordas, P.; Bottacini, E.; Bregeon, J.; Brose, R.; Bucciantini, N.; Bulgarelli, A.; Capasso, M.; Dolcetta, R. A. Capuzzo; Caraveo, P.; Cardillo, M.; Carosi, R.; Casanova, S.; Cascone, E.; Cassol, F.; Catalani, F.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiavassa, A.; Chudoba, J.; Coimbra-Araujo, C.; Conforti, V.; Contreras, J. L.; Costa, A.; Costantini, H.; Cristofari, P.; Crocker, R.; D'Amico, G.; D'Ammando, F.; De Angelis, A.; De Caprio, V.; Pino, E. M. de Gouveia Dal; Wilhelmi, E. de Ona; de Souza, V.; Delgado, C.; della Volp, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Diebold, S.; Djuvsland, J. I.; Donini, A.; Doro, M.; Dos Anjos, R. d. C.; Dwarkadas, V. V.; Einecke, S.; Elsaesser, D.; Emery, G.; Evoli, C.; Falceta-Goncalves, D.; Fedorova, E.; Fegan, S.; Ferrand, G.; Fiandrini, E.; Filipovic, M.; Fioretti, V.; Fiori, M.; Foffano, L.; Fontaine, G.; Fukami, S.; Galanti, G.; Galaz, G.; Gammaldi, V.; Gasbarra, C.; Ghalumyan, A.; Ghirlanda, G.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Giroletti, M.; Giuliani, A.; Giunti, L.; Godinovic, N.; Coelho, J. Goulart; Greaux, L.; Green, D.; Grondin, M. -H.; Gueta, O.; Gunji, S.; Hassan, T.; Heller, M.; Hernandez-Cadena, S.; Hinton, J.; Hnatyk, B.; Hnatyk, R.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horvath, P.; Hrabovsky, M.; Hrupec, D.; Inada, T.; Incardona, F.; Inoue, S.; Ishio, K.; Jamrozy, M.; Janecek, P.; Martinez, I. Jimenez; Jin, W.; Jung-Richardt, I.; Jurysek, J.; Kaaret, P.; Karas, V.; Katz, U.; Kerszberg, D.; Khelifi, B.; Kieda, D. B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluzniak, W.; Knodlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kubo, H.; La Palombara, N.; Lainez, M.; Lamastra, A.; Lapington, J.; Lemoine-Goumard, M.; Lenain, J. -P.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Liodakis, I.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez-Coto, R.; Lopez-Moya, M.; Lopez-Oramas, A.; Loporchio, S.; Luque-Escamilla, P. L.; Macias, O.; Mackey, J.; Majumdar, P.; Mandat, D.; Manganaro, M.; Manico, G.; Marconi, M.; Marti, J.; Martinez, G.; Martinez, M.; Martinez, O.; Mello, A. J. T. S.; Menchiari, S.; Meyer, D. M. -A.; Micanovic, S.; Miceli, D.; Miceli, M.; Michalowski, J.; Miener, T.; Miranda, J. M.; Mitchell, A.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Morcuende, D.; Morlino, G.; Morselli, A.; Mose, M.; Moulin, E.; Mukherjee, R.; Munari, K.; Murach, T.; Nagai, A.; Nagataki, S.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nievas Rosillo, M.; Nikolajuk, M.; Nishijima, K.; Noda, K.; Novosyadlyj, B.; Nozaki, S.; Ohishi, M.; Ohm, S.; Ohtani, Y.; Okumura, A.; Olmi, B.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Orlando, S.; Ostrowski, M.; Oya, I.; Pantaleo, F. R.; Paredes, J. M.; Patricelli, B.; Pecimotika, M.; Peresano, M.; Perez-Romero, J.; Persic, M.; Petruk, O.; Piano, G.; Pietropaolo, E.; Pirola, G.; Pittori, C.; Pohl, M.; Ponti, G.; Prandini, E.; Principe, G.; Priyadarshi, C.; Pueschel, E.; Puehlhofer, G.; Pumo, M. L.; Quirrenbach, A.; Rando, R.; Razzaque, S.; Reichherzer, P.; Reimer, A.; Reimer, O.; Renaud, M.; Reposeur, T.; Ribo, M.; Richtler, T.; Rico, J.; Rieger, F.; Rigoselli, M.; Riitano, L.; Rizi, V.; Roache, E.; Romano, P.; Romeo, G.; Rosado, J.; Rowell, G.; Rudak, B.; Sadeh, I.; Safi-Harb, S.; Saha, L.; Sailer, S.; Sanchez-Conde, M.; Sarkar, S.; Satalecka, K.; Saturni, F. G.; Scherer, A.; Schovanek, P.; Schussler, F.; Schwanke, U.; Scuderi, S.; Seglar-Arroyo, M.; Sergijenko, O.; Servillat, M.; Shang, R. -Y.; Sharma, P.; Siejkowski, H.; Sliusar, V.; Slowikowska, A.; Sol, H.; Specovius, A.; Spencer, S. T.; Spengler, G.; Stamerra, A.; Stanic, S.; Starecki, T.; Starling, R.; Stolarczyk, T.; Stuani Pereira, L. A.; Suda, Y.; Suomijarvi, T.; Sushch, I.; Tajima, H.; Tam, P. -H. T.; Tanaka, S. J.; Tavecchio, F.; Testa, V.; Tian, W.; Tibaldo, L.; Torres, D. F.; Tothill, N.; Vallage, B.; Vallania, P.; van Eldik, C.; van Scherpenberg, J.; Vandenbroucke, J.; Vazquez Acosta, M.; Vecchi, M.; Vercellone, S.; Verna, G.; Viana, A.; Vignatti, J.; Vitale, V.; Vodeb, V.; Vorobiov, S.; Vuillaume, T.; Wagner, S. J.; Walter, R.; White, M.; Wierzcholska, A.; Will, M.; Williams, D.; Yang, L.; Yoshida, T.; Yoshikoshi, T.; Zaharijas, G.; Zampieri, L.; Zavrtanik, D.; Zavrtanik, M.; Zhdanov, V. I.; Zivec, M.
    The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3 PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy y-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte-Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a y-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 h of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with O(100) hours of exposure per source.