Author: "Santo, M." / Publication Type: Electronic Resources - Searchworks@Jio Institute Digital Library Search Results

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625 results on '"Santo, M."'

1. Ecological and social factors influence interspecific pathogens occurrence among bees

Author: Tiritelli, R, Flaminio, S, Zavatta, L, Ranalli, R, Giovanetti, M, Grasso, D, Leonardi, S, Bonforte, M, Boni, C, Cargnus, E, Catania, R, Coppola, F, Di Santo, M, Pusceddu, M, Quaranta, M, Bortolotti, L, Nanetti, A, Cilia, G, Tiritelli R., Flaminio S., Zavatta L., Ranalli R., Giovanetti M., Grasso D. A., Leonardi S., Bonforte M., Boni C. B., Cargnus E., Catania R., Coppola F., Di Santo M., Pusceddu M., Quaranta M., Bortolotti L., Nanetti A., Cilia G., Tiritelli, R, Flaminio, S, Zavatta, L, Ranalli, R, Giovanetti, M, Grasso, D, Leonardi, S, Bonforte, M, Boni, C, Cargnus, E, Catania, R, Coppola, F, Di Santo, M, Pusceddu, M, Quaranta, M, Bortolotti, L, Nanetti, A, Cilia, G, Tiritelli R., Flaminio S., Zavatta L., Ranalli R., Giovanetti M., Grasso D. A., Leonardi S., Bonforte M., Boni C. B., Cargnus E., Catania R., Coppola F., Di Santo M., Pusceddu M., Quaranta M., Bortolotti L., Nanetti A., and Cilia G.
Abstract: The interspecific transmission of pathogens can occur frequently in the environment. Among wild bees, the main spillover cases are caused by pathogens associated with Apis mellifera, whose colonies can act as reservoirs. Due to the limited availability of data in Italy, it is challenging to accurately assess the impact and implications of this phenomenon on the wild bee populations. In this study, a total of 3372 bees were sampled from 11 Italian regions within the BeeNet project, evaluating the prevalence and the abundance of the major honey bee pathogens (DWV, BQCV, ABPV, CBPV, KBV, Nosema ceranae, Ascosphaera apis, Crithidia mellificae, Lotmaria passim, Crithidia bombi). The 68.4% of samples were positive for at least one pathogen. DWV, BQCV, N. ceranae and CBPV showed the highest prevalence and abundance values, confirming them as the most prevalent pathogens spread in the environment. For these pathogens, Andrena, Bombus, Eucera and Seladonia showed the highest mean prevalence and abundance values. Generally, time trends showed a prevalence and abundance decrease from April to July. In order to predict the risk of infection among wild bees, statistical models were developed. A low influence of apiary density on pathogen occurrence was observed, while meteorological conditions and agricultural management showed a greater impact on pathogen persistence in the environment. Social and biological traits of wild bees also contributed to defining a higher risk of infection for bivoltine, communal, mining and oligolectic bees. Out of all the samples tested, 40.5% were co-infected with two or more pathogens. In some cases, individuals were simultaneously infected with up to five different pathogens. It is essential to increase knowledge about the transmission of pathogens among wild bees to understand dynamics, impact and effects on pollinator populations. Implementing concrete plans for the conservation of wild bee species is important to ensure the health of wild and
Published: 2024

2. Engineered mesoporous silica-based nanoparticles as smart chemotherapy nanodevice for bortezomib administration

Author: De Santo, M, Giovinazzo, A, Fava, M, Mazzotta, E, De Napoli, I, Greco, M, Comande, A, Nigro, A, Argurio, P, Perrotta, I, Davoli, M, Tagarelli, A, Elliani, R, Granato, T, Nicolini, G, Chiorazzi, A, Semperboni, S, Ballarini, E, Crocamo, C, Cavaletti, G, Lombardo, D, Sisci, D, Morelli, C, Leggio, A, Pasqua, L, De Santo M., Giovinazzo A., Fava M., Mazzotta E., De Napoli I. E., Greco M., Comande A., Nigro A., Argurio P., Perrotta I., Davoli M., Tagarelli A., Elliani R., Granato T., Nicolini G., Chiorazzi A., Semperboni S., Ballarini E., Crocamo C., Cavaletti G., Lombardo D., Sisci D., Morelli C., Leggio A., Pasqua L., De Santo, M, Giovinazzo, A, Fava, M, Mazzotta, E, De Napoli, I, Greco, M, Comande, A, Nigro, A, Argurio, P, Perrotta, I, Davoli, M, Tagarelli, A, Elliani, R, Granato, T, Nicolini, G, Chiorazzi, A, Semperboni, S, Ballarini, E, Crocamo, C, Cavaletti, G, Lombardo, D, Sisci, D, Morelli, C, Leggio, A, Pasqua, L, De Santo M., Giovinazzo A., Fava M., Mazzotta E., De Napoli I. E., Greco M., Comande A., Nigro A., Argurio P., Perrotta I., Davoli M., Tagarelli A., Elliani R., Granato T., Nicolini G., Chiorazzi A., Semperboni S., Ballarini E., Crocamo C., Cavaletti G., Lombardo D., Sisci D., Morelli C., Leggio A., and Pasqua L.
Abstract: Adverse reactions, toxicity, and poor compliance from patients still represent major challenges for conventional chemotherapy treatments. Localized drug delivery would ideally improve therapeutic efficacy, minimizing the side effects. An MSU-type mesoporous silica-based nanodevice (FOL-MSN-BTZ), able to selectively deliver the antineoplastic drug bortezomib (BTZ) to folate receptor over-expressing multiple myeloma (FR+ MM) cells is described. The receptor-specific ligand, folic acid, grafted on the external surface of the nanosystem, allows tumor recognition and cell internalization, while BTZ, mainly linked to the pore internal surface through a covalent pH-sensitive bond, is released in an acidic tumor environment. A detailed investigation showed that only the fine balancing of different functionalities of the nanodevice around the external and internal surfaces of MSN particles shows the absence of toxicity towards healthy cells in vitro and negligible BTZ-release at physiological pH, which are suitable features for applicative purposes in the engineering of therapies. After complete characterization in vitro, an accurate suspendability assessment, which considered the sedimentation process that reduces the particle amount and, consequently, drug content in the suspensions, allowed the development of an injectable formulation of FOL-MSN-BTZ that showed higher antitumor efficacy and an overall tendency to lower toxicity in a MM mice model compared to the conventional bortezomib chemotherapy.
Published: 2023

3. A transient ultraluminous X-ray source in NGC 55

Author: Robba, A, Pinto, C, Pintore, F, Rodriguez, G, Ambrosi, E, Barra, F, Cusumano, G, D'Ai, A, Del Santo, M, Kosec, P, Marino, A, Middleton, M, Roberts, T, Salvaggio, C, Soria, R, Wolter, A, Walton, D, Robba A., Pinto C., Pintore F., Rodriguez G., Ambrosi E., Barra F., Cusumano G., D'Ai A., Del Santo M., Kosec P., Marino A., Middleton M., Roberts T., Salvaggio C., Soria R., Wolter A., Walton D., Robba, A, Pinto, C, Pintore, F, Rodriguez, G, Ambrosi, E, Barra, F, Cusumano, G, D'Ai, A, Del Santo, M, Kosec, P, Marino, A, Middleton, M, Roberts, T, Salvaggio, C, Soria, R, Wolter, A, Walton, D, Robba A., Pinto C., Pintore F., Rodriguez G., Ambrosi E., Barra F., Cusumano G., D'Ai A., Del Santo M., Kosec P., Marino A., Middleton M., Roberts T., Salvaggio C., Soria R., Wolter A., and Walton D.
Abstract: Ultraluminous X-ray sources (ULXs) are a class of accreting compact objects with X-ray luminosities above 1039 erg s-1. The average number of ULXs per galaxy is still not well-constrained, especially given the uncertainty on the fraction of ULX transients. Here, we report the identification of a new transient ULX in the galaxy NGC 55 (which we label as ULX-2), thanks to recent XMM-Newton and the Neil Gehrels Swift Observatory observations. This object was previously classified as a transient X-ray source with a luminosity around a few 1038 erg s-1 in a 2010 XMM-Newton observation. Thanks to new and deeper observations (∼130 ks each), we show that the source reaches a luminosity peak >1.6 × 1039 erg s-1. The X-ray spectrum of ULX-2 is much softer than in previous observations and fits in the class of soft ULXs. It can be well-described using a model with two thermal components, as often found in ULXs. The time-scales of the X-ray variability are of the order of a month and are likely driven by small changes in the accretion rate or due to super-orbital modulations, attributed to precession of the accretion disc, which is similar to other ULXs.
Published: 2022

4. MoCRiS a low-cost stratospheric balloon platform to measure the particle flux of cosmic ray showers in the high atmosphere

Author: Bocci, V, Brosio, A, Muscio, G, Iacoangeli, F, Liguori, D, Tripodi, M, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Aramo, C, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Buscemi, M, Caccianiga, B, Caccianiga, L, Candela, A, Capone, A, Cariello, M, Caruso, R, Cataldi, G, Chiodi, G, Chiodini, G, Colalillo, R, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Evoli, C, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giampaoli, A, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Hemmer, S, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miozzi, S, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Otto-Nello, G, Pantaleo, F, Paoletti, R, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Rozza, D, Salamida, F, Savina, P, Scherini, V, Schioppa, M, Scotti, V, Se-Rini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Veronesi, I, Zampa, G, Bocci V., Brosio A., Muscio G. G., Iacoangeli F., Liguori D., Tripodi M. A., Alemanno F., Aloisio R., Altomare C., Antolini R., Aramo C., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Buscemi M., Caccianiga B., Caccianiga L., Candela A., Capone A., Cariello M., Caruso R., Cataldi G., Chiodi G., Chiodini G., Colalillo R., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Evoli C., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giampaoli A., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Hemmer S., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miozzi S., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Otto-Nello G., Pantaleo F., Paoletti R., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Rozza D., Salamida F., Savina P., Scherini V., Schioppa M., Scotti V., Se-Rini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., Veronesi I., Zampa G., Bocci, V, Brosio, A, Muscio, G, Iacoangeli, F, Liguori, D, Tripodi, M, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Aramo, C, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Buscemi, M, Caccianiga, B, Caccianiga, L, Candela, A, Capone, A, Cariello, M, Caruso, R, Cataldi, G, Chiodi, G, Chiodini, G, Colalillo, R, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Evoli, C, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giampaoli, A, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Hemmer, S, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miozzi, S, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Otto-Nello, G, Pantaleo, F, Paoletti, R, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Rozza, D, Salamida, F, Savina, P, Scherini, V, Schioppa, M, Scotti, V, Se-Rini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Veronesi, I, Zampa, G, Bocci V., Brosio A., Muscio G. G., Iacoangeli F., Liguori D., Tripodi M. A., Alemanno F., Aloisio R., Altomare C., Antolini R., Aramo C., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Buscemi M., Caccianiga B., Caccianiga L., Candela A., Capone A., Cariello M., Caruso R., Cataldi G., Chiodi G., Chiodini G., Colalillo R., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Evoli C., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giampaoli A., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Hemmer S., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miozzi S., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Otto-Nello G., Pantaleo F., Paoletti R., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Rozza D., Salamida F., Savina P., Scherini V., Schioppa M., Scotti V., Se-Rini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., Veronesi I., and Zampa G.
Abstract: In June 2019 from the region of Calabria (Italy) our group launched the Stratospheric Balloon MoCRiS (Measurement of Cosmic Ray in Stratosphere) that reached up to 35111 meters. MoCRiS is a didactical project that uses a Light Balloon with a payload of only 2.1 Kg payload box included. The capsule was Lithium-ion batteries operated and fully instrumented with two Hi-Res Camera, one for picture and one for video, GPS Tracker, two Particle detectors, and sensors for temperature and pressure. Two ArduSiPM [6] scintillation detectors, made by the INFN group in Rome, were used as cosmic ray flux meters. The technology used for these types of devices makes them very economical, light (<150 g), and with low power consumption (<1 Watt). These characteristics are optimal for use with the balloon and in space (e.g. in CubeSat), and very attractive for educational use, even on the ground. During the school year, the students of the scientific high school "Stefano Patrizi" of Cariati (CS) Italy, participated in the definition of the project following theoretical and practical lessons on aerospace techniques and particle physics with regard to cosmic ray showers in the atmosphere. The mission was completely successful by experimentally verifying the pressure-to-height relation, the height of the thermal inversion in the atmosphere, reaching and exceeding the maximum Regener-Pfotzer level of the shower development. The instrumental and didactic platform created is easily replicable even with further upgrades. We are expanding the collaboration with other schools for further launches.
Published: 2022

5. The online laboratories for OCRA - Outreach Cosmic Ray Activities INFN project

Author: Aramo, C, Antolini, R, Bocci, V, Buscemi, M, Caccianiga, L, Candela, A, Cataldi, G, Colalillo, R, Convenga, F, Coluccia, M, de Palma, F, Di Nezza, P, Di Sciascio, G, Evoli, C, Galbato, G, Hemmer, S, Giampaoli, A, Iacoangeli, F, Liguori, D, Miozzi, S, Paoletti, R, Rossi, N, Rozza, D, Schioppa, M, Veronesi, I, Alemanno, F, Aloisio, R, Altomare, C, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Caccianiga, B, Capone, A, Cariello, M, Caruso, R, Chiodi, G, Chiodini, G, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Salamida, F, Savina, P, Scherini, V, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Zampa, G, Aramo C., Antolini R., Bocci V., Buscemi M., Caccianiga L., Candela A., Cataldi G., Colalillo R., Convenga F., Coluccia M. R., de Palma F., Di Nezza P., Di Sciascio G., Evoli C., Galbato G., Hemmer S., Giampaoli A., Iacoangeli F., Liguori D., Miozzi S., Paoletti R., Rossi N., Rozza D., Schioppa M., Veronesi I., Alemanno F., Aloisio R., Altomare C., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Caccianiga B., Capone A., Cariello M., Caruso R., Chiodi G., Chiodini G., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Salamida F., Savina P., Scherini V., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., Zampa G., Aramo, C, Antolini, R, Bocci, V, Buscemi, M, Caccianiga, L, Candela, A, Cataldi, G, Colalillo, R, Convenga, F, Coluccia, M, de Palma, F, Di Nezza, P, Di Sciascio, G, Evoli, C, Galbato, G, Hemmer, S, Giampaoli, A, Iacoangeli, F, Liguori, D, Miozzi, S, Paoletti, R, Rossi, N, Rozza, D, Schioppa, M, Veronesi, I, Alemanno, F, Aloisio, R, Altomare, C, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Caccianiga, B, Capone, A, Cariello, M, Caruso, R, Chiodi, G, Chiodini, G, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Salamida, F, Savina, P, Scherini, V, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Zampa, G, Aramo C., Antolini R., Bocci V., Buscemi M., Caccianiga L., Candela A., Cataldi G., Colalillo R., Convenga F., Coluccia M. R., de Palma F., Di Nezza P., Di Sciascio G., Evoli C., Galbato G., Hemmer S., Giampaoli A., Iacoangeli F., Liguori D., Miozzi S., Paoletti R., Rossi N., Rozza D., Schioppa M., Veronesi I., Alemanno F., Aloisio R., Altomare C., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Caccianiga B., Capone A., Cariello M., Caruso R., Chiodi G., Chiodini G., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Salamida F., Savina P., Scherini V., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., and Zampa G.
Abstract: OCRA - Outreach Cosmic Ray Activities was born in 2018 as a national outreach project of INFN with the aim of collecting, within a national framework, the numerous public engagement activities in the field of cosmic ray physics already present at a local level in the divisions and laboratories. Since spring 2020 OCRA offers also a series of online laboratories on its website https://web.infn.it/OCRA/, designed not only to be used by students individually but also to be offered in the classroom by teachers. The cosmic ray path, present on the website, will be presented together with the online laboratories on the measurement of muons, from the one related to the dependence on the zenith angle made during the International Cosmic Day up to measurements of the flux dependency on the altitude in the atmosphere and in the water. Also, a laboratory allowing to analyze public data of the Pierre Auger Observatory will be presented. In addition, some teaching methods included in the "Teachers' area" of the OCRA website will be described. The developed cosmic ray path was also used to organize an online course for teachers of Italian high schools with the purpose of accompanying teachers when approaching the subject for the first time. About 70 teachers participated for a total of 9 lessons. ã Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)
Published: 2022

6. Discovering cosmic rays with OCRA: outreach activities for students and teachers

Author: Hemmer, S, Aramo, C, Bissaldi, E, Bocci, V, Bottino, B, Buscemi, M, Caccianiga, L, Cataldi, G, Dimiccoli, F, Di Pierro, F, Evoli, C, Giampaoli, A, La Vacca, G, Menegolli, A, Miozzi, S, Morsani, F, Munini, R, Paoletti, R, Rozza, D, Schioppa, M, Tomassetti, N, Vannuccini, E, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Caccianiga, B, Candela, A, Capone, A, Cariello, M, Caruso, R, Chiodi, G, Chiodini, G, Colalillo, R, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Iacoangeli, F, Insolia, A, Iovenitti, S, Ippolito, V, La Verde, G, Leonora, E, Levorato, S, Liguori, D, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Miyamoto, H, Mocchiutti, E, Morganti, S, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Salamida, F, Savina, P, Scherini, V, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomei, C, Tosta E Melo, I, Turco, P, Vecchiotti, V, Veronesi, I, Zampa, G, Hemmer S., Aramo C., Bissaldi E., Bocci V., Bottino B., Buscemi M., Caccianiga L., Cataldi G., Dimiccoli F., Di Pierro F., Evoli C., Giampaoli A., La Vacca G., Menegolli A., Miozzi S., Morsani F., Munini R., Paoletti R., Rozza D., Schioppa M., Tomassetti N., Vannuccini E., Alemanno F., Aloisio R., Altomare C., Antolini R., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Caccianiga B., Candela A., Capone A., Cariello M., Caruso R., Chiodi G., Chiodini G., Colalillo R., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimitrios K., Donnini F., Doro M., Duranti M., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Iacoangeli F., Insolia A., Iovenitti S., Ippolito V., La Verde G., Leonora E., Levorato S., Liguori D., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Miyamoto H., Mocchiutti E., Morganti S., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Salamida F., Savina P., Scherini V., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomei C., Tosta E Melo I., Turco P., Vecchiotti V., Veronesi I., Zampa G., Hemmer, S, Aramo, C, Bissaldi, E, Bocci, V, Bottino, B, Buscemi, M, Caccianiga, L, Cataldi, G, Dimiccoli, F, Di Pierro, F, Evoli, C, Giampaoli, A, La Vacca, G, Menegolli, A, Miozzi, S, Morsani, F, Munini, R, Paoletti, R, Rozza, D, Schioppa, M, Tomassetti, N, Vannuccini, E, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Caccianiga, B, Candela, A, Capone, A, Cariello, M, Caruso, R, Chiodi, G, Chiodini, G, Colalillo, R, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Iacoangeli, F, Insolia, A, Iovenitti, S, Ippolito, V, La Verde, G, Leonora, E, Levorato, S, Liguori, D, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Miyamoto, H, Mocchiutti, E, Morganti, S, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Salamida, F, Savina, P, Scherini, V, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomei, C, Tosta E Melo, I, Turco, P, Vecchiotti, V, Veronesi, I, Zampa, G, Hemmer S., Aramo C., Bissaldi E., Bocci V., Bottino B., Buscemi M., Caccianiga L., Cataldi G., Dimiccoli F., Di Pierro F., Evoli C., Giampaoli A., La Vacca G., Menegolli A., Miozzi S., Morsani F., Munini R., Paoletti R., Rozza D., Schioppa M., Tomassetti N., Vannuccini E., Alemanno F., Aloisio R., Altomare C., Antolini R., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Caccianiga B., Candela A., Capone A., Cariello M., Caruso R., Chiodi G., Chiodini G., Colalillo R., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimitrios K., Donnini F., Doro M., Duranti M., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Iacoangeli F., Insolia A., Iovenitti S., Ippolito V., La Verde G., Leonora E., Levorato S., Liguori D., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Miyamoto H., Mocchiutti E., Morganti S., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Salamida F., Savina P., Scherini V., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomei C., Tosta E Melo I., Turco P., Vecchiotti V., Veronesi I., and Zampa G.
Abstract: The Outreach Cosmic Ray Activities (OCRA) project offers a platform for all outreach activities focusing on cosmic rays within the Italian Istituto Nazionale di Fisica Nucleare (INFN). Created in 2018, OCRA now counts 21 of the institute's divisions all over Italy as members. The project's core activity is the participation of all its members in the International Cosmic Day, organized by DESY, and inviting high school students to carry out hands-on measurements of the cosmic ray flux and learn about the related physics background. Two students from each division are then selected to participate in the annual OCRA science camp, a three-day full immersion into the life of a physicist. The national activities are complemented by local initiatives of the OCRA member groups: workshops and tutorship programs, science competitions and the development of new detectors for outreach activities offer a multitude of possibilities for students to engage with our researchers and to explore the world of cosmic rays. Since spring of 2020 OCRA also offers a series of online laboratories on its website https://web.infn.it/OCRA/, designed not only to be used by students individually but also to be used in the classroom by teachers. Here we will give an overview on all activities offered by OCRA with a particular focus on the 2020 online event organized in occasion of the International Cosmic Day, that saw the participation of more than 3000 students.
Published: 2022

7. “A scuola di Astroparticelle”: a synergy between school education and scientific research

Author: Colalillo, R, Aramo, C, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Bocci, V, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Buscemi, M, Caccianiga, B, Caccianiga, L, Candela, A, Capone, A, Cariello, M, Caruso, R, Cataldi, G, Chiodi, G, Chiodini, G, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Evoli, C, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giampaoli, A, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Hemmer, S, Iacoangeli, F, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Liguori, D, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miozzi, S, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Paoletti, R, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Rozza, D, Salamida, F, Savina, P, Scherini, V, Schioppa, M, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Veronesi, I, Zampa, G, Colalillo R., Aramo C., Alemanno F., Aloisio R., Altomare C., Antolini R., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Bocci V., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Buscemi M., Caccianiga B., Caccianiga L., Candela A., Capone A., Cariello M., Caruso R., Cataldi G., Chiodi G., Chiodini G., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Evoli C., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giampaoli A., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Hemmer S., Iacoangeli F., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Liguori D., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miozzi S., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Paoletti R., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Rozza D., Salamida F., Savina P., Scherini V., Schioppa M., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., Veronesi I., Zampa G., Colalillo, R, Aramo, C, Alemanno, F, Aloisio, R, Altomare, C, Antolini, R, Arcaro, C, Barbato, F, Battaglieri, M, Battisti, M, Bau, A, Bellinzona, V, Bernardini, P, Bersani, A, Bertaina, M, Berti, A, Bertucci, B, Bisconti, F, Bissaldi, E, Bocci, V, Boezio, M, Boncioli, D, Bondi, M, Bonechi, L, Bonino, R, Bonnoli, G, Bonvicini, V, Bossini, E, Bottino, B, Buscemi, M, Caccianiga, B, Caccianiga, L, Candela, A, Capone, A, Cariello, M, Caruso, R, Cataldi, G, Chiodi, G, Chiodini, G, Coluccia, M, Convenga, F, Copello, S, Corosu, M, D'Urso, D, Dal Corso, F, Davini, S, De Deo, M, De Gateano, S, De Laurentis, M, De Mitri, I, De Palma, F, De Vito, E, Dell'Aquila, D, Depaoli, D, Di Luca, A, Di Pierro, F, Di Ruzza, B, Di Santo, M, Di Sciascio, G, Di Venere, L, Dimiccoli, F, Dimitrios, K, Donnini, F, Doro, M, Duranti, M, Evoli, C, Fenu, F, Fontanelli, F, Fusco, P, Gargano, F, Gervasi, M, Giampaoli, A, Giglietto, N, Giordano, F, Gnesi, I, Gonzi, S, Grandi, D, Graziani, M, Hemmer, S, Iacoangeli, F, Insolia, A, Iovenitti, S, Ippolito, V, La Vacca, G, La Verde, G, Leonora, E, Levorato, S, Liguori, D, Lipari, P, Longo, F, Loparco, F, Lopez Coto, R, Loporchio, S, Marino, A, Marsella, G, Martello, D, Mazziotta, M, Menegolli, A, Miozzi, S, Miyamoto, H, Mocchiutti, E, Morganti, S, Morsani, F, Munini, R, Mussa, R, Nozzoli, F, Nucita, A, Organtini, G, Ottonello, G, Pantaleo, F, Paoletti, R, Parodi, F, Perrone, L, Pesenti, L, Petrera, S, Petronio, C, Pillera, R, Pilo, F, Pizzolotto, C, Prandini, E, Pugliese, M, Raino, S, Randazzo, N, Rando, R, Recchia, L, Ricci, E, Rinaudo, M, Rizi, V, Rossi, N, Rozza, D, Salamida, F, Savina, P, Scherini, V, Schioppa, M, Scotti, V, Serini, D, Sipala, V, Surdo, A, Tiberio, A, Tomassetti, N, Tomei, C, Tosta E Melo, I, Turco, P, Vannuccini, E, Vecchiotti, V, Veronesi, I, Zampa, G, Colalillo R., Aramo C., Alemanno F., Aloisio R., Altomare C., Antolini R., Arcaro C., Barbato F. C. T., Battaglieri M., Battisti M., Bau A., Bellinzona V. E., Bernardini P., Bersani A., Bertaina M., Berti A., Bertucci B., Bisconti F., Bissaldi E., Bocci V., Boezio M., Boncioli D., Bondi M., Bonechi L., Bonino R., Bonnoli G., Bonvicini V., Bossini E., Bottino B., Buscemi M., Caccianiga B., Caccianiga L., Candela A., Capone A., Cariello M., Caruso R., Cataldi G., Chiodi G., Chiodini G., Coluccia M. R., Convenga F., Copello S., Corosu M., D'Urso D., Dal Corso F., Davini S., De Deo M., De Gateano S., De Laurentis M., De Mitri I., De Palma F., De Vito E., Dell'Aquila D., Depaoli D., Di Luca A., Di Pierro F., Di Ruzza B., Di Santo M., Di Sciascio G., Di Venere L., Dimiccoli F., Dimitrios K., Donnini F., Doro M., Duranti M., Evoli C., Fenu F., Fontanelli F., Fusco P., Gargano F., Gervasi M., Giampaoli A., Giglietto N., Giordano F., Gnesi I., Gonzi S., Grandi D., Graziani M., Hemmer S., Iacoangeli F., Insolia A., Iovenitti S., Ippolito V., La Vacca G., La Verde G., Leonora E., Levorato S., Liguori D., Lipari P., Longo F., Loparco F., Lopez Coto R., Loporchio S., Marino A., Marsella G., Martello D., Mazziotta M. N., Menegolli A., Miozzi S., Miyamoto H., Mocchiutti E., Morganti S., Morsani F., Munini R., Mussa R., Nozzoli F., Nucita A., Organtini G. C., Ottonello G., Pantaleo F., Paoletti R., Parodi F., Perrone L., Pesenti L., Petrera S., Petronio C., Pillera R., Pilo F., Pizzolotto C., Prandini E., Pugliese M., Raino S., Randazzo N., Rando R., Recchia L., Ricci E., Rinaudo M., Rizi V., Rossi N., Rozza D., Salamida F., Savina P., Scherini V., Schioppa M., Scotti V., Serini D., Sipala V., Surdo A., Tiberio A., Tomassetti N., Tomei C., Tosta E Melo I., Turco P., Vannuccini E., Vecchiotti V., Veronesi I., and Zampa G.
Abstract: The outreach program “A scuola di Astroparticelle” was proposed in 2016 by the National Institute for Nuclear Physics (INFN - Napoli Division) in collaboration with the Physics Department “Ettore Pancini” of the Federico II University in Napoli, CNR-SPIN and CNR-ISASI Institutes. Its main goal is to engage teachers and students of High Schools in astroparticle physics projects. For the third edition (2018/19), the activities, which are also part of the Italian Educational Program PCTO - “Percorsi per le Competenze Trasversali e per l'Orientamento”, involved 18 schools for a total of 21 projects on several topics. Some projects were strictly related to astroparticles as cosmic rays, while others were more technical, as the development of particle detectors, or cross-disciplinary projects. Students worked for the entire school year and prepared materials for the final event. More than 600 students attended the event and presented their work to a jury with a poster and an oral presentation in plenary sessions. Since 2018, the program is part of OCRA - Outreach Cosmic Ray Activities - a national outreach project of INFN with the aim of collecting, within a common framework, the numerous outreach activities in cosmic-ray field carried out at the local level. The fourth edition (2019-20), in spite of the difficult situation due to the COVID-19 pandemic, has also seen the participation of 22 schools that carried out part of the activities in an online format. The project realized using the open data of the Pierre Auger Observatory will be presented in detail.
Published: 2022

8. The accretion/ejection link in the neutron star X-ray binary 4U 1820-30 I: A boundary layer-jet coupling?

Author: Marino, A., Russell, T. D., Del Santo, M., Beri, A., Sanna, A., Zelati, F. Coti, Degenaar, N., Altamirano, D., Ambrosi, E., Anitra, A., Carotenuto, F., D'Ai, A., Di Salvo, T., Manca, A., Motta, S. E., Pinto, C., Pintore, F., Rea, N., Eijnden, J. Van den, Marino, A., Russell, T. D., Del Santo, M., Beri, A., Sanna, A., Zelati, F. Coti, Degenaar, N., Altamirano, D., Ambrosi, E., Anitra, A., Carotenuto, F., D'Ai, A., Di Salvo, T., Manca, A., Motta, S. E., Pinto, C., Pintore, F., Rea, N., and Eijnden, J. Van den
Abstract: The accretion flow / jet correlation in neutron star (NS) low-mass X-ray binaries (LMXBs) is far less understood when compared to black hole (BH) LMXBs. In this paper we will present the results of a dense multi-wavelength observational campaign on the NS LMXB 4U 1820-30, including X-ray (Nicer, NuSTAR and AstroSAT) and quasi-simultaneous radio (ATCA) observations in 2022. 4U 1820-30 shows a peculiar 170 day super-orbital accretion modulation, during which the system evolves between "modes" of high and low X-ray flux. During our monitoring, the source did not show any transition to a full hard state. X-ray spectra were well described using a disc blackbody, a Comptonisation spectrum along with a Fe K emission line at 6.6 keV. Our results show that the observed X-ray flux modulation is almost entirely produced by changes in the size of the region providing seed photons for the Comptonisation spectrum. This region is large (about 15 km) in the high mode and likely coincides with the whole boundary layer, while it shrinks significantly (<10 km) in low mode. The electron temperature of the corona and the observed RMS variability in the hard X-rays also exhibit a slight increase in low mode. As the source moves from high to low mode, the radio emission due to the jet becomes about 5 fainter. These radio changes appear not to be strongly connected to the hard-to-soft transitions as in BH systems, while they seem to be connected mostly to variations observed in the boundary layer., Comment: 12 pages, 6 figures. Accepted for publication by MNRAS
Published: 2023
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9. An ultrafast outflow in the black hole candidate MAXI J1810-222?

Author: Del Santo, M., Pinto, C., Marino, A., D'Aì, A., Petrucci, P. -O., Malzac, J., Ferreira, J., Pintore, F., Motta, S. E., Russell, T. D., Segreto, A., Sanna, A., Del Santo, M., Pinto, C., Marino, A., D'Aì, A., Petrucci, P. -O., Malzac, J., Ferreira, J., Pintore, F., Motta, S. E., Russell, T. D., Segreto, A., and Sanna, A.
Abstract: The transient X-ray source MAXI J1810-222 was discovered in 2018 and has been active ever since. A long combined radio and X-ray monitoring campaign was performed with ATCA and Swift respectively. It has been proposed that MAXI J1810-222 is a relatively distant black hole X-ray binary, albeit showing a very peculiar outburst behaviour. Here, we report on the spectral study of this source making use of a large sample of NICER observations performed between 2019 February and 2020 September. We detected a strong spectral absorption feature at $\sim$1 keV, which we have characterised with a physical photoionisation model. Via a deep scan of the parameters space, we obtained evidence for a spectral-state dependent outflow, with mildly relativistic speeds. In particular, the soft and intermediate states point to a hot plasma outflowing at 0.05-0.15 $c$. This speeds rule-out thermal winds and, hence, they suggest that such outflows could be radiation pressure or (most likely) magnetically-driven winds. Our results are crucial to test current theoretical models of wind formation in X-ray binaries., Comment: 6 pages, 10 figures, accepted for publication in MNRAS Letter
Published: 2023
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10. The High Energy X-ray Probe (HEX-P): A New Window into Neutron Star Accretion

Author: Ludlam, R. M., Malacaria, C., Sokolova-Lapa, E., Fuerst, F., Pradhan, P., Shaw, A. W., Pottschmidt, K., Pike, S., Vasilopoulos, G., Wilms, J., García, J. A., Madsen, K., Stern, D., Maitra, C., Del Santo, M., Walton, D. J., Brumback, M. C., Eijnden, J. van den, Ludlam, R. M., Malacaria, C., Sokolova-Lapa, E., Fuerst, F., Pradhan, P., Shaw, A. W., Pottschmidt, K., Pike, S., Vasilopoulos, G., Wilms, J., García, J. A., Madsen, K., Stern, D., Maitra, C., Del Santo, M., Walton, D. J., Brumback, M. C., and Eijnden, J. van den
Abstract: Accreting neutron stars (NSs) represent a unique laboratory for probing the physics of accretion in the presence of strong magnetic fields ($B\gtrsim 10^8$ G). Additionally, the matter inside the NS itself exists in an ultra-dense, cold state that cannot be reproduced in Earth-based laboratories. Hence, observational studies of these objects are a way to probe the most extreme physical regimes. Here we present an overview of the field and discuss the most important outstanding problems related to NS accretion. We show how these open questions regarding accreting NSs in both low-mass and high-mass X-ray binary systems can be addressed with the High-Energy X-ray Probe (HEX-P) via simulated data. In particular, with the broad X-ray passband and improved sensitivity afforded by a low X-ray background, HEX-P will be able to 1) distinguish between competing continuum emission models; 2) provide tighter upper limits on NS radii via reflection modeling techniques that are independent and complementary to other existing methods; 3) constrain magnetic field geometry, plasma parameters, and accretion column emission patterns by characterizing fundamental and harmonic cyclotron lines and exploring their behavior with pulse phase; 4) directly measure the surface magnetic field strength of highly magnetized NSs at the lowest accretion luminosities; as well as 5) detect cyclotron line features in extragalactic sources and probe their dependence on luminosity in the super-Eddington regime in order to distinguish between geometrical evolution and accretion-induced decay of the magnetic field. In these ways HEX-P will provide an essential new tool for exploring the physics of NSs, their magnetic fields, and the physics of extreme accretion., Comment: 37 pages, 13 figures, 4 tables, To be published in a special topical issue by Frontiers in Astronomy and Space Sciences on probe-class mission concept HEX-P
Published: 2023

11. Search for relativistic fractionally charged particles in space

Author: DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De-Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. F., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. L., Li, W. H., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. M., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, E. H., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhu, Y., DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De-Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. F., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. L., Li, W. H., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. M., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, E. H., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.
Abstract: More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been few searches for FCPs in cosmic rays carried out in orbit other than AMS-01 flown by a space shuttle and BESS by a balloon at the top of the atmosphere. In this study, we conduct an FCP search in space based on on-orbit data obtained using the DArk Matter Particle Explorer (DAMPE) satellite over a period of five years. Unlike underground experiments, which require an FCP energy of the order of hundreds of GeV, our FCP search starts at only a few GeV. An upper limit of $6.2\times 10^{-10}~~\mathrm{cm^{-2}sr^{-1} s^{-1}}$ is obtained for the flux. Our results demonstrate that DAMPE exhibits higher sensitivity than experiments of similar types by three orders of magnitude that more stringently restricts the conditions for the existence of FCP in primary cosmic rays., Comment: 19 pages, 6 figures, accepted by PRD
Published: 2022
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12. Search for relativistic fractionally charged particles in space

Author: DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De-Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. F., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. L., Li, W. H., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. M., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, E. H., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhu, Y., DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De-Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. F., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. L., Li, W. H., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. M., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, E. H., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.
Abstract: More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been few searches for FCPs in cosmic rays carried out in orbit other than AMS-01 flown by a space shuttle and BESS by a balloon at the top of the atmosphere. In this study, we conduct an FCP search in space based on on-orbit data obtained using the DArk Matter Particle Explorer (DAMPE) satellite over a period of five years. Unlike underground experiments, which require an FCP energy of the order of hundreds of GeV, our FCP search starts at only a few GeV. An upper limit of $6.2\times 10^{-10}~~\mathrm{cm^{-2}sr^{-1} s^{-1}}$ is obtained for the flux. Our results demonstrate that DAMPE exhibits higher sensitivity than experiments of similar types by three orders of magnitude that more stringently restricts the conditions for the existence of FCP in primary cosmic rays., Comment: 19 pages, 6 figures, accepted by PRD
Published: 2022
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13. A transient ultraluminous X-ray source in NGC 55

Author: Robba, A., Pinto, C., Pintore, F., Rodriguez, G., Ambrosi, E., Barra, F., Cusumano, G., D'Aì, A., Del Santo, M., Kosec, P., Marino, A., Middleton, M., Roberts, T., Salvaggio, C., Soria, R., Wolter, A., Walton, D., Robba, A., Pinto, C., Pintore, F., Rodriguez, G., Ambrosi, E., Barra, F., Cusumano, G., D'Aì, A., Del Santo, M., Kosec, P., Marino, A., Middleton, M., Roberts, T., Salvaggio, C., Soria, R., Wolter, A., and Walton, D.
Abstract: Ultraluminous X-ray sources (ULXs) are a class of accreting compact objects with X-ray luminosities above 10$^{39}$ erg s$^{-1}$. The average number of ULXs per galaxy is still not well constrained, especially given the uncertainty on the fraction of ULX transients. Here, we report the identification of a new transient ULX in the galaxy NGC 55 (which we label as ULX-2), thanks to recent XMM-Newton and the Neil Gehrels Swift Observatory observations. This object was previously classified as a transient X-ray source with a luminosity around a few 10$^{38}$ erg s$^{-1}$ in a 2010 XMM-Newton observation. Thanks to new and deeper observations ($\sim$ 130 ks each), we show that the source reaches a luminosity peak $>1.6 \times 10^{39}$ erg s$^{-1}$. The X-ray spectrum of ULX-2 is much softer than in previous observations and fits in the class of soft ULXs. It can be well described using a model with two thermal components, as often found in ULXs. The time scales of the X-ray variability are of the order of a month and are likely driven by small changes in the accretion rate or due to super-orbital modulations, attributed to precession of the accretion disc, which is similar to other ULXs., Comment: 6 pages, including 4 figures and 2 tables, accepted for pubblication in MNRAS
Published: 2022
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14. Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

Author: MIT Kavli Institute for Astrophysics and Space Research, Alston, W N, Pinto, C, Barret, D, D’Aì, A, Del Santo, M, Earnshaw, H, Fabian, A C, Fuerst, F, Kara, E, Kosec, P, Middleton, M J, Parker, M L, Pintore, F, Robba, A, Roberts, T P, Sathyaprakash, R, Walton, D, Ambrosi, E, MIT Kavli Institute for Astrophysics and Space Research, Alston, W N, Pinto, C, Barret, D, D’Aì, A, Del Santo, M, Earnshaw, H, Fabian, A C, Fuerst, F, Kara, E, Kosec, P, Middleton, M J, Parker, M L, Pintore, F, Robba, A, Roberts, T P, Sathyaprakash, R, Walton, D, and Ambrosi, E
Abstract: ABSTRACT Most ultraluminous X-ray sources (ULXs) are believed to be stellar mass black holes or neutron stars accreting beyond the Eddington limit. Determining the nature of the compact object and the accretion mode from broad-band spectroscopy is currently a challenge, but the observed timing properties provide insight into the compact object and details of the geometry and accretion processes. Here, we report a timing analysis for an 800 ks XMM–Newton campaign on the supersoft ultraluminous X-ray source, NGC 247 ULX-1. Deep and frequent dips occur in the X-ray light curve, with the amplitude increasing with increasing energy band. Power spectra and coherence analysis reveals the dipping preferentially occurs on ∼5 and ∼10 ks time-scales. The dips can be caused by either the occultation of the central X-ray source by an optically thick structure, such as warping of the accretion disc, or from obscuration by a wind launched from the accretion disc, or both. This behaviour supports the idea that supersoft ULXs are viewed close to edge-on to the accretion disc.
Published: 2022

15. Unveiling the disc structure in ultraluminous X-ray source NGC 55 ULX-1

Author: Barra, F., Pinto, C., Walton, D. J., Kosec, P., D'Aì, A., Di Salvo, T., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Marino, A., Pintore, F., Robba, A., Roberts, T. P., Barra, F., Pinto, C., Walton, D. J., Kosec, P., D'Aì, A., Di Salvo, T., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Marino, A., Pintore, F., Robba, A., and Roberts, T. P.
Abstract: Despite two decades of studies, it is still not clear whether ULX spectral transitions are due to stochastic variability in the wind or variations in the accretion rate or in the source geometry. The compact object is also unknown for most ULXs. In order to place constraints onto such scenarios and on the structure of the accretion disc, we studied the temporal evolution of the spectral components of the variable source NGC 55 ULX-1. Using recent and archival data obtained with the XMM-Newton satellite, we modelled the spectra with two blackbody components which we interpret as thermal emission from the inner accretion flow and the regions around or beyond the spherization radius. The luminosity-temperature (L-T) relation of each spectral component agrees with the L proportional T^4 relationship expected from a thin disc model, which suggests that the accretion rate is close to the Eddington limit. However, there are some small deviations at the highest luminosities, possibly due to an expansion of the disc and a contribution from the wind at higher accretion rates. Assuming that such deviations are due to the crossing of the Eddington or supercritical accretion rate, we estimate a compact object mass of 6-14 Msun, favouring a stellar-mass black hole as the accretor., Comment: 12 pages, 9 figures, accepted for publication in MNRAS
Published: 2022
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16. The chameleon on the branches: spectral state transition and dips in NGC 247 ULX-1

Author: MIT Kavli Institute for Astrophysics and Space Research, D’Aì, A, Pinto, C, Del Santo, M, Pintore, F, Soria, R, Robba, A, Ambrosi, E, Alston, W, Barret, D, Fabian, AC, Fürst, F, Kara, E, Kosec, P, Middleton, M, Roberts, T, Rodriguez-Castillo, G, Walton, DJ, MIT Kavli Institute for Astrophysics and Space Research, D’Aì, A, Pinto, C, Del Santo, M, Pintore, F, Soria, R, Robba, A, Ambrosi, E, Alston, W, Barret, D, Fabian, AC, Fürst, F, Kara, E, Kosec, P, Middleton, M, Roberts, T, Rodriguez-Castillo, G, and Walton, DJ
Abstract: ABSTRACT Soft Ultra-Luminous X-ray (ULXs) sources are a subclass of the ULXs that can switch from a supersoft spectral state, where most of the luminosity is emitted below 1 keV, to a soft spectral state with significant emission above 1 keV. In a few systems, dips have been observed. The mechanism behind this state transition and the dips nature are still debated. To investigate these issues, we obtained a long XMM–Newton monitoring campaign of a member of this class, NGC 247 ULX-1. We computed the hardness–intensity diagram for the whole data set and identified two different branches: the normal branch and the dipping branch, which we study with four and three hardness–intensity resolved spectra, respectively. All seven spectra are well described by two thermal components: a colder (kTbb ∼ 0.1–0.2 keV) blackbody, interpreted as emission from the photosphere of a radiatively driven wind, and a hotter (kTdisc ∼ 0.6 keV) multicolour disc blackbody, likely due to reprocessing of radiation emitted from the innermost regions. In addition, a complex pattern of emission and absorption lines has been taken into account based on previous high-resolution spectroscopic results. We studied the evolution of spectral parameters and flux of the two thermal components along the two branches and discuss two scenarios possibly connecting the state transition and the dipping phenomenon. One is based on geometrical occultation of the emitting regions, the other invokes the onset of a propeller effect.
Published: 2022

17. Galactic Observatory Science with the ASTRI Mini-Array at the Observatorio del Teide

Author: D'Aì, A., Amato, E., Burtovoi, A., Compagnino, A. A., Fiori, M., Giuliani, A., La Palombara, N., Paizis, A., Piano, G., Saturni, F. G., Tutone, A., Belfiore, A., Cardillo, M., Crestan, S., Cusumano, G., Della Valle, M., Del Santo, M., La Barbera, A., La Parola, V., Lombardi, S., Mereghetti, S., Morlino, G., Pintore, F., Romano, P., Vercellone, S., Antonelli, A., Arcaro, C., Bigongiari, C., Böettcher, M., Bruno, P., Bulgarelli, A., Conforti, V., Costa, A., Pino, E. de Gouveia Dal, Fioretti, V., Germani, S., Ghedina, A., Gianotti, F., Giordano, V., Incardona, F., Leto, G., Longo, F., Oramas, A. López, Lucarelli, F., Olmi, B., Pagliaro, A., Parmiggiani, N., Romeo, G., Stamerra, A., Testa, V., Tosti, G., Umana, G., Zampieri, L., Caraveo, P., Pareschi, G., D'Aì, A., Amato, E., Burtovoi, A., Compagnino, A. A., Fiori, M., Giuliani, A., La Palombara, N., Paizis, A., Piano, G., Saturni, F. G., Tutone, A., Belfiore, A., Cardillo, M., Crestan, S., Cusumano, G., Della Valle, M., Del Santo, M., La Barbera, A., La Parola, V., Lombardi, S., Mereghetti, S., Morlino, G., Pintore, F., Romano, P., Vercellone, S., Antonelli, A., Arcaro, C., Bigongiari, C., Böettcher, M., Bruno, P., Bulgarelli, A., Conforti, V., Costa, A., Pino, E. de Gouveia Dal, Fioretti, V., Germani, S., Ghedina, A., Gianotti, F., Giordano, V., Incardona, F., Leto, G., Longo, F., Oramas, A. López, Lucarelli, F., Olmi, B., Pagliaro, A., Parmiggiani, N., Romeo, G., Stamerra, A., Testa, V., Tosti, G., Umana, G., Zampieri, L., Caraveo, P., and Pareschi, G.
Abstract: The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Mini-Array will be composed of nine imaging atmospheric Cherenkov telescopes at the Observatorio del Teide site. The array will be best suited for astrophysical observations in the 0.3-200 TeV range with an angular resolution of few arc-minutes and an energy resolution of 10-15\%. A core-science programme in the first four years will be devoted to a limited number of key targets, addressing the most important open scientific questions in the very-high energy domain. At the same time, thanks to a wide field of view of about 10 degrees, ASTRI Mini-Array will observe many additional field sources, which will constitute the basis for the long-term observatory programme that will eventually cover all the accessible sky. In this paper, we review different astrophysical Galactic environments, e.g. pulsar wind nebulae, supernova remnants, and gamma-ray binaries, and show the results from a set of ASTRI Mini-Array simulations of some of these field sources made to highlight the expected performance of the array (even at large offset angles) and the important additional observatory science that will complement the core-science program., Comment: Accepted for publication in Journal of High-Energy Astrophysics
Published: 2022
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18. ASTRI Mini-Array Core Science at the Observatorio del Teide

Author: Vercellone, S., Bigongiari, C., Burtovoi, A., Cardillo, M., Catalano, O., Franceschini, A., Lombardi, S., Nava, L., Pintore, F., Stamerra, A., Tavecchio, F., Zampieri, L., Batista, R. Alves, Amato, E., Antonelli, L. A., Arcaro, C., Gonzalez, J. Becerra, Bonnoli, G., Bottcher, M., Brunetti, G., Compagnino, A. A., Crestan, S., Ai, A. D, Fiori, M., Galanti, G., Giuliani, A., Pino, E. M. de Gouveia Dal, Green, J. G., Lamastra, A., Landoni, M., Lucarelli, F., Morlino, G., Olmi, B., Peretti, E., Piano, G., Ponti, G., Poretti, E., Romano, P., Saturni, F. G., Scuderi, S., Tutone, A., Umana, G., Acosta-Pulido, J. A., Barai, P., Bonanno, A., Bonanno, G., Bruno, P., Bulgarelli, A., Conforti, V., Costa, A., Cusumano, G., Del Santo, M., del Valle, M. V., Della Ceca, R., Falceta-Goncalves, D. A., Fioretti, V., Germani, S., Garcia-Lopez, R. J., Ghedina, A., Giordano, V., Kreter, M., Incardona, F., Iovenitti, S., La Barbera, A., La Palombara, N., La Parola, V., Leto, G., Longo, F., Lopez-Oramas, A., Maccarone, M. C., Mereghetti, S., Millul, R., Naletto, G., Pagliaro, A., Parmiggiani, N., Righi, C., Rodriguez-Ramirez, J. C., Romeo, G., Sangiorgi, P., de Lima, R. Santos, Tagliaferri, G., Testa, V., Tosti, G., Acosta, M. Vazquez, Zywucka, N., Caraveo, P. A., Pareschi, G., Vercellone, S., Bigongiari, C., Burtovoi, A., Cardillo, M., Catalano, O., Franceschini, A., Lombardi, S., Nava, L., Pintore, F., Stamerra, A., Tavecchio, F., Zampieri, L., Batista, R. Alves, Amato, E., Antonelli, L. A., Arcaro, C., Gonzalez, J. Becerra, Bonnoli, G., Bottcher, M., Brunetti, G., Compagnino, A. A., Crestan, S., Ai, A. D, Fiori, M., Galanti, G., Giuliani, A., Pino, E. M. de Gouveia Dal, Green, J. G., Lamastra, A., Landoni, M., Lucarelli, F., Morlino, G., Olmi, B., Peretti, E., Piano, G., Ponti, G., Poretti, E., Romano, P., Saturni, F. G., Scuderi, S., Tutone, A., Umana, G., Acosta-Pulido, J. A., Barai, P., Bonanno, A., Bonanno, G., Bruno, P., Bulgarelli, A., Conforti, V., Costa, A., Cusumano, G., Del Santo, M., del Valle, M. V., Della Ceca, R., Falceta-Goncalves, D. A., Fioretti, V., Germani, S., Garcia-Lopez, R. J., Ghedina, A., Giordano, V., Kreter, M., Incardona, F., Iovenitti, S., La Barbera, A., La Palombara, N., La Parola, V., Leto, G., Longo, F., Lopez-Oramas, A., Maccarone, M. C., Mereghetti, S., Millul, R., Naletto, G., Pagliaro, A., Parmiggiani, N., Righi, C., Rodriguez-Ramirez, J. C., Romeo, G., Sangiorgi, P., de Lima, R. Santos, Tagliaferri, G., Testa, V., Tosti, G., Acosta, M. Vazquez, Zywucka, N., Caraveo, P. A., and Pareschi, G.
Abstract: The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Project led by the Italian National Institute for Astrophysics (INAF) is developing and will deploy at the Observatorio del Teide a mini-array (ASTRI Mini-Array) composed of nine telescopes similar to the small-size dual-mirror Schwarzschild-Couder telescope (ASTRI-Horn) currently operating on the slopes of Mt. Etna in Sicily. The ASTRI Mini-Array will surpass the current Cherenkov telescope array differential sensitivity above a few tera-electronvolt (TeV), extending the energy band well above hundreds of TeV. This will allow us to explore a new window of the electromagnetic spectrum, by convolving the sensitivity performance with excellent angular and energy resolution figures. In this paper we describe the Core Science that we will address during the first four years of operation, providing examples of the breakthrough results that we will obtain when dealing with current open questions, such as the acceleration of cosmic rays, cosmology and fundamental physics and the new window, for the TeV energy band, of the time-domain astrophysics., Comment: Published in Journal of High Energy Astrophysics. 46 Figures, 7 Tables
Published: 2022
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19. Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

Author: Alston, WN, Pinto, C, Barret, D, D’Aì, A, Del Santo, M, Earnshaw, H, Fabian, AC, Fuerst, F, Kara, E, Kosec, P, Middleton, MJ, Parker, ML, Pintore, F, Robba, A, Roberts, TP, Sathyaprakash, R, Walton, D, Ambrosi, E, Alston, WN, Pinto, C, Barret, D, D’Aì, A, Del Santo, M, Earnshaw, H, Fabian, AC, Fuerst, F, Kara, E, Kosec, P, Middleton, MJ, Parker, ML, Pintore, F, Robba, A, Roberts, TP, Sathyaprakash, R, Walton, D, and Ambrosi, E
Abstract: ABSTRACT Most ultraluminous X-ray sources (ULXs) are believed to be stellar mass black holes or neutron stars accreting beyond the Eddington limit. Determining the nature of the compact object and the accretion mode from broad-band spectroscopy is currently a challenge, but the observed timing properties provide insight into the compact object and details of the geometry and accretion processes. Here, we report a timing analysis for an 800 ks XMM–Newton campaign on the supersoft ultraluminous X-ray source, NGC 247 ULX-1. Deep and frequent dips occur in the X-ray light curve, with the amplitude increasing with increasing energy band. Power spectra and coherence analysis reveals the dipping preferentially occurs on ∼5 and ∼10 ks time-scales. The dips can be caused by either the occultation of the central X-ray source by an optically thick structure, such as warping of the accretion disc, or from obscuration by a wind launched from the accretion disc, or both. This behaviour supports the idea that supersoft ULXs are viewed close to edge-on to the accretion disc.
Published: 2022

20. Investigating the nature and properties of MAXI J1810-222 with radio and X-ray observations

Author: Russell, T. D., Del Santo, M., Marino, A., Segreto, A., Motta, S. E., Bahramian, A., Corbel, S., D'Aì, A., Di Salvo, T., Miller-Jones, J. C. A., Pinto, C., Pintore, F., Tzioumis, A., Russell, T. D., Del Santo, M., Marino, A., Segreto, A., Motta, S. E., Bahramian, A., Corbel, S., D'Aì, A., Di Salvo, T., Miller-Jones, J. C. A., Pinto, C., Pintore, F., and Tzioumis, A.
Abstract: We present results from radio and X-ray observations of the X-ray transient MAXI J1810-222. The nature of the accretor in this source has not been identified. In this paper, we show results from a quasi-simultaneous radio and X-ray monitoring campaign taken with the Australia Telescope Compact Array (ATCA), the Neil Gehrels Swift observatory X-ray telescope (XRT), and the Swift Burst Alert Telescope (BAT). We also analyse the X-ray temporal behaviour using observations from the Neutron star Interior Composition Explorer (NICER). Results show a seemingly peculiar X-ray spectral evolution of MAXI J1810-222 during this outburst, where the source was initially only detected in the soft X-ray band for the early part of the outburst. Then, ~200 days after MAXI J1810-222 was first detected the hard X-ray emission increased and the source transitioned to a long-lived (~1.5 years) bright, harder X-ray state. After this hard state, MAXI J1810-222 returned back to a softer state, before fading and transitioning again to a harder state and then appearing to follow a more typical outburst decay. From the X-ray spectral and timing properties, and the source's radio behaviour, we argue that the results from this study are most consistent with MAXI J1810-222 being a relatively distant ($\gtrsim$6 kpc) black hole X-ray binary. A sufficiently large distance to source can simply explain the seemingly odd outburst evolution that was observed, where only the brightest portion of the outburst was detectable by the all-sky X-ray telescopes., Comment: 15 pages, 8 figures, 5 tables, accepted for publication in MNRAS
Published: 2022
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21. Time domain astronomy with the THESEUS satellite

Author: Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., and Zhang, B.
Abstract: 29 november 2021, Contains fulltext : 246535.pdf (Publisher’s version ) (Closed access) Contains fulltext : 246535pre.pdf (Author’s version preprint ) (Closed access)
Published: 2021

22. Tracking the evolution of the accretion flow in MAXI J1820+070 during its hard state with the JED-SAD model

Author: Marino, A., Barnier, S., Petrucci, P. O., Del Santo, M., Malzac, J., Ferreira, J., Marcel, G., Segreto, A., Motta, S. E., D'Aì, A., Di Salvo, T., Guillot, S., Russell, T. D., Marino, A., Barnier, S., Petrucci, P. O., Del Santo, M., Malzac, J., Ferreira, J., Marcel, G., Segreto, A., Motta, S. E., D'Aì, A., Di Salvo, T., Guillot, S., and Russell, T. D.
Abstract: X-ray binaries in outburst typically show two canonical X-ray spectral states, i.e. hard and soft states, in which the physical properties of the accretion flow and of the jet are known to change. Recently, the JED-SAD paradigm has been proposed for black hole X-ray binaries, aimed to address the accretion-ejection interplay in these systems. According to this model, the accretion flow is composed by an outer standard Shakura-Sunyaev disk (SAD) and an inner hot Jet Emitting Disk (JED). The JED produces both the hard X-ray emission, effectively playing the role of the hot corona, and the radio jets. In this paper, we use the JED-SAD model to describe the evolution of the accretion flow in the black hole transient MAXI J1820+070 during its hard and hard-intermediate states. Contrarily to the previous applications of this model, the Compton reflection component has been taken into account. We use eight broadband X-rays spectra, including NuSTAR, NICER and Swift data, providing a total spectral coverage of 0.8-190 keV. The data were directly fitted with the JED-SAD model. Our results suggest that the optically thick disk (i.e. the SAD) does not extend down to the ISCO in any of the considered epochs. In particular, as the system evolves towards the hard/intermediate state, we find that the inner radius decreases from $\sim$60 R$_{\rm G}$ in the first observation down to $\sim$30 R$_{\rm G}$ in the last one. This trend is accompanied by an increase of the mass-accretion rate. In all hard-intermediate state observations, two reflection components, characterized by different values of ionization, are required to adequately explain the data. These components likely originate from different regions of the SAD. We show that a flared outer disk could, in principle, explain the double reflection component., Comment: 15 pages, 11 figures. Accepted for publication in A&A
Published: 2021
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23. The chameleon on the branches: spectral state transition and dips in NGC 247 ULX-1

Author: D'Aì, A., Pinto, C., Del Santo, M., Pintore, F., Soria, R., Robba, A., Ambrosi, E., Alston, W., Barret, D., Fabian, A. C., Fürst, F., Kara, E., Kosec, P., Middleton, M., Roberts, T., Rodriguez-Castillo, G., Walton, D. J., D'Aì, A., Pinto, C., Del Santo, M., Pintore, F., Soria, R., Robba, A., Ambrosi, E., Alston, W., Barret, D., Fabian, A. C., Fürst, F., Kara, E., Kosec, P., Middleton, M., Roberts, T., Rodriguez-Castillo, G., and Walton, D. J.
Abstract: Soft Ultra-Luminous X-ray (ULXs) sources are a subclass of the ULXs that can switch from a supersoft spectral state, where most of the luminosity is emitted below 1 keV, to a soft spectral state with significant emission above 1 keV. In a few systems, dips have been observed. The mechanism behind this state transition and the dips nature are still debated. To investigate these issues, we obtained a long XMM-Newton monitoring campaign of a member of this class, NGC 247 ULX-1. We computed the hardness-intensity diagram for the whole dataset and identified two different branches: the normal branch and the dipping branch, which we study with four and three hardness-intensity resolved spectra, respectively. All seven spectra are well described by two thermal components: a colder ($kT_{\rm bb}$ $\sim$ 0.1-0.2 keV) black-body, interpreted as emission from the photo-sphere of a radiatively-driven wind, and a hotter ($kT_{\rm disk}$ $\sim$ 0.6 keV) multicolour disk black-body, likely due to reprocessing of radiation emitted from the innermost regions. In addition, a complex pattern of emission and absorption lines has been taken into account based on previous high-resolution spectroscopic results. We studied the evolution of spectral parameters and the flux of the two thermal components along the two branches and discuss two scenarios possibly connecting the state transition and the dipping phenomenon. One is based on geometrical occultation of the emitting regions, the other invokes the onset of a propeller effect., Comment: 13 pages, accepted by MNRAS on 2021/08/16
Published: 2021
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24. The evolving radio jet from the neutron star X-ray binary 4U 1820$-$30

Author: Russell, T. D., Degenaar, N., Eijnden, J. van den, Del Santo, M., Segreto, A., Altamirano, D., Beri, A., Trigo, M. Diaz, Miller-Jones, J. C. A., Russell, T. D., Degenaar, N., Eijnden, J. van den, Del Santo, M., Segreto, A., Altamirano, D., Beri, A., Trigo, M. Diaz, and Miller-Jones, J. C. A.
Abstract: The persistently bright ultra-compact neutron star low-mass X-ray binary 4U 1820$-$30 displays a $\sim$170 d accretion cycle, evolving between phases of high and low X-ray modes, where the 3 -- 10 keV X-ray flux changes by a factor of up to $\approx 8$. The source is generally in a soft X-ray spectral state, but may transition to a harder state in the low X-ray mode. Here, we present new and archival radio observations of 4U 1820$-$30 during its high and low X-ray modes. For radio observations taken within a low mode, we observed a flat radio spectrum consistent with 4U 1820$-$30 launching a compact radio jet. However, during the high X-ray modes the compact jet was quenched and the radio spectrum was steep, consistent with optically-thin synchrotron emission. The jet emission appeared to transition at an X-ray luminosity of $L_{\rm X (3-10 keV)} \sim 3.5 \times 10^{37} (D/\rm{7.6 kpc})^{2}$ erg s$^{-1}$. We also find that the low-state radio spectrum appeared consistent regardless of X-ray hardness, implying a connection between jet quenching and mass accretion rate in 4U 1820$-$30, possibly related to the properties of the inner accretion disk or boundary layer., Comment: 6 pages, 2 Figures. Online supplementary information supplied in the appendix. Accepted for publication by MNRAS Letters
Published: 2021
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25. The INTEGRAL view on Black Hole X-ray Binaries

Author: Motta, S. E., Rodriguez, J., Jourdain, E., Del Santo, M., Belanger, G., Cangemi, F., Grinberg, V., Kajava, J. J. E., Kuulkers, E., Malzac, J., Pottschmidt, K., Roques, J. P., Sanchez-Fernandez, C., Wilms, J., Motta, S. E., Rodriguez, J., Jourdain, E., Del Santo, M., Belanger, G., Cangemi, F., Grinberg, V., Kajava, J. J. E., Kuulkers, E., Malzac, J., Pottschmidt, K., Roques, J. P., Sanchez-Fernandez, C., and Wilms, J.
Abstract: INTEGRAL is an ESA mission in fundamental astrophysics that was launched in October 2002. It has been in orbit for over 18 years, during which it has been observing the high-energy sky with a set of instruments specifically designed to probe the emission from hard X-ray and soft gamma-ray sources. This paper is devoted to the subject of black hole binaries, which are among the most important sources that populate the high-energy sky. We present a review of the scientific literature based on INTEGRAL data, which has significantly advanced our knowledge in the field of relativistic astrophysics. We briefly summarise the state-of-the-art of the study of black hole binaries, with a particular focus on the topics closer to the INTEGRAL science. We then give an overview of the results obtained by INTEGRAL and by other observatories on a number of sources of importance in the field. Finally, we review the main results obtained over the past 18 years on all the black hole binaries that INTEGRAL has observed. We conclude with a summary of the main contributions of INTEGRAL to the field, and on the future perspectives., Comment: 44 pages, 11 figures. Accepted for publication on New Astronomy Reviews
Published: 2021
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26. Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

Author: Alston, W. N., Pinto, C., Barret, D., D'Ai, A., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Kara, E., Kosec, P., Middleton, M. J., Parker, M. L., Pintore, F., Robba, A., Roberts, T. P., Sathyaprakash, R., Walton, D., Ambrosi, E., Alston, W. N., Pinto, C., Barret, D., D'Ai, A., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Kara, E., Kosec, P., Middleton, M. J., Parker, M. L., Pintore, F., Robba, A., Roberts, T. P., Sathyaprakash, R., Walton, D., and Ambrosi, E.
Abstract: Most ultraluminous X-ray sources (ULXs) are believed to be stellar mass black holes or neutron stars accreting beyond the Eddington limit. Determining the nature of the compact object and the accretion mode from broadband spectroscopy is currently a challenge, but the observed timing properties provide insight into the compact object and details of the geometry and accretion processes. Here we report a timing analysis for an 800 ks XMM-Newton campaign on the supersoft ultraluminous X-ray source, NGC 247 ULX-1. Deep and frequent dips occur in the X-ray light curve, with the amplitude increasing with increasing energy band. Power spectra and coherence analysis reveals the dipping preferentially occurs on $\sim 5$ ks and $\sim 10$ ks timescales. The dips can be caused by either the occultation of the central X-ray source by an optically thick structure, such as warping of the accretion disc, or from obscuration by a wind launched from the accretion disc, or both. This behaviour supports the idea that supersoft ULXs are viewed close to edge-on to the accretion disc., Comment: Accepted MNRAS version following minor comments. 8 pages, 6 figures
Published: 2021
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27. XMM-Newton campaign on the ultraluminous X-ray source NGC 247 ULX-1: outflows

Author: Pinto, C., Soria, R., Walton, D., D'Ai, A., Pintore, F., Kosec, P., Alston, W. N., Fuerst, F., Middleton, M. J., Roberts, T. P., Del Santo, M., Barret, D., Ambrosi, E., Robba, A., Earnshaw, H., Fabian, A., Pinto, C., Soria, R., Walton, D., D'Ai, A., Pintore, F., Kosec, P., Alston, W. N., Fuerst, F., Middleton, M. J., Roberts, T. P., Del Santo, M., Barret, D., Ambrosi, E., Robba, A., Earnshaw, H., and Fabian, A.
Abstract: Most ULXs are believed to be powered by super-Eddington accreting neutron stars and, perhaps, black holes. Above the Eddington rate the disc is expected to thicken and to launch powerful winds through radiation pressure. Winds have been recently discovered in several ULXs. However, it is yet unclear whether the thickening of the disc or the wind variability causes the switch between the classical soft and supersoft states observed in some ULXs. In order to understand such phenomenology and the overall super-Eddington mechanism, we undertook a large (800 ks) observing campaign with XMM-Newton to study NGC 247 ULX-1, which shifts between a supersoft and classical soft ULX state. The new observations show unambiguous evidence of a wind in the form of emission and absorption lines from highly-ionised ionic species, with the latter indicating a mildly-relativistic outflow (-0.17c) in line with the detections in other ULXs. Strong dipping activity is observed in the lightcurve and primarily during the brightest observations, which is typical among soft ULXs, and indicates a close relationship between the accretion rate and the appearance of the dips. The latter is likely due to a thickening of the disc scale-height and the wind as shown by a progressively increasing blueshift in the spectral lines., Comment: 18 pages, 16 figures, accepted for publication in MNRAS
Published: 2021
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28. Taking the pulse of Earth's tropical forests using networks of highly distributed plots

Author: Blundo, C, Carilla, J, Grau, R, Malizia, A, Malizia, L, Osinaga-Acosta, O, Bird, M, Bradford, M, Catchpole, D, Ford, A, Graham, A, Hilbert, D, Kemp, J, Laurance, S, Laurance, W, Ishida, FY, Marshall, A, Waite, C, Woell, H, Bastin, JF, Bauters, M, Beeckman, H, Boeckx, P, Bogaert, J, De Canniere, C, de Haulleville, T, Doucet, JL, Hardy, O, Hubau, W, Kearsley, E, Verbeeck, H, Vleminckx, J, Brewer, SW, Alarcón, A, Araujo-Murakami, A, Arets, E, Arroyo, L, Chavez, E, Fredericksen, T, Villaroel, RG, Sibauty, GG, Killeen, T, Licona, JC, Lleigue, J, Mendoza, C, Murakami, S, Gutierrez, AP, Pardo, G, Peña-Claros, M, Poorter, L, Toledo, M, Cayo, JV, Viscarra, LJ, Vos, V, Ahumada, J, Almeida, E, Almeida, J, de Oliveira, EA, da Cruz, WA, de Oliveira, AA, Carvalho, FA, Obermuller, FA, Andrade, A, Vieira, SA, Aquino, AC, Aragão, L, Araújo, AC, Assis, MA, Gomes, JAMA, Baccaro, F, de Camargo, PB, Barni, P, Barroso, J, Bernacci, LC, Bordin, K, de Medeiros, MB, Broggio, I, Camargo, JL, Cardoso, D, Carniello, MA, Rochelle, ALC, Castilho, C, Castro, AAJF, Castro, W, Ribeiro, SC, Costa, F, de Oliveira, RC, Coutinho, I, Cunha, J, da Costa, L, da Costa Ferreira, L, da Costa Silva, R, da Graça Zacarias Simbine, M, de Andrade Kamimura, V, de Lima, HC, de Oliveira Melo, L, de Queiroz, L, de Sousa Lima, JR, do Espírito Santo, M, Blundo, C, Carilla, J, Grau, R, Malizia, A, Malizia, L, Osinaga-Acosta, O, Bird, M, Bradford, M, Catchpole, D, Ford, A, Graham, A, Hilbert, D, Kemp, J, Laurance, S, Laurance, W, Ishida, FY, Marshall, A, Waite, C, Woell, H, Bastin, JF, Bauters, M, Beeckman, H, Boeckx, P, Bogaert, J, De Canniere, C, de Haulleville, T, Doucet, JL, Hardy, O, Hubau, W, Kearsley, E, Verbeeck, H, Vleminckx, J, Brewer, SW, Alarcón, A, Araujo-Murakami, A, Arets, E, Arroyo, L, Chavez, E, Fredericksen, T, Villaroel, RG, Sibauty, GG, Killeen, T, Licona, JC, Lleigue, J, Mendoza, C, Murakami, S, Gutierrez, AP, Pardo, G, Peña-Claros, M, Poorter, L, Toledo, M, Cayo, JV, Viscarra, LJ, Vos, V, Ahumada, J, Almeida, E, Almeida, J, de Oliveira, EA, da Cruz, WA, de Oliveira, AA, Carvalho, FA, Obermuller, FA, Andrade, A, Vieira, SA, Aquino, AC, Aragão, L, Araújo, AC, Assis, MA, Gomes, JAMA, Baccaro, F, de Camargo, PB, Barni, P, Barroso, J, Bernacci, LC, Bordin, K, de Medeiros, MB, Broggio, I, Camargo, JL, Cardoso, D, Carniello, MA, Rochelle, ALC, Castilho, C, Castro, AAJF, Castro, W, Ribeiro, SC, Costa, F, de Oliveira, RC, Coutinho, I, Cunha, J, da Costa, L, da Costa Ferreira, L, da Costa Silva, R, da Graça Zacarias Simbine, M, de Andrade Kamimura, V, de Lima, HC, de Oliveira Melo, L, de Queiroz, L, de Sousa Lima, JR, and do Espírito Santo, M
Abstract: Tropical forests are the most diverse and productive ecosystems on Earth. While better understanding of these forests is critical for our collective future, until quite recently efforts to measure and monitor them have been largely disconnected. Networking is essential to discover the answers to questions that transcend borders and the horizons of funding agencies. Here we show how a global community is responding to the challenges of tropical ecosystem research with diverse teams measuring forests tree-by-tree in thousands of long-term plots. We review the major scientific discoveries of this work and show how this process is changing tropical forest science. Our core approach involves linking long-term grassroots initiatives with standardized protocols and data management to generate robust scaled-up results. By connecting tropical researchers and elevating their status, our Social Research Network model recognises the key role of the data originator in scientific discovery. Conceived in 1999 with RAINFOR (South America), our permanent plot networks have been adapted to Africa (AfriTRON) and Southeast Asia (T-FORCES) and widely emulated worldwide. Now these multiple initiatives are integrated via ForestPlots.net cyber-infrastructure, linking colleagues from 54 countries across 24 plot networks. Collectively these are transforming understanding of tropical forests and their biospheric role. Together we have discovered how, where and why forest carbon and biodiversity are responding to climate change, and how they feedback on it. This long-term pan-tropical collaboration has revealed a large long-term carbon sink and its trends, as well as making clear which drivers are most important, which forest processes are affected, where they are changing, what the lags are, and the likely future responses of tropical forests as the climate continues to change. By leveraging a remarkably old technology, plot networks are sparking a very modern revolution in tropical forest sc
Published: 2021

29. Time domain astronomy with the THESEUS satellite

Author: Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., and Zhang, B.
Abstract: 29 november 2021, Contains fulltext : 246535.pdf (Publisher’s version ) (Closed access) Contains fulltext : 246535pre.pdf (Author’s version preprint ) (Closed access)
Published: 2021

30. Time domain astronomy with the THESEUS satellite

Author: Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-García, M.D., Santo, M. Del, Doroshenko, V, Erkut, M.H., Jonker, P.G., Zane, S., and Zhang, B.
Abstract: 29 november 2021, Contains fulltext : 246535.pdf (Publisher’s version ) (Closed access) Contains fulltext : 246535pre.pdf (Author’s version preprint ) (Closed access)
Published: 2021

31. Measurement of the cosmic ray helium energy spectrum from 70 GeV to 80 TeV with the DAMPE space mission

Author: Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Santo, M., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, K., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, H., Wang, J. Z., Wang, L. G., Wang, S., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhu, Y., Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Santo, M., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, K., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, H., Wang, J. Z., Wang, L. G., Wang, S., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.
Abstract: The measurement of the energy spectrum of cosmic ray helium nuclei from 70 GeV to 80 TeV using 4.5 years of data recorded by the DArk Matter Particle Explorer (DAMPE) is reported in this work. A hardening of the spectrum is observed at an energy of about 1.3 TeV, similar to previous observations. In addition, a spectral softening at about 34 TeV is revealed for the first time with large statistics and well controlled systematic uncertainties, with an overall significance of $4.3\sigma$. The DAMPE spectral measurements of both cosmic protons and helium nuclei suggest a particle charge dependent softening energy, although with current uncertainties a dependence on the number of nucleons cannot be ruled out., Comment: 11 pages, 13 figures, published in Phys. Rev. Lett. Add one more digit for first three columns in Table S2
Published: 2021
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32. Time domain astronomy with the THESEUS satellite

Author: Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Rivera Sandoval, L., Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D’Aí, A., D’Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, V., Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P. G., Kong, A. K.H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O’Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Rivera Sandoval, L., Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D’Aí, A., D’Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, V., Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P. G., Kong, A. K.H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O’Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., and Zhang, B.
Abstract: THESEUS is a medium size space mission of the European Space Agency, currently under evaluation for a possible launch in 2032. Its main objectives are to investigate the early Universe through the observation of gamma-ray bursts and to study the gravitational waves electromagnetic counterparts and neutrino events. On the other hand, its instruments, which include a wide field of view X-ray (0.3-5 keV) telescope based on lobster-eye focussing optics and a gamma-ray spectrometer with imaging capabilities in the 2-150 keV range, are also ideal for carrying out unprecedented studies in time domain astrophysics. In addition, the presence onboard of a 70 cm near infrared telescope will allow simultaneous multiwavelegth studies. Here we present the THESEUS capabilities for studying the time variability of different classes of sources in parallel to, and without affecting, the gamma-ray bursts hunt.
Published: 2021

33. Taking the pulse of Earth's tropical forests using networks of highly distributed plots

Author: Blundo, C, Carilla, J, Grau, R, Malizia, A, Malizia, L, Osinaga-Acosta, O, Bird, M, Bradford, M, Catchpole, D, Ford, A, Graham, A, Hilbert, D, Kemp, J, Laurance, S, Laurance, W, Ishida, FY, Marshall, A, Waite, C, Woell, H, Bastin, JF, Bauters, M, Beeckman, H, Boeckx, P, Bogaert, J, De Canniere, C, de Haulleville, T, Doucet, JL, Hardy, O, Hubau, W, Kearsley, E, Verbeeck, H, Vleminckx, J, Brewer, SW, Alarcón, A, Araujo-Murakami, A, Arets, E, Arroyo, L, Chavez, E, Fredericksen, T, Villaroel, RG, Sibauty, GG, Killeen, T, Licona, JC, Lleigue, J, Mendoza, C, Murakami, S, Gutierrez, AP, Pardo, G, Peña-Claros, M, Poorter, L, Toledo, M, Cayo, JV, Viscarra, LJ, Vos, V, Ahumada, J, Almeida, E, Almeida, J, de Oliveira, EA, da Cruz, WA, de Oliveira, AA, Carvalho, FA, Obermuller, FA, Andrade, A, Vieira, SA, Aquino, AC, Aragão, L, Araújo, AC, Assis, MA, Gomes, JAMA, Baccaro, F, de Camargo, PB, Barni, P, Barroso, J, Bernacci, LC, Bordin, K, de Medeiros, MB, Broggio, I, Camargo, JL, Cardoso, D, Carniello, MA, Rochelle, ALC, Castilho, C, Castro, AAJF, Castro, W, Ribeiro, SC, Costa, F, de Oliveira, RC, Coutinho, I, Cunha, J, da Costa, L, da Costa Ferreira, L, da Costa Silva, R, da Graça Zacarias Simbine, M, de Andrade Kamimura, V, de Lima, HC, de Oliveira Melo, L, de Queiroz, L, de Sousa Lima, JR, do Espírito Santo, M, Blundo, C, Carilla, J, Grau, R, Malizia, A, Malizia, L, Osinaga-Acosta, O, Bird, M, Bradford, M, Catchpole, D, Ford, A, Graham, A, Hilbert, D, Kemp, J, Laurance, S, Laurance, W, Ishida, FY, Marshall, A, Waite, C, Woell, H, Bastin, JF, Bauters, M, Beeckman, H, Boeckx, P, Bogaert, J, De Canniere, C, de Haulleville, T, Doucet, JL, Hardy, O, Hubau, W, Kearsley, E, Verbeeck, H, Vleminckx, J, Brewer, SW, Alarcón, A, Araujo-Murakami, A, Arets, E, Arroyo, L, Chavez, E, Fredericksen, T, Villaroel, RG, Sibauty, GG, Killeen, T, Licona, JC, Lleigue, J, Mendoza, C, Murakami, S, Gutierrez, AP, Pardo, G, Peña-Claros, M, Poorter, L, Toledo, M, Cayo, JV, Viscarra, LJ, Vos, V, Ahumada, J, Almeida, E, Almeida, J, de Oliveira, EA, da Cruz, WA, de Oliveira, AA, Carvalho, FA, Obermuller, FA, Andrade, A, Vieira, SA, Aquino, AC, Aragão, L, Araújo, AC, Assis, MA, Gomes, JAMA, Baccaro, F, de Camargo, PB, Barni, P, Barroso, J, Bernacci, LC, Bordin, K, de Medeiros, MB, Broggio, I, Camargo, JL, Cardoso, D, Carniello, MA, Rochelle, ALC, Castilho, C, Castro, AAJF, Castro, W, Ribeiro, SC, Costa, F, de Oliveira, RC, Coutinho, I, Cunha, J, da Costa, L, da Costa Ferreira, L, da Costa Silva, R, da Graça Zacarias Simbine, M, de Andrade Kamimura, V, de Lima, HC, de Oliveira Melo, L, de Queiroz, L, de Sousa Lima, JR, and do Espírito Santo, M
Abstract: Tropical forests are the most diverse and productive ecosystems on Earth. While better understanding of these forests is critical for our collective future, until quite recently efforts to measure and monitor them have been largely disconnected. Networking is essential to discover the answers to questions that transcend borders and the horizons of funding agencies. Here we show how a global community is responding to the challenges of tropical ecosystem research with diverse teams measuring forests tree-by-tree in thousands of long-term plots. We review the major scientific discoveries of this work and show how this process is changing tropical forest science. Our core approach involves linking long-term grassroots initiatives with standardized protocols and data management to generate robust scaled-up results. By connecting tropical researchers and elevating their status, our Social Research Network model recognises the key role of the data originator in scientific discovery. Conceived in 1999 with RAINFOR (South America), our permanent plot networks have been adapted to Africa (AfriTRON) and Southeast Asia (T-FORCES) and widely emulated worldwide. Now these multiple initiatives are integrated via ForestPlots.net cyber-infrastructure, linking colleagues from 54 countries across 24 plot networks. Collectively these are transforming understanding of tropical forests and their biospheric role. Together we have discovered how, where and why forest carbon and biodiversity are responding to climate change, and how they feedback on it. This long-term pan-tropical collaboration has revealed a large long-term carbon sink and its trends, as well as making clear which drivers are most important, which forest processes are affected, where they are changing, what the lags are, and the likely future responses of tropical forests as the climate continues to change. By leveraging a remarkably old technology, plot networks are sparking a very modern revolution in tropical forest sc
Published: 2021

34. Time domain astronomy with the THESEUS satellite

Author: Istituto Nazionale di Astrofisica, Science Foundation Ireland, Agenzia Spaziale Italiana, European Commission, Ministerio de Ciencia e Innovación (España), Mereghetti, S., Balman, S., Caballero-García, María Dolores, Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, Peter, Markowitz, A., Osborne, J. P., Pian, E., Rivera Sandoval, L., Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozz, Enrico, Burderi, L., Campana, S., Casella, P., D'Aí, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Götz, Diego, Grinberg, Victoria, Guidorzi, C., Hudec, René, Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P.G., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, Alessio, Martin-Carrillo, A., Mignani, R., Miniutti, Giovanni, Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, Fabio, Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodríguez, J., Saha, T., Sanna, Antonio, Santangelo, Andrea, Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., Zhang, B., Istituto Nazionale di Astrofisica, Science Foundation Ireland, Agenzia Spaziale Italiana, European Commission, Ministerio de Ciencia e Innovación (España), Mereghetti, S., Balman, S., Caballero-García, María Dolores, Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, Peter, Markowitz, A., Osborne, J. P., Pian, E., Rivera Sandoval, L., Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozz, Enrico, Burderi, L., Campana, S., Casella, P., D'Aí, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Götz, Diego, Grinberg, Victoria, Guidorzi, C., Hudec, René, Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P.G., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, Alessio, Martin-Carrillo, A., Mignani, R., Miniutti, Giovanni, Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, Fabio, Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodríguez, J., Saha, T., Sanna, Antonio, Santangelo, Andrea, Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., and Zhang, B.
Abstract: THESEUS is a medium size space mission of the European Space Agency, currently under evaluation for a possible launch in 2032. Its main objectives are to investigate the early Universe through the observation of gamma-ray bursts and to study the gravitational waves electromagnetic counterparts and neutrino events. On the other hand, its instruments, which include a wide field of view X-ray (0.3-5 keV) telescope based on lobster-eye focussing optics and a gamma-ray spectrometer with imaging capabilities in the 2-150 keV range, are also ideal for carrying out unprecedented studies in time domain astrophysics. In addition, the presence onboard of a 70 cm near infrared telescope will allow simultaneous multiwavelegth studies. Here we present the THESEUS capabilities for studying the time variability of different classes of sources in parallel to, and without affecting, the gamma-ray bursts hunt. © 2021, The Author(s), under exclusive licence to Springer Nature B.V.
Published: 2021

35. Tracking the evolution of the accretion flow in MAXI J1820+070 during its hard state with the JED-SAD model

Author: Marino, A., Barnier, S., Petrucci, P. O., Del Santo, M., Malzac, J., Ferreira, J., Marcel, G., Segreto, A., Motta, S. E., D'Aì, A., Di Salvo, T., Guillot, S., Russell, T. D., Marino, A., Barnier, S., Petrucci, P. O., Del Santo, M., Malzac, J., Ferreira, J., Marcel, G., Segreto, A., Motta, S. E., D'Aì, A., Di Salvo, T., Guillot, S., and Russell, T. D.
Abstract: X-ray binaries in outburst typically show two canonical X-ray spectral states, i.e. hard and soft states, in which the physical properties of the accretion flow and of the jet are known to change. Recently, the JED-SAD paradigm has been proposed for black hole X-ray binaries, aimed to address the accretion-ejection interplay in these systems. According to this model, the accretion flow is composed by an outer standard Shakura-Sunyaev disk (SAD) and an inner hot Jet Emitting Disk (JED). The JED produces both the hard X-ray emission, effectively playing the role of the hot corona, and the radio jets. In this paper, we use the JED-SAD model to describe the evolution of the accretion flow in the black hole transient MAXI J1820+070 during its hard and hard-intermediate states. Contrarily to the previous applications of this model, the Compton reflection component has been taken into account. We use eight broadband X-rays spectra, including NuSTAR, NICER and Swift data, providing a total spectral coverage of 0.8-190 keV. The data were directly fitted with the JED-SAD model. Our results suggest that the optically thick disk (i.e. the SAD) does not extend down to the ISCO in any of the considered epochs. In particular, as the system evolves towards the hard/intermediate state, we find that the inner radius decreases from $\sim$60 R$_{\rm G}$ in the first observation down to $\sim$30 R$_{\rm G}$ in the last one. This trend is accompanied by an increase of the mass-accretion rate. In all hard-intermediate state observations, two reflection components, characterized by different values of ionization, are required to adequately explain the data. These components likely originate from different regions of the SAD. We show that a flared outer disk could, in principle, explain the double reflection component., Comment: 15 pages, 11 figures. Accepted for publication in A&A
Published: 2021
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36. The chameleon on the branches: spectral state transition and dips in NGC 247 ULX-1

Author: D'Aì, A., Pinto, C., Del Santo, M., Pintore, F., Soria, R., Robba, A., Ambrosi, E., Alston, W., Barret, D., Fabian, A. C., Fürst, F., Kara, E., Kosec, P., Middleton, M., Roberts, T., Rodriguez-Castillo, G., Walton, D. J., D'Aì, A., Pinto, C., Del Santo, M., Pintore, F., Soria, R., Robba, A., Ambrosi, E., Alston, W., Barret, D., Fabian, A. C., Fürst, F., Kara, E., Kosec, P., Middleton, M., Roberts, T., Rodriguez-Castillo, G., and Walton, D. J.
Abstract: Soft Ultra-Luminous X-ray (ULXs) sources are a subclass of the ULXs that can switch from a supersoft spectral state, where most of the luminosity is emitted below 1 keV, to a soft spectral state with significant emission above 1 keV. In a few systems, dips have been observed. The mechanism behind this state transition and the dips nature are still debated. To investigate these issues, we obtained a long XMM-Newton monitoring campaign of a member of this class, NGC 247 ULX-1. We computed the hardness-intensity diagram for the whole dataset and identified two different branches: the normal branch and the dipping branch, which we study with four and three hardness-intensity resolved spectra, respectively. All seven spectra are well described by two thermal components: a colder ($kT_{\rm bb}$ $\sim$ 0.1-0.2 keV) black-body, interpreted as emission from the photo-sphere of a radiatively-driven wind, and a hotter ($kT_{\rm disk}$ $\sim$ 0.6 keV) multicolour disk black-body, likely due to reprocessing of radiation emitted from the innermost regions. In addition, a complex pattern of emission and absorption lines has been taken into account based on previous high-resolution spectroscopic results. We studied the evolution of spectral parameters and the flux of the two thermal components along the two branches and discuss two scenarios possibly connecting the state transition and the dipping phenomenon. One is based on geometrical occultation of the emitting regions, the other invokes the onset of a propeller effect., Comment: 13 pages, accepted by MNRAS on 2021/08/16
Published: 2021
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37. The evolving radio jet from the neutron star X-ray binary 4U 1820$-$30

Author: Russell, T. D., Degenaar, N., Eijnden, J. van den, Del Santo, M., Segreto, A., Altamirano, D., Beri, A., Trigo, M. Diaz, Miller-Jones, J. C. A., Russell, T. D., Degenaar, N., Eijnden, J. van den, Del Santo, M., Segreto, A., Altamirano, D., Beri, A., Trigo, M. Diaz, and Miller-Jones, J. C. A.
Abstract: The persistently bright ultra-compact neutron star low-mass X-ray binary 4U 1820$-$30 displays a $\sim$170 d accretion cycle, evolving between phases of high and low X-ray modes, where the 3 -- 10 keV X-ray flux changes by a factor of up to $\approx 8$. The source is generally in a soft X-ray spectral state, but may transition to a harder state in the low X-ray mode. Here, we present new and archival radio observations of 4U 1820$-$30 during its high and low X-ray modes. For radio observations taken within a low mode, we observed a flat radio spectrum consistent with 4U 1820$-$30 launching a compact radio jet. However, during the high X-ray modes the compact jet was quenched and the radio spectrum was steep, consistent with optically-thin synchrotron emission. The jet emission appeared to transition at an X-ray luminosity of $L_{\rm X (3-10 keV)} \sim 3.5 \times 10^{37} (D/\rm{7.6 kpc})^{2}$ erg s$^{-1}$. We also find that the low-state radio spectrum appeared consistent regardless of X-ray hardness, implying a connection between jet quenching and mass accretion rate in 4U 1820$-$30, possibly related to the properties of the inner accretion disk or boundary layer., Comment: 6 pages, 2 Figures. Online supplementary information supplied in the appendix. Accepted for publication by MNRAS Letters
Published: 2021
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38. Measurement of the cosmic ray helium energy spectrum from 70 GeV to 80 TeV with the DAMPE space mission

Author: Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Santo, M., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, K., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, H., Wang, J. Z., Wang, L. G., Wang, S., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhu, Y., Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Santo, M., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, K., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, H., Wang, J. Z., Wang, L. G., Wang, S., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.
Abstract: The measurement of the energy spectrum of cosmic ray helium nuclei from 70 GeV to 80 TeV using 4.5 years of data recorded by the DArk Matter Particle Explorer (DAMPE) is reported in this work. A hardening of the spectrum is observed at an energy of about 1.3 TeV, similar to previous observations. In addition, a spectral softening at about 34 TeV is revealed for the first time with large statistics and well controlled systematic uncertainties, with an overall significance of $4.3\sigma$. The DAMPE spectral measurements of both cosmic protons and helium nuclei suggest a particle charge dependent softening energy, although with current uncertainties a dependence on the number of nucleons cannot be ruled out., Comment: 11 pages, 13 figures, published in Phys. Rev. Lett. Add one more digit for first three columns in Table S2
Published: 2021
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39. The INTEGRAL view on Black Hole X-ray Binaries

Author: Motta, S. E., Rodriguez, J., Jourdain, E., Del Santo, M., Belanger, G., Cangemi, F., Grinberg, V., Kajava, J. J. E., Kuulkers, E., Malzac, J., Pottschmidt, K., Roques, J. P., Sanchez-Fernandez, C., Wilms, J., Motta, S. E., Rodriguez, J., Jourdain, E., Del Santo, M., Belanger, G., Cangemi, F., Grinberg, V., Kajava, J. J. E., Kuulkers, E., Malzac, J., Pottschmidt, K., Roques, J. P., Sanchez-Fernandez, C., and Wilms, J.
Abstract: INTEGRAL is an ESA mission in fundamental astrophysics that was launched in October 2002. It has been in orbit for over 18 years, during which it has been observing the high-energy sky with a set of instruments specifically designed to probe the emission from hard X-ray and soft gamma-ray sources. This paper is devoted to the subject of black hole binaries, which are among the most important sources that populate the high-energy sky. We present a review of the scientific literature based on INTEGRAL data, which has significantly advanced our knowledge in the field of relativistic astrophysics. We briefly summarise the state-of-the-art of the study of black hole binaries, with a particular focus on the topics closer to the INTEGRAL science. We then give an overview of the results obtained by INTEGRAL and by other observatories on a number of sources of importance in the field. Finally, we review the main results obtained over the past 18 years on all the black hole binaries that INTEGRAL has observed. We conclude with a summary of the main contributions of INTEGRAL to the field, and on the future perspectives., Comment: 44 pages, 11 figures. Accepted for publication on New Astronomy Reviews
Published: 2021
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40. Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

Author: Alston, W. N., Pinto, C., Barret, D., D'Ai, A., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Kara, E., Kosec, P., Middleton, M. J., Parker, M. L., Pintore, F., Robba, A., Roberts, T. P., Sathyaprakash, R., Walton, D., Ambrosi, E., Alston, W. N., Pinto, C., Barret, D., D'Ai, A., Del Santo, M., Earnshaw, H., Fabian, A. C., Fuerst, F., Kara, E., Kosec, P., Middleton, M. J., Parker, M. L., Pintore, F., Robba, A., Roberts, T. P., Sathyaprakash, R., Walton, D., and Ambrosi, E.
Abstract: Most ultraluminous X-ray sources (ULXs) are believed to be stellar mass black holes or neutron stars accreting beyond the Eddington limit. Determining the nature of the compact object and the accretion mode from broadband spectroscopy is currently a challenge, but the observed timing properties provide insight into the compact object and details of the geometry and accretion processes. Here we report a timing analysis for an 800 ks XMM-Newton campaign on the supersoft ultraluminous X-ray source, NGC 247 ULX-1. Deep and frequent dips occur in the X-ray light curve, with the amplitude increasing with increasing energy band. Power spectra and coherence analysis reveals the dipping preferentially occurs on $\sim 5$ ks and $\sim 10$ ks timescales. The dips can be caused by either the occultation of the central X-ray source by an optically thick structure, such as warping of the accretion disc, or from obscuration by a wind launched from the accretion disc, or both. This behaviour supports the idea that supersoft ULXs are viewed close to edge-on to the accretion disc., Comment: Accepted MNRAS version following minor comments. 8 pages, 6 figures
Published: 2021
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41. XMM-Newton campaign on the ultraluminous X-ray source NGC 247 ULX-1: outflows

Author: Pinto, C., Soria, R., Walton, D., D'Ai, A., Pintore, F., Kosec, P., Alston, W. N., Fuerst, F., Middleton, M. J., Roberts, T. P., Del Santo, M., Barret, D., Ambrosi, E., Robba, A., Earnshaw, H., Fabian, A., Pinto, C., Soria, R., Walton, D., D'Ai, A., Pintore, F., Kosec, P., Alston, W. N., Fuerst, F., Middleton, M. J., Roberts, T. P., Del Santo, M., Barret, D., Ambrosi, E., Robba, A., Earnshaw, H., and Fabian, A.
Abstract: Most ULXs are believed to be powered by super-Eddington accreting neutron stars and, perhaps, black holes. Above the Eddington rate the disc is expected to thicken and to launch powerful winds through radiation pressure. Winds have been recently discovered in several ULXs. However, it is yet unclear whether the thickening of the disc or the wind variability causes the switch between the classical soft and supersoft states observed in some ULXs. In order to understand such phenomenology and the overall super-Eddington mechanism, we undertook a large (800 ks) observing campaign with XMM-Newton to study NGC 247 ULX-1, which shifts between a supersoft and classical soft ULX state. The new observations show unambiguous evidence of a wind in the form of emission and absorption lines from highly-ionised ionic species, with the latter indicating a mildly-relativistic outflow (-0.17c) in line with the detections in other ULXs. Strong dipping activity is observed in the lightcurve and primarily during the brightest observations, which is typical among soft ULXs, and indicates a close relationship between the accretion rate and the appearance of the dips. The latter is likely due to a thickening of the disc scale-height and the wind as shown by a progressively increasing blueshift in the spectral lines., Comment: 18 pages, 16 figures, accepted for publication in MNRAS
Published: 2021
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42. Time Domain Astronomy with the THESEUS Satellite

Author: Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Sandoval, L. Rivera, Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D'Aì, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, V., Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Sandoval, L. Rivera, Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D'Aì, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, V., Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., and Zhang, B.
Abstract: THESEUS is a medium size space mission of the European Space Agency, currently under evaluation for a possible launch in 2032. Its main objectives are to investigate the early Universe through the observation of gamma-ray bursts and to study the gravitational waves electromagnetic counterparts and neutrino events. On the other hand, its instruments, which include a wide field of view X-ray (0.3-5 keV) telescope based on lobster-eye focusing optics and a gamma-ray spectrometer with imaging capabilities in the 2-150 keV range, are also ideal for carrying out unprecedented studies in time domain astrophysics. In addition, the presence onboard of a 70 cm near infrared telescope will allow simultaneous multi-wavelegth studies. Here we present the THESEUS capabilities for studying the time variability of different classes of sources in parallel to, and without affecting, the gamma-ray bursts hunt., Comment: Submitted to Experimental Astronomy
Published: 2021
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43. Looking through the photoionisation wake: Vela X-1 at $\varphi_\mathrm{orb} \approx 0.75$ with Chandra/HETG

Author: Amato, R., Grinberg, V., Hell, N., Bianchi, S., Pinto, C., D'Aí, D., Del Santo, M., Mineo, T., Santangelo, A., Amato, R., Grinberg, V., Hell, N., Bianchi, S., Pinto, C., D'Aí, D., Del Santo, M., Mineo, T., and Santangelo, A.
Abstract: The Supergiant X-ray binary Vela X-1 represents one of the best astrophysical sources to investigate the wind environment of a O/B star irradiated by an accreting neutron star. Previous studies and hydrodynamic simulations of the system revealed a clumpy environment and the presence of two wakes: an accretion wake surrounding the compact object and a photoionisation wake trailing it along the orbit. Our goal is to conduct, for the first time, high-resolution spectroscopy on Chandra/HETG data at the orbital phase $\varphi_\mathrm{orb} \approx 0.75$, when the line of sight is crossing the photoionisation wake. We aim to conduct plasma diagnostics, inferring the structure and the geometry of the wind. We perform a blind search employing a Bayesian Block algorithm to find discrete spectral features and identify them thanks to the most recent laboratory results or through atomic databases. Plasma properties are inferred both with empirical techniques and with photoionisation models within CLOUDY and SPEX. We detect and identify five narrow radiative recombination continua (Mg XI-XII, Ne IX-X, O VIII) and several emission lines from Fe, S, Si, Mg, Ne, Al, and Na, including four He-like triplets (S XV, Si XIII, Mg XI, and Ne IX). Photoionisation models well reproduce the overall spectrum, except for the near-neutral fluorescence lines of Fe, S, and Si. We conclude that the plasma is mainly photoionised, but more than one component is most likely present, consistent with a multi-phase plasma scenario, where denser and colder clumps of matter are embedded in the hot, photoionised wind of the companion star. Simulations with the future X-ray satellites Athena and XRISM show that a few hundred seconds of exposure will be sufficient to disentangle the lines of the Fe K$\alpha$ doublet and the He-like Fe XXV, improving, in general, the determination of the plasma parameters., Comment: 13 pages, 14 figures. Accepted for publication on A&A
Published: 2021
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44. Observations of a radio-bright, X-ray obscured GRS 1915+105

Author: Motta, S. E., Kajava, J. J. E., Giustini, M., Williams, D. R. A., Del Santo, M., Fender, R., Green, D. A., Heywood, I., Rhodes, L., Segreto, A., Sivakoff, G., Woudt, P. A., Motta, S. E., Kajava, J. J. E., Giustini, M., Williams, D. R. A., Del Santo, M., Fender, R., Green, D. A., Heywood, I., Rhodes, L., Segreto, A., Sivakoff, G., and Woudt, P. A.
Abstract: The Galactic black hole transient GRS1915+105 is famous for its markedly variable X-ray and radio behaviour, and for being the archetypal galactic source of relativistic jets. It entered an X-ray outburst in 1992 and has been active ever since. Since 2018 GRS1915+105 has declined into an extended low-flux X-ray plateau, occasionally interrupted by multi-wavelength flares. Here we report the radio and X-ray properties of GRS1915+105 collected in this new phase, and compare the recent data to historic observations. We find that while the X-ray emission remained unprecedentedly low for most of the time following the decline in 2018, the radio emission shows a clear mode change half way through the extended X-ray plateau in 2019 June: from low flux (~3mJy) and limited variability, to marked flaring with fluxes two orders of magnitude larger. GRS1915+105 appears to have entered a low-luminosity canonical hard state, and then transitioned to an unusual accretion phase, characterised by heavy X-ray absorption/obscuration. Hence, we argue that a local absorber hides from the observer the accretion processes feeding the variable jet responsible for the radio flaring. The radio-X-ray correlation suggests that the current low X-ray flux state may be a signature of a super-Eddington state akin to the X-ray binaries SS433 or V404 Cyg., Comment: 10 pages, 5 figures. Accepted for publication on MNRAS
Published: 2021
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45. Time domain astronomy with the THESEUS satellite

Author: Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V. T., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Sandoval, L. Rivera, Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D'Ai, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, Daniel, Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P. G., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., Zhang, B., Mereghetti, S., Balman, S., Caballero-Garcia, M., Del Santo, M., Doroshenko, V. T., Erkut, M. H., Hanlon, L., Hoeflich, P., Markowitz, A., Osborne, J. P., Pian, E., Sandoval, L. Rivera, Webb, N., Amati, L., Ambrosi, E., Beardmore, A. P., Blain, A., Bozzo, E., Burderi, L., Campana, S., Casella, P., D'Ai, A., D'Ammando, F., De Colle, F., Della Valle, M., De Martino, D., Di Salvo, T., Doyle, M., Esposito, P., Frontera, F., Gandhi, P., Ghisellini, G., Gotz, D., Grinberg, Daniel, Guidorzi, C., Hudec, R., Iaria, R., Izzo, L., Jaisawal, G. K., Jonker, P. G., Kong, A. K. H., Krumpe, M., Kumar, P., Manousakis, A., Marino, A., Martin-Carrillo, A., Mignani, R., Miniutti, G., Mundell, C. G., Mukai, K., Nucita, A. A., O'Brien, P. T., Orlandini, M., Orio, M., Palazzi, E., Papitto, A., Pintore, F., Piranomonte, S., Porquet, D., Ricci, C., Riggio, A., Rigoselli, M., Rodriguez, J., Saha, T., Sanna, A., Santangelo, A., Saxton, R., Sidoli, L., Stiele, H., Tagliaferri, G., Tavecchio, F., Tiengo, A., Tsygankov, S., Turriziani, S., Wijnands, R., Zane, S., and Zhang, B.
Abstract: THESEUS is a medium size space mission of the European Space Agency, currently under evaluation for a possible launch in 2032. Its main objectives are to investigate the early Universe through the observation of gamma-ray bursts and to study the gravitational waves electromagnetic counterparts and neutrino events. On the other hand, its instruments, which include a wide field of view X-ray (0.3-5 keV) telescope based on lobster-eye focussing optics and a gamma-ray spectrometer with imaging capabilities in the 2-150 keV range, are also ideal for carrying out unprecedented studies in time domain astrophysics. In addition, the presence onboard of a 70 cm near infrared telescope will allow simultaneous multiwavelegth studies. Here we present the THESEUS capabilities for studying the time variability of different classes of sources in parallel to, and without affecting, the gamma-ray bursts hunt.
Published: 2021

46. Yield And Fruit Quality Of Tomato Grafted Onto Rootstocks Partially Resistant To Root-Knot Nematodes In A Naturally Infested Greenhouse

Author: Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, Costa, Sofia R., Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, and Costa, Sofia R.
Abstract: Root-knot-nematodes (RKN), Meloidogyne spp., are major soilborne diseases in protected tomato production and grafting with resistant or partially resistant rootstocks has been showing promising results. The experiment was carried out in a sandy soil greenhouse in the Littoral NW Portugal. Tomato cv. Anairis was grafted onto rootstocks Embajador, Emperador, Multifort and Silex, with non-grafted and self-grafted plants used as controls, in an experimental design of 6 treatments in three randomized blocks, to evaluate the effects on yield and fruit quality. Soil samples were collected at planting and at the end of the trial to estimate soil populations of RKN. At the end of the trial, plants were uprooted to evaluate the numbers of galls, egg masses and female fecundity. The potential benefits of increased yield by plant grafting have not been revealed. However, plants grafted onto any of the tested rootstocks suffered significantly less nematode damage, which are in agreement with previous findings in organic and transitional fields when soil RKN pressure was low. As tomato production in organic greenhouses can be affected by RKN due to relatively short rotations, grafting with appropriate rootstocks may play an effective role in RKN management when high populations of nematodes are present.
Published: 2021

47. Yield And Fruit Quality Of Tomato Grafted Onto Rootstocks Partially Resistant To Root-Knot Nematodes In A Naturally Infested Greenhouse

Author: Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, Costa, Sofia R., Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, and Costa, Sofia R.
Abstract: Root-knot-nematodes (RKN), Meloidogyne spp., are major soilborne diseases in protected tomato production and grafting with resistant or partially resistant rootstocks has been showing promising results. The experiment was carried out in a sandy soil greenhouse in the Littoral NW Portugal. Tomato cv. Anairis was grafted onto rootstocks Embajador, Emperador, Multifort and Silex, with non-grafted and self-grafted plants used as controls, in an experimental design of 6 treatments in three randomized blocks, to evaluate the effects on yield and fruit quality. Soil samples were collected at planting and at the end of the trial to estimate soil populations of RKN. At the end of the trial, plants were uprooted to evaluate the numbers of galls, egg masses and female fecundity. The potential benefits of increased yield by plant grafting have not been revealed. However, plants grafted onto any of the tested rootstocks suffered significantly less nematode damage, which are in agreement with previous findings in organic and transitional fields when soil RKN pressure was low. As tomato production in organic greenhouses can be affected by RKN due to relatively short rotations, grafting with appropriate rootstocks may play an effective role in RKN management when high populations of nematodes are present.
Published: 2021

48. Yield And Fruit Quality Of Tomato Grafted Onto Rootstocks Partially Resistant To Root-Knot Nematodes In A Naturally Infested Greenhouse

Author: Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, Costa, Sofia R., Mourão, Isabel, Gil Sá, Carlos, Moura, Luísa, Brito, L. Miguel, Vieira Santo, M. Clara, and Costa, Sofia R.
Abstract: Root-knot-nematodes (RKN), Meloidogyne spp., are major soilborne diseases in protected tomato production and grafting with resistant or partially resistant rootstocks has been showing promising results. The experiment was carried out in a sandy soil greenhouse in the Littoral NW Portugal. Tomato cv. Anairis was grafted onto rootstocks Embajador, Emperador, Multifort and Silex, with non-grafted and self-grafted plants used as controls, in an experimental design of 6 treatments in three randomized blocks, to evaluate the effects on yield and fruit quality. Soil samples were collected at planting and at the end of the trial to estimate soil populations of RKN. At the end of the trial, plants were uprooted to evaluate the numbers of galls, egg masses and female fecundity. The potential benefits of increased yield by plant grafting have not been revealed. However, plants grafted onto any of the tested rootstocks suffered significantly less nematode damage, which are in agreement with previous findings in organic and transitional fields when soil RKN pressure was low. As tomato production in organic greenhouses can be affected by RKN due to relatively short rotations, grafting with appropriate rootstocks may play an effective role in RKN management when high populations of nematodes are present.
Published: 2021

49. The Galactic LMXB Population and the Galactic Centre Region

Author: Sazonov, S., Paizis, A., Bazzano, A., Chelovekov, I., Khabibullin, I., Postnov, K., Mereminskiy, I., Fiocchi, M., Bélanger, G., Bird, A. J., Bozzo, E., Chenevez, J., Del Santo, M., Falanga, M., Farinelli, R., Ferrigno, C., Grebenev, S., Krivonos, R., Kuulkers, E., Lund, N., Sanchez-Fernandez, C., Tarana, A., Ubertini, P., Wilms, J., Sazonov, S., Paizis, A., Bazzano, A., Chelovekov, I., Khabibullin, I., Postnov, K., Mereminskiy, I., Fiocchi, M., Bélanger, G., Bird, A. J., Bozzo, E., Chenevez, J., Del Santo, M., Falanga, M., Farinelli, R., Ferrigno, C., Grebenev, S., Krivonos, R., Kuulkers, E., Lund, N., Sanchez-Fernandez, C., Tarana, A., Ubertini, P., and Wilms, J.
Abstract: Seventeen years of hard X-ray observations with the instruments of the INTEGRAL observatory, with a focus on the Milky Way and in particular on the Galactic Centre region, have provided a unique database for exploration of the Galactic population of low-mass X-ray binaries (LMXBs). Our understanding of the diverse energetic phenomena associated with accretion of matter onto neutron stars and black holes has greatly improved. We review the large variety of INTEGRAL based results related to LMXBs. In particular, we discuss the spatial distribution of LMXBs over the Galaxy and their X-ray luminosity function as well as various physical phenomena associated with Atoll and Z sources, bursters, symbiotic X-ray binaries, ultracompact X-ray binaries and persistent black hole LMXBs. We also present an up-to-date catalogue of confirmed LMXBs detected by INTEGRAL, which comprises 166 objects. Last but not least, the long-term monitoring of the Galactic Centre with INTEGRAL has shed light on the activity of Sgr A* in the recent past, confirming previous indications that our supermassive black hole experienced a major accretion episode just ~100 years ago. This exciting topic is covered in this review too., Comment: 60 pages, 26 figures, 2 tables, accepted for publication in New Astronomy Reviews
Published: 2020
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50. On the nature of the soft gamma-ray emission in the hard state of the black hole transient GRS 1716-249

Author: Bassi, T., Malzac, J., Del Santo, M., Jourdain, E., Roques, J. -P., D'Aì, A., Miller-Jones, J. C. A., Belmont, R., Motta, S. E., Segreto, A., Testa, V., Casella, P., Bassi, T., Malzac, J., Del Santo, M., Jourdain, E., Roques, J. -P., D'Aì, A., Miller-Jones, J. C. A., Belmont, R., Motta, S. E., Segreto, A., Testa, V., and Casella, P.
Abstract: The black hole transient GRS 1716-249 was monitored from the radio to the gamma-ray band during its 2016-2017 outburst. This paper focuses on the Spectral Energy Distribution (SED) obtained in 2017 February-March, when GRS 1716-249 was in a bright hard spectral state. The soft gamma-ray data collected with the INTEGRAL/SPI telescope show the presence of a spectral component which is in excess of the thermal Comptonisation emission. This component is usually interpreted as inverse Compton emission from a tiny fraction of non-thermal electrons in the X-ray corona. We find that hybrid thermal/non-thermal Comptonisation models provide a good fit to the X/gamma-ray spectrum of GRS 1716-249. The best-fit parameters are typical of the bright hard state spectra observed in other black hole X-ray binaries. Moreover, the magnetised hybrid Comptonisation model BELM provides an upper limit on the intensity of the coronal magnetic field of about 1E+06 G. Alternatively, this soft gamma-ray emission could originate from synchrotron emission in the radio jet. In order to test this hypothesis, we fit the SED with the irradiated disc plus Comptonisation model combined with the jet internal shock emission model ISHEM. We found that a jet with an electron distribution of p~2.1 can reproduce the soft gamma-ray emission of GRS 1716-249. However, if we introduce the expected cooling break around 10 keV, the jet model can no longer explain the observed soft gamma-ray emission, unless the index of the electron energy distribution is significantly harder (p<2)., Comment: 14 pages, 8 figures. Accepted for publication in MNRAS
Published: 2020
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