Cosmology and Nongalactic Astrophysics (astro-ph.CO)

Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array

2024-11-09T01:08:51Z

Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array Abe, K.; Abe, S.; Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Alfaro, R.; Alvarez-Crespo, N.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Angüner, E. O.; Antonelli, L. A.; Aramo, C.; Araya, M.; Arcaro, C.; Arrabito, L.; Asano, K.; Ascasíbar, Y.; Aschersleben, J.; Ashkar, H.; Augusto Stuani, L.; Baack, D.; Backes, M.; Baktash, A.; Balazs, C.; Balbo, M.; Ballester, O.; Baquero Larriva, A.; Barbosa Martins, V.; Barres de Almeida, U.; Barrio, J. A.; Batista, P. I.; Batkovic, I.; Batzofin, R.; Baxter, J.; Becerra González, J.; Beck, G.; Becker Tjus, J.; Benbow, W.; Bernete Medrano, J.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Bhattacharjee, P.; Bhattacharyya, S.; Bi, B.; Biederbeck, N.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Boisson, C.; Bolmont, J.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Bradascio, F.; Braiding, C.; Bronzini, E.; Brose, R.; Brown, A. M.; Brun, F.; Brunetti, G.; Bucciantini, N.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Burton, M.; Bylund, T.; Calisse, P. G.; Campoy-Ordaz, A.; Cantlay, B. K.; Capalbi, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Caroff, S.; Carosi, R.; Carquin, E.; Carrasco, M. -S.; Cascone, E.; Cassol, F.; Castro-Tirado, A. J.; Cerasole, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A. W.; Chernyakova, M.; Chiavassa, A.; Chudoba, J.; Chytka, L.; Cifuentes, A.; Coimbra Araujo, C. H.; Conforti, V.; Conte, F.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Cristofari, P.; Cuevas, O.; Curtis-Ginsberg, Z.; D'Amico, G.; D'Ammando, F.; Dalchenko, M.; Dazzi, F.; de Bony de Lavergne, M.; De Caprio, V.; De Frondat Laadim, F.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Lucia, M.; De Martino, D.; de Menezes, R.; de Naurois, M.; De Simone, N.; de Souza, V.; del Valle, M. V.; Delagnes, E.; Delgado Giler, A. G.; Delgado, C.; Dell'aiera, M.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Diebold, S.; Djannati-Ataï, A.; Djuvsland, J.; Dominik, R. M.; Donini, A.; Dorner, D.; Dörner, J.; Doro, M.; dos Anjos, R. D. C.; Dournaux, J. -L.; Duangchan, C.; Dubos, C.; Dumora, D.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Elsässer, D.; Emery, G.; Escobar Godoy, M.; Escudero, J.; Esposito, P.; Ettori, S.; Evoli, C.; Falceta-Goncalves, D.; Fallah Ramazani, V.; Fattorini, A.; Faure, A.; Fedorova, E.; Fegan, S.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrarotto, F.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Foffano, L.; Font Guiteras, L.; Fontaine, G.; Fröse, S.; Fukazawa, Y.; Fukui, Y.; Gaggero, D.; Galanti, G.; Gallozzi, S.; Gammaldi, V.; Garczarczyk, M.; Gasbarra, C.; Gasparrini, D.; Gaug, M.; Ghalumyan, A.; Gianotti, F.; Giarrusso, M.; Giesbrecht, J.; Giglietto, N.; Giordano, F.; Glicenstein, J. -F.; Göksu, H.; Goldoni, P.; González, J. M.; González, M. M.; Goulart Coelho, J.; Granot, J.; Grau, R.; Gréaux, L.; Green, D.; Green, J. G.; Grenier, I.; Grolleron, G.; Grube, J.; Gueta, O.; Hackfeld, J.; Hadasch, D.; Hamal, P.; Hanlon, W.; Hara, S.; Harvey, V. M.; Hassan, T.; Heckmann, L.; Heller, M.; Hernández Cadena, S.; Hervet, O.; Hie, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hoang, J.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horvath, P.; Hrupec, D.; Hütten, M.; Iarlori, M.; Inada, T.; Incardona, F.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jarnot, C.; Jean, P.; Jiménez Martínez, I.; Jin, W.; Juramy-Gilles, C.; Jurysek, J.; Kagaya, M.; Kantzas, D.; Karas, V.; Katagiri, H.; Kataoka, J.; Kaufmann, S.; Kerszberg, D.; Khélifi, B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluźniak, W.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kosack, K.; Kowal, G.; Kubo, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; Láinez, M.; Lamastra, A.; Lapington, J.; Laporte, P.; Lazarević, S.; Leitgeb, F.; Lemoine-Goumard, M.; Lenain, J. -P.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Linhoff, M.; Liodakis, I.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Luque-Escamilla, P. L.; Macias, O.; Mackey, J.; Majumdar, P.; Malyshev, D.; Mandat, D.; Manganaro, M.; Manicò, G.; Mariotti, M.; Markoff, S.; Márquez, I.; Marquez, P.; Marsella, G.; Martínez, G. A.; Martínez, M.; Martinez, O.; Marty, C.; Mas-Aguilar, A.; Mastropietro, M.; Maurin, G.; Mazin, D.; Melkumyan, D.; Mello, A. J. T. S.; Meunier, J. -L.; Meyer, D. M. -A.; Meyer, M.; Miceli, D.; Michailidis, M.; Michałowski, J.; Miener, T.; Miranda, J. M.; Mitchell, A.; Mizote, M.; Mizuno, T.; Moderski, R.; Molero, M.; Molfese, C.; Molina, E.; Montaruli, T.; Morcuende, D.; Morik, K.; Morlino, G.; Morselli, A.; Moulin, E.; Moya Zamanillo, V.; Munari, K.; Murach, T.; Muraczewski, A.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Nemmen, R.; Neyroud, N.; Nickel, L.; Niemiec, J.; Nieto, D.; Nievas Rosillo, M.; Nikołajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Novotny, V.; Nozaki, S.; O'Brien, P.; Ohishi, M.; Ohtani, Y.; Okumura, A.; Olive, J. -F.; Olmi, B.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Ostrowski, M.; Oya, I.; Pagliaro, A.; Palatiello, M.; Panebianco, G.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Parmiggiani, N.; Patel, S. R.; Patricelli, B.; Pavlović, D.; Pech, M.; Pecimotika, M.; Pensec, U.; Peresano, M.; Pérez-Romero, J.; Peron, G.; Persic, M.; Petrucci, P. -O.; Petruk, O.; Piano, G.; Pierre, E.; Pietropaolo, E.; Pintore, F.; Pirola, G.; Pita, S.; Plard, C.; Podobnik, F.; Pohl, M.; Polo, M.; Pons, E.; Ponti, G.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Produit, N.; Pueschel, E.; Pühlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Rando, R.; Razzaque, S.; Recchia, S.; Regeard, M.; Reichherzer, P.; Reimer, A.; Reimer, O.; Reisenegger, A.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Righi, C.; Riitano, L.; Rizi, V.; Roache, E.; Rodriguez Fernandez, G.; Rodríguez-Vázquez, J. J.; Romano, P.; Romeo, G.; Rosado, J.; Rosales de Leon, A.; Rowell, G.; Rudak, B.; Rulten, C. B.; Russo, F.; Sadeh, I.; Saha, L.; Saito, T.; Salzmann, H.; Sanchez, D.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santangelo, A.; Santos-Lima, R.; Sanuy, A.; Šarić, T.; Sarkar, A.; Sarkar, S.; Satalecka, K.; Saturni, F. G.; Savchenko, V.; Scherer, A.; Schipani, P.; Schleicher, B.; Schubert, J. L.; Schussler, F.; Schwanke, U.; Schwefer, G.; Seglar Arroyo, M.; Seiji, S.; Semikoz, D.; Sergijenko, O.; Servillat, M.; Sguera, V.; Shang, R. Y.; Sharma, P.; Siejkowski, H.; Sinha, A.; Siqueira, C.; Sliusar, V.; Slowikowska, A.; Sol, H.; Specovius, A.; Spencer, S. T.; Spiga, D.; Stamerra, A.; Stanič, S.; Starecki, T.; Starling, R.; Stawarz, Ł.; Steppa, C.; Stolarczyk, T.; Strišković, J.; Suda, Y.; Suomijärvi, T.; Tajima, H.; Tak, D.; Takahashi, M.; Takeishi, R.; Tanaka, S. J.; Tavernier, T.; Tejedor, L. A.; Terauchi, K.; Terrier, R.; Teshima, M.; Tian, W. W.; Tibaldo, L.; Tibolla, O.; Torradeflot, F.; Torres, D. F.; Torresi, E.; Tosti, G.; Tosti, L.; Tothill, N.; Toussenel, F.; Touzard, V.; Tramacere, A.; Travnicek, P.; Tripodo, G.; Truzzi, S.; Tsiahina, A.; Tutone, A.; Vacula, M.; Vallage, B.; Vallania, P.; van Eldik, C.; van Scherpenberg, J.; Vandenbroucke, J.; Vassiliev, V.; Vázquez Acosta, M.; Vecchi, M.; Ventura, S.; Vercellone, S.; Verna, G.; Viana, A.; Viaux, N.; Vigliano, A.; Vigorito, C. F.; Vitale, V.; Vodeb, V.; Voisin, V.; Vorobiov, S.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Wagner, S. J.; Walter, R.; Wechakama, M.; White, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wohlleben, F.; Wolter, A.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A. A.; Zech, A.; Zhdanov, V. I.; Živec, M.; Zuriaga-Puig, J.; De la Torre Luque, P.; The CTA consortium; CTA consortium Galaxy clusters are expected to be both dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at γ-ray energies and are predicted to be sources of large-scale γ-ray emission due to hadronic interactions in the intracluster medium (ICM). In this paper, we estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse γ-ray emission from the Perseus galaxy cluster. We first perform a detailed spatial and spectral modelling of the expected signal for both the DM and the CRp components. For each case, we compute the expected CTA sensitivity accounting for the CTA instrument response functions. The CTA observing strategy of the Perseus cluster is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio X ₅₀₀ within the characteristic radius R ₅₀₀ down to about X ₅₀₀ < 3 × 10^-3, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index α_CRp = 2.3. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure α_CRp down to about Δα_CRp ≃ 0.1 and the CRp spatial distribution with 10% precision, respectively. Regarding DM, CTA should improve the current ground-based γ-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to ∼ 5, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with τ _χ > 10²⁷ s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario.

The maximum black hole mass at solar metallicity

2024-10-03T01:07:36Z

The maximum black hole mass at solar metallicity Vink, Jorick S.; Sabhahit, Gautham N.; Higgins, Erin R. We analyse the current knowledge and uncertainties in detailed stellar evolution and wind modelling to evaluate the mass of the most massive stellar black hole (BH) at solar metallicity. Contrary to common expectations that it is the most massive stars that produce the most massive BHs, we find that the maximum M_BH^Max ≃ 30 ± 10 M_⊙ is found in the canonical intermediate range between M_ZAMS ≃ 30 and 50 M_⊙ instead. The prime reason for this seemingly counter-intuitive finding is that very massive stars (VMS) have increasingly high mass-loss rates that lead to substantial mass evaporation before they expire as stars and end as lighter BHs than their canonical O-star counterparts.

X-Shooting ULLYSES: Massive Stars at Low Metallicity

2024-05-09T01:09:00Z

X-Shooting ULLYSES: Massive Stars at Low Metallicity Vink, J. S.; Crowther, P.; Fullerton, A.; Garcia, M.; Martins, F.; Morrell, N.; Oskinova, L.; St Louis, N.; ud-Doula, A.; Sander, A.; Sana, H.; Bouret, J. -C.; Kubatova, B.; Marchant, P.; Martins, L. P.; Wofford, A.; van Loon, J.; Telford, O. G.; Götberg, Y.; Bowman, D.; Erba, C.; Kalari, V.; XShootU Collaboration The Hubble Space Telescope has devoted 500 orbits to observing 250 massive stars with low metallicity in the ultraviolet (UV) range within the framework of the ULLYSES program. The X-Shooting ULLYSES (XShootU) project enhances the legacy value of this UV dataset by providing high-quality optical and near-infrared spectra, which are acquired using the wide-wavelength- coverage X-shooter spectrograph at ESO's Very Large Telescope. XShootU emphasises the importance of combining UV with optical spectra for the consistent determination of key stellar parameters such as effective temperature, surface gravity, luminosity, abundances, and wind characteristics including mass-loss rates as a function of metallicity. Since uncertainties in these parameters have implications across various branches of astrophysics, the data and modelling generated by the XShootU project are poised to significantly advance our understanding of massive stars at low metallicity. This is particularly crucial for confidently interpreting James Webb Space Telescope (JWST) data of the earliest stellar generations, making XShootU a unique resource for comprehending individual spectra of low-metallicity stars.

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

2024-05-09T01:08:06Z

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation Jin, Shoko; Trager, Scott C.; Dalton, Gavin B.; Aguerri, J. Alfonso L.; Drew, J. E.; Falcón-Barroso, Jesús; Gänsicke, Boris T.; Hill, Vanessa; Iovino, Angela; Pieri, Matthew M.; Poggianti, Bianca M.; Smith, D. J. B.; Vallenari, Antonella; Abrams, Don Carlos; Aguado, David S.; Antoja, Teresa; Aragón-Salamanca, Alfonso; Ascasibar, Yago; Babusiaux, Carine; Balcells, Marc; Barrena, R.; Battaglia, Giuseppina; Belokurov, Vasily; Bensby, Thomas; Bonifacio, Piercarlo; Bragaglia, Angela; Carrasco, Esperanza; Carrera, Ricardo; Cornwell, Daniel J.; Domínguez-Palmero, Lilian; Duncan, Kenneth J.; Famaey, Benoit; Fariña, Cecilia; Gonzalez, Oscar A.; Guest, Steve; Hatch, Nina A.; Hess, Kelley M.; Hoskin, Matthew J.; Irwin, Mike; Knapen, Johan H.; Koposov, Sergey E.; Kuchner, Ulrike; Laigle, Clotilde; Lewis, Jim; Longhetti, Marcella; Lucatello, Sara; Méndez-Abreu, Jairo; Mercurio, Amata; Molaeinezhad, Alireza; Monguió, Maria; Morrison, Sean; Murphy, David N. A.; Peralta de Arriba, Luis; Pérez, Isabel; Pérez-Ràfols, Ignasi; Picó, Sergio; Raddi, Roberto; Romero-Gómez, Mercè; Royer, Frédéric; Siebert, Arnaud; Seabroke, George M.; Som, Debopam; Terrett, David; Thomas, Guillaume; Wesson, Roger; Worley, C. Clare; Alfaro, Emilio J.; Allende Prieto, Carlos; Alonso-Santiago, Javier; Amos, Nicholas J.; Ashley, Richard P.; Balaguer-Núñez, Lola; Balbinot, Eduardo; Bellazzini, Michele; Benn, Chris R.; Berlanas, Sara R.; Bernard, Edouard J.; Best, Philip; Bettoni, Daniela; Bianco, Andrea; Bishop, Georgia; Blomqvist, Michael; Boeche, Corrado; Bolzonella, Micol; Bonoli, Silvia; Bosma, Albert; Britavskiy, Nikolay; Busarello, Gianni; Caffau, Elisabetta; Cantat-Gaudin, Tristan; Castro-Ginard, Alfred; Couto, Guilherme; Carbajo-Hijarrubia, Juan; Carter, David; Casamiquela, Laia; Conrado, Ana M.; Corcho-Caballero, Pablo; Costantin, Luca; Deason, Alis; de Burgos, Abel; De Grandi, Sabrina; Di Matteo, Paola; Domínguez-Gómez, Jesús; Dorda, Ricardo; Drake, Alyssa; Dutta, Rajeshwari; Erkal, Denis; Feltzing, Sofia; Ferré-Mateu, Anna; Feuillet, Diane; Figueras, Francesca; Fossati, Matteo; Franciosini, Elena; Frasca, Antonio; Fumagalli, Michele; Gallazzi, Anna; García-Benito, Rubén; Gentile Fusillo, Nicola; Gebran, Marwan; Gilbert, James; Gledhill, T. M.; González Delgado, Rosa M.; Greimel, Robert; Guarcello, Mario Giuseppe; Guerra, Jose; Gullieuszik, Marco; Haines, Christopher P.; Hardcastle, Martin J.; Harris, Amy; Haywood, Misha; Helmi, Amina; Hernandez, Nauzet; Herrero, Artemio; Hughes, Sarah; Iršič, Vid; Jablonka, Pascale; Jarvis, Matt J.; Jordi, Carme; Kondapally, Rohit; Kordopatis, Georges; Krogager, Jens-Kristian; La Barbera, Francesco; Lam, Man I.; Larsen, Søren S.; Lemasle, Bertrand; Lewis, Ian J.; Lhomé, Emilie; Lind, Karin; Lodi, Marcello; Longobardi, Alessia; Lonoce, Ilaria; Magrini, Laura; Maíz Apellániz, Jesús; Marchal, Olivier; Marco, Amparo; Martin, Nicolas F.; Matsuno, Tadafumi; Maurogordato, Sophie; Merluzzi, Paola; Miralda-Escudé, Jordi; Molinari, Emilio; Monari, Giacomo; Morelli, Lorenzo; Mottram, Christopher J.; Naylor, Tim; Negueruela, Ignacio; Oñorbe, Jose; Pancino, Elena; Peirani, Sébastien; Peletier, Reynier F.; Pozzetti, Lucia; Rainer, Monica; Ramos, Pau; Read, Shaun C.; Rossi, Elena Maria; Röttgering, Huub J. A.; Rubiño-Martín, Jose Alberto; Sabater, Jose; San Juan, José; Sanna, Nicoletta; Schallig, Ellen; Schiavon, Ricardo P.; Schultheis, Mathias; Serra, Paolo; Shimwell, Timothy W.; Simón-Díaz, Sergio; Smith, Russell J.; Sordo, Rosanna; Sorini, Daniele; Soubiran, Caroline; Starkenburg, Else; Steele, Iain A.; Stott, John; Stuik, Remko; Tolstoy, Eline; Tortora, Crescenzo; Tsantaki, Maria; Van der Swaelmen, Mathieu; van Weeren, Reinout J.; Vergani, Daniela; Verheijen, Marc A. W.; Verro, Kristiina; Vink, Jorick S.; Vioque, Miguel; Walcher, C. Jakob; Walton, Nicholas A.; Wegg, Christopher; Weijmans, Anne-Marie; Williams, Wendy L.; Wilson, Andrew J.; Wright, Nicholas J.; Xylakis-Dornbusch, Theodora; Youakim, Kris; Zibetti, Stefano; Zurita, Cristina WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959 nm at R ~ 5000, or two shorter ranges at $R\sim 20\, 000$. After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for ~3 million stars and detailed abundances for ~1.5 million brighter field and open-cluster stars; (ii) survey ~0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ~400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in ${\sim} 25\, 000$ field galaxies at 0.3 ≲ z ≲ 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.