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13 results on '"Buat, Veronique"'

1. SFR estimations from z = 0 to z = 0.9: A Comparison of SFR Calibrators for Star-Forming Galaxies from z=0 to z=0.9

Author

Figueira, Miguel, Pollo, Agnieszka, Małek, Katarzyna, Buat, Veronique, Boquien, Médéric, Pistis, Francesco, Cassarà, L. P., Vergani, Daniela, Hamed, Mahmoud, Salim, Samir, National Centre for Nuclear Research [Otwock], Narodowe Centrum Badań Jądrowych (NCBJ), The Andrzej Soltan Institute for Nuclear Studies, 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), Centro de Astronomia [Antofagasta] (CITEVA), Universidad de Antofagasta, National Observatory of Athens (NOA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Indiana University [Bloomington], Indiana University System, University of Szczecin, Ewa Szuszkiewicz, Agnieszka Majczyna, Agata Różańska, Radosław Smolec, and Krzysztof Leszczyński

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

35 pages, 28 figures, o be published in A&A; International audience; Based on the VIMOS Public Extragalactic Redshift Survey (VIPERS, z>0.5) and on the GALEX-SDSS-WISE Legacy Catalog (GSWLC, z

Published
2021

2. Getting ready for the LSST data -- estimating the physical properties of $z<2.5$ main sequence galaxies

Author

Riccio, Gabriele, Małek, Katarzyna, Nanni, Ambra, Boquien, Mederic, Buat, Veronique, Burgarella, Denis, Donevski, Darko, Hamed, Mahmoud, Hurley, Peter, Shirley, Raphael, Pollo, Agnieszka, Laboratoire d'Astrophysique de Marseille (LAM), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

In this work we study how to employ the upcoming Legacy Survey of Space and Time (LSST) data to constrain physical properties of normal, star forming galaxies. We use simulated LSST data and existing real observations to test the estimations of the physical properties of galaxies, such as star formation rate (SFR), stellar mass ($M_{star}$), and dust luminosity ($L_{dust}$). We focus on normal star-forming galaxies, as they form the majority of the galaxy population in the universe and therefore are more likely to be observed by the LSST. We perform a simulation of LSST observations and uncertainties of 50,385 real galaxies within redshift range $0, Comment: Accepted to A&A

Published
2021

3. The Herschel-SPIRE Legacy Survey (HSLS): the scientific goals of a shallow and wide submillimeter imaging survey with SPIRE

Author

Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, Bernardis, Francesco, Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Caitlin Casey, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Ram Chary, Ranga, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, Da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, Bernardis, Paolo, Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, Mcmahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, Heyden, Kurt, Werf, Paul P., Kampen, Eelco, Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, Yun, Min S., Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A large sub-mm survey with Herschel will enable many exciting science opportunities, especially in an era of wide-field optical and radio surveys and high resolution cosmic microwave background experiments. The Herschel-SPIRE Legacy Survey (HSLS), will lead to imaging data over 4000 sq. degrees at 250, 350, and 500 micron. Major Goals of HSLS are: (a) produce a catalog of 2.5 to 3 million galaxies down to 26, 27 and 33 mJy (50% completeness; 5 sigma confusion noise) at 250, 350 and 500 micron, respectively, in the southern hemisphere (3000 sq. degrees) and in an equatorial strip (1000 sq. degrees), areas which have extensive multi-wavelength coverage and are easily accessible from ALMA. Two thirds of the of the sources are expected to be at z > 1, one third at z > 2 and about a 1000 at z > 5. (b) Remove point source confusion in secondary anisotropy studies with Planck and ground-based CMB data. (c) Find at least 1200 strongly lensed bright sub-mm sources leading to a 2% test of general relativity. (d) Identify 200 proto-cluster regions at z of 2 and perform an unbiased study of the environmental dependence of star formation. (e) Perform an unbiased survey for star formation and dust at high Galactic latitude and make a census of debris disks and dust around AGB stars and white dwarfs., White paper supplement to the proposal submitted by the HSLS science team to ESA for Herschel open-time programs

Published
2020

4. MOONS: The New Multi-Object Spectrograph for the VLT

Author

Cirasuolo, Michele, Fairley, Alasdair, Rees, Phil, Gonzalez, Oscar A., Taylor, William, Maiolino, Roberto, Afonso, Jose, Evans, Chris, Flores, Hector, Lilly, Simon, Oliva, Ernesto, Paltani, Stephane, Vanzi, Leonardo, Abreu, Manuel, Accardo, Matteo, Adams, Nathan, Méndez, Domingo Álvarez, Amans, Jean-Philippe, Amarantidis, Stergios, Atek, Hakim, Atkinson, David, Banerji, Manda, Barrett, Joe, Barrientos, Felipe, Bauer, Franz, Beard, Steven, Béchet, Clementine, Belfiore, Andrea, Bellazzini, Michele, Benoist, Christophe, Best, Philip, Biazzo, Katia, Black, Martin, Boettger, David, Bonifacio, Piercarlo, Bowler, Rebecca, Bragaglia, Angela, Brierley, Saskia, Brinchmann, Jarle, Brinkmann, Martin, Buat, Veronique, Buitrago, Fernando, Burgarella, Denis, Burningham, Ben, Buscher, David, Cabral, Alexandre, Caffau, Elisabetta, Cardoso, Leandro, Carnall, Adam, Carollo, Marcella, Castillo, Roberto, Castignani, Gianluca, Catelan, Marco, Cicone, Claudia, Cimatti, Andrea, Cioni, Maria-Rosa L., Clementini, Gisella, Cochrane, William, Coelho, João, Colling, Miriam, Contini, Thierry, Contreras, Rodrigo, Conzelmann, Ralf, Cresci, Giovanni, Cropper, Mark, Cucciati, Olga, Cullen, Fergus, Cumani, Claudio, Curti, Mirko, da Silva, Antonio, Daddi, Emanuele, Dalessandro, Emanuele, Dalessio, Francesco, Dauvin, Louise, Davidson, George, de Laverny, Patrick, Delplancke-Ströbele, Françoise, de Lucia, Gabriella, del Vecchio, Ciro, Dessauges-Zavadsky, Miroslava, Di Matteo, Paola, Dole, Herve, Drass, Holger, Dunlop, Jim, Dünner, Rolando, Eales, Steve, Ellis, Richard, Enriques, Bruno, Fasola, Giles, Ferguson, Annette, Ferruzzi, Debora, Fisher, Martin, Flores, Mauricio, Fontana, Adriano, Forchi, Vincenzo, Francois, Patrick, Franzetti, Paolo, Gargiulo, Adriana, Garilli, Bianca, Gaudemard, Julien, Gieles, Mark, Gilmore, Gerry, Ginolfi, Michele, Gomes, Jean Michel, Guinouard, Isabelle, Gutierrez, Pablo, Haigron, Régis, Hammer, François, Hammersley, Peter, Haniff, Chris, Harrison, Chris, Haywood, Misha, Hill, Vanessa, Hubin, Norbert, Humphrey, Andrew, Ibata, Rodrigo, Infante, Leopoldo, Ives, Derek, Ivison, Rob, Iwert, Olaf, Jablonka, Pascale, Jakob, Gerd, Jarvis, Matt, King, David, Kneib, Jean-Paul, Laporte, Philippe, Lawrence, Andy, Lee, David, Causi, Gianluca Li, Lorenzoni, Silvio, Lucatello, Sara, Luco, Yerco, Macleod, Alastair, Magliocchetti, Manuela, Magrini, Laura, Mainieri, Vincenzo, Maire, Charles, Mannucci, Filippo, Martin, Nicolas, Matute, Israel, Maurogordato, Sophie, Mcgee, Sean, Mcleod, Derek, Mclure, Ross, Mcmahon, Richard, Melse, Basile-Thierry, Messias, Hugo, Mucciarelli, Alessio, Nisini, Brunella, Nix, Johannes, Norberg, Peder, Oesch, Pascal, Oliveira, António, Origlia, Livia, Padilla, Nelson, Palsa, Ralf, Pancino, Elena, Papaderos, Polychronis, Pappalardo, Ciro, Parry, Ian, Pasquini, Luca, Peacock, John, Pedichini, Fernando, Pello, Roser, Peng, Yingjie, Pentericci, Laura, Pfuhl, Oliver, Piazzesi, Roberto, Popovic, Dan, Pozzetti, Lucia, Puech, Mathieu, Puzia, Thomas, Raichoor, Anand, Randich, Sofia, Recio-Blanco, Alejandra, Reis, Sandra, Reix, Florent, Renzini, Alvio, Rodrigues, Myriam, Rojas, Felipe, Rojas-Arriagada, Álvaro, Rota, Stefano, Royer, Frédéric, Sacco, Germano, Sanchez-Janssen, Ruben, Sanna, Nicoletta, Santos, Pedro, Sarzi, Marc, Schaerer, Daniel, Schiavon, Ricardo, Schnell, Robin, Schultheis, Mathias, Scodeggio, Marco, Serjeant, Steve, Shen, Tzu-Chiang, Simmonds, Charlotte, Smoker, Jonathan, Sobral, David, Sordet, Michael, Spérone, Damien, Strachan, Jonathan, Sun, Xiaowei, Swinbank, Mark, Tait, Graham, Tereno, Ismael, Tojeiro, Rita, Torres, Miguel, Tosi, Monica, Tozzi, Andrea, Tresiter, Ezequiel, Valenti, Elena, Navarro, Álvaro Valenzuela, Vanzella, Eros, Vergani, Susanna, Verhamme, Anne, Vernet, Joël, Vignali, Cristian, Vinther, Jakob, von Dran, Lauren, Waring, Chris, Watson, Stephen, Wild, Vivienne, Willesme, Bart, Woodward, Brian, Wuyts, Stijn, Yang, Yanbin, Zamorani, Gianni, Zoccali, Manuela, Bluck, Asa, Trussler, James, 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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 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 Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), 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), MOONS Consortium, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

MOONS is the new Multi-Object Optical and Near-infrared Spectrograph currently under construction for the Very Large Telescope (VLT) at ESO. This remarkable instrument combines, for the first time, the collecting power of an 8-m telescope, 1000 fibres with individual robotic positioners, and both low- and high-resolution simultaneous spectral coverage across the 0.64-1.8 micron wavelength range. This facility will provide the astronomical community with a powerful, world-leading instrument able to serve a wide range of Galactic, extragalactic and cosmological studies. Construction is now proceeding full steam ahead and this overview article presents some of the science goals and the technical description of the MOONS instrument. More detailed information on the MOONS surveys is provided in the other dedicated articles in this Messenger issue., Comment: 8 pages, 5 Figures, Published on the ESO Messenger No. 180

Published
2020

5. Properties of LBGs with [OIII] detection at z ∼ 3.5

Author

Yuan, Fang-Ting, Burgarella, Denis, Corre, David, Buat, Veronique, Boquien, Médéric, Shen, Shiyin, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; Context. Nebular emission lines are critical to measure physical properties in the ionized gas (e.g., metallicity, the star formation rate, or dust attenuation). They also account for a significant fraction of broadband fluxes, in particular at the highest redshifts, and therefore can strongly affect the determination of other physical properties, such as the stellar mass, which are crucial in shaping our understanding of galaxy formation and evolution. Aims. We investigate a sample of 51 Lyman break galaxies at 3.0 < z spec < 3.8 with detected [OIII] line emissions and estimated the physical properties of these galaxies to examine the impact of including nebular emission data in the Spectral energy distribution (SED) fitting. Methods. We used the Code Investigating GALaxy Emission (CIGALE) to fit the rest-frame ultraviolet-to-near-infrared SEDs of these galaxies and their emission line data simultaneously. We ran CIGALE with and without the nebular model or the emission line data, and compare the results to show the importance of including the nebular emission line data in the SED fitting. Results. We find that without the nebular model, the SED fitting overestimates the stellar mass due to the strong [OIII] lines that are redshifted to the K s -band, which is consistent with previous results. The emission line data are necessary to constrain the nebular model in the SED fitting. We examine the K s -band excess, which is mostly used to estimate the emissions of the [OIII]+H β lines when there is no spectral data, and we find that the estimation and observation are statistically consistent. However, the difference can reach up to more than 1 dex in some catastrophic cases, which shows the importance of obtaining spectroscopic measurements for these lines. We also estimate the equivalent width of the H β absorption and find it negligible compared to the H β emission. Conclusions. Line emission is important to constrain the nebular models and to obtain reliable estimates of the physical properties of galaxies. These data should be taken into account in the SED fitting.

Published
2019

6. HYPER SUPRIME-CAMERA SURVEY OF THE AKARI NEP WIDE FIELD

Author

Goto, Tomotsugu, Toba, Yoshiki, Utsumi, Yousuke, Oi, Nagisa, Takagi, Toshinobu, Malkan, Matt, Ohayma, Youichi, Murata, Kazumi, Price, Paul, Karouzos, Marios, Matsuhara, Hideo, Nakagawa, Takao, Wada, Takehido, Serjeant, Steve, Burgarella, Denis, Buat, Veronique, Takada, Masahiro, Miyazaki, Satoshi, Oguri, Masamune, Miyaji, Takamitsu, Oyabu, Shinki, White, Glenn, Takeuchi, Tsutomu, Inami, Hanae, Perason, Chris, Malek, Katarzyna, Marchetti, Lucia, HyungMoK, Lee, Im, Myung, Kim, Seong Jin, Koptelova, Ekaterina, Chao, Dani, Wu, Yi-Han, AKARI NEP Survey Team, AKARI All Sky Survey Team, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Photometric redshift, Luminous infrared galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), COSMIC cancer database, 010308 nuclear & particles physics, Star formation, General Medicine, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Redshift, Stars, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The extragalactic background suggests half the energy generated by stars reprocessed into the infrared (IR) by dust. At z$\sim$1.3, 90\% of star formation is obscured by dust. To fully understand the cosmic star formation history, it is critical to investigate infrared emission. AKARI has made deep mid-IR observation using its continuous 9-band filters in the NEP field (5.4 deg$^2$), using $\sim$10\% of the entire pointed observations available throughout its lifetime. However, there remain 11,000 AKARI's infrared sources undetected with the previous CFHT/Megacam imaging ($r\sim$25.9ABmag). Redshift and IR luminosity of these sources are unknown. These sources may contribute significantly to the cosmic star-formation rate density (CSFRD). For example, if they all lie at 1$, Comment: Proceedings of THE UNIVERSE IN THE LIGHT OF AKARI and Synergy with future Large Space Telescopes

Published
2017

7. Evolution of mid-infrared galaxy luminosity functions from the entire AKARI NEP deep field with new CFHT photometry

Author

Malkan, Matthew, Karouzos, Marios, Im, Myungshin, Buat, Veronique, Burgarella, Denis, Sedgwick, Chris, Jeong, Woong-Seob, Marchetti, Lucia, Marek, Katarzyna, Koptelova, Ekaterina, Chao, Dani, Wu, Yi-Han, Pearson, Chris, Lee, Hyung Mok, Serjeant, Stephen, Kim, Seong Jin, Goto, Tomotsugu, Oi, Nagisa, Ohyama, Youichi, Matsuhara, Hideo, Wada, Takehiko, Nakagawa, Takao, Toba, Yoshiki, Malek, Katarzyna, Takagi, Toshinobu, Takeuchi, Tsutomu T., Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-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), Department of Physiology, The University of Hong Kong (HKU), School of Environmental Systems Engineering (SESE), The University of Western Australia (UWA), Centre for Water Research (CWR), Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), and Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hubble Deep Field, astro-ph.GA, FOS: Physical sciences, Ecliptic pole, Astrophysics, Astronomy & Astrophysics, galaxies [infrared], law.invention, infrared: galaxies, Photometry (optics), Telescope, law, galaxies: high-redshift, evolution [galaxies], luminosity function [galaxies], Physics, Luminous infrared galaxy, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), galaxies: luminosity function, mass function, astro-ph.CO, Spectral energy distribution, galaxies: evolution, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 25名, Accepted: 2015-06-23, 資料番号: SA1150154000

Published
2015

8. The emission of galaxies over the whole electromagnetic spectrum

Author

Burgarella, Denis, Médéric Boquien, Roehily, Yannick, Ciesla, Laure, Buat, Veronique, 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), Universidad de Antofagasta, 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), Polskie Towarzystwo Astronomiczne - Société polonaise d'astronomie, Monika Biernacka, Katarzyna Bajan, Greg Stachowski, and Piotr Flin

Subjects
ISBN: 978-83-938279-2-3, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; The Spectral Energy Distributions (SEDs) of galaxies contain a wealth of information on the physical processes at play in galaxies and on their components: gas, stars, dust, Active Galactic Nuclei (AGN). Many of the fundamental properties which shape stellar population ensembles are encoded in their SEDs. In this paper, we will try to keep track of the main properties, e.g. star formation history, total mass in stars, characteristics of the AGN, but also the physical state and amount of gas and dust. We will also see how to use modern tools to collect information on the source of the emission in a way consistent with the observed data from the observed far-ultraviolet to far-infrared ranges.

Published
2015

9. The Evolution of the Visible and Hidden Star Formation in the Universe: Implication from the Luminosity Functions at FUV and FIR

Author

Takeuchi, Tsutomu T., Buat, Veronique, Burgarella, Denis, 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), Beaussier, Catherine, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Based on GALEX and IRAS/Spitzer datasets, we have found that both FUV and FIR luminosity functions (LFs) show a strong evolution from z=0 to z=1, but the FIR LF evolves much stronger than the FUV one. Consequently, the FIR/FUV luminosity density ratio increases from 4 (z=0) to 15 (z=1). It means that more than 80% of the star-forming activity in the Universe is hidden by dust at z=1. To explore this issue further, we have performed a combined analysis of the galaxy sample in FUV and FIR. For the Local Universe we used GALEX-IRAS sample, whereas at z=1 we used the Lyman-break galaxy sample selected by GALEX bands constructed by Burgarella et al. (2005), which is known to be representative of visible (i.e., non-obscured) star-forming galaxies at z=1. From these datasets, we constructed the LFs of the FUV-selected galaxies by the survival analysis to, take into account the upper-limit data properly. We discovered that the FIR LF of the Lyman-break galaxies show a significant evolution comparing with the local FIR LF, but it is a factor of 2-3 lower than the global FIR LF (Le Floc'h et al. 2005). This indicates that the evolution of visible galaxies is not strong enough to explain the drastic evolution of the FIR LF. Namely, a FIR-luminous, rapidly diminishing population of galaxies is required., 4 pages, 4 figures, conference proceedings of "At the Edge of the Universe", Sintra 9-13 October 2006

Published
2006

10. UV and FIR selected star-forming galaxies at z=0: differences and overlaps

Author

Xu, C. Kevin, Buat, Veronique, Iglesias-Páramo, Jorge, Takeuchi, Tsutomu T., Barlow, Tom A., Bianchi, Luciana, Donas, Jose, Forster, Karl, Heckman, Timothy M., Jelinsky, Patrick N., Lee, Young-Wook, Madore, Barry F., Malina, Roger F., Martin, D. Christopher, Milliard, Bruno, Morrissey, Patrick, Rich, R. Michael, Neff, Susan G., Schiminovich, David, Siegmund, Oswald H. W., Small, Todd, Szalay, Alex S., Welsh, Barry Y., Wyder, Ted K., Yi, Sukyoung, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Beaussier, Catherine, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We study two samples of local galaxies, one is UV (GALEX) selected and the other FIR (IRAS) selected, to address the question whether UV and FIR surveys see the two sides ('bright' and 'dark') of the star formation of the same population of galaxies or two different populations of star forming galaxies. No significant difference between the L$_{tot}$ ($=L_{60}+L_{FUV}$) luminosity functions of the UV and FIR samples is found. Also, after the correction for the `Malmquist bias' (bias for flux limited samples), the FIR-to-UV ratio v.s. L$_{tot}$ relations of the two samples are consistent with each other. In the range of $9 \la \log(L_{tot}/L_\sun) \la 12$, both can be approximated by a simple linear relation of $\log (L_{60}/L_{FUV})=\log(L_{tot}/L_\sun)-9.66$. These are consistent with the hypothesis that the two samples represent the same population of star forming galaxies, and their well documented differences in L$_{tot}$ and in FIR-to-UV ratio are due only to the selection effect. A comparison between the UV luminosity functions shows marginal evidence for a population of faint UV galaxies missing in the FIR selected sample. The contribution from these 'FIR-quiet' galaxies to the overall UV population is insignificant, given that the K-band luminosity functions (i.e. the stellar mass functions) of the two samples do not show any significant difference., Comment: 21 pages, 7 figures. Accepted by ApJ

Published
2006

11. The evolution of the ultraviolet and infrared luminosity densities in the universe at 0

Author

Takeuchi, Tsutomu T., Buat, Veronique, Burgarella, Denis, 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
galaxies -methods, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], methods: statistical, extinction, Astrophysics (astro-ph), FOS: Physical sciences, dust, extinction -galaxies, statistical, galaxies: statistics, infrared: galaxies, statistics -infrared
Abstract

The ratio between far-ultraviolet (FUV) and infrared (IR) luminosity densities from z=0 to z=1 is discussed by using the luminosity functions (LFs) of both wavelengths. The FUV LF (z=0-1) based on GALEX has been reported by Arnouts et al. (2005), whilst for the IR LF, we used the IRAS PSCz 60-um LF for the local universe and the Spitzer 15-um LF at higher-z as used by Le Floch et al. (2005). Both luminosity densities show a significant evolutionary trend, but the IR evolves much faster than the FUV. Consequently, the ratio $��_{dust}/��_{FUV}$ increases toward higher-z, from 4 (local) to 15 (z = 1). It is also shown that more than 70% of the star formation activity in the universe is obscured by dust at 0.5 < z < 1.2., 5 pages, 3 figures, accepted for publication in A&A Letters

Published
2005

12. Close-up view of a luminous star-forming galaxy at z = 2.95

Author

A. Carnero Rosell, I. Perez-Fournon, C. N. Herrera, Steve Serjeant, Andrew I. Harris, R. Neri, C. Yang, Axel Weiß, Lucia Marchetti, A. J. Young, Catherine Vlahakis, Hugo Messias, M. Krips, T. Bakx, Mattia Negrello, David H. Hughes, Asantha Cooray, Guilaine Lagache, Alexandre Beelen, Rob Ivison, Helmut Dannerbauer, Matthew D. Lehnert, Pierre Cox, S. Urquhart, Andrew J. Baker, P. van der Werf, Simon Dye, B. M. Jones, Alain Omont, V. Buat, Dominik Riechers, Shuowen Jin, Isabella Cortzen, Raphael Gavazzi, Loretta Dunne, F. Stanley, S. Berta, Steve Eales, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Tongji University, Department of Astronomy [Ithaca], Cornell University [New York], Institut für Astronomie [Wien], Universität Wien, Instituto de Astrofisica de Canarias (IAC), 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), 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), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), School of Physics and Astronomy [Cardiff], Cardiff University, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Radioastronomie (MPIFR), AUTRES, CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Irvine] (UCI), University of California-University of California, and BUAT, Veronique

Subjects
submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Absorption spectroscopy, Einstein ring, Infrared, Astrophysics - cosmology and nongalactic astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Spectral line, [SDU] Sciences of the Universe [physics], symbols.namesake, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, [PHYS]Physics [physics], radio lines: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], galaxies: star formation, symbols, Millimeter, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

(Abridged) Exploiting the sensitivity and broad band width of NOEMA, we have studied the molecular gas and dust in the galaxy HerBS-89a, at z=2.95. High angular resolution images reveal a partial 1.0" diameter Einstein ring in the dust continuum emission and the molecular emission lines of 12CO(9-8) and H2O(2_02-1_11). We report the detection of the three fundamental transitions of the molecular ion OH+, seen in absorption; the molecular ion CH+(1-0) seen in absorption (and tentatively in emission); two transitions of amidogen (NH2), seen in emission; and HCN(11-10) and/or NH(1_2-0_1) seen in absorption. The NOEMA data are complemented with VLA data tracing the 12CO(1-0) emission line, which provides a measurement of the total mass of molecular gas and an anchor for a CO excitation analysis. In addition, we present HST imaging that reveals the foreground lensing galaxy in the near-infrared. Together with data from the GTC, we derive a photometric redshift of z(phot)~0.9 for the foreground lensing galaxy. Modelling the lensing of HerBS-89a, we reconstruct the dust continuum and molecular emission lines (magnified by a factor ~4-5) in the source plane. The 12CO(9-8) and H2O emission lines have comparable spatial and kinematic distributions; the source-plane reconstructions do not clearly distinguish between a one-component and a two-component scenario, but the latter accounts for the observed broad line widths. HerBS-89a is a powerful star forming galaxy with a dust-to-gas ratio delta(GDR)~80, a SFR = 614 +/- 59 Msun/yr and a depletion timescale tau(depl) = (3.4 +/- 1.0) 1e8 years. The OH+ and CH+ absorption lines, all have their main velocity component red-shifted by \Delta(V)~100 km/s relative to the global CO reservoir. We argue that these absorption lines trace a rare example of gas inflow towards the center of the galaxy., Comment: 33 pages, Accepted for publication on A&A

Published
2021

13. X-ray flux in the SED modelling: An application of X-CIGALE in the XMM-XXL field

Author

G. Mountrichas, Laure Ciesla, Denis Burgarella, Guang Yang, Médéric Boquien, V. Buat, BUAT, Veronique, Instituto de Física de Cantabria (IFCA), Universidad de Cantabria [Santander]-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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 Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), active [Galaxies], Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Luminosity, Photometry (optics), [SDU] Sciences of the Universe [physics], Flux (metallurgy), Methods: data analysis, general [X-rays], 0103 physical sciences, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxies: active, Redshift, galaxies [X-rays], X-rays: galaxies, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Spectral energy distribution, Polar, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

arXiv:2011.09220v1, X-CIGALE is built on the spectral energy distribution (SED) code of CIGALE and implements important new features: the code accounts for obscuring material in the poles of AGNs and has the ability to fit X-ray fluxes. In this work, we used ∼2500 spectroscopic X-ray AGNs from the XMM-XXL-north field and examined the improvements the new features bring to the SED modelling analysis. Based on our results, X-CIGALE successfully connects the X-ray with the UV luminosity in the whole range spanned by our sample (log LX(2−10 keV) = (42−46) erg s−1). The addition of the new features generally improves the efficiency of X-CIGALE in the estimation and characterisation of the AGN component. Classification as type 1 or type 2 based on their inclination angle is improved, especially at redshifts lower than 1. The statistical significance of AGN fraction, fracAGN, measurements is increased, in particular for luminous X-ray sources (LX > 1045 erg s−1). These conclusions hold under the condition that (mid-) IR photometry is available in the SED fitting process. The addition of polar dust increases the AGN fraction and the efficiency of the SED decomposition to detect AGNs among X-ray selected sources. X-CIGALE estimates a strong AGN (fracAGN > 0.3) in more than 90% of the IR-selected AGNs and 75% of X-ray-detected AGNs not selected by IR colour criteria. The latter drops to ∼50% when polar dust is not included. The ability of X-CIGALE to include X-ray information in the SED fitting process can be instrumental in the optimal exploitation of the wealth of data that current (eROSITA) and future (ATHENA) missions will provide us., GM acknowledges support by the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. MB acknowledges FONDECYT regular grant 1170618.

Published
2020

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