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1. Astrophysics with the Laser Interferometer Space Antenna

Author

Seoane, Pau Amaro, Andrews, Jeff, Sedda, Manuel Arca, Askar, Abbas, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stephane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ross, Colpi, Monica, D'Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriakos, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tassos, Fryer, Chris, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Tomas, Kokkotas, Kostas, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thomas, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Tomas, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Steéphane, Mayer, Lucio, McGee, Sean, McKernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S, Nelemans, Gijs, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlos, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Tomas, Tauris, Thomas, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonios, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Rivera, Alexander Bonilla, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Fragione, Giacomo, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O'Shaughnessy, Richard, Zwart, Simon Portegies, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Amaro-Seoane, Pau, Andrews, Jeff, Arca Sedda, Manuel, Askar, Abba, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stéphane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ro, Colpi, Monica, D’Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriako, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tasso, Fryer, Chri, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Toma, Kokkotas, Kosta, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thoma, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Toma, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Stéphane, Mayer, Lucio, Mcgee, Sean, Mckernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S., Nelemans, Gij, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlo, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Toma, Tauris, Thoma, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonio, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Bonilla Rivera, Alexander, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O’Shaughnessy, Richard, Portegies Zwart, Simon, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Columbia University, Columbia University [New York], Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Fisk University, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Ministerio de Ciencia e Innovación (España), European Research Council, European Commission, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, and National Aeronautics and Space Administration (US)

Subjects
Astrofísica, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Black hole, Astronomy, Stellar remnant, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), TIDAL DISRUPTION EVENTS, General Relativity and Quantum Cosmology, Gravitational waves, MOCCA-SURVEY DATABASE, Settore FIS/05 - Astronomia e Astrofisica, Stellar remnants, Software Science, Multi-messenger, GRAVITATIONAL-WAVE SOURCES, Instrumentation and Methods for Astrophysics (astro-ph.IM), Extreme mass ratio in-spirals, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Black holes, Data Science, Astrophysics::Instrumentation and Methods for Astrophysics, Extreme mass ratio in-spiral, AM-CVN STARS, Astrophysics - Astrophysics of Galaxies, WHITE-DWARF BINARIES, DOUBLE NEUTRON-STARS, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astronomia, MASSIVE BLACK-HOLE, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, X-RAY BINARIES, COMMON-ENVELOPE EVOLUTION, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Full list of authors: Amaro-Seoane, Pau; Andrews, Jeff; Sedda, Manuel Arca; Askar, Abbas.; Baghi, Quentin; Balasov, Razvan; Bartos, Imre; Bavera, Simone S.; Bellovary, Jillian; Berry, Christopher P. L.; Berti, Emanuele; Bianchi, Stefano; Blecha, Laura; Blondin, Stephane; Bogdanovic, Tamara; Boissier, Samuel; Bonetti, Matteo; Bonoli, Silvia; Bortolas, Elisa; Breivik, Katelyn; Capelo, Pedro R.; Caramete, Laurentiu; Cattorini, Federico; Charisi, Maria; Chaty, Sylvain; Chen, Xian; Chruslinska, Martyna; Chua, Alvin J. K.; Church, Ross; Colpi, Monica; D'Orazio, Daniel; Danielski, Camilla; Davies, Melvyn B.; Dayal, Pratika; De Rosa, Alessandra; Derdzinski, Andrea; Destounis, Kyriakos; Dotti, Massimo; Dutan, Ioana; Dvorkin, Irina; Fabj, Gaia; Foglizzo, Thierry; Ford, Saavik; Fouvry, Jean-Baptiste; Franchini, Alessia; Fragos, Tassos; Fryer, Chris; Gaspari, Massimo; Gerosa, Davide; Graziani, Luca; Groot, Paul; Habouzit, Melanie; Haggard, Daryl; Haiman, Zoltan; Han, Wen-Biao; Istrate, Alina; Johansson, Peter H.; Khan, Fazeel Mahmood; Kimpson, Tomas; Kokkotas, Kostas; Kong, Albert; Korol, Valeriya; Kremer, Kyle; Kupfer, Thomas; Lamberts, Astrid; Larson, Shane; Lau, Mike; Liu, Dongliang; Lloyd-Ronning, Nicole; Lodato, Giuseppe; Lupi, Alessandro; Ma, Chung-Pei; Maccarone, Tomas; Mandel, Ilya; Mangiagli, Alberto; Mapelli, Michela; Mathis, Stephane; Mayer, Lucio; McGee, Sean; McKernan, Berry; Miller, M. Coleman; Mota, David F.; Mumpower, Matthew; Nasim, Syeda S.; Nelemans, Gijs; Noble, Scott; Pacucci, Fabio; Panessa, Francesca; Paschalidis, Vasileios; Pfister, Hugo; Porquet, Delphine; Quenby, John; Ricarte, Angelo; Roepke, Friedrich K.; Regan, John; Rosswog, Stephan; Ruiter, Ashley; Ruiz, Milton; Runnoe, Jessie; Schneider, Raffaella; Schnittman, Jeremy; Secunda, Amy; Sesana, Alberto; Seto, Naoki; Shao, Lijing; Shapiro, Stuart; Sopuerta, Carlos; Stone, Nicholas C.; Suvorov, Arthur; Tamanini, Nicola; Tamfal, Tomas; Tauris, Thomas; Temmink, Karel; Tomsick, John; Toonen, Silvia; Torres-Orjuela, Alejandro; Toscani, Martina; Tsokaros, Antonios; Unal, Caner; Vazquez-Aceves, Veronica; Valiante, Rosa; van Putten, Maurice; van Roestel, Jan; Vignali, Christian; Volonteri, Marta; Wu, Kinwah; Younsi, Ziri; Yu, Shenghua; Zane, Silvia; Zwick, Lorenz; Antonini, Fabio; Baibhav, Vishal; Barausse, Enrico; Bonilla Rivera, Alexander; Branchesi, Marica; Branduardi-Raymont, Graziella; Burdge, Kevin; Chakraborty, Srija; Cuadra, Jorge; Dage, Kristen; Davis, Benjamin; de Mink, Selma E.; Decarli, Roberto; Doneva, Daniela; Escoffier, Stephanie; Gandhi, Poshak; Haardt, Francesco; Lousto, Carlos O.; Nissanke, Samaya; Nordhaus, Jason; O'Shaughnessy, Richard; Portegies Zwart, Simon; Pound, Adam; Schussler, Fabian; Sergijenko, Olga; Spallicci, Alessandro; Vernieri, Daniele; Vigna-Gomez, Alejandro.-- This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/., The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe. © The Author(s) 2023, corrected publication 2023., P. Dayal acknowledges support from the European Research council (ERC-717001) and from the Netherlands Research Council NWO (016.VIDI.189.162). P.H. Johansson acknowledges the support from the European Research Council (ERC-818930). S. Toonen acknowledges support from the Netherlands Research Council NWO (VENI 639.041.645 Grants) C. Unal is supported by European Structural and Investment Funds and the Czech Ministry of Education, Youth and Sports (Project CoGraDS - CZ.02.1.01/0.0/0.0/15_003/0000437). S. Chaty acknowledges the LabEx UnivEarthS for the funding of Interface project I10 “From binary evolution towards merging of compact objects”. A. De Rosa acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.O E. Berti is supported by NSF Grants No. PHY-1912550 and AST-2006538, NASA ATP Grants No. 17-ATP17-0225 and 19-ATP19-0051, NSF-XSEDE Grant No. PHY-090003, and NSF Grant PHY-20043. D. Gerosa is supported by European Union’s H2020 ERC Starting Grant No. 945155–GWmining, Leverhulme Trust Grant No. RPG-2019-350 and Royal Society Grant No. RGS-R2-202004. T. Bogdanovic acknowledges support by the NASA award No. 80NSSC19K0319 and by the NSF award AST-1908042. D. Porquet acknowledges funding support from CNES. C. Danielski acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) B.L. Davis acknowledges support from Tamkeen under the NYU Abu Dhabi Research Institute Grant CAP3. F. Pacucci acknowledges support from a Clay Fellowship by the SAO and from the Black Hole Initiative, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation. A.J. Ruiter acknowledges support from the Australian Research Council Future Fellowship Grant FT170100243. V. Paschalidis is supported by NSF Grant PHY-1912619 and NASA Grant 80NSSC20K1542 to the University of Arizona, and NSF-XSEDE Grant TG-PHY190020. D. Haggard acknowledges support from the NSERC Discovery Grant and Canada Research Chairs programs, and the Bob Wares Science Innovation Prospectors Fund. M. Toscani acknowledges European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant Agreement No. 823823 (RISE DUSTBUSTERS project) and COST Action CA16104 - Gravitational waves, black holes and fundamental physics, supported by COST (European Cooperation in Science and Technology). M. Chruslinska, A. Istrate and G. Nelemans acknowledge support from Netherlands Research Council NWO. T. Fragos and S. Bavera acknowledge support from a Swiss National Science Foundation Professorship Grant (project numbers PP00P2_176868 and PP00P2_211006)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

Published
2023

2. Euclid preparation - XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields

Author

Euclid Collaboration, Moneti, A., McCracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Chary, R., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Cuby, J., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., ANDREON, Stefano, BARDELLI, Sandro, Faisst, A. L., Camera, S., Graciá-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Sureau, F., Tenti, M., Vassallo, T., ZACCHEI, Andrea, Masters, D. C., ZUCCA, Elena, Baccigalupi, C., Balaguera-Antolínez, A., Bernardeau, F., BIVIANO, ANDREA, BOLZONELLA, MICOL, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CAPPI, Alberto, McPartland, C., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., FARINA, Maria, FINELLI, FABIO, Flose-Reimberg, P., Mobasher, B., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Sanders, D. B., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, SCARAMELLA, Roberto, Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Stern, D., Scottez, V., SEFUSATTI, Emiliano, Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Hildebrandt, H., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., AURICCHIO, NATALIA, Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillis, B., GIOCOLI, Carlo, Granett, B. R., GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Moscardini, L., Munari, Emiliano, Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Moneti, A., Mccracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Chary, R., Cuby, J., Faisst, A. L., Masters, D. C., Mcpartland, C., Mobasher, B., Sanders, D. B., Scaramella, R., Stern, D., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Granett, B. R., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., K??mmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Cresp??, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Camera, S., Graci??-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Sureau, F., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antol??nez, A., Bernardeau, F., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., Farina, M., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., S??nchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., Viel, M., Hildebrandt, H., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, UAM. Departamento de Física Teórica, Moneti A., Mccracken H.J., Shuntov M., Kauffmann O.B., Capak P., Davidzon I., Ilbert O., Scarlata C., Toft S., Weaver J., Chary R., Cuby J., Faisst A.L., Masters D.C., Mcpartland C., Mobasher B., Sanders D.B., Scaramella R., Stern D., Szapudi I., Teplitz H., Zalesky L., Amara A., Auricchio N., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Capobianco V., Carbone C., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Fosalba P., Frailis M., Franceschi E., Fumana M., Garilli B., Gillis B., Giocoli C., Granett B.R., Grazian A., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Rix H., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Andreon S., Bardelli S., Camera S., Gracia-Carpio J., Medinaceli E., Mei S., Polenta G., Romelli E., Sureau F., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Bernardeau F., Biviano A., Bolzonella M., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Di Ferdinando D., Farina M., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I., Joachimi B., Kansal V., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., Maturi M., Metcalf R.B., Morgante G., Morisset N., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tubio O., Tutusaus I., Valiviita J., Viel M., Hildebrandt H., Kummel, M., Tallada-Crespi, P., Gracia-Carpio, J., Balaguera-Antolinez, A., and Sanchez, A. G.

Subjects
SAMPLE, Large-scale structure of Universe, DATA RELEASE, Formation, Surveys, observations, Dark energy, Dark matter, Galaxy: formation, Large-scale structure of Universe, Surveys [Cosmology], kosmologia, Astrophysics, Cosmology: observation, dark matter, galaksijoukot, pimeä aine, surveys, Dark energy, Dark matter, observations [Cosmology], dark energy, Observations, LEGACY SURVEY, Astrophysics of Galaxies, Física, Astronomy and Astrophysics, 115 Astronomy, Space science, EVOLUTION, Cosmology, galaksit, GALAXIES, Cosmology: observations, Galaxy: formation, Galaxy, formation [Galaxy], Space and Planetary Science, cosmology: observations, large-scale structure of Universe, pimeä energia, Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Artículo escrito por un elevado núnmero de autores, sólo se referencian el qque aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope's Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg2 in the 3.6 and 4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and 8 μm bands. They reach at least 24 AB magnitude (measured to 5σ, in a 2″​​.5 aperture) in the 3.6 μm band and up to ∼5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16 "< "[3.6]< 19 is ≲ 0″​​.15. The photometric calibration is in excellent agreement with previous WISE measurements. We extracted source number counts from the 3.6 μm band mosaics, and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s

Published
2022

3. Euclid preparation - XIII. Forecasts for galaxy morphology with the Euclid Survey using deep generative models: XIII. Forecasts for galaxy morphology with the Euclid Survey using deep generative models

Author

Bretonnière, H., Huertas-Company, M., Boucaud, A., Lanusse, F., Jullo, E., Merlin, E., Tuccillo, D., Castellano, M., Brinchmann, J., Conselice, C. J., Dole, H., Cabanac, R., Courtois, H. M., Castander, F. J., Duc, P. A., Fosalba, P., Guinet, D., Kruk, S., Kuchner, U., Serrano, S., Soubrie, E., Tramacere, A., Wang, L., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Capobianco, V., Carbone, C., Carretero, J., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., Meneghetti, M., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Baldi, M., Bardelli, S., Camera, S., Farinelli, R., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., de La Torre, S., Fabricius, M., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Mccracken, H. J., Metcalf, R. B., Morgante, G., Morisset, N., Nightingale, J., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tutusaus, I., Valiviita, J., Viel, M., Whittaker, L., Knapen, J. H., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie et Statistiques (LCS - COSMOSTAT), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Paris-Saclay, Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Università degli Studi di Roma Tor Vergata [Roma], Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Centre National de la Recherche Scientifique (CNRS), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Euclid Collaboration

Subjects
[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], surveys, cosmology: observations, galaxies: structure, techniques: image processing, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present a machine learning framework to simulate realistic galaxies for the Euclid Survey, producing more complex and realistic galaxies than the analytical simulations currently used in Euclid. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of $0.4\,\rm{deg}^2$ as it will be seen by the Euclid visible imager VIS, and we show that galaxy structural parameters are recovered to an accuracy similar to that for pure analytic Sérsic profiles. Based on these simulations, we estimate that the Euclid Wide Survey (EWS) will be able to resolve the internal morphological structure of galaxies down to a surface brightness of $22.5\,\rm{mag}\,\rm{arcsec}^{-2}$, and the Euclid Deep Survey (EDS) down to $24.9\,\rm{mag}\,\rm{arcsec}^{-2}$. This corresponds to approximately $250$ million galaxies at the end of the mission and a $50\,\%$ complete sample for stellar masses above $10^{10.6}\,\rm{M}_\odot$ (resp. $10^{9.6}\,\rm{M}_\odot$) at a redshift $z\sim0.5$ for the EWS (resp. EDS). The approach presented in this work can contribute to improving the preparation of future high-precision cosmological imaging surveys by allowing simulations to incorporate more realistic galaxies.

Published
2022

4. A CHEOPS-enhanced view of the HD 3167 system

Author

Bourrier, V., Deline, A., Krenn, A., Egger, J. A., Petit, A. C., Malavolta, L., Cretignier, M., Billot, N., Broeg, C., Florén, H.-G., Queloz, D., Alibert, Y., Bonfanti, A., Bonomo, A. S., Delisle, J.-B., Demangeon, O. D. S., Demory, B.-O., Dumusque, X., Ehrenreich, D., Haywood, R. D., Howell, S. B., Lendl, M., Mortier, A., Nigro, G., Salmon, S., Sousa, S. G., Wilson, T. G., Adibekyan, V., Alonso, R., Anglada, G., Bárczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, M., Benz, W., Biondi, F., Bonfils, X., Brandeker, A., Cabrera, J., Charnoz, S., Csizmadia, Sz., Collier Cameron, A., Damasso, M., Davies, M. B., Deleuil, M., Delrez, L., Di Fabrizio, L., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Lecavelier des Etangs, A., Lorenzi, V., Lovis, C., Magrin, D., Massa, A., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Grootel, V., Verrecchia, F., Walton, N., Beck, T., Buder, M., Ratti, F., Ulmer, B., Viotto, V., Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Austrian Academy of Sciences (OeAW), University of Bern, University of Copenhagen = Københavns Universitet (UCPH), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), AlbaNova University Center, Stockholm University, Departement Physik [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Cavendish Laboratory, University of Cambridge [UK] (CAM), INAF - Osservatorio Astrofisico di Torino (OATo), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Center for Space and Habitability (CSH), University of Exeter, NASA Ames Research Center (ARC), Università degli Studi di Padova = University of Padua (Unipd), University of St Andrews [Scotland], Faculdade de Ciências [Lisboa], Universidade de Lisboa = University of Lisbon (ULISBOA), Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, German Aerospace Center (DLR), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Lund University [Lund], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Liège, Fundación Galileo Galilei - INAF, Leiden Observatory [Leiden], Universiteit Leiden, Università degli studi di Torino = University of Turin (UNITO), University of Vienna [Vienna], European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Keele University [Keele], INAF - Osservatorio Astrofisico di Catania (OACT), University of Warwick [Coventry], ESA - ESTEC (Netherlands), Gothard Astrophysical Observatory, Space Sciences, Technologies and Astrophysics Research Institute (STAR), INAF - Osservatorio Astronomico di Roma (OAR), Swiss National Science Foundation, European Research Council, European Commission, European Space Agency, Ministerio de Economía y Competitividad (España), Fundação para a Ciência e a Tecnologia (Portugal), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Planet-star interactions, planets and satellites: physical evolution, planets and satellites: dynamical evolution and stability, 530 Physics, FOS: Physical sciences, individual: HD 3167 [Planets and satellites], techniques: photometric, techniques: radial velocities, planet-star interactions, QB Astronomy, planets and satellites: individual: HD 3167, Solar and Stellar Astrophysics (astro-ph.SR), physical evolution [Planets and satellites], QB, Earth and Planetary Astrophysics (astro-ph.EP), MCC, radial velocities [Techniques], 520 Astronomy, photometric [Techniques], 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, Astronomy and Astrophysics, 3rd-DAS, 500 Science, 620 Engineering, dynamical evolution and stability [Planets and satellites], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics
Abstract

CHEOPS Consortium: V. Bourrier et al., Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations., This work has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). D. E. acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project SPICE DUNE, grant agreement No 947634; project FOUR ACES, grant agreement 724427; project SCORE, grant agreement No 851555). CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. A. C. C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. S. G. S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). A. C. C. and T. G. W. acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. Y. A., M. J. H. and J. A. E. acknowledge the support of the Swiss National Fund under grant 200020_172746. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S. C. C. B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X. B., S. C., D. G., M. F. and J. L. acknowledge their role as ESA-appointed CHEOPS science team members. A. Br. was supported by the SNSA. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L. D. is an F. R. S.-FNRS Postdoctoral Researcher. This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacão by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987, O. D. S. D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B. -O. D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). R. D. H. is funded by the UK Science and Technology Facilities Council (STFC)’s Ernest Rutherford Fellowship (grant number ST/V004735/1). M. F. and C. M. P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D. G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. M. G. is an F.R.S.-FNRS Senior Research Associate. S. H. gratefully acknowledges CNES funding through the grant 837319. K. G. I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. This work was granted access to the HPC resources of MesoPSL financed by the Region Île-de-France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervized by the Agence Nationale pour la Recherche. M. L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. PM acknowledges support from STFC research grant number ST/M001040/1. GSc, GPi, IPa, LBo, VNa and RRa acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015 CHEOPS Fasi A/B/C”. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). I. R. I. acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. Gy. M. Sz. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Institute Agreement between the ELTE Eötvös Loránd University and the European Space Agency (ESA-D/SCI-LE-2021-0025), the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S-FNRS Research Associate. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Some of the observations in the paper made use of the High-Resolution Imaging instrument ‘Alopeke obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. ‘Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Alopeke was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).

Published
2022

5. The Black Hole Universe (BHU) from a FLRW cloud

Author

Gaztanaga, Enrique, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), and Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmology: dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, cosmological parameters, inflation, early Universe
Abstract

submitted to MNRAS, see darkcosmos.com; A FLRW cloud is a solution of classical General Relativity (GR) were a homogeneous star or cloud of mass $M$ and size $R(\tau)$, is collapsing/expanding under its own gravity following a geodesic of the FLRW metric as a function of proper (comoving) time $\tau$.This solution can be used to model the interior of a Black Hole (BH) with regular matter/radiation, without the need of negative pressure or surface terms. Our Universe could emerged from a FLRW dust cloud of $M \simeq 5 \times 10^{22} M_{\odot}$ that collapsed $\tau \simeq 25$ Gyrs ago inside its own event horizon $r_{S}=2GM$. The resulting BH had a very low density, $\rho$, and therefore no pressure support, so the collapse continues free fall inside $r_S$, increasing $\rho$ as $\Delta \tau$ square. After $\Delta \tau \simeq 11$ Gyrs, $\rho$ reaches neutron star density and explodes, like a Supernova, into the hot Big Bang expansion that we observe today. The BHU expansion is trapped inside $r_{S}=2GM$, which acts like a cosmological constant $\Lambda=3/r_{S}^2$. The BHU solution follows $R \simeq [r_H^2 r_S]^{1/3}$ so a large fraction of $M$ is outside its Hubble radius $r_H=H^{-1}$. This solves the horizon problem and could be the source for the observed large scale structure (LSS). Thus, the observed cosmic acceleration and LSS could just be caused by the original collapsing $M$, without the need for any exotic Dark Energy or Cosmic Inflation. The observable universe today is larger than $r_{S}$, so we can test this BHU model using Cosmic maps.

Published
2021

6. The Black Hole Universe (BHU)

Author

Gaztanaga, Enrique, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), and Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena, Cosmology: dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, cosmological parameters, inflation, early Universe
Abstract

The full Universe can be modeled with a Big Bang (BB) homogeneous (FLRW) solution to General Relativity (GR), with an age which is only three times larger than the age of our planet. This is in agreement with most observations and with a Cosmological Principle were spacetime is homogeneous in space, but not in time. But recent observations show that cosmic expansion is dominated by an effective cosmological constant Λ > 0. This indicates that we are inside a trapped surface < Λ ≡ 3/Λ, which corresponds to the interior of a Black Hole (BH). CMB observations show that such BH Universe (BHU) is not empty outside Λ. Our BHU is a Bubble Universe connecting two FLRW metrics. This new solution to classical GR can be used to model a universe or a stellar BH. Both types of BHU can originate in the formation of a false vacuum by kinetic damping within an expanding background, such as cosmic inflation or a supernova explosion. Observed stellar and galactic BHs (and possibly BHs making the Dark Matter, DM) could also be made of BHUs. In comoving coordinates the BHU is expanding while in Schwarzschild coordinates it is asymptotically static. Such frame duality allows for a Perfect Cosmological Principle where spacetime can be homogeneous both in space and time, in better agreement with the relativity principle that the standard BB.

Published
2021

7. A Peek Outside Our Universe

Author

Enrique Gaztanaga, Pablo Fosalba Vela, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, and Generalitat de Catalunya

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), General Mathematics, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, 01 natural sciences, General Relativity and Quantum Cosmology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark energy, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Computer Science (miscellaneous), cosmology, dark energy, general relativity, black holes, Black holes, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Cosmology, General relativity, High Energy Physics - Theory (hep-th), Chemistry (miscellaneous), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Computer Science::Programming Languages, 020201 artificial intelligence & image processing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

According to general relativity (GR), a universe with a cosmological constant Λ, like ours, is trapped inside an event horizon, r, This work has been supported by Spanish MINECO grants PGC2018-102021 and ESP2017-89838-C3-1-R and EU grants LACEGAL 734374 and EWC 776247 with ERDF funds and grant 2017-SGR-885 of the Generalitat de Catalunya.

Published
2022

8. Structured velocity field in the inner envelope of B335: ALMA observations of rare CO isotopologues

Author

Marco Padovani, Anaëlle Maury, Victoria Cabedo, Josep M. Girart, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), European Project: 679937,H2020,ERC-2015-STG,MagneticYSOs(2016), and Harvard University [Cambridge]-Smithsonian Institution

Subjects
FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rotation, circumstellar matter, 01 natural sciences, spectroscopic [Techniques], protostars [Stars], 0103 physical sciences, Optical depth (astrophysics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), formation [Stars], Line (formation), Envelope (waves), Physics, stars: formation, stars: protostars, Accretion (meteorology), 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Circumstellar matter, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, techniques: interferometric, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), interferometric [Techniques], Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract

[Context] Studies of Class 0 objects allow to characterize the dynamical processes taking place at the onset of the star formation process and to determine the physical mechanisms responsible for the outcome of the collapse. Observations of dense gas tracers allow for the characterization of key kinematics of the gas that are directly involved in the star formation process, such as infall, outflow, and rotation. [Aims] This work is aimed at investigating the molecular line velocity profiles of the Class 0 protostellar object B335 and attempts to place constraints on the infall motions happening in the circumstellar gas of the object. [Methods] We present observations of C17O (1-0), C18O (1-0), and 12CO (2-1) transitions along with an analysis of spectral profiles at envelope radii between 100 and 860 au. [Results] C17O emission presents a double-peaked line profile distributed in a complex velocity field. Both peaks present an offset of 0.2-1 km s-1 from the systemic velocity of the source in the probed area. The optical depth of the C17O emission has been estimated and found to be less than 1, suggesting that the two velocity peaks trace two distinct velocity components of the gas in the inner envelope. [Conclusions] After discarding possible motions that could produce the complex velocity pattern, such as rotation and outflow, we conclude that infall motions are responsible for producing the velocity field. Because inside-out symmetric collapse cannot explain those observed profiles, it is suggested that these are produced by non-isotropic accretion from the envelope into the central source along the outflow cavity walls., This project has received funding from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (MagneticYSOs project, grant agreement N° 679937). J.M.G. is supported by the grant AYA2017-84390-C2-R (AEI/FEDER, UE).

Published
2021

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