100 results on '"Jean-Gabriel Cuby"'
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2. MOSAIC on the ELT: Planification of the instrument AITV
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Kacem El Hadi, Kjetil Dohlen, Zalpha Challita, Johan Floriot, Laurent Martin, Tony Pamplona, Marc Jaquet, Franck Ducret, Christian Surace, Myriam Rodrigues, Marie Larrieu, Éric Prieto, Jean-Gabriel Cuby, Mathieu Puech, and Lidia Tasca
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- 2022
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3. MOSAIC on the ELT : optomechanical design of the NIR spectrograph
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Johan . Floriot, Laurent Martin, Tony Pamplona, Zalpha Challita, Bernard Delabre, Kjetil Dohlen, Kacem El Hadi, Éric Prieto, Jean-Gabriel Cuby, Mathieu Puech, Lidia . Tasca, Centre National d'Études Spatiales [Toulouse] (CNES), Aix-Marseille Université - Faculté de pharmacie (AMU PHARM), Aix Marseille Université (AMU), 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), European Southern Observatory, Germany, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and 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)
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[SDU]Sciences of the Universe [physics] - Abstract
International audience; Context. The circumgalactic medium (CGM) is the location where the interplay between large-scale outflows and accretion onto galaxies occurs. Metals in different ionization states flowing between the circumgalactic and intergalactic mediums are affected by large galactic outflows and low-ionization state inflowing gas. Observational studies on their spatial distribution and their relation with galaxy properties may provide important constraints on models of galaxy formation and evolution. Aims. The main goal of this paper is to provide new insights into the spatial distribution of the circumgalactic of star-forming galaxies at 1.5 < z 1.5) and stellar mass (log[ M ⋆ / M ⊙ ] > 10.2) show stronger C IV absorptions compared with those low SFR (log[SFR/( M ⊙ yr −1 )]
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- 2022
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4. MOSAIC on the ELT: development of a camera prototype for the near-infrared spectrograph unit
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Laurent Martin, Tony Pamplona, Florian Ramage, Johan Floriot, Vincent Lapère, Zalpha Challita, Michael Carle, Bernard Delabre, Philippe Maquet, Philippe Godefroy, Kjetil Dohlen, Kacem El Hadi, Éric Prieto, Jean-Gabriel Cuby, Roser Pello, Mathieu Puech, Lidia Tasca, 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), Laboratoire Hippolyte Fizeau (FIZEAU), 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), Station Concordia, IPEV, European Southern Observatory, Germany, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and 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)
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[SDU]Sciences of the Universe [physics] - Abstract
International audience
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- 2022
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5. Euclid preparation. XII. Optimizing the photometric sample of the Euclid survey for galaxy clustering and galaxy-galaxy lensing analyses
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Martin Crocce, Chiara Sirignano, O. Mansutti, L. Whittaker, Massimo Meneghetti, I. Ferrero, Alina Kiessling, Edwin A. Valentijn, Gianluca Castignani, S. Maurogordato, Giuseppe Riccio, P. B. Lilje, Carlo Burigana, Rafael Toledo-Moreo, B. Gillis, Davide Maino, Felix Hormuth, G. Sirri, F. Sureau, W. A. Holmes, Marco Baldi, Richard Massey, Knud Jahnke, K. Pedersen, A. Da Silva, Enrico Bozzo, E. Romelli, Simona Mei, C. Bodendorf, Jussi Valiviita, L. Popa, R. Cledassou, Luigi Guzzo, Andrea Cimatti, A. Pocino, F. Raison, Hélène M. Courtois, M. Tenti, Jarle Brinchmann, Robert C. Nichol, M. Poncet, Massimo Brescia, D. Di Ferdinando, Ghassem Gozaliasl, G. Meylan, D. Bonino, C. Neissner, C. S. Carvalho, Anne Costille, C. A. J. Duncan, M. Viel, A. Balaguera-Antolínez, Valeria Pettorino, Leonardo Corcione, S. Serrano, X. Dupac, Jean Coupon, C. Baccigalupi, R. Benton Metcalf, S. Farrens, Lauro Moscardini, V. Scottez, Yu Wang, Marco Castellano, G. Zamorani, Roberto P. Saglia, Andrea Biviano, Martin Kunz, F. Grupp, S. Casas, S. M. Niemi, J. Nightingale, Enzo Branchini, A. Secroun, N. Martinet, Mark Cropper, G. Seidel, Ismael Tereno, L. Stanco, L. Conversi, E. Medinaceli, Doug Potter, Stefano Cavuoti, Lucia Pozzetti, A. Cappi, F. J. Castander, C. C. Kirkpatrick, G. Congedo, R. Nakajima, Emanuel Rossetti, B. Morin, Fabio Finelli, F. Lacasa, Y. Copin, C. Padilla, Andrea Tramacere, W. Gillard, M. Martinelli, E. Keihänen, S. Kermiche, Mauro Roncarelli, Domenico Sapone, B. Garilli, I. Lloro, E. Munari, Sotiria Fotopoulou, Ariel G. Sánchez, Julien Zoubian, T. Vassallo, Romain Teyssier, Stefano Camera, Ole Marggraf, S. de la Torre, Z. Sakr, V. Capobianco, L. Patrizii, Carlo Giocoli, Stefano Andreon, S. Dusini, M. Frailis, A. Balestra, Ralf Bender, Pedro G. Ferreira, A. Boucaud, Jason Rhodes, Luca Valenziano, E. Zucca, F. Dubath, S. Bardelli, G. Polenta, Pablo Fosalba, Peter Schneider, Elisabetta Maiorano, Fabio Pasian, Hannu Kurki-Suonio, Jean-Gabriel Cuby, N. Welikala, Natalia Auricchio, Thomas D. Kitching, A. Porredon, V. F. Cardone, C. Colodro-Conde, Michele Moresco, Andy Taylor, Will J. Percival, Alkistis Pourtsidou, Christopher J. Conselice, S. Paltani, E. Franceschi, Sebastiano Ligori, Roberto Scaramella, Javier Graciá-Carpio, A. Renzi, Remi A. Cabanac, S. Galeotta, S. Pires, Federico Marulli, Andrea Zacchei, I. Tutusaus, Astronomy, Pocino, A., Tutusaus, I., Castander, F. J., Fosalba, P., Crocce, M., Porredon, A., Camera, S., Cardone, V., Casas, S., Kitching, T., Lacasa, F., Martinelli, M., Pourtsidou, A., Sakr, Z., Andreon, S., Auricchio, N., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Balestra, A., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Boucaud, A., Bozzo, E., Branchini, E., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Capobianco, V., Cappi, A., Carvalho, C. S., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Coupon, J., Courtois, H. M., Cropper, M., Cuby, J. -G., Da Silva, A., De La Torre, S., Di Ferdinando, D., Dubath, F., Duncan, C., Dupac, X., Dusini, S., Farrens, S., Ferreira, P. G., Ferrero, I., Finelli, F., Fotopoulou, S., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kirkpatrick, C. C., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Mansutti, O., Marggraf, O., Martinet, N., Marulli, F., Massey, R., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Benton Metcalf, R., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Nichol, R. C., Niemi, S., Nightingale, J., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sanchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Taylor, A. N., Tenti, M., Tereno, I., Teyssier, R., Toledo-Moreo, R., Tramacere, A., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Welikala, N., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Institut de recherche en astrophysique et planétologie (IRAP), 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), 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 de Paris (UP), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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), Euclid, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Pocino A., Tutusaus I., Castander F.J., Fosalba P., Crocce M., Porredon A., Camera S., Cardone V., Casas S., Kitching T., Lacasa F., Martinelli M., Pourtsidou A., Sakr Z., Andreon S., Auricchio N., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Balestra A., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Boucaud A., Bozzo E., Branchini E., Brescia M., Brinchmann J., Burigana C., Cabanac R., Capobianco V., Cappi A., Carvalho C.S., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Coupon J., Courtois H.M., Cropper M., Cuby J.-G., Da Silva A., De La Torre S., Di Ferdinando D., Dubath F., Duncan C., Dupac X., Dusini S., Farrens S., Ferreira P.G., Ferrero I., Finelli F., Fotopoulou S., Frailis M., Franceschi E., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kirkpatrick C.C., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Mansutti O., Marggraf O., Martinet N., Marulli F., Massey R., Maurogordato S., Medinaceli E., Mei S., Meneghetti M., Benton Metcalf R., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Neissner C., Nichol R.C., Niemi S., Nightingale J., Padilla C., Paltani S., Pasian F., Patrizii L., Pedersen K., Percival W.J., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Scaramella R., Schneider P., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Sureau F., Taylor A.N., Tenti M., Tereno I., Teyssier R., Toledo-Moreo R., Tramacere A., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Viel M., Wang Y., Welikala N., Whittaker L., Zacchei A., Zamorani G., Zoubian J., and Zucca E.
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luminous red galaxies ,Cosmological parameter ,Astrophysics ,Surveys ,01 natural sciences ,Cosmology ,techniques: photometric ,galaxies ,Galaxies: distances and redshift ,distances and redshifts ,Survey ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Physics ,Redshift survey ,lsst ,astro-ph.CO ,galaxies: distances and redshifts ,constraints ,Astrophysics - Cosmology and Nongalactic Astrophysics ,redshift survey ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmological parameters ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,photometric ,Settore FIS/05 - Astronomia e Astrofisica ,surveys ,0103 physical sciences ,distances and redshifts [Galaxies] ,cosmological parameters ,Spurious relationship ,Cluster analysis ,dark energy survey ,Astrophysics::Galaxy Astrophysics ,010308 nuclear & particles physics ,photometric [Techniques] ,Astronomy and Astrophysics ,space ,115 Astronomy, Space science ,Redshift ,Galaxy ,Space and Planetary Science ,Galaxies: distances and redshifts ,Techniques: photometric ,techniques ,Focus (optics) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,cosmology ,cosmic shear ,intrinsic alignments - Abstract
Pocino, A., et al. (Euclid Collaboration), Photometric redshifts (photo-zs) are one of the main ingredients in the analysis of cosmological probes. Their accuracy particularly affects the results of the analyses of galaxy clustering with photometrically selected galaxies (GCph) and weak lensing. In the next decade, space missions such as Euclid will collect precise and accurate photometric measurements for millions of galaxies. These data should be complemented with upcoming ground-based observations to derive precise and accurate photo-zs. In this article we explore how the tomographic redshift binning and depth of ground-based observations will affect the cosmological constraints expected from the Euclid mission. We focus on GCph and extend the study to include galaxy-galaxy lensing (GGL). We add a layer of complexity to the analysis by simulating several realistic photo-z distributions based on the Euclid Consortium Flagship simulation and using a machine learning photo-z algorithm. We then use the Fisher matrix formalism together with these galaxy samples to study the cosmological constraining power as a function of redshift binning, survey depth, and photo-z accuracy. We find that bins with an equal width in redshift provide a higher figure of merit (FoM) than equipopulated bins and that increasing the number of redshift bins from ten to 13 improves the FoM by 35% and 15% for GCph and its combination with GGL, respectively. For GCph, an increase in the survey depth provides a higher FoM. However, when we include faint galaxies beyond the limit of the spectroscopic training data, the resulting FoM decreases because of the spurious photo-zs. When combining GCph and GGL, the number density of the sample, which is set by the survey depth, is the main factor driving the variations in the FoM. Adding galaxies at faint magnitudes and high redshift increases the FoM, even when they are beyond the spectroscopic limit, since the number density increase compensates for the photo-z degradation in this case. We conclude that there is more information that can be extracted beyond the nominal ten tomographic redshift bins of Euclid and that we should be cautious when adding faint galaxies into our sample since they can degrade the cosmological constraints.
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- 2021
- Full Text
- View/download PDF
6. Euclid Preparation. XIV. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Data Release 3
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P. Tallada Crespí, Alina Kiessling, L. Stanco, Y. Copin, E. Zucca, Edwin A. Valentijn, L. Moscardini, C. A. J. Duncan, F. Torradeflot, G. Sirri, Bahram Mobasher, F. J. Castander, Harry I. Teplitz, F. Pasian, H. Degaudenzi, Marian Douspis, Santiago Serrano, E. Munari, Henk Hoekstra, Stefano Cavuoti, C. Sirignano, Jean Coupon, G. Mainetti, Massimo Brescia, S. Bardelli, Ariel G. Sánchez, Stefano Camera, Matteo Viel, Pablo Fosalba, V. Scottez, A. Balaguera-Antolínez, D. Di Ferdinando, G. Polenta, R. B. Metcalf, J. Nightingale, Andrea Zacchei, G. A. Verdoes Kleijn, Jason Rhodes, V. Capobianco, Enrico Bozzo, Gianluca Castignani, Florent Sureau, Natalia Auricchio, L. Patrizii, Ivan Lloro, L. Whittaker, Doug Potter, C. S. Carvalho, B. Kubik, S. Casas, M. Fabricius, R. Cledassou, Andrea Biviano, J. Valiviita, Nabila Aghanim, E. Borsato, Peter Schneider, K. Pedersen, M. Frailis, Carlo Baccigalupi, Lucia Pozzetti, I. Davidzon, Sandrine Pires, Andrea Cimatti, Domenico Sapone, Eugenio Maiorano, Massimo Meneghetti, C. C. Kirkpatrick, S. de la Torre, J. Carretero, S. Dusini, Roberto Scaramella, M. Farina, R. Nakajima, G. Congedo, Ralf Bender, Pedro G. Ferreira, David B. Sanders, B. Morin, Ole Marggraf, Peter Capak, Martin Kunz, P. Flose-Reimberg, Luca Conversi, Giuseppe Riccio, A. Balestra, Stéphane Paltani, M. Tenti, W. Gillard, Luca Valenziano, M. Schultheis, Carlo Giocoli, Martin Kilbinger, Carlo Burigana, P. B. Lilje, P. Hudelot, Ken Ganga, Marco Baldi, A. Da Silva, P. Franzetti, D. Masters, S. Kermiche, N. Hernitschek, F. Raison, Anne Costille, S. A. Stanford, C. Bodendorf, Leonardo Corcione, Daniel Stern, Frank Grupp, Romain Teyssier, Stefano Andreon, Herve Aussel, Mischa Schirmer, Cristobal Padilla, Adam Amara, E. Romelli, Ghassem Gozaliasl, Yu Wang, Marco Castellano, Enzo Branchini, N. Martinet, Mark Cropper, M. Poncet, Sami-Matias Niemi, G. Seidel, Ismael Tereno, F. Dubath, Hélène M. Courtois, C. J. Conselice, Katarina Markovic, Davide Maino, Felix Hormuth, A. Cappi, S. Maurogordato, D. Bonino, Roberto P. Saglia, Simona Mei, V. Lindholm, E. Keihänen, Richard Massey, Knud Jahnke, Georges Meylan, Mauro Roncarelli, S. Farrens, Sotiria Fotopoulou, A. N. Taylor, Matteo Maturi, W. Holmes, A. Renzi, Federico Marulli, M. Fumana, Ricard Casas, C. Colodro-Conde, Bianca Garilli, Michele Moresco, Jarle Brinchmann, G. Zamorani, M. Kümmel, R. Kohley, Sebastiano Ligori, E. Franceschi, Rafael Toledo-Moreo, Achille A. Nucita, X. Dupac, Stein Vidar Hagfors Haugan, L. Popa, Javier Graciá-Carpio, C. Neissner, Remi A. Cabanac, Hannu Kurki-Suonio, S. Galeotta, Jean-Gabriel Cuby, Thomas D. Kitching, Behnam Darvish, Emanuel Rossetti, Julien Zoubian, T. Vassallo, A. Secroun, E. Medinaceli, J. G. Cohen, Valeria Pettorino, Carmelita Carbone, René J. Laureijs, Fabio Finelli, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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 de Paris (UP), 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), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 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), Stanford, S. A., Masters, D., Darvish, B., Stern, D., Cohen, J. G., Capak, P., Hernitschek, N., Davidzon, I., Rhodes, J., Sanders, D. B., Mobasher, B., Castander, F. J., Paltani, S., Aghanim, N., Amara, A., Auricchio, N., Balestra, A., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Casas, R., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Conselice, C. J., Corcione, L., Costille, A., Cropper, M., Degaudenzi, H., Douspis, M., Dubath, F., Dusini, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Giocoli, C., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kiessling, A., Kilbinger, M., Kitching, T., Kubik, B., Kummel, M., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Markovic, K., Massey, R., Meneghetti, M., Meylan, G., Moscardini, L., Niemi, S. M., Padilla, C., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Taylor, A. N., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Valentijn, E. A., Valenziano, L., Verdoes Kleijn, G. A., Wang, Y., Zamorani, G., Zoubian, J., Brescia, M., Congedo, G., Conversi, L., Copin, Y., Kermiche, S., Kohley, R., Medinaceli, E., Mei, S., Moresco, M., Morin, B., Munari, E., Polenta, G., Sureau, F., Tallada Crespi, P., Vassallo, T., Zacchei, A., Andreon, S., Aussel, H., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Bardelli, S., Biviano, A., Borsato, E., Bozzo, E., Burigana, C., Cabanac, R., Camera, S., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J. -G., Da Silva, A., De La Torre, S., Di Ferdinando, D., Duncan, C. A. J., Dupac, X., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Gillard, W., Gozaliasl, G., Gracia-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Marulli, F., Maturi, M., Maurogordato, S., Metcalf, R. B., Nakajima, R., Neissner, C., Nightingale, J. W., Nucita, A. A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Romelli, E., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Stanco, L., Tenti, M., Teyssier, R., Torradeflot, F., Valiviita, J., Viel, M., Whittaker, L., Zucca, E., Astronomy, Stanford S.A., Masters D., Darvish B., Stern D., Cohen J.G., Capak P., Hernitschek N., Davidzon I., Rhodes J., Sanders D.B., Mobasher B., Castander F.J., Paltani S., Aghanim N., Amara A., Auricchio N., Balestra A., Bender R., Bodendorf C., Bonino D., Branchini E., Brinchmann J., Capobianco V., Carbone C., Carretero J., Casas R., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Conselice C.J., Corcione L., Costille A., Cropper M., Degaudenzi H., Douspis M., Dubath F., Dusini S., Fosalba P., Frailis M., Franceschi E., Franzetti P., Fumana M., Garilli B., Giocoli C., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kiessling A., Kilbinger M., Kitching T., Kubik B., Kummel M., Kunz M., Kurki-Suonio H., Laureijs R., Ligori S., Lilje P.B., Lloro I., Maiorano E., Marggraf O., Markovic K., Massey R., Meneghetti M., Meylan G., Moscardini L., Niemi S.M., Padilla C., Pasian F., Pedersen K., Pettorino V., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Roncarelli M., Rossetti E., Saglia R., Scaramella R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Taylor A.N., Teplitz H.I., Tereno I., Toledo-Moreo R., Valentijn E.A., Valenziano L., Verdoes Kleijn G.A., Wang Y., Zamorani G., Zoubian J., Brescia M., Congedo G., Conversi L., Copin Y., Kermiche S., Kohley R., Medinaceli E., Mei S., Moresco M., Morin B., Munari E., Polenta G., Sureau F., Tallada Crespi P., Vassallo T., Zacchei A., Andreon S., Aussel H., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Bardelli S., Biviano A., Borsato E., Bozzo E., Burigana C., Cabanac R., Camera S., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Cuby J.-G., Da Silva A., De La Torre S., Di Ferdinando D., Duncan C.A.J., Dupac X., Fabricius M., Farina M., Farrens S., Ferreira P.G., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Gillard W., Gozaliasl G., Gracia-Carpio J., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Martinet N., Marulli F., Maturi M., Maurogordato S., Metcalf R.B., Nakajima R., Neissner C., Nightingale J.W., Nucita A.A., Patrizii L., Potter D., Renzi A., Riccio G., Romelli E., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Stanco L., Tenti M., Teyssier R., Torradeflot F., Valiviita J., Viel M., Whittaker L., and Zucca E.
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Calibration (statistics) ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Color space ,01 natural sciences ,Cosmology ,Large-scale structure ,010309 optics ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,galaxy, spectroscopy ,Settore FIS/05 - Astronomia e Astrofisica ,Spitzer Space Telescope ,0103 physical sciences ,DISTRIBUTIONS ,Astrophysics::Solar and Stellar Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,PHOTOMETRIC REDSHIFTS ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Astrophysics::Galaxy Astrophysics ,Physics ,Hardware_MEMORYSTRUCTURES ,Astrophysics::Instrumentation and Methods for Astrophysics ,Euclid ,Astronomy and Astrophysics ,Redshift ,Galaxy ,Space and Planetary Science ,Galaxy spectroscopy ,Dark energy ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Stanford, S. A., et al., The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage iv dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < zp < 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al.) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman.
- Published
- 2021
- Full Text
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7. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography
- Author
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C. Colodro-Conde, Marco Baldi, K. Pedersen, F. Sureau, Sebastiano Ligori, M. Fabricius, F. Torradeflot, Chiara Sirignano, L. Whittaker, Michele Moresco, J. Valiviita, Sandrine Pires, Christopher J. Conselice, Andrea Zacchei, Natalia Auricchio, A. Renzi, Peter Schneider, M. Tenti, E. Romelli, Elisabetta Maiorano, P. Tallada Crespa, A. Ealet, Eric Jullo, Yu Wang, Marco Castellano, Hendrik Hildebrandt, S. Paltani, K. Markovic, Fabio Pasian, Hélène M. Courtois, E. Franceschi, Enzo Branchini, A. Secroun, N. Martinet, Mark Cropper, Stein Vidar Hagfors Haugan, Adam Amara, Ghassem Gozaliasl, D. Masters, Martin Kunz, G. Seidel, Ismael Tereno, A. Cappi, Leonardo Corcione, Emanuel Rossetti, Ralf Bender, Pedro G. Ferreira, Giuseppe Riccio, Massimo Brescia, D. Di Ferdinando, G. Zamorani, Stefano Borgani, D. Bonino, X. Dupac, Lauro Moscardini, C. Baccigalupi, B. Morin, Rafael Toledo-Moreo, Federico Marulli, C. Padilla, A. Boucaud, Jason Rhodes, F. Dubath, Javier Graciá-Carpio, Remi A. Cabanac, S. Casas, Roberto P. Saglia, F. Grupp, S. Galeotta, Enrico Bozzo, V. Scottez, Luca Valenziano, B. Gillis, Alina Kiessling, L. Popa, R. Cledassou, V. Capobianco, L. Patrizii, Julien Zoubian, Iary Davidzon, Carlo Burigana, Hannu Kurki-Suonio, Jean Coupon, L. Conversi, H. J. McCracken, Lucia Pozzetti, T. Vassallo, Edwin A. Valentijn, G. Sirri, Jean-Gabriel Cuby, N. Welikala, S. Dusini, R. Nakajima, Matteo Maturi, H. Degaudenzi, P. Franzetti, A. Balestra, Stefano Cavuoti, Ole Marggraf, C. S. Carvalho, S. Bardelli, Ruyman Azzollini, W. Gillard, E. Keihänen, A. Da Silva, R. Benton Metcalf, G. Polenta, Gianluca Castignani, S. Maurogordato, M. Poncet, O. Ilbert, Stefano Andreon, Richard Massey, Knud Jahnke, E. Zucca, E. Medinaceli, Mauro Roncarelli, S. Farrens, C. A. J. Duncan, C. Neissner, Doug Potter, Andrea Tramacere, Jochen Weller, Sotiria Fotopoulou, F. J. Castander, J. Carretero, S. Serrano, Pablo Fosalba, Andrea Cimatti, E. Munari, R. Pello, Anne Costille, Tim Schrabback, Stefano Camera, Y. Copin, L. Stanco, W. A. Holmes, Domenico Sapone, I. Lloro, Harry I. Teplitz, B. Garilli, Clotilde Laigle, Ariel G. Sánchez, Luigi Guzzo, F. Raison, N. Mauri, P. B. Lilje, C. Bodendorf, A. Balaguera-Antolínez, Valeria Pettorino, Carmelita Carbone, Fabio Finelli, Andrea Biviano, Angus H. Wright, J. Nightingale, S. de la Torre, S. Niemi, Carlo Giocoli, G. Congedo, S. Kermiche, C. C. Kirkpatrick, Davide Maino, Felix Hormuth, Simona Mei, Astronomy, 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), University of New South Wales [Sydney] (UNSW), 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), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (KU), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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 de Paris (UP), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of California [Merced], University of California, Centre National d'Études Spatiales [Toulouse] (CNES), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), University of Geneva [Switzerland], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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 de Paris (UP), University of Oxford [Oxford], 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), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), University of Bordeaux, CNRS, UMR 5805 EPOC, Pessac, France, Recherche en Pharmaco-épidémiologie et Recours aux Soins (REPERES), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-École des Hautes Études en Santé Publique [EHESP] (EHESP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Fondation FondaMental [Créteil], Université Paris-Sorbonne - Paris 4 - École des hautes études en sciences de l'information et de la communication (UP4 CELSA), Université Paris-Sorbonne (UP4), Laboratoire Européen Performance Santé Altitude (LEPSA), Université de Perpignan Via Domitia (UPVD), Wuhan University [China], Euclid Collaboration, Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Ilbert, O., De La Torre, S., Martinet, N., Wright, A. H., Paltani, S., Laigle, C., Davidzon, I., Jullo, E., Hildebrandt, H., Masters, D. C., Amara, A., Conselice, C. J., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Balestra, A., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Borgani, S., Boucaud, A., Bozzo, E., Branchini, E., Brescia, M., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Coupon, J., Courtois, H. M., Cropper, M., Cuby, J., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Dubath, F., Duncan, C., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farrens, S., Ferreira, P. G., Finelli, F., Fosalba, P., Fotopoulou, S., Franceschi, E., Franzetti, P., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kirkpatrick, C. C., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maturi, M., Mauri, N., Maurogordato, S., Mccracken, H. J., Medinaceli, E., Mei, S., Benton Metcalf, R., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S., Nightingale, J., Padilla, C., Pasian, F., Patrizii, L., Pedersen, K., Pello, R., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sanchez, A. G., Sapone, D., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Tallada Crespa, P., Tenti, M., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tramacere, A., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Wang, Y., Welikala, N., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., 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), University of Copenhagen = Københavns Universitet (UCPH), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), 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), 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), Université de Genève = University of Geneva (UNIGE), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), 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), University of Zurich, Ilbert, O, Ilbert O., De La Torre S., Martinet N., Wright A.H., Paltani S., Laigle C., Davidzon I., Jullo E., Hildebrandt H., Masters D.C., Amara A., Conselice C.J., Andreon S., Auricchio N., Azzollini R., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Balestra A., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Borgani S., Boucaud A., Bozzo E., Branchini E., Brescia M., Burigana C., Cabanac R., Camera S., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas S., Castander F.J., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conversi L., Copin Y., Corcione L., Costille A., Coupon J., Courtois H.M., Cropper M., Cuby J., Da Silva A., Degaudenzi H., Di Ferdinando D., Dubath F., Duncan C., Dupac X., Dusini S., Ealet A., Fabricius M., Farrens S., Ferreira P.G., Finelli F., Fosalba P., Fotopoulou S., Franceschi E., Franzetti P., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Haugan S.V.H., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kirkpatrick C.C., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Markovic K., Marulli F., Massey R., Maturi M., Mauri N., Maurogordato S., McCracken H.J., Medinaceli E., Mei S., Benton Metcalf R., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Neissner C., Niemi S., Nightingale J., Padilla C., Pasian F., Patrizii L., Pedersen K., Pello R., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Schneider P., Schrabback T., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Sureau F., Tallada Crespa P., Tenti M., Teplitz H.I., Tereno I., Toledo-Moreo R., Torradeflot F., Tramacere A., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Wang Y., Welikala N., Weller J., Whittaker L., Zacchei A., Zamorani G., Zoubian J., Zucca E., German Research Foundation, European Commission, Centre National D'Etudes Spatiales (France), and Duncan, C
- Subjects
statistical [Methods] ,IMPACT ,UNIVERSE ,Astrophysics ,01 natural sciences ,Dark energy ,Galaxies: distances and redshift ,dark energy ,PHOTOMETRIC REDSHIFTS ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Photometric redshift ,media_common ,Physics ,distances and redshift [Galaxies] ,Galaxies: distances and redshifts ,Methods: statistical ,SIMULATION ,astro-ph.CO ,3103 Astronomy and Astrophysics ,Probability distribution ,Spectral energy distribution ,galaxies: distances and redshifts ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,530 Physics ,astro-ph.GA ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,1912 Space and Planetary Science ,0103 physical sciences ,distances and redshifts [Galaxies] ,DISTRIBUTIONS ,methods: statistical ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,PERFORMANCE ,115 Astronomy, Space science ,Astrophysics - Astrophysics of Galaxies ,EVOLUTION ,Galaxy ,Universe ,Redshift ,STELLAR ,RESOLUTION ,Space and Planetary Science ,10231 Institute for Computational Science ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Ilbert, O., et al. (Euclid Collaboration), The analysis of weak gravitational lensing in wide-field imaging surveys is considered to be a major cosmological probe of dark energy. Our capacity to constrain the dark energy equation of state relies on an accurate knowledge of the galaxy mean redshift ⟨ z⟩. We investigate the possibility of measuring ⟨ z»with an accuracy better than 0.002(1 + z) in ten tomographic bins spanning the redshift interval 0.2 99.8%. The zPDF approach can also be successful if the zPDF is de-biased using a spectroscopic training sample. This approach requires deep imaging data but is weakly sensitive to spectroscopic redshift failures in the training sample. We improve the de-biasing method and confirm our finding by applying it to real-world weak-lensing datasets (COSMOS and KiDS+VIKING-450)., H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). A.H. Wright is supported by the ERC Consolidator Grant (No. 770935). This work relied on the HPC resources of CINES (Jade) under the allocation 2013047012 and c2014047012 made by GENCI and on the Horizon Cluster hosted by Institut d’Astrophysique de Paris. ID acknowledges that he received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 896225. We warmly thank S. Rouberol for running the cluster on which the simulation was post-processed. This research is also partly supported by the Centre National d’Etudes Spatiales (CNES). We would also like to recognise the contributions from all of the members of the COSMOS team who helped in obtaining and reducing the large amount of multi-wavelength and spectroscopic data. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018, 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). SA thank the support PRIN MIUR2015 “Cosmology and Fundamental Physics: Illuminating the Dark Universe with Euclid”.
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- 2021
- Full Text
- View/download PDF
8. MOSAIC: the high-multiplex and multi-IFU spectrograph for the ELT
- Author
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Sylvestre Taburet, Susan A. Kassin, Lidia Tasca, Beatriz Barbuy, Lex Kaper, Myriam Rodrigues, Yanbin Yang, Kjetil Dohlen, Jose Afonso, Simon L. Morris, Tim P. Morris, Christopher C. Evans, Marie Larrieu, Marc Dubbeldam, Francois Hammer, Fanny Chemla, Timothy Butterley, Ramon Navarro, Andreas Kelz, Rubén Sánchez-Janssen, Jean-Gabriel Cuby, Fatima De Frondat, Jesús Gallego, Christopher J. Miller, Edwin A. Bergin, S. Zanchetta, Bodo L. Ziegler, Gavin Dalton, David Le Mignant, Jean-Marc Conan, Walter Seifert, M. Puech, Ian Lewis, Göran Östlin, Alexis Finoguenov, Laura Pentericci, Kacem El Hadi, Matthias Steinmetz, Daniel Schaerer, Mike MacIntosh, A. Janssen, C. B. Lim, Thierry Fusco, DOTA, ONERA, Université Paris Saclay [Châtillon], and ONERA-Université Paris-Saclay
- Subjects
010308 nuclear & particles physics ,Computer science ,Astronomy ,FOS: Physical sciences ,Mosaic (geodemography) ,First light ,01 natural sciences ,Galaxy ,law.invention ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Telescope ,law ,0103 physical sciences ,Extremely Large Telescope ,[SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic ,Multiplex ,Astrophysics - Instrumentation and Methods for Astrophysics ,010303 astronomy & astrophysics ,Spectrograph ,Instrumentation and Methods for Astrophysics (astro-ph.IM) - Abstract
MOSAIC is the planned multi-object spectrograph for the 39m Extremely Large Telescope (ELT). Conceived as a multi-purpose instrument, it offers both high multiplex and multi-IFU capabilities at a range of intermediate to high spectral resolving powers in the visible and the near-infrared. MOSAIC will enable unique spectroscopic surveys of the faintest sources, from the oldest stars in the Galaxy and beyond to the first populations of galaxies that completed the reionisation of the Universe--while simultaneously opening up a wide discovery space. In this contribution we present the status of the instrument ahead of Phase B, showcasing the key science cases as well as introducing the updated set of top level requirements and the adopted architecture. The high readiness level will allow MOSAIC to soon enter the construction phase, with the goal to provide the ELT community with a world-class MOS capability as soon as possible after the telescope first light., Accepted to SPIE
- Published
- 2020
- Full Text
- View/download PDF
9. Euclid preparation
- Author
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Stein Vidar Hagfors Haugan, S. Paltani, S. de la Torre, W. A. Holmes, Javier Graciá-Carpio, Ghassem Gozaliasl, Remi A. Cabanac, S. Niemi, Ibrahim Almosallam, S. Galeotta, X. Dupac, Natalia Auricchio, Lauro Moscardini, Carlo Giocoli, Giuseppe Longo, Valeria Pettorino, Carmelita Carbone, E. Zucca, Luigi Guzzo, C. Bodendorf, Enzo Branchini, A. Secroun, N. Martinet, H. Degaudenzi, M. Kilbinger, F. Raison, M. Kuemmel, Roberto P. Saglia, Stefano Cavuoti, Audrey Galametz, B. Gillis, Fabio Finelli, N. Mauri, Massimo Meneghetti, S. Kermiche, M. H. Fabricius, Ismael Tereno, D. Stern, Frank Grupp, P. B. Lilje, Pablo Fosalba, V. Scottez, Andy Taylor, A. Cappi, W. G. Hartley, Giulio Fabbian, E. Keihänen, V. Capobianco, C. C. Kirkpatrick, L. Patrizii, Martin Kunz, Doug Potter, Andrea Tramacere, P. Tallada Crespí, M. Poncet, A. Alvarez-Ayllon, Sandrine Pires, Andrea Biviano, S. Serrano, C. Colodro-Conde, Chiara Sirignano, Joshua S. Speagle, K. Markovic, Yu Wang, Marco Castellano, Andrea Zacchei, Gianluca Castignani, G. Congedo, Emiliano Merlin, G. Desprez, G. Zamorani, F. Sureau, Sebastiano Ligori, Domenico Sapone, I. Lloro, A. Renzi, S. Bardelli, O. Ilbert, Stefano Andreon, A. Da Silva, M. Tenti, Michele Moresco, V. Amaro, Davide Maino, R. Saha, Felix Hormuth, A. Ealet, P. W. Hatfield, Ole Marggraf, G. Polenta, A. Balaguera-Antolinez, S. Farrens, M. Frailis, Carlo Baccigalupi, R. Benton Metcalf, Simona Mei, Sotiria Fotopoulou, Andrew Humphrey, Mark Brodwin, Federico Marulli, M. Fumana, E. Medinaceli, Rafael Toledo-Moreo, Ralf Bender, Pedro G. Ferreira, Emanuel Rossetti, Jarle Brinchmann, G. Meylan, Hannu Kurki-Suonio, C. Padilla, Leonardo Corcione, M. Hailey, Jason Rhodes, Jean-Gabriel Cuby, N. Welikala, L. Conversi, J. De Vicente-Albendea, Thomas D. Kitching, Peter Schneider, Andrea Cimatti, Luca Valenziano, Hélène M. Courtois, Matt J. Jarvis, D. Tavagnacco, Julien Zoubian, T. Vassallo, N. Fourmanoit, S. Pilo, Joseph J. Mohr, Enrico Bozzo, F. Dubath, F. J. Castander, D. Bonino, Marian Douspis, Carlo Burigana, L. Stanco, Elisabetta Maiorano, E. Munari, C. S. Carvalho, G. Sirri, L. Whittaker, Stefano Camera, Matteo Viel, L. Popa, R. Cledassou, Matteo Maturi, Ricard Casas, Fabio Pasian, Jussi-Pekka Väliviita, Jean Coupon, Marco Baldi, F. Torradeflot, Y. Copin, Massimo Brescia, D. Di Ferdinando, C. A. J. Duncan, Mara Salvato, C. J. Conselice, B. Garilli, Clotilde Laigle, B. Kubik, S. Maurogordato, Richard Massey, Knud Jahnke, M. M. Rau, Giuseppe Riccio, S. Casas, R. Kohley, Lucia Pozzetti, W. Gillard, J. Carretero, E. Franceschi, Swiss National Science Foundation, German Research Foundation, Agenzia Nazionale di Valutazione del Sistema Universitario e della Ricerca, European Commission, Academy of Finland, Agenzia Spaziale Italiana, Belgian Science Policy Office, Canadian Euclid Consortium, Centre National D'Etudes Spatiales (France), German Centre for Air and Space Travel, Danish Space Research Institute, Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), Netherlands Research School for Astronomy, Norwegian Space Agency, Romanian Space Agency, State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), 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), 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), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-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), Laboratoire d'Etudes et Recherche en Mathématiques Appliquées (LERMA), Ecole Mohammadia d'Ingénieurs (EMI), EUCLID Collaboration, Department of Physics, Helsinki Institute of Physics, ITA, USA, GBR, FRA, DEU, ESP, 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 Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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 de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Desprez, G., Paltani, S., Coupon, J., Almosallam, I., Alvarez-Ayllon, A., Amaro, V., Brescia, M., Brodwin, M., Cavuoti, S., De Vicente-Albendea, J., Fotopoulou, S., Hatfield, P. W., Hartley, W. G., Ilbert, O., Jarvis, M. J., Longo, G., Rau, M. M., Saha, R., Speagle, J. S., Tramacere, A., Castellano, M., Dubath, F., Galametz, A., Kuemmel, M., Laigle, C., Merlin, E., Mohr, J. J., Pilo, S., Salvato, M., Andreon, S., Auricchio, N., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Bozzo, E., Branchini, E., Brinchmann, J., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, R., Casas, S., Castander, F. J., Castignani, G., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courtois, H. M., Cuby, J. -G., Da Silva, A., De La Torre, S., Degaudenzi, H., DI Ferdinando, D., Douspis, M., Duncan, C. A. J., Dupac, X., Ealet, A., Fabbian, G., Fabricius, M., Farrens, S., Ferreira, P. G., Finelli, F., Fosalba, P., Fourmanoit, N., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Hailey, M., Haugan, S. V. H., Holmes, W., Hormuth, F., Humphrey, A., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kitching, T. D., Kohley, R., Kubik, B., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Markovic, K., Martinet, N., Marulli, F., Massey, R., Maturi, M., Mauri, N., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Benton Metcalf, R., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S., Padilla, C., Pasian, F., Patrizii, L., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Rossetti, E., Saglia, R., Sapone, D., Schneider, P., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Stern, D., Sureau, F., Tallada Crespi, P., Tavagnacco, D., Taylor, A. N., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Welikala, N., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., Desprez G., Paltani S., Coupon J., Almosallam I., Alvarez-Ayllon A., Amaro V., Brescia M., Brodwin M., Cavuoti S., De Vicente-Albendea J., Fotopoulou S., Hatfield P.W., Hartley W.G., Ilbert O., Jarvis M.J., Longo G., Rau M.M., Saha R., Speagle J.S., Tramacere A., Castellano M., Dubath F., Galametz A., Kuemmel M., Laigle C., Merlin E., Mohr J.J., Pilo S., Salvato M., Andreon S., Auricchio N., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Bozzo E., Branchini E., Brinchmann J., Burigana C., Cabanac R., Camera S., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas R., Casas S., Castander F.J., Castignani G., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Courtois H.M., Cuby J.-G., Da Silva A., De La Torre S., Degaudenzi H., DI Ferdinando D., Douspis M., Duncan C.A.J., Dupac X., Ealet A., Fabbian G., Fabricius M., Farrens S., Ferreira P.G., Finelli F., Fosalba P., Fourmanoit N., Frailis M., Franceschi E., Fumana M., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Hailey M., Haugan S.V.H., Holmes W., Hormuth F., Humphrey A., Jahnke K., Keihanen E., Kermiche S., Kilbinger M., Kirkpatrick C.C., Kitching T.D., Kohley R., Kubik B., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Markovic K., Martinet N., Marulli F., Massey R., Maturi M., Mauri N., Maurogordato S., Medinaceli E., Mei S., Meneghetti M., Benton Metcalf R., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S., Padilla C., Pasian F., Patrizii L., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Rossetti E., Saglia R., Sapone D., Schneider P., Scottez V., Secroun A., Serrano S., Sirignano C., Sirri G., Stanco L., Stern D., Sureau F., Tallada Crespi P., Tavagnacco D., Taylor A.N., Tenti M., Tereno I., Toledo-Moreo R., Torradeflot F., Valenziano L., Valiviita J., Vassallo T., Viel M., Wang Y., Welikala N., Whittaker L., Zacchei A., Zamorani G., Zoubian J., and Zucca E.
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PREDICTION ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astrophysics ,Surveys ,01 natural sciences ,TELESCOPE ADVANCED CAMERA ,Cosmology ,galaxies ,Galaxies: distances and redshift ,PROBABILITY DENSITY-ESTIMATION ,Survey ,010303 astronomy & astrophysics ,Photometric redshift ,COSMOS ,Physics ,Ground truth ,distances and redshift [Galaxies] ,distances and redshifts -surveys -techniques ,Outlier ,astro-ph.CO ,Probability distribution ,Catalog ,[SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,Algorithm ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,astro-ph.GA ,miscellaneous [Techniques] ,Catalogs ,Galaxies: distances and redshifts ,Techniques: miscellaneous ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Photometry (optics) ,Settore FIS/05 - Astronomia e Astrofisica ,0103 physical sciences ,distances and redshifts [Galaxies] ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,115 Astronomy, Space science ,Catalogues ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,EVOLUTION ,miscellaneous -catalogs ,MACHINE ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,EMISSION - Abstract
Forthcoming large photometric surveys for cosmology require precise and accurate photometric redshift (photo-z) measurements for the success of their main science objectives. However, to date, no method has been able to produce photo-zs at the required accuracy using only the broad-band photometry that those surveys will provide. An assessment of the strengths and weaknesses of current methods is a crucial step in the eventual development of an approach to meet this challenge. We report on the performance of 13 photometric redshift code single value redshift estimates and redshift probability distributions (PDZs) on a common set of data, focusing particularly on the 0.2pdbl-pdbl2.6 redshift range that the Euclid mission will probe. We designed a challenge using emulated Euclid data drawn from three photometric surveys of the COSMOS field. The data was divided into two samples: one calibration sample for which photometry and redshifts were provided to the participants; and the validation sample, containing only the photometry to ensure a blinded test of the methods. Participants were invited to provide a redshift single value estimate and a PDZ for each source in the validation sample, along with a rejection flag that indicates the sources they consider unfit for use in cosmological analyses. The performance of each method was assessed through a set of informative metrics, using cross-matched spectroscopic and highly-accurate photometric redshifts as the ground truth. We show that the rejection criteria set by participants are efficient in removing strong outliers, that is to say sources for which the photo-z deviates by more than 0.15(1pdbl+pdblz) from the spectroscopic-redshift (spec-z). We also show that, while all methods are able to provide reliable single value estimates, several machine-learning methods do not manage to produce useful PDZs. We find that no machine-learning method provides good results in the regions of galaxy color-space that are sparsely populated by spectroscopic-redshifts, for example zpdbl> pdbl1. However they generally perform better than template-fitting methods at low redshift (zpdbl< pdbl0.7), indicating that template-fitting methods do not use all of the information contained in the photometry. We introduce metrics that quantify both photo-z precision and completeness of the samples (post-rejection), since both contribute to the final figure of merit of the science goals of the survey (e.g., cosmic shear from Euclid). Template-fitting methods provide the best results in these metrics, but we show that a combination of template-fitting results and machine-learning results with rejection criteria can outperform any individual method. On this basis, we argue that further work in identifying how to best select between machine-learning and template-fitting approaches for each individual galaxy should be pursued as a priority., GD and AG acknowledge the support from the Sinergia program of the Swiss National Science Foundation. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. MB acknowledges the financial contribution from the agreement ASI/INAF 2018-23-HH.0, Euclid ESA mission – Phase D and the INAF PRIN-SKA 2017 program 1.05.01.88.04. SC acknowledges the financial contribution from FFABR 2017. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (http://www.euclid-ec.org).
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- 2020
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10. High-redshift quasar selection from the CFHQSIR survey
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Chris J. Willott, Jean-Gabriel Cuby, P. Hudelot, Jean-Charles Cuillandre, S. Basa, Stéphane Arnouts, S. Pipien, 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 [Ottawa], University of Ottawa [Ottawa], 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), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
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Infrared ,Population ,galaxies: active ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,law.invention ,Telescope ,law ,quasars: general ,0103 physical sciences ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,education.field_of_study ,methods: statistical ,010308 nuclear & particles physics ,Near-infrared spectroscopy ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,Quasar ,Billion years ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Stars ,galaxies: photometry ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,cosmology: observations ,infrared: general ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Being observed only one billion years after the Big Bang, z ~ 7 quasars are a unique opportunity for exploring the early Universe. However, only two z ~ 7 quasars have been discovered in near-infrared surveys: the quasars ULAS J1120+0641 and ULAS J1342+0928 at z = 7.09 and z = 7.54, respectively. The Canada-France High-z Quasar Survey in the Near Infrared (CFHQSIR) has been carried out to search for z ~ 7 quasars using near-infrared and optical imaging from the Canada-France Hawaii Telescope (CFHT). Our data consist of $\rm{\sim 130\,deg^{2}}$ of Wide-field Infrared Camera (WIRCam) Y-band images up to a 5{\sigma} limit of $\rm{Y_{AB}}$ ~ 22.4 distributed over the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) Wide fields. After follow-up observations in J band, a first photometric selection based on simple colour criteria led us to identify 36 sources with measured high-redshift quasar colours. However, we expect to detect only ~ 2 quasars in the redshift range 6.8 < z < 7.5 down to a rest-frame absolute magnitude of $\rm{M_{1450}}$ = -24.6. With the motivation of ranking our high-redshift quasar candidates in the best possible way, we developed an advanced classification method based on Bayesian formalism in which we model the high-redshift quasars and low-mass star populations. The model includes the colour diversity of the two populations and the variation in space density of the low-mass stars with Galactic latitude, and it is combined with our observational data. For each candidate, we compute the probability of being a high-redshift quasar rather than a low-mass star. This results in a refined list of the most promising candidates. Our Bayesian selection procedure has proven to be a powerful technique for identifying the best candidates of any photometrically selected sample of objects, and it is easily extendable to other surveys., Comment: 13 pages, 9 figures, accepted for publication in A&A
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- 2018
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11. Assembly, integration, test, and verification scenarios for the ELT MOSAIC instrument
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D. Le Mignant, Francois Hammer, F. Madec, Marc Ferrari, Kjetil Dohlen, Ewan Fitzsimons, Thierry Fusco, P. Vola, Marc Dubbeldam, Jean-Gabriel Cuby, K. El Hadi, Tim Morris, Fanny Chemla, P. Jagourel, Benoit Neichel, 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), W.M. Keck Observatory, Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Durham University, 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), Compagnie industrielle des lasers [Orléans] (CILAS), Compagnie industrielle des lasers (CILAS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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 Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)
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ADAPTIVE OPTICS ,AIV ,Computer science ,Integration testing ,business.industry ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,AIT ,Mosaic (geodemography) ,Modular design ,LAM ,EXTREMELY LARGE TELESCOPES ,[PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,01 natural sciences ,ELT-MOS ,MOSAIC ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,010309 optics ,MULTI-OBJECT SPECTROGRAPH ,Identification (information) ,0103 physical sciences ,Systems engineering ,business ,010303 astronomy & astrophysics - Abstract
International audience; Assembly, Integration, Test and Validation (AIT/V) phases for AO instruments, in laboratory as in the telescope, represent numerous technical challenges. The Laboratoire d’Astrophysique de Marseille (LAM) is in charge of the AIT/V preparation and planning for the MOSAIC (ELT-MOS) instrument, from identification of needs, challenges, risks, to defining the optimal AIT strategy for this highly modular and serialized instrument. In this paper, we present the status of this study and describe several AIT/V scenarios as well as a planning for AIT phases in Europe and in Chile. We also show our capabilities, experience and expertise to lead the instrument MOSAIC AIT/V activities.
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- 2018
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12. Integration and testing of the DESI multi-object spectrograph: performance tests and results for the first unit out of ten
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Patrick Jelinsky, G. Tarle, Stephanie Escoffier, K. Honscheid, Eric Jullo, C. Magneville, A. Secroun, P. E. Blanc, P. Repain, David J. Brooks, M. C. Cousinou, S. Perruchot, A. Elliot, S. Ronayette, Julien Guy, S. Karkar, A. Le Van Suu, G. Castagnoli, P. Ghislain, Eduardo Enrique Sepulveda, Anne Ealet, Jean-Gabriel Cuby, L. Le Guillou, X. Régal, P. H. Carton, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), University College of London [London] (UCL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), 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), 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département de Physique des Particules (ex SPP) (DPP), 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, Ohio State University [Columbus] (OSU), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Physics [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Christopher J. Evans, Luc Simard, Hideki Takami, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Department of Physics, University of Michigan, Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
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Computer science ,business.industry ,Integration testing ,multi-object spectrograph ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,integration ,Object (computer science) ,01 natural sciences ,7. Clean energy ,Unit (housing) ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,010309 optics ,DESI ,0103 physical sciences ,Dark energy ,[SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic ,qualification ,business ,010303 astronomy & astrophysics ,Spectrograph ,Throughput (business) ,Computer hardware ,performance - Abstract
International audience; The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 deg² will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. A consortium of Aix-Marseille University (AMU) and CNRS laboratories (LAM, OHP and CPPM) together with LPNHE (CNRS, Universities Pierre et Marie Curie and Paris-Diderot) and the WINLIGHT Systems company based in Pertuis (France), are in charge of integrating and validating the performance requirements of the full spectrographs. This includes the cryostats, shutters and other mechanisms. The first spectrograph of the series of ten has been fully tested and the performance requirements verified for the following items: focus, image quality, straylight, stability, detector properties and throughput. We present the experimental setup, the test procedures and the results.
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- 2018
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13. The ELT-MOS (MOSAIC): towards the construction phase
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Francois Hammer, Simon Morris, Pascal Jagourel, Richard Myers, Olivier Le Fèvre, Alexis Finogenov, Jari Kotilainen, Bruno Castilho, Göran Östlin, Jose Afonso, Marc Dubbledam, Madeline Close, Phil Parr-Burman, Timothy Morris, Fanny Chemla, Fatima de Frondat, Andreas Kelz, Isabelle Guinouard, Ian Lewis, Kevin Middleton, Ramon Navarro, Marie Larrieu, Johan Pragt, Annemieke Janssen, Kjetil Dohlen, Kacem El Hadi, Eric Gendron, Yanbin Yang, Martyn Wells, Marc Conan, Thierry Fusco, Sylvestre Taburet, Mickael Frotin, Nadia Berkourn, Edwin Bergin, Mathieu Puech, Gavin Dalton, Myriam Rodrigues, Ruben Janssen, Ewan Fitzsimons, Beatriz Barbuy, Jean-Gabriel Cuby, Lex Kaper, Martin Roth, Gérard Rousset, Sofia Feltzing, Andreas Korn, Jesús Gallego, África Castillo Morales, Jorge Iglesias-Paramo, Laura Pentericci, Bodo Ziegler, Daniel Schaerer, Hideki Takami, Christopher Evans, Luc Simard, Beaussier, Catherine, 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 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), Oskar Klein Centre [Stockholm], Stockholm University, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], and ONERA-Université Paris Saclay (COmUE)
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[SDU] Sciences of the Universe [physics] ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,[SDU]Sciences of the Universe [physics] ,[SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph] ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience
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- 2018
14. The WIRCam Ultra Deep Survey (WUDS)
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Nicolas Laporte, Marc Balcells, Frédéric Boone, Mercedes Prieto, R. Pello, Daniel Schaerer, P. Hudelot, Johan Richard, Yannick Mellier, Jean-Gabriel Cuby, J. F. Le Borgne, Nicolás Cardiel, Matthew Hayes, Rafael Guzman, Jesús Gallego, H. J. McCracken, Francisco Garzón, K. Disseau, Laurence Tresse, Stéphane Arnouts, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Department of Chemistry, RIDER UNIVERSITY, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), AGROCAMPUS OUEST, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), and 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
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Population ,first stars ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Luminosity ,surveys ,galaxies: high-redshift ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,dark ages ,education ,010303 astronomy & astrophysics ,Reionization ,Astrophysics::Galaxy Astrophysics ,Luminosity function (astronomy) ,Physics ,education.field_of_study ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,reionization ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Lyman-break galaxy - Abstract
The aim of this paper is to introduce the WIRCam Ultra Deep Survey (WUDS), a near-IR photometric public survey carried out at the CFH Telescope in the field of the CFHTLS-D3 field (Groth Strip). WUDS includes four near-IR bands (Y, J, H and K_s) over a field of view of ~400 arcmin^2. The typical depth of WUDS data reaches between ~26.8 in Y and J, and ~26 in H and K_s (AB, 3 sigma in 1.3 arcsec aperture). The area and depth of this survey were specifically tailored to set strong constraints on the cosmic star formation rate and the luminosity function brighter or around L* in the z~6-10 redshift domain, although these data are also useful for a variety of extragalactic projects.This first paper is intended to present the properties of WUDS: catalog building, completeness and depth, number counts, photometric redshifts, and global properties of the galaxy population. We have also concentrated on the study of galaxy samples at z~[4.5-7] in this field. UV luminosity functions were derived at z~5 and z~6 taking advantage from the fact that WUDS covers a particularly interesting regime at intermediate luminosities, which allows a combined determination of M* and Phi* with increased accuracy. Our results on the luminosity function are consistent with a small evolution of both M* and Phi* between z=5 and z=6, irrespective of the method used to derive them, either photometric redshifts applied to blindly-selected dropout samples or the classical Lyman Break Galaxy color-preselected samples. Our results lend support to higher Phi* determinations at z=6 than usually reported. The selection and combined analysis of different galaxy samples at z>7 will be presented in a forthcoming paper. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey (Abridged), Accepted for publication in Astronomy & Astrophysics. 17 pages, 11 figures
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- 2018
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15. The THESEUS space mission concept: science case, design and expected performances
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Martino Marisaldi, Enrico Bozzo, Valerie Connaughton, Dorottya Szécsi, D. Malesani, L. Maraschi, B. Cordier, P. D'Avanzo, Salvatore Capozziello, Darach Watson, C. Contini, Maryam Modjaz, Pierluigi Bellutti, M. de Pasquale, C. Guidorzi, Colleen A. Wilson-Hodge, O. Boulade, C. Adami, Y. Evangelista, A. Argan, Johan P. U. Fynbo, Y.-W. Dong, Poshak Gandhi, Allan Hornstrup, Eliana Palazzi, Andrea Bulgarelli, Andrea Comastri, E. Geza, Luciano Burderi, Giuseppe Malaguti, D. de Martino, Irfan Kuvvetli, S.-N. Zhang, Claudio Labanti, Fiamma Capitanio, Luca Izzo, Bradley Cenko, A. Melandri, Umberto Maio, Nicola Omodei, Stefano Ettori, C. Butler, S. D. Vergani, S. Zhang, Lajos G. Balázs, Patricia Schady, Federica B. Bianco, M. Branchesi, Jens Hjorth, Jochen Greiner, Felix Ryde, Jean-Gabriel Cuby, Piero Malcovati, Lorraine Hanlon, Peter G. Jonker, M. Della Valle, Elena Pian, Piotr Orleanski, Etienne Renotte, W. Skidmore, L. Sabau-Graziati, Mauro Dadina, Carl Budtz-Jørgensen, Tomaz Rodic, Giancarlo Ghirlanda, Luigi Piro, Sheila McBreen, M. Fiorini, M. Topinka, Jan Harms, Riccardo Ciolfi, Yi Chen, Giacomo Vianello, Ester Piedipalumbo, Zsolt Bagoly, Aniello Grado, Yuki Kaneko, Vito Sguera, B. Morelli, E. Le Floc'h, Luciano Rezzolla, K. Wiersema, Remo Ruffini, E. Del Monte, J. P. Osborne, M. G. Bernardini, A. Gomboc, A. De Luca, Stefano Covino, Ian Hutchinson, A. Antonelli, Enzo Brocato, Mark R. Sims, M. Razzano, Elisabetta Maiorano, Jean-Luc Atteia, J. Zicha, S. Korpela, Eros Vanzella, V. D'Elia, M. H. P. M. van Putten, Marco Feroci, Carole Mundell, A. V. Penacchioni, J. Soomin, Gabriele Ghisellini, Sandra Savaglio, N. Shigehiro, Andrea Santangelo, Antonio Martin-Carrillo, Avishay Gal-Yam, A. M. Read, Piergiorgio Casella, Giuseppe Baldazzi, B. Ciardi, Pawan Kumar, Li Song, V. Lebrun, G. Zampa, Daisuke Yonetoku, S. Vojtech, Gregor Rauw, Piero Rosati, A. J. Castro-Tirado, Bruce Gendre, Tsvi Piran, A. Rachevski, S. Basa, T. Li, Michela Uslenghi, Gianluca Morgante, Michèle Lavagna, Pascal Chardonnet, Andrew MacFadyen, Asaf Pe'er, Sandro Mereghetti, Alessandro Drago, M. Hafizi, Richard Willingale, D. Morris, Bing Zhang, Paolo Giommi, Andrea Ferrara, Mauro Orlandini, Maria Giovanna Dainotti, N. Masetti, Yuji Urata, Maxim Lyutikov, A. Vacchi, László L. Kiss, E. Campolongo, M. Boer, Lorenzo Amati, Diego Götz, Andrew Blain, M. T. Botticella, C. Tenzer, Monica Colpi, Victor Reglero, Roberto Mignani, Michael S. Briggs, Joseph Caruana, Elizabeth R. Stanway, S. Colafrancesco, Francesca Panessa, H. U. Nargaard-Nielsen, F. Lu, Giuseppe Bertuccio, A. Paizis, P. Romano, S. Vercellone, Luciano Nicastro, S. Paltani, G. Pareschi, G. Stratta, V. Petrosian, João Braga, N. Zampa, Nial Tanvir, James E. Rhoads, Raffaella Margutti, Luca Valenziano, Søren Brandt, S. Boci, Andrea Rossi, Paul J. Callanan, Annalisa Celotti, N. Kawai, René Hudec, Francesco Longo, Primo Attina, G. L. Israel, F. Fuschino, Fabio Finelli, M. Hernanz, Ruben Salvaterra, F. Frontera, P. T. O'Brien, Sergio Campana, Rupal Basak, Riccardo Campana, Eleonora Troja, Jordan Camp, Petr Páta, S. Piranomonte, G. Tagliaferri, Sylvain Guiriec, R. L. C. Starling, B. B. Zhang, Natalia Auricchio, Serena Vinciguerra, Département d'Astrophysique (ex SAP) (DAP), 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, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agenzia Spaziale Italiana, European Commission, Czech Grant Agency, ITA, 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), 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 des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), THESEUS, Amati, L, O'Brien, P, Götz, D, Bozzo, E, Tenzer, C, Frontera, F, Ghirlanda, G, Labanti, C, Osborne, J, Stratta, G, Tanvir, N, Willingale, R, Attina, P, Campana, R, Castro-Tirado, A, Contini, C, Fuschino, F, Gomboc, A, Hudec, R, Orleanski, P, Renotte, E, Rodic, T, Bagoly, Z, Blain, A, Callanan, P, Covino, S, Ferrara, A, Le Floch, E, Marisaldi, M, Mereghetti, S, Rosati, P, Vacchi, A, D'Avanzo, P, Giommi, P, Piranomonte, S, Piro, L, Reglero, V, Rossi, A, Santangelo, A, Salvaterra, R, Tagliaferri, G, Vergani, S, Vinciguerra, S, Briggs, M, Campolongo, E, Ciolfi, R, Connaughton, V, Cordier, B, Morelli, B, Orlandini, M, Adami, C, Argan, A, Atteia, J, Auricchio, N, Balazs, L, Baldazzi, G, Basa, S, Basak, R, Bellutti, P, Bernardini, M, Bertuccio, G, Braga, J, Branchesi, M, Brandt, S, Brocato, E, Budtz-Jorgensen, C, Bulgarelli, A, Burderi, L, Camp, J, Capozziello, S, Caruana, J, Casella, P, Cenko, B, Chardonnet, P, Ciardi, B, Colafrancesco, S, Dainotti, M, D'Elia, V, De Martino, D, De Pasquale, M, Del Monte, E, Della Valle, M, Drago, A, Evangelista, Y, Feroci, M, Finelli, F, Fiorini, M, Fynbo, J, Gal-Yam, A, Gendre, B, Ghisellini, G, Grado, A, Guidorzi, C, Hafizi, M, Hanlon, L, Hjorth, J, Izzo, L, Kiss, L, Kumar, P, Kuvvetli, I, Lavagna, M, Li, T, Longo, F, Lyutikov, M, Maio, U, Maiorano, E, Malcovati, P, Malesani, D, Margutti, R, Martin-Carrillo, A, Masetti, N, Mcbreen, S, Mignani, R, Morgante, G, Mundell, C, Nargaard-Nielsen, H, Nicastro, L, Palazzi, E, Paltani, S, Panessa, F, Pareschi, G, Pe'Er, A, Penacchioni, A, Pian, E, Piedipalumbo, E, Piran, T, Rauw, G, Razzano, M, Read, A, Rezzolla, L, Romano, P, Ruffini, R, Savaglio, S, Sguera, V, Schady, P, Skidmore, W, Song, L, Stanway, E, Starling, R, Topinka, M, Troja, E, van Putten, M, Vanzella, E, Vercellone, S, Wilson-Hodge, C, Yonetoku, D, Zampa, G, Zampa, N, Zhang, B, Zhang, S, Antonelli, A, Bianco, F, Boci, S, Boer, M, Botticella, M, Boulade, O, Butler, C, Campana, S, Capitanio, F, Celotti, A, Chen, Y, Colpi, M, Comastri, A, Cuby, J, Dadina, M, De Luca, A, Dong, Y, Ettori, S, Gandhi, P, Geza, E, Greiner, J, Guiriec, S, Harms, J, Hernanz, M, Hornstrup, A, Hutchinson, I, Israel, G, Jonker, P, Kaneko, Y, Kawai, N, Wiersema, K, Korpela, S, Lebrun, V, Lu, F, Macfadyen, A, Malaguti, G, Maraschi, L, Melandri, A, Modjaz, M, Morris, D, Omodei, N, Paizis, A, Páta, P, Petrosian, V, Rachevski, A, Rhoads, J, Ryde, F, Sabau-Graziati, L, Shigehiro, N, Sims, M, Soomin, J, Szécsi, D, Urata, Y, Uslenghi, M, Valenziano, L, Vianello, G, Vojtech, S, Watson, D, Zicha, J, Amati, L., O'Brien, P., Götz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J. P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A. J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., Orleanski, P., Renotte, E., Rodic, T., Bagoly, Z., Blain, A., Callanan, P., Covino, S., Ferrara, A., Le Floch, E., Marisaldi, M., Mereghetti, S., Rosati, P., Vacchi, A., D'Avanzo, P., Giommi, P., Piranomonte, S., Piro, L., Reglero, V., Rossi, A., Santangelo, A., Salvaterra, R., Tagliaferri, G., Vergani, S., Vinciguerra, S., Briggs, M., Campolongo, E., Ciolfi, R., Connaughton, V., Cordier, B., Morelli, B., Orlandini, M., Adami, C., Argan, A., Atteia, J. -L., Auricchio, N., Balazs, L., Baldazzi, G., Basa, S., Basak, R., Gian Luca, Israel, Bellutti, P., Bernardini, M. G., Bertuccio, G., Braga, J., Branchesi, M., Brandt, S., Brocato, E., Budtz-Jorgensen, C., Bulgarelli, A., Burderi, L., Camp, J., Capozziello, S., Caruana, J., Casella, P., Cenko, B., Chardonnet, P., Ciardi, B., Colafrancesco, S., Dainotti, M. G., D'Elia, V., De Martino, D., De Pasquale, M., Del Monte, E., Della Valle, M., Drago, A., Evangelista, Y., Feroci, M., Finelli, F., Fiorini, M., Fynbo, J., Gal-Yam, A., Gendre, B., Ghisellini, G., Grado, A., Guidorzi, C., Hafizi, M., Hanlon, L., Hjorth, J., Izzo, L., Kiss, L., Kumar, P., Kuvvetli, I., Lavagna, M., Li, T., Longo, F., Lyutikov, M., Maio, U., Maiorano, E., Malcovati, P., Malesani, D., Margutti, R., Martin-Carrillo, A., Masetti, N., Mcbreen, S., Mignani, R., Morgante, G., Mundell, C., Nargaard-Nielsen, H. U., Nicastro, L., Palazzi, E., Paltani, S., Panessa, F., Pareschi, G., Pe'Er, A., Penacchioni, A. V., Pian, E., Piedipalumbo, E., Piran, T., Rauw, G., Razzano, M., Read, A., Rezzolla, L., Romano, P., Ruffini, R., Savaglio, S., Sguera, V., Schady, P., Skidmore, W., Song, L., Stanway, E., Starling, R., Topinka, M., Troja, E., van Putten, M., Vanzella, E., Vercellone, S., Wilson-Hodge, C., Yonetoku, D., Zampa, G., Zampa, N., Zhang, B., Zhang, B. B., Zhang, S., Zhang, S. -N., Antonelli, A., Bianco, F., Boci, S., Boer, M., Botticella, M. T., Boulade, O., Butler, C., Campana, S., Capitanio, F., Celotti, A., Chen, Y., Colpi, M., Comastri, A., Cuby, J. -G., Dadina, M., De Luca, A., Dong, Y. -W., Ettori, S., Gandhi, P., Geza, E., Greiner, J., Guiriec, S., Harms, J., Hernanz, M., Hornstrup, A., Hutchinson, I., Israel, G., Jonker, P., Kaneko, Y., Kawai, N., Wiersema, K., Korpela, S., Lebrun, V., Lu, F., Macfadyen, A., Malaguti, G., Maraschi, L., Melandri, A., Modjaz, M., Morris, D., Omodei, N., Paizis, A., Páta, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szécsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., Zicha, J., 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), 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), ANR-16-CE31-0003,BEaPro,Using the most powerful explosion as probes of the high-redshift Universe(2016), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -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'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Gotz, D., Pata, P., Szecsi, D., Department of Physics, and Amati, L. and O'Brien, P. and Götz, D. and Bozzo, E. and Tenzer, C. and Frontera, F. and Ghirlanda, G. and Labanti, C. and Osborne, J.P. and Stratta, G. and Tanvir, N. and Willingale, R. and Attina, P. and Campana, R. and Castro-Tirado, A.J. and Contini, C. and Fuschino, F. and Gomboc, A. and Hudec, R. and Orleanski, P. and Renotte, E. and Rodic, T. and Bagoly, Z. and Blain, A. and Callanan, P. and Covino, S. and Ferrara, A. and Le Floch, E. and Marisaldi, M. and Mereghetti, S. and Rosati, P. and Vacchi, A. and D'Avanzo, P. and Giommi, P. and Piranomonte, S. and Piro, L. and Reglero, V. and Rossi, A. and Santangelo, A. and Salvaterra, R. and Tagliaferri, G. and Vergani, S. and Vinciguerra, S. and Briggs, M. and Campolongo, E. and Ciolfi, R. and Connaughton, V. and Cordier, B. and Morelli, B. and Orlandini, M. and Adami, C. and Argan, A. and Atteia, J.-L. and Auricchio, N. and Balazs, L. and Baldazzi, G. and Basa, S. and Basak, R. and Bellutti, P. and Bernardini, M.G. and Bertuccio, G. and Braga, J. and Branchesi, M. and Brandt, S. and Brocato, E. and Budtz-Jorgensen, C. and Bulgarelli, A. and Burderi, L. and Camp, J. and Capozziello, S. and Caruana, J. and Casella, P. and Cenko, B. and Chardonnet, P. and Ciardi, B. and Colafrancesco, S. and Dainotti, M.G. and D'Elia, V. and De Martino, D. and De Pasquale, M. and Del Monte, E. and Della Valle, M. and Drago, A. and Evangelista, Y. and Feroci, M. and Finelli, F. and Fiorini, M. and Fynbo, J. and Gal-Yam, A. and Gendre, B. and Ghisellini, G. and Grado, A. and Guidorzi, C. and Hafizi, M. and Hanlon, L. and Hjorth, J. and Izzo, L. and Kiss, L. and Kumar, P. and Kuvvetli, I. and Lavagna, M. and Li, T. and Longo, F. and Lyutikov, M. and Maio, U. and Maiorano, E. and Malcovati, P. and Malesani, D. and Margutti, R. and Martin-Carrillo, A. and Masetti, N. and McBreen, S. and Mignani, R. and Morgante, G. and Mundell, C. and Nargaard-Nielsen, H.U. and Nicastro, L. and Palazzi, E. and Paltani, S. and Panessa, F. and Pareschi, G. and Pe'er, A. and Penacchioni, A.V. and Pian, E. and Piedipalumbo, E. and Piran, T. and Rauw, G. and Razzano, M. and Read, A. and Rezzolla, L. and Romano, P. and Ruffini, R. and Savaglio, S. and Sguera, V. and Schady, P. and Skidmore, W. and Song, L. and Stanway, E. and Starling, R. and Topinka, M. and Troja, E. and van Putten, M. and Vanzella, E. and Vercellone, S. and Wilson-Hodge, C. and Yonetoku, D. and Zampa, G. and Zampa, N. and Zhang, B. and Zhang, B.B. and Zhang, S. and Zhang, S.-N. and Antonelli, A. and Bianco, F. and Boci, S. and Boer, M. and Botticella, M.T. and Boulade, O. and Butler, C. and Campana, S. and Capitanio, F. and Celotti, A. and Chen, Y. and Colpi, M. and Comastri, A. and Cuby, J.-G. and Dadina, M. and De Luca, A. and Dong, Y.-W. and Ettori, S. and Gandhi, P. and Geza, E. and Greiner, J. and Guiriec, S. and Harms, J. and Hernanz, M. and Hornstrup, A. and Hutchinson, I. and Israel, G. and Jonker, P. and Kaneko, Y. and Kawai, N. and Wiersema, K. and Korpela, S. and Lebrun, V. and Lu, F. and MacFadyen, A. and Malaguti, G. and Maraschi, L. and Melandri, A. and Modjaz, M. and Morris, D. and Omodei, N. and Paizis, A. and Páta, P. and Petrosian, V. and Rachevski, A. and Rhoads, J. and Ryde, F. and Sabau-Graziati, L. and Shigehiro, N. and Sims, M. and Soomin, J. and Szécsi, D. and Urata, Y. and Uslenghi, M. and Valenziano, L. and Vianello, G. and Vojtech, S. and Watson, D. and Zicha, J.
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Ionization ,Atmospheric Science ,cosmological model ,Cherenkov Telescope Array ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Astronomy ,Dark age ,MASSIVE SINGLE STARS ,Star formation rates, Gamma ray ,01 natural sciences ,Cosmology: observation ,localization ,law.invention ,Astrophysic ,Einstein Telescope ,observational cosmology ,law ,Observational cosmology ,Re-ionization ,Cosmology: observations ,Dark ages ,First stars ,Gamma-ray: bursts ,LIGO ,observations [Cosmology] ,Telescope ,010303 astronomy & astrophysics ,High sensitivity ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Multi-wavelength ,energy: high ,sezele ,gamma-ray bursts ,Aerospace Engineering ,Space and Planetary Science ,Astrophysics::Instrumentation and Methods for Astrophysics ,imaging ,star: formation ,burst [Gamma-ray] ,observatory ,Geophysics ,X rays, Cosmology: observation ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,signature ,Star ,TIDAL DISRUPTION ,Gamma-ray: burst ,Astrophysics::High Energy Astrophysical Phenomena ,SIMILAR-TO 6 ,Socio-culturale ,FOS: Physical sciences ,observation [Cosmology] ,galaxy: luminosity ,X-ray astronomy: instrumentation ,7 CANDIDATE GALAXIES ,Astrophysics::Cosmology and Extragalactic Astrophysics ,gamma ray: burst ,114 Physical sciences ,Settore FIS/03 - Fisica della Materia ,X-ray ,bursts [Gamma-ray] ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Settore FIS/05 - Astronomia e Astrofisica ,First star ,0103 physical sciences ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,KAGRA ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,LIGHT CURVES ,010308 nuclear & particles physics ,Gravitational wave ,gravitational radiation ,Astronomy and Astrophysics ,115 Astronomy, Space science ,redshift ,sensitivity ,Redshift ,NEUTRON-STAR MERGER ,messenger ,VIRGO ,electromagnetic ,LUMINOSITY FUNCTION ,BLACK-HOLE ,General Earth and Planetary Sciences ,Gamma-ray burst ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5¿1 arcmin localization, an energy band extending from several MeV down to 0.3¿keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7¿m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late ¿20s/early ¿30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).© 2018 COSPAR, S.E. acknowledges the financial support from contracts ASI-INAF 1/009/10/0, NARO15 ASI-INAF 1/037/12/0 and ASI 2015-046-R.0. R.H. acknowledges GACR grant 13-33324S. S.V. research leading to these results has received funding from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement no 606176. D.S. was supported by the Czech grant 1601116S GA CR. Maria Giovanna Dainotti acknowledges funding from the European Union through the Marie Curie Action FP7-PEOPLE-2013-IOF, under grant agreement No. 626267 (>Cosmological Candles>).
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- 2018
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16. VIMOS Ultra-Deep Survey (VUDS): IGM transmission towards galaxies with $2.5 < z < 5.5$ and the colour selection of high-redshift galaxies
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Daniela Vergani, Yannick Mellier, C. Lopez-Sanjuan, Nick Scoville, Paolo Cassata, Rajat M. Thomas, Laurence Tresse, S. Paltani, B. Ribeiro, Ricardo Amorín, Letizia P. Cassarà, Andrea Cimatti, Brian C. Lemaux, Bianca Garilli, Andrea Grazian, Stéphane Charlot, Margherita Talia, Laura Pentericci, D. Maccagni, Adriano Fontana, Nimish P. Hathi, G. Zamorani, V. Le Brun, Lidia Tasca, O. Ilbert, Peter Capak, A. Durkalec, Thierry Contini, E. Zucca, S. Bardelli, Daniel Schaerer, Anton M. Koekemoer, Marco Castellano, James Dunlop, Mauro Giavalisco, V. Sommariva, Marco Scodeggio, P. W. Wang, Jean-Gabriel Cuby, Mara Salvato, Yoshiaki Taniguchi, Eros Vanzella, O. Cucciati, S. de la Torre, Sotiria Fotopoulou, Janine Pforr, O. Le Fevre, 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), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), 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 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Thomas, R., Le Fèvre, O., Le Brun, V., Cassata, P., Garilli, B., Lemaux, B.C., Maccagni, D., Pentericci, L., Tasca, L.A.M., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Pforr, J., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vanzella, E., Vergani, D., Capak, P., Charlot, S., Contini, T., Cuby, J.G., De La Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P.W., 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), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), 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 de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )
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QSOS ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Extinction (astronomy) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Cosmology: observation ,Spectral line ,galaxies: high-redshift ,0103 physical sciences ,Galaxy formation and evolution ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Galaxy: evolution ,Line-of-sight ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Cosmic variance ,Astronomy and Astrophysic ,Redshift ,Galaxy ,Cosmology: observations ,Galaxies: high-redshift ,Galaxy: formation ,Large-scale structure of Universe ,Space and Planetary Science ,cosmology: observations ,large-scale structure of Universe ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
(arXiv abridged abstract) The observed UV rest-frame spectra of distant galaxies are the result of their intrinsic emission combined with absorption along the line of sight produced by the inter-galactic medium (IGM). Here we analyse the evolution of the mean IGM transmission Tr(Ly_alpha) and its dispersion along the line of sight for 2127 galaxies with 2.5= 4 compared to results from QSOs, but a degeneracy between dust extinction and IGM prevents to draw firm conclusions if the internal dust extinction for star-forming galaxies at z>4 takes a mean value significantly in excess of E(B-V)>0.15. Most importantly, we find a large dispersion of IGM transmission along the lines of sight towards distant galaxies with 68% of the distribution within 10 to 17% of the median value in delta z=0.5 bins, similar to what is found on the LOS towards QSOs. We demonstrate the importance of taking into account this large range of IGM transmission when selecting high redshift galaxies based on their colour properties (e.g. LBG or photometric redshift selection) or otherwise face a significant incompleteness in selecting high redshift galaxy populations., Comment: 15 pages, 11 figures, submitted to A&A
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- 2017
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17. EAGLE: A MOAO fed multi-IFU NIR workhorse for E-ELT
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Emmanuel Hugot, Peter Hastings, Mark Swinbank, Simon L. Morris, Chris Evans, Richard M. Myers, Nigel Dipper, Damien Gratadour, David Le Mignant, I. Bryson, Clélia Robert, Niraj Welikala, Vincent Lebrun, Pascal Vola, Matthew D. Lehnert, Jean-Luc Gimenez, Fabrice Madec, William Taylor, Martyn Wells, Philippe Laporte, Tim Morris, Mathieu Cohen, Sébastien Vivès, G. Talbot, Benoit Neichel, Jean-Gabriel Cuby, Stephen Beard, Hermine Schnetler, Gérard Rousset, Eric Gendron, P. Jagourel, Zoltan Hubert, P. Parr-Burman, Marc Ferrari, François Vidal, Thierry Fusco, Jean-Philippe Amans, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
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Physics ,Eagle ,Galactic astronomy ,biology ,James Webb Space Telescope ,Astronomy ,Field of view ,law.invention ,Telescope ,law ,biology.animal ,Extremely Large Telescope ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Adaptive optics ,Baseline (configuration management) - Abstract
EAGLE is an instrument under consideration for the European Extremely Large Telescope (E-ELT). EAGLE will be installed at the Gravity Invariant Focal Station of the E-ELT. The baseline design consists of 20 IFUs deployable over a patrol field of ∼40 arcmin2. Each IFU has an individual field of view of ∼ 1.65″ x 1.65″. While EAGLE can operate with the Adaptive Optics correction delivered by the telescope, its full and unrivaled scientific power will be reached with the added value of its embedded Multi-Object Adaptive Optics System (MOAO). EAGLE will be a unique and efficient facility for spatially-resolved, spectroscopic surveys of high-redshift galaxies and resolved stellar populations. We detail the three main science drivers that have been used to specify the top level science requirements. We then present the baseline design of the instrument at the end of Phase A, and in particular its Adaptive Optics System. We show that the instrument has a readiness level that allows us to proceed directly into phase B, and we indicate how the instrument development is planned. © 2010 Copyright SPIE - The International Society for Optical Engineering.
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- 2016
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18. Smart warping harnesses for active mirrors and stress polishing
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Anne Costille, Kjetil Dohlen, Emmanuel Hugot, Michel Marcos, Gabby Kroes, Jean-Luc Beuzit, Jean-Gabriel Cuby, Hermine Schnetler, Z. Challita, and Sabri Lemared
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business.industry ,Computer science ,Mechanical engineering ,Polishing ,Active optics ,02 engineering and technology ,Astigmatism ,medicine.disease ,01 natural sciences ,Finite element method ,010309 optics ,Stress (mechanics) ,020210 optoelectronics & photonics ,Optics ,0103 physical sciences ,0202 electrical engineering, electronic engineering, information engineering ,medicine ,Image warping ,business ,Actuator - Abstract
We present two ways to generate or compensate for first order optical aberrations using smart warping harnesses. In these cases, we used the same methodology leading to replace a previous actuation system currently on-sky and to get a freeform mirror intended to a demonstrator. Starting from specifications, a warping harness is designed, followed by a meshing model in the finite elements software. For the two projects, two different ways of astigmatism generation are presented. The first one, on the VLT-SPHERE instrument, with a single actuator, is able to generate a nearly pure astigmatism via a rotating motorization. Two actuators are sufficient to produce the same aberration for the active freeform mirror, main part of the OPTICON-FAME project, in order to use stress-polishing method.
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- 2016
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19. Integration and testing of the DESI spectrograph prototype
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P. E. Blanc, Patrick N. Jelinsky, A. Elliot, Jean-Gabriel Cuby, K. Honscheid, X. Régal, A. Le Van Suu, G. Castagnoli, S. Ronayette, Anne Ealet, S. Perruchot, A. Secroun, Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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)
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Physics ,Optics ,business.industry ,Integration testing ,[SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Dark energy ,Baryon acoustic oscillations ,business ,Spectroscopy ,7. Clean energy ,Spectrograph ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] - Abstract
International audience; The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation probe. The KPNO Mayall telescope will deliver light to 5000 fibers feeding ten broadband spectrographs. A consortium of Aix-Marseille University (AMU) and CNRS laboratories (LAM, OHP and CPPM) together with the WINLIGHT Systems company (Pertuis-France) has committed to integrate and validate the performance requirements of the full spectrographs, equipped with their cryostats, shutters and other mechanisms. An AIT plan has been defined and dedicated test equipment has been designed and implemented. This equipment simulates the fiber input illumination from the telescope, and offers a variety of continuum and line sources. Flux levels are adjustable and can illuminate one or several fibers along the test slit. It is fully remotely controlled and interfaced to the Instrument Control System. Specific analysis tools have also been developed to verify and monitor the performance and stability of the spectrographs. All these developments are described in details.
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- 2016
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20. MUSE observations of the lensing cluster Abell 1689
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Joel Vernet, J. Lewis, Johan Richard, R. Pello, Jean-Gabriel Cuby, G. Soucail, Anne Verhamme, Benjamin Clément, David J. Lagattuta, Lutz Wisotzki, Peter M. Weilbacher, Roland Bacon, Kurt T. Soto, Sebastiano Cantalupo, D. Bina, Edmund Christian Herenz, V. Patrício, 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), Bina, D, Pello, R, Richard, J, Lewis, J, Patricio, V, Cantalupo, S, Herenz, E, Soto, K, Weilbacher, P, Bacon, R, Vernet, J, Wisotzki, L, Clement, B, Cuby, J, Lagattuta, D, Soucail, G, Verhamme, A, 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)
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Physics ,Very Large Telescope ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Gravitational lensing: strong ,Galaxies: high-redshift ,FOS: Physical sciences ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Multi Unit Spectroscopic Explorer ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Galaxies: clusters: individual: Abell 1689 ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Spectral resolution ,010306 general physics ,010303 astronomy & astrophysics ,Reionization ,Astrophysics::Galaxy Astrophysics ,Luminosity function (astronomy) - Abstract
We present the results obtained with MUSE on the core of the lensing cluster A1689. Integral-field observations with MUSE provide a unique view of the central region, allowing us to conduct a complete census on both cluster galaxies and lensed background sources, identified based on their spectral features without preselection. We investigate the multiple-image configuration for all known sources in the field. Previous to our survey, 28 different lensed galaxies displaying 46 multiple images were known in the MUSE field of view, most of them based on photometric redshifts and lensing considerations. Among them, we spectroscopically confirm 12 images based on their emission-lines, corresponding to 7 different lensed galaxies between z = 0.95 and 5.0. In addition, 14 new galaxies have been spectroscopically identified in this area, with redshifts ranging between 0.8 and 6.2. All background sources within the MUSE field of view correspond to multiple-imaged systems lensed by A1689. 17 sources in total are found at z > 3 based on their Lyman-alpha emission, with Lyman-alpha luminosities ranging between 40.5 < log(Ly{\alpha}) < 42.5 after correction for magnification. This sample is particularly sensitive to the slope of the LF toward the faintest-end. The density of sources obtained in this survey is consistent with a steep value of {\alpha} < -1.5, although this result still needs further investigation. These results illustrate the efficiency of MUSE in the characterization of lensing clusters on one hand, and the study of faint and distant populations of galaxies on the other hand. In particular, our current survey of lensing clusters should provide a unique census of sources responsible for the reionization in a representative volume at z ~ 4-7., Comment: 12 pages, 11 figures
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- 2016
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21. Emission-line-selected galaxies at z=0.6-2 in GOODS South: Stellar masses, SFRs, and large-scale structure
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Bo Milvang-Jensen, Johannes Zabl, Lise Christensen, Jean-Gabriel Cuby, Johan P. U. Fynbo, Benjamin Clément, Wolfram Freudling, Palle Møller, Stefano Zibetti, I. Kochiashvili, Laboratoire de Physique Statistique de l'ENS (LPS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Oncology 54B1, Herlev and Gentofte Hospital, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Green Infrastructure approach: linking environmental with social aspects in studying and managing urban forests, COST, European Cooperation in Science and Technology, 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), 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)
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Physics ,Field (physics) ,010308 nuclear & particles physics ,media_common.quotation_subject ,FOS: Physical sciences ,Astronomy and Astrophysics ,Type-cD galaxy ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Universe ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,H-alpha ,Emission spectrum ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,media_common - Abstract
We have obtained deep NIR narrow and broad (J and Y) band imaging data of the GOODS-South field. The narrow band filter is centered at 1060 nm corresponding to redshifts $z = 0.62, 1.15, 1.85$ for the strong emission lines H$\alpha$, $[$OIII$]$/H$\beta$ and $[$OII$]$, respectively. From those data we extract a well defined sample ($M(AB)=24.8$ in the narrow band) of objects with large emission line equivalent widths in the narrow band. Via SED fits to published broad band data we identify which of the three lines we have detected and assign redshifts accordingly. This results in a well defined, strong emission line selected sample of galaxies down to lower masses than can easily be obtained with only continuum flux limited selection techniques. We compare the (SED fitting-derived) main sequence of star-formation (MS) of our sample to previous works and find that it has a steeper slope than that of samples of more massive galaxies. We conclude that the MS steepens at lower (below $M_{\star} = 10^{9.4} M_{\odot}$) galaxy masses. We also show that the SFR at any redshift is higher in our sample. We attribute this to the targeted selection of galaxies with large emission line equivalent widths, and conclude that our sample presumably forms the upper boundary of the MS. We briefly investigate and outline how samples with accurate redshifts down to those low stellar masses open a new window to study the formation of large scale structure in the early universe. In particular we report on the detection of a young galaxy cluster at $z=1.85$ which features a central massive galaxy which is the candidate of an early stage cD galaxy, and we identify a likely filament mapped out by $[$OIII$]$ and $H\beta$ emitting galaxies at $z=1.15$., Comment: 18 pages, 19 figures, version accepted for publication in A&A
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- 2015
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22. The science case for multi-object spectroscopy on the European ELT
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Chris Evans, Mathieu Puech, Jose Afonso, Omar Almaini, Philippe Amram, Hervé Aussel, Beatriz Barbuy, Alistair Basden, Nate Bastian, Giuseppina Battaglia, Beth Biller, Piercarlo Bonifacio, Nicholas Bouché, Andy Bunker, Elisabetta Caffau, Stephane Charlot, Michele Cirasuolo, Yann Clenet, Francoise Combes, Chris Conselice, Thierry Contini, Jean-Gabriel Cuby, Gavin Dalton, Alex de Koter, Karen Disseau, Jim Dunlop, Benoît Epinat, Fabrizio Fiore, Sofia Feltzing, Annette Ferguson, Hector Flores, Adriano Fontana, Thierry Fusco, Dimitri Gadotti, Anna Gallazzi, Jesus Gallego, Emanuele Giallongo, Thiago Gonçalves, Damien Gratadour, Eike Guenther, Francois Hammer, Vanessa Hill, Marc Huertas-Company, Roridgo Ibata, Lex Kaper, Andreas Korn, Søren Larsen, Olivier Le Fèvre, Bertrand Lemasle, Claudia Maraston, Simona Mei, Yannick Mellier, Simon Morris, Göran Östlin, Thibaut Paumard, Roser Pello, Laura Pentericci, Celine Peroux, Patrick Petitjean, Myriam Rodrigues, Lucía Rodríguez-Muñoz, Daniel Rouan, Hugues Sana, Daniel Schaerer, Eduardo Telles, Scott Trager, Laurence Tresse, Niraj Welikala, Stefano Zibetti, and Bodo Ziegler
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astro-ph.SR ,astro-ph.GA ,astro-ph.IM - Abstract
This White Paper presents the scientific motivations for a multi-object spectrograph (MOS) on the European Extremely Large Telescope (E-ELT). The MOS case draws on all fields of contemporary astronomy, from extra-solar planets, to the study of the halo of the Milky Way and its satellites, and from resolved stellar populations in nearby galaxies out to observations of the earliest 'first-light' structures in the partially-reionised Universe. The material presented here results from thorough discussions within the community over the past four years, building on the past competitive studies to agree a common strategy toward realising a MOS capability on the E-ELT. The cases have been distilled to a set of common requirements which will be used to define the MOSAIC instrument, entailing two observational modes ('high multiplex' and 'high definition'). When combined with the unprecedented sensitivity of the E-ELT, MOSAIC will be the world's leading MOS facility. In analysing the requirements we also identify a high-multiplex MOS for the longer-term plans for the E-ELT, with an even greater multiplex (>1000 targets) to enable studies of large-scale structures in the high-redshift Universe. Following the green light for the construction of the E-ELT the MOS community, structured through the MOSAIC consortium, is eager to realise a MOS on the E-ELT as soon as possible. We argue that several of the most compelling cases for ELT science, in highly competitive areas of modern astronomy, demand such a capability. For example, MOS observations in the early stages of E-ELT operations will be essential for follow-up of sources identified by the James Webb Space Telescope (JWST). In particular, multi-object adaptive optics and accurate sky subtraction with fibres have both recently been demonstrated on sky, making fast-track development of MOSAIC feasible.
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- 2015
23. The VIMOS ultra-deep survey: 10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 < z ≃ 6
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Stéphane Charlot, O. Cucciati, S. de la Torre, G. Zamorani, Peter Capak, Yannick Mellier, Jean-Gabriel Cuby, E. Zucca, Laura Pentericci, V. Sommariva, A. Grazian, Marco Scodeggio, V. Le Brun, L. A. M. Tasca, Olivier Ilbert, Rajat M. Thomas, A. Durkalec, Ricardo Amorín, M. Castellano, P. W. Wang, Mara Salvato, D. Vergani, Letizia P. Cassarà, O. Le Fevre, Daniel Schaerer, Paolo Cassata, A. Cimatti, T. Contini, C. Moreau, E. Vanzella, Brian Lemaux, B. Garilli, S. Bardelli, Adriano Fontana, Yoshiaki Taniguchi, C. Lopez-Sanjuan, Nick Scoville, L. Tresse, M. Giavalisco, S. Fotopoulo, Nimish P. Hathi, Margherita Talia, D. Maccagni, Stéphane Paltani, B. Ribeiro, Le Fèvre, O., Tasca, L.A.M., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Capak, P., Cassarà, L., Castellano, M., Cimatti, A., Cuby, J.G., Cucciati, O., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Lemaux, B.C., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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), and 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)
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Stellar mass ,Large-scale structure of Universe ,Population ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Surveys ,Galaxies: formation ,Lambda ,Cosmology: observation ,Spectral line ,Astrophysics::Solar and Stellar Astrophysics ,[INFO]Computer Science [cs] ,education ,Survey ,Astrophysics::Galaxy Astrophysics ,Cosmology: observations ,Galaxies: evolution ,Galaxies: high-redshift ,Astronomy and Astrophysics ,Space and Planetary Science ,Physics ,education.field_of_study ,Star formation ,Astronomy and Astrophysic ,Redshift survey ,Redshift ,Galaxy ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present the VIMOS Ultra Deep Survey (VUDS), a spectroscopic redshift survey of ~10.000 very faint galaxies to study the major phase of galaxy assembly 2, Comment: 43 pages, 30 figures, submitted to A&A
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- 2015
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24. Hα Spectroscopy of Galaxies atz> 2: Kinematics and Star Formation
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Alice E. Shapley, Charles C. Steidel, Max Pettini, Matthew P. Hunt, Jean-Gabriel Cuby, Dawn K. Erb, Kurt L. Adelberger, and Alan Moorwood
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Physics ,010504 meteorology & atmospheric sciences ,Star formation ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Kinematics ,01 natural sciences ,Galaxy ,Redshift ,Virial theorem ,Space and Planetary Science ,0103 physical sciences ,H-alpha ,Emission spectrum ,Spectroscopy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences - Abstract
We present near-infrared spectroscopy of H-alpha emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 4e10 M_sun. One-dimensional velocity dispersions for the 16 galaxies range from ~50 to ~260 km/s, and in cases where we have both virial masses implied by the velocity dispersions and dynamical masses derived from the spatially extended emission lines, they are in rough agreement. We compare our kinematic results to similar measurements made at z~3, and find that both the observed rotational velocities and velocity dispersions tend to be larger at z~2 than at z~3. We find a mean SFR_H-alpha of 16 M_sun/yr and an average SFR_H-alpha/SFR_UV ratio of 2.4, without correcting for extinction. We see moderate evidence for an inverse correlation between the UV continuum luminosity and the ratio SFR_H-alpha/SFR_UV, such as might be observed if the UV-faint galaxies suffered greater extinction. We discuss the effects of dust and star formation history on the SFRs, and conclude that extinction is the most likely explanation for the discrepancy between the two SFRs.
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- 2003
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25. Discovery of az= 6.17 galaxy from CFHT and VLT observations
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O. Le Fèvre, Jean-Gabriel Cuby, Jean-Charles Cuillandre, H. J. McCracken, B. Meneux, Eugene A. Magnier, European Southern Observatory, 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), INAF-Osservatorio Astronomico di Bologna (OABO), Canada-France-Hawaii Telescope Corporation (CFHT), and National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH)
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Physics ,Narrow-band imaging ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Velocity dispersion ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Redshift ,Galaxy ,Narrow band ,Space and Planetary Science ,Emission spectrum ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Formation rate ,Astrophysics::Galaxy Astrophysics - Abstract
We report the discovery of a galaxy at a redshift z = 6.17 identified from deep narrow band imaging and spectroscopic follow-up in one of the CFHT-VIRMOS deep survey fields at 0226-04. In addition to the existing deep BVRI images of this field, we obtained a very deep narrow band image at 920 nm with the aim of detecting Lyalpha emission at redshift ~ 6.5. Spectroscopic follow-up of some of the candidates selected on the basis of their excess flux in the NB920 filter was performed at the VLT-UT4 with the FORS2 instrument. For one object a strong and asymmetric emission line associated with a strong break in continuum emission is identified as Lyalpha at z = 6.17. This galaxy was selected from its continuum emission in the 920 nm filter rather than for its Lyalpha emission, in effect performing a Lyman Break detection at z = 6.17. We estimate a star formation rate of several tens of M/yr for this object, with a velocity dispersion 400 km/s. The spectroscopic follow-up of other high $z$ galaxy candidates is on-going., Comment: 4 pages, 3 figures, letter. Revised after referee comments. Accepted for publication in A&A
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- 2003
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26. Optical and Infrared Spectroscopy of SN 1999[CLC]ee[/CLC] and SN 1999[CLC]ex[/CLC]
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Nicholas B. Suntzeff, Jose Maza, T. Augusteijn, Leonardo Vanzi, D. J. Pinfield, Christopher Lidman, S. Brillant, Robert Blum, E. Le Floc'h, M. Chadid, Mario Hamuy, Mark M. Phillips, Philip A. Pinto, Knut Olsen, Jean-Gabriel Cuby, Olivier Hainaut, E. Pompei, Valentin D. Ivanov, V. Doublier, and Monika G. Petr-Gotzens
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Physics ,Supernova ,Wavelength ,Space and Planetary Science ,Infrared ,Infrared spectroscopy ,Astronomy and Astrophysics ,Astrophysics ,Absorption (electromagnetic radiation) ,Galaxy - Abstract
We report optical and infrared spectroscopic observations of the Type Ia SN 1999ee and the Type Ib/c SN 1999ex, both of which were hosted by the galaxy IC 5179. For SN 1999ee we obtained a continuous sequence with an unprecedented wavelength and temporal coverage beginning 9 days before maximum light and extending through day 42. Before maximum light SN 1999ee displayed a normal spectrum with a strong Si II 6355 absorption, thus showing that not all slow-declining SNe are spectroscopically peculiar at these evolutionary phases. A comparative study of the infrared spectra of SN 1999ee and other Type Ia supernovae shows that there is a remarkable homogeneity among the Branch-normal SNe Ia during their first 60 days of evolution. SN 1991bg-like objects, on the other hand, display spectroscopic peculiarities at infrared wavelengths. SN 1999ex was characterized by the lack of hydrogen lines, weak optical He I lines, and strong He I 10830,20581, thus providing an example of an intermediate case between pure Ib and Ic supernovae. We conclude therefore that SN 1999ex provides first clear evidence for a link between the Ib and Ic classes and that there is a continuous spectroscopic sequence ranging from the He deficient SNe Ic to the SNe Ib which are characterized by strong optical He I lines.
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- 2002
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27. Discovery of a rich proto-cluster at z = 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)
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Letizia P. Cassarà, Alessandro Cimatti, C. Moreau, Mara Salvato, V. Le Brun, Paolo Cassata, Margherita Talia, Nimish P. Hathi, O. Le Fèvre, Laurence Tresse, S. de la Torre, S. Bardelli, A. Durkalec, Sotiria Fotopoulou, C. López-Sanjuan, Adriano Fontana, P. W. Wang, Yoshiaki Taniguchi, Eros Vanzella, R. Thomas, Thierry Contini, M. Giavalisco, Peter Capak, Stephane Charlot, E. Zucca, Andrea Grazian, B. Ribeiro, G. Zamorani, Olga Cucciati, Yannick Mellier, D. Maccagni, Stéphane Paltani, Marco Castellano, M. Scodeggio, Olivier Ilbert, Ricardo Amorín, Laura Pentericci, N. Z. Scoville, Bianca Garilli, Daniela Vergani, Jean-Gabriel Cuby, Brian C. Lemaux, V. Sommariva, Lidia Tasca, Daniel Schaerer, 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), Cucciati, O., Zamorani, G., Lemaux, B.C., Bardelli, S., Cimatti, A., Le Fèvre, O., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Tasca, L.A.M., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Capak, P., Cassarà, L.P., Castellano, M., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., 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
Physics ,Line-of-sight ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,Radio galaxy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Rest frame ,Astronomy and Astrophysic ,Cosmology: observations ,Galaxies: high-redshift ,Large-scale structure of Universe ,Space and Planetary Science ,Cosmology: observation ,Redshift ,Galaxy ,galaxies: high-redshift ,cosmology: observations ,Galaxy formation and evolution ,[INFO]Computer Science [cs] ,Halo ,large-scale structure of Universe ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,ComputingMilieux_MISCELLANEOUS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
[Abridged] We characterise a massive proto-cluster at z=2.895 that we found in the COSMOS field using the spectroscopic sample of the VIMOS Ultra-Deep Survey (VUDS). This is one of the rare structures at z~3 not identified around AGNs or radio galaxies, so it is an ideal laboratory to study galaxy formation in dense environments. The structure comprises 12 galaxies with secure spectroscopic redshift in an area of 7'x8', in a z bin of Dz=0.016. The measured galaxy number overdensity is delta_g=12+/-2. This overdensity has total mass of M~8.1x10^(14)M_sun in a volume of 13x15x17 Mpc^3. Simulations indicate that such an overdensity at z~2.9 is a proto-cluster that will collapse in a cluster of total mass M~2.5x10^(15)M_sun at z=0. We compare the properties of the galaxies within the overdensity with a control sample at the same z but outside the overdensity. We did not find any statistically significant difference between the properties (stellar mass, SFR, sSFR, NUV-r, r-K) of the galaxies inside and outside the overdensity. The stacked spectrum of galaxies in the overdensity background shows a significant absorption feature at the wavelength of Lya redshifted at z=2.895 (lambda=4736 A), with a rest frame EW = 4+/- 1.4 A. Stacking only background galaxies without intervening sources at z~2.9 along their line of sight, we find that this absorption feature has a rest frame EW of 10.8+/-3.7 A, with a detection S/N of ~4. These EW values imply a high column density (N(HI)~3-20x10^(19)cm^(-2)), consistent with a scenario where such absorption is due to intervening cold gas streams, falling into the halo potential wells of the proto-cluster galaxies. However, we cannot exclude the hypothesis that this absorption is due to the diffuse gas within the overdensity., Comment: 15 pages, 9 figures, accepted for publication in A&A (revised version after referee's comments and language editing)
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- 2014
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28. FAME: Freeform Active Mirrors Experiment: manufacturing process development
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Marc Ferrari, Hermine Schnetler, Jean-Gabriel Cuby, Lars Venema, Emmanuel Hugot, and Z. Challita
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Fine-tuning ,Optics ,Materials science ,business.industry ,Manufacturing process ,Process (computing) ,Millimeter ,Active optics ,Development (differential geometry) ,business ,Residual ,Finite element method - Abstract
Extreme freeform mirrors couple a non-axisymmetrical shape and an extreme asphericity, i.e. more than one millimeter of deviation from the best fit sphere. In astronomical instrumentation, such a large asphericity allows compact instruments, using less optical components. However, the lack of freeform mirrors manufacturing facilities is a real issue. We present the concept and development of an innovative manufacturing process based on plasticity forming which allow imprinting permanent deformations on mirrors, following a pre-defined mold. The aim of this activity, pursued in the frame of the OPTICON-FAME (Freeform Active Mirrors Experiment) project, is to demonstrate the suitability of this method for VIS/NIR/MIR applications. The process developed can operate on thin and flat polished initial substrates. Three study cases have been highlighted by FEA (Finite Element Analysis) and the real tests associated were performed on thin substrates in AISI420b stainless steel with 100 mm optical diameter. A comparison between FEA and tests is performed to study the evolution of the mechanical behaviour and the optical quality. The opto-mechanical results will allow a fine tuning of FEA parameters to optimize the residual form errors obtained through this process to converge toward an innovative and recurrent process.
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- 2014
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29. Discovering extremely compact and metal-poor, star-forming dwarf galaxies out to z ~ 0.9 in the VIMOS Ultra-Deep Survey
- Author
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D. Maccagni, C. López-Sanjuan, Stéphane Paltani, Yoshiaki Taniguchi, Eros Vanzella, Daniela Vergani, Andrea Grazian, O. Le Fèvre, Thierry Contini, Ricardo Amorín, Margherita Talia, M. Giavalisco, Nimish P. Hathi, Peter Capak, G. Zamorani, S. Bardelli, V. Le Brun, Rajat M. Thomas, E. Zucca, Sotiria Fotopoulou, Letizia P. Cassarà, S. de la Torre, P. Cassata, M. Scodeggio, Brian C. Lemaux, N. Z. Scoville, Jean-Gabriel Cuby, Alessandro Cimatti, Bianca Garilli, Adriano Fontana, Laura Pentericci, Laurence Tresse, Mara Salvato, P. W. Wang, B. Ribeiro, Lidia Tasca, A. Durkalec, C. Moreau, V. Sommariva, Daniel Schaerer, Yannick Mellier, Olga Cucciati, Stephane Charlot, Marco Castellano, Olivier Ilbert, Amorín, R., Sommariva, V., Castellano, M., Grazian, A., Tasca, L.A.M., Fontana, A., Pentericci, L., Cassata, P., Garilli, B., Le Brun, V., Le Fèvre, O., Maccagni, D., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Bardelli, S., Capak, P., Cassará, L.P., Cimatti, A., Cuby, J.G., Cucciati, O., De La Torre, S., Durkalec, A., Giavalisco, M., Hathi, N.P., Ilbert, O., Lemaux, B.C., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), 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), and 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)
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Galaxies: fundamental parameters ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,Galaxies: abundances ,Galaxies: fundamental parameter ,FOS: Physical sciences ,Astrophysics ,Photometry (optics) ,Ionization ,Galaxies: dwarf ,Galaxies: evolution ,Galaxies: high-redshift ,Galaxies: starburst ,Astronomy and Astrophysics ,Space and Planetary Science ,[INFO]Computer Science [cs] ,Emission spectrum ,Dwarf galaxy ,Physics ,Star formation ,Astronomy and Astrophysic ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Galaxies: abundance ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We report the discovery of 31 low-luminosity (-14.5 > M_{AB}(B) > -18.8), extreme emission line galaxies (EELGs) at 0.2 < z < 0.9 identified by their unusually high rest-frame equivalent widths (100 < EW[OIII] < 1700 A) as part of the VIMOS Ultra Deep Survey (VUDS). VIMOS optical spectra of unprecedented sensitivity ($I_{AB}$ ~ 25 mag) along with multiwavelength photometry and HST imaging are used to investigate spectrophotometric properties of this unique sample and explore, for the first time, the very low stellar mass end (M* < 10^8 M$_{\odot}$) of the luminosity-metallicity (LZR) and mass-metallicity (MZR) relations at z < 1. Characterized by their extreme compactness (R50 < 1 kpc), low stellar mass and enhanced specific star formation rates (SFR/M* ~ 10^{-9} - 10^{-7} yr^{-1}), the VUDS EELGs are blue dwarf galaxies likely experiencing the first stages of a vigorous galaxy-wide starburst. Using T_e-sensitive direct and strong-line methods, we find that VUDS EELGs are low-metallicity (7.5 < 12+log(O/H) < 8.3) galaxies with high ionization conditions, including at least three EELGs showing HeII 4686A emission and four EELGs of extremely metal-poor (, Letter in A&A 568, L8 (2014). This replacement matches the published version
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- 2014
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30. Design and development of a freeform active mirror for an astronomy application
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Hermine Schnetler, Jean-Gabriel Cuby, Tibor Agócs, Attila Jaskó, Zalpha Challita, L. Mosoni, Lars Venema, Gabby Kroes, Emmanuel Hugot, William D. Taylor, Marc Ferrari, Chris Miller, David Le Mignant, 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)
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Hydroforming ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Computer science ,General Engineering ,FOS: Physical sciences ,Mechanical engineering ,01 natural sciences ,Atomic and Molecular Physics, and Optics ,010309 optics ,Thermoelastic damping ,0103 physical sciences ,Limit (music) ,Development (differential geometry) ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Image resolution - Abstract
The advent of extremely large telescopes will bring unprecedented light-collecting power and spatial resolution, but it will also lead to a significant increase in the size and complexity of focal-plane instruments. The use of freeform mirrors could drastically reduce the number of components in optical systems. Currently, manufacturing issues limit the common use of freeform mirrors at short wavelengths. This article outlines the use of freeform mirrors in astronomical instruments with a description of two efficient freeform optical systems. A new manufacturing method is presented which seeks to overcome the manufacturing issues through hydroforming of thin polished substrates. A specific design of an active array is detailed, which will compensate for residual manufacturing errors, thermoelastic deformation, and gravity-induced errors during observations. The combined hydroformed mirror and the active array comprise the Freeform Active Mirror Experiment, which will produce an accurate, compact, and stable freeform optics dedicated to visible and near-infrared observations., Comment: 11 pages, 12 figures
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- 2014
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31. Active optics for high-dynamic variable curvature mirrors
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Sébastien Vivès, Fabrice Madec, Marc Ferrari, Emmanuel Hugot, Gerard R. Lemaitre, David Le Mignant, Elodie Chardin, and Jean-Gabriel Cuby
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Physics ,Aperture ,business.industry ,FOS: Physical sciences ,Active optics ,Plasticity ,Curvature ,Atomic and Molecular Physics, and Optics ,Finite element method ,Amplitude ,Optics ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,Adaptive optics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Optical aberration - Abstract
Variable curvature mirrors of large amplitude are designed by using finite element analysis. The specific case studied reaches at least a 800 {\mu}m sag with an optical quality better than {\lambda}/5 over a 120 mm clear aperture. We highlight the geometrical nonlinearity and the plasticity effect., Comment: 3 pages, 4 figures
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- 2014
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32. VIMOS Ultra-Deep Survey (VUDS): Witnessing the Assembly of a Massive Cluster at z~3.3
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R. Thomas, Andrea Grazian, Jean-Gabriel Cuby, Daniel Schaerer, S. de la Torre, E. Zucca, Laurence Tresse, Letizia P. Cassarà, Dale D. Kocevski, Marco Castellano, Olivier Ilbert, D. Maccagni, N. Z. Scoville, Ricardo Amorín, Andrea Cimatti, T. Sadibekova, Stéphane Paltani, V. Sommariva, Sotiria Fotopoulou, Lidia Tasca, Stephane Charlot, Thierry Contini, C. López-Sanjuan, A. Durkalec, Margherita Talia, Yannick Mellier, Bianca Garilli, G. Zamorani, S. Bardelli, Olga Cucciati, L. M. Lubin, Daniela Vergani, Adriano Fontana, M. Scodeggio, B. Ribeiro, M. Giavalisco, P. W. Wang, Laura Pentericci, Peter Capak, Nimish P. Hathi, Brian C. Lemaux, V. Le Brun, Paolo Cassata, Yoshiaki Taniguchi, Eros Vanzella, C. Moreau, O. Le Fèvre, Roy R. Gal, Mara Salvato, 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 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 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), 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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Lemaux, B.C., Cucciati, O., Tasca, L.A.M., Le Fèvre, O., Zamorani, G., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Capak, P., Cassarà, L.P., Castellano, M., Cimatti, A., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., Gal, R.R., Kocevski, D.D., López-Sanjuan, C., Lubin, L.M., Mellier, Y., Sadibekova, T., and Scoville, N.
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,galaxies: active ,FOS: Physical sciences ,Astrophysics ,Spectral line ,techniques: photometric ,galaxies: high-redshift ,Coma Cluster ,Galaxies: active ,Galaxies: clusters: general ,Galaxies: evolution ,Galaxies: high-redshift ,Techniques: photometric ,Techniques: spectroscopic ,Astronomy and Astrophysics ,Space and Planetary Science ,Photometric redshift ,media_common ,Physics ,Star formation ,Astronomy and Astrophysic ,Redshift ,Galaxy ,Universe ,galaxies: clusters: general ,Halo ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,techniques: spectroscopic ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we perform a systematic search for overdense environments in the early universe ($z>2$) and report here on the discovery of Cl J0227-0421, a massive protocluster at $z=3.29$. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, $\delta_{gal}=10.5\pm2.8$, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated, by a variety of methods, to be roughly $3\times10^{14}$ $\mathcal{M}_{\odot}$ at $z\sim3.3$, which, evolved to $z=0$ results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally-induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics which are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates amongst and differences in stacked spectra of member galaxies with respect to the field, we defer any conclusions of these trends to future work with the ensemble of protostructures that are found in the full VUDS sample., Comment: 23 pages, 15 figures, 3 tables, accepted for publication in A&A after minor changes, v3/v4 contains an additional online table and minor topical changes
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- 2014
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33. Science case and requirements for the MOSAIC concept for a multi-object spectrograph for the European Extremely Large Telescope
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Damien Gratadour, Elisabetta Caffau, Lex Kaper, James Dunlop, Thierry Contini, Roser Pello, Simon L. Morris, Chris Evans, Bertrand Lemasle, Scott Trager, Anna Gallazzi, Beatriz Barbuy, Philippe Amram, Beth Biller, Simona Mei, Daniel Schaerer, Fabrizio Fiore, Jose Afonso, Stephane Charlot, Hector Flores, Stefano Zibetti, E. Guenther, Daniel Rouan, Herve Aussel, M. Puech, Yannick Mellier, K. Disseau, Alastair Basden, Nate Bastian, Jean-Gabriel Cuby, Markus Roth, Thibaut Paumard, Bodo L. Ziegler, Gavin Dalton, Patrick Petitjean, Claudia Maraston, Giuseppina Battaglia, Nicolas Bouché, Marc Huertas-Company, Yann Clénet, Emanuele Giallongo, Eduardo Telles, Thiago S. Gonçalves, Rodrigo A. Ibata, Thierry Fusco, L. Pentericci, C. J. Conselice, S. S. Larsen, Ben Davies, Vanessa Hill, Francoise Combes, Pascal Jagourel, Francois Hammer, O. Le Fèvre, Dimitri A. Gadotti, Niraj Welikala, Piercarlo Bonifacio, Göran Östlin, Low Energy Astrophysics (API, FNWI), Astronomy, 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 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Services communs OMP (UMS 831), 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 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'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Ramsay, S.K.
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Computer science ,Astronomy ,FOS: Physical sciences ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Field (computer science) ,Galaxy formation and evolution ,Extremely Large Telescope ,Spectroscopy ,Adaptive optics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Spectrograph ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,[PHYS]Physics [physics] ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Exoplanet ,Astrophysics - Solar and Stellar Astrophysics ,Astrophysics of Galaxies (astro-ph.GA) ,ComputingMethodologies_DOCUMENTANDTEXTPROCESSING ,Astrophysics::Earth and Planetary Astrophysics ,SPIE proceedings ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Over the past 18 months we have revisited the science requirements for a multi-object spectrograph (MOS) for the European Extremely Large Telescope (E-ELT). These efforts span the full range of E-ELT science and include input from a broad cross-section of astronomers across the ESO partner countries. In this contribution we summarise the key cases relating to studies of high-redshift galaxies, galaxy evolution, and stellar populations, with a more expansive presentation of a new case relating to detection of exoplanets in stellar clusters. A general requirement is the need for two observational modes to best exploit the large (>40 sq. arcmin) patrol field of the E-ELT. The first mode ('high multiplex') requires integrated-light (or coarsely resolved) optical/near-IR spectroscopy of >100 objects simultaneously. The second ('high definition'), enabled by wide-field adaptive optics, requires spatially-resolved, near-IR of >10 objects/sub-fields. Within the context of the conceptual study for an ELT-MOS called MOSAIC, we summarise the top-level requirements from each case and introduce the next steps in the design process., 17 pages, to be published in Proc SPIE 9147: Ground-based & Airborne Instrumentation for Astronomy V
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- 2014
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34. Photometric and spectroscopic observations of Sycorax, satellite of Uranus
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A. Le Bras, J. Romon, M. A. Barucci, Bernard Schmitt, Sylvain Douté, C. de Bergh, Alain Doressoundiram, and Jean-Gabriel Cuby
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Physics ,Photometry (optics) ,Space and Planetary Science ,Uranus ,Astronomy ,Astronomy and Astrophysics ,Satellite ,Astrophysics ,Centaur ,Spectroscopy ,Reflectivity - Abstract
Sycorax is the brightest of the ve irregular Uranian satellites recently discovered. These satellites are supposed to be captured bodies. We present visible and near-infrared photometry, as well as near-infrared spectroscopy of Sycorax. The overall shape of the spectrum is quite puzzling: it has a red slope in the visible (such as Centaurs and Transneptunian objects), whereas the reflectivity strongly decreases beyond 1 ma nd is rather flat over the near-infrared range. We were not able to reproduce the spectral behaviour of Sycorax using simple materials. A rotational eect is suggested to explain the shape of the spectrum. BVRIJ magnitudes have been measured over a period of 1 hour, with ve V measurements which do not show any strong variation. So only a strong change in the magnitude between the V measurements and the J measurement (30 min later) could explain the shape of the spectrum, but further investigation is required to conclude.
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- 2001
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35. Kinematics of molecular gas in the nucleus of NGC 1068, from H$\boldmath\mathsf{_{2}}$ line emission observed with VLT
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Emmanuel Galliano, O. Marco, Alberto Franceschini, Y. Clénet, Jean-Gabriel Cuby, D. Rouan, Gian Luigi Granato, and Danielle Alloin
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Physics ,Solar mass ,Knot (unit) ,medicine.anatomical_structure ,Space and Planetary Science ,medicine ,Astronomy and Astrophysics ,Kinematics ,Astrophysics ,First order ,Nucleus ,Line (formation) - Abstract
We present results about the distribution and kinematics of the molecular environment of the AGN in NGC1068, over a 1.5'' x 3.5'' region around the central engine in NGC1068, derived from H2 line emission detected with ISAAC at VLT/ANTU on ESO/Paranal. The H2 emitting molecular gas is found to be distributed along the East-West direction and with two main peak emission (knots) located at a distance of about 70 pc from the central engine. The eastern H2 knot is more intense than the western one. The line profiles mapped across the entire 1.5'' x 3.5'' region, at a spatial resolution of 0.3'' x 0.45'', appear to be quite complex with either a blue or red wing. At first order, we find a velocity difference of 140 km/s between the two knots; if interpreted as quasi-keplerian velocity, this implies a central enclosed mass of 10^8 solar masses.
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- 2001
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36. Spatially-resolved dust properties of the GRB 980425 host galaxy
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Darach Watson, S. D. Vergani, Stefano Covino, Dong Xu, Silvia Piranomonte, Maarten Baes, J. Juul Rasmussen, Gianfranco Gentile, Andrea Rossi, Eliana Palazzi, Michał J. Michałowski, A. de Ugarte Postigo, Valerio D'Elia, S. Berta, Nial R. Tanvir, E. Le Floc'h, Diego Götz, Patrizia Ferrero, D. Malesani, Leslie K. Hunt, Jesper Sollerman, P. van der Werf, Jens Hjorth, D. Burlon, Sandra Savaglio, Simone Bianchi, J. M. Castro Cerón, D. Le Borgne, M. P. Koprowski, S. Basa, Tara Murphy, Jean-Gabriel Cuby, Elena Pian, Ghent University [Belgium] (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), European Project: 322307,EC:FP7:PEOPLE,FP7-PEOPLE-2012-CIG,HETRANSIENTS(2012), Universiteit Gent = Ghent University [Belgium] (UGENT), Astrophysics, Astronomy and Astrophysics Research Group, Universiteit Gent = Ghent University (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
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HERSCHEL REFERENCE SURVEY ,submillimeter: galaxies ,galaxies: individual: ESO 184-G82 ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar population ,MASS-METALLICITY RELATION ,Metallicity ,Astrophysics::High Energy Astrophysical Phenomena ,individual: ESO 184-G82 [galaxies] ,galaxies [submillimeter] ,gamma-ray burst: individual: 980425 ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,GAMMA-RAY BURST ,CORE-COLLAPSE SUPERNOVAE ,COMPACT DWARF GALAXIES ,STAR-FORMING GALAXIES ,Astrophysics::Solar and Stellar Astrophysics ,NEARBY GALAXIES ,Astrophysics::Galaxy Astrophysics ,SPITZER-SPACE-TELESCOPE ,Dwarf galaxy ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,GRB 980425 ,ISM [galaxies] ,extinction ,Star formation ,Astronomy and Astrophysics ,Atacama Large Millimeter Array ,Galaxy ,SPECTRAL ENERGY-DISTRIBUTION ,Physics and Astronomy ,13. Climate action ,Space and Planetary Science ,galaxies: star formation ,individual: 980425 [gamma-ray burst] ,LARGE-MAGELLANIC-CLOUD ,dust, extinction ,dust ,Astrophysics::Earth and Planetary Astrophysics ,star formation [galaxies] ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Gamma-ray burst ,galaxies: ISM ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Gamma-ray bursts (GRBs) have been proposed as a tool for studying star formation in the Universe, so it is crucial to investigate whether their host galaxies and immediate environments are in any way special compared with other star-forming galaxies. Here we present spatially resolved maps of dust emission of the host galaxy of the closest known GRB 980425 at z=0.0085 using our new high-resolution observations from Herschel, Atacama Pathfinder Experiment (APEX), Atacama Large Millimeter Array (ALMA) and Australia Telescope Compact Array (ATCA). We modelled the spectral energy distributions of the host and of the star-forming region displaying the Wolf-Rayet signatures in the spectrum (WR region), located 800 pc from the GRB position. The host is characterised by low dust content and a high fraction of UV-visible star formation, similar to other dwarf galaxies. These galaxies are abundant in the local universe, so it is not surprising to find a GRB in one of them, assuming the correspondence between the GRB rate and star formation. The WR region contributes substantially to the host emission at the far-infrared, millimetre, and radio wavelengths and we propose that this is a consequence of its high gas density. If dense environments are also found close to the positions of other GRBs, then the ISM density should also be considered, along with metallicity, an important factor influencing whether a given stellar population can produce a GRB., Comment: Accepted by A&A. 14 pages, 7 figures, 2 tables. V2: minor updates to match the published version
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- 2013
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37. Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62
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B. Clement, Carlos Gomez-Guijarro, L. Rodríguez-Muñoz, Víctor Villar, Jesús Gallego, and Jean-Gabriel Cuby
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Physics ,Luminous infrared galaxy ,010308 nuclear & particles physics ,Star formation ,Extinction (astronomy) ,Astronomy ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Function (mathematics) ,Astrophysics ,01 natural sciences ,Galaxy ,Spectral line ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Luminosity function (astronomy) - Abstract
Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 z α -based studies. Aims. Our main goal is to study the properties of a sample of faint H α emitters at z ~ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 μ m. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V / V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 H α -selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = - 1.46 -0.08 +0.16 . The derived star formation rate density at z ~ 0.62 is ρ SFR = 0.036 -0.008 +0.012 M ⊙ yr -1 Mpc -3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sersic indexes n ~ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ~ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.
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- 2016
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38. Extremely aspheric mirrors: prototype development of an innovative manufacturing process based on active optics
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Emmanuel Hugot, David Le Mignant, Z. Challita, Jean-Gabriel Cuby, Joël Le Merrer, and Marc Ferrari
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Fabrication ,Optics ,Computer science ,business.industry ,Process (computing) ,Mechanical engineering ,Context (language use) ,Active optics ,Work hardening ,Actuator ,business ,Microstructure ,Finite element method - Abstract
The next generation of focal-plane astronomical instruments requires technological breakthroughs to reduce their system complexity while increasing their scientific performances. Applied to the optical systems, recent studies show that the use of freeform reflective optics allows competitive compact systems with less optical components. In this context, our challenge is to supply an active freeform mirror system, using a combination of different active optics techniques. The optical shape will be provided during the fabrication using the mechanical property of metals to plasticize and will be coupled with a specific actuator system to compensate for the residual form errors, during the instrument operation phase. We present in this article the development of an innovative manufacturing process based on cold hydro-forming method, with the aim to adapt it for VIS/NIR requirements in terms of optical surface quality. It can operate on thin and flat polished initial substrates. The realization of a first prototype for a 100 mm optical diameter mirror is in progress, to compare the mechanical behaviours obtained by tests and by Finite Element Analysis (FEA), for different materials. Then, the formed samples will be characterized optically. The opto-mechanical results will allow a fine tuning of FEA parameters to optimize the residual form errors obtained through this process. It concerns the microstructure considerations, the springback effects and the work hardening evolutions of the samples, depending on the initial substrate properties and the boundary conditions applied. Modeling and tests have started with axi-symmetric spherical and aspherical shapes and will continue with highly aspherics and freeforms.
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- 2012
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39. New modelling of freeform surfaces for optical design of astronomical instruments
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Sandrine Pascal, D. Le Mignant, Marc Ferrari, S. Vives, M. Gray, Kjetil Dohlen, and Jean-Gabriel Cuby
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business.industry ,Computer science ,Mechanical engineering ,Context (language use) ,Computer vision ,Artificial intelligence ,Degrees of freedom (mechanics) ,Instrument design ,business ,Focus (optics) ,Bernstein polynomial - Abstract
Freeform optics offer additional degrees of freedom that can lead to a simplification of instrument optical designs with compact solutions. In this context, we propose a new mathematical description of freeform surfaces. This new mathematical formalism, based on the "eigen-modes" of Bernstein polynomials was developed for off-axis highly aspherical surfaces modelling. It allows to take into account different kinds of deformations of the optical surface with local influence capabilities. We present the mathematical formalism developed and then we focus on the optical analysis of an innovative instrument design. The advantages provided by this new modelling are examined.
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- 2012
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40. The Chinese-French SVOM Mission: studying the brightest astronomical explosions
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Jian-Yan Wei, J. A. Paul, Weimin Yuan, Arnaud Claret, Jean-Gabriel Cuby, P. Mandrou, J. Wang, Stéphane Basa, J. P. Osborne, D. Gotz, J-L. Atteia, Zhendong Dai, J. Y. Hu, J. S. Deng, Shuang-Nan Zhang, Y. Dong, B. Cordier, F. Daigne, Yulei Qiu, C. Wu, O. Godet, Didier Barret, and Bobing Wu
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Physics ,Spacecraft ,Spectrometer ,business.industry ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,X-ray telescope ,Astrophysics ,law.invention ,Telescope ,law ,Hard X-rays ,Astrophysics::Earth and Planetary Astrophysics ,business ,Gamma-ray burst - Abstract
We present the SVOM mission that the Chinese National Space Agency and the French Space Agency have decided to jointly implement. SVOM has been designed to detect, characterise and quickly localise gamma-ray bursts (GRBs) and other types of high-energy transients. For this task the spacecraft will carry two widefield high-energy instruments: ECLAIRs, a hard X-ray imager, and the Gamma-Ray Monitor, a broadband spectrometer. Upon localising a transient, SVOM will quickly slew towards the source and start deep followup observations with two narrow-field telescopes: the Micro-channel X-ray Telescope in X-rays and the Visible Telescope in the visible. The nearly anti-solar pointing of SVOM combined with the fast transmission of GRB positions to the ground in less than 1 minute, will facilitate the observations of SVOM transients by the largest ground based telescopes.
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- 2012
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41. The EAGLE instrument for the E-ELT: developments since delivery of Phase A
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Phil Parr-Burman, Simon L. Morris, Chris Evans, Gérard Rousset, Pascal Jagourel, Hermine Schnetler, Marc Dubbeldam, Richard M. Myers, Jean-Gabriel Cuby, Thierry Fusco, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Galactic astronomy ,Computer science ,FOS: Physical sciences ,Astronomy ,First light ,Redshift ,Galaxy ,Integral field spectrograph ,Observatory ,Extremely Large Telescope ,William Herschel Telescope ,Adaptive optics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Spectrograph ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The EAGLE instrument is a Multi-Object Adaptive Optics (MOAO) fed, multiple Integral Field Spectrograph (IFS), working in the Near Infra-Red (NIR), on the European Extremely Large Telescope (E-ELT). A Phase A design study was delivered to the European Southern Observatory (ESO) leading to a successful review in October 2009. Since that time there have been a number of developments, which we summarize here. Some of these developments are also described in more detail in other submissions at this meeting. The science case for the instrument, while broad, highlighted in particular: understanding the stellar populations of galaxies in the nearby universe, the observation of the evolution of galaxies during the period of rapid stellar build-up between redshifts of 2-5, and the search for 'first light' in the universe at redshifts beyond 7. In the last 2 years substantial progress has been made in these areas, and we have updated our science case to show that EAGLE is still an essential facility for the E-ELT. This in turn allowed us to revisit the science requirements for the instrument, confirming most of the original decisions, but with one modification. The original location considered for the instrument (a gravity invariant focal station) is no longer in the E-ELT Construction Proposal, and so we have performed some preliminary analyses to show that the instrument can be simply adapted to work at the E-ELT Nasmyth platform. Since the delivery of the Phase A documentation, MOAO has been demonstrated on-sky by the CANARY experiment at the William Herschel Telescope., 10 pages, SPIE Conference proceedings, Amsterdam, July 2012
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- 2012
42. Active Optics techniques and complex instrumentation for future ELTs
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Fabrice Madec, David Le Mignant, Emmanuel Hugot, Zalpha Challita, Marc Ferrari, Marie Laslandes, and Jean-Gabriel Cuby
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Physics ,Optics ,business.industry ,Extremely Large Telescope ,Active optics ,Instrumentation (computer programming) ,Aerospace engineering ,Manufacturing methods ,business ,Adaptive optics - Abstract
In the frame of the future European Extremely Large Telescope, the Laboratoire d’Astrophysique de Marseille is developing manufacturing methods and complex instrumentation for astronomy, based on the active bending of mirrors.
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- 2012
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43. A complex multi-notch astronomical filter to suppress the bright infrared sky
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Martin M. Roth, Anthony Horton, Sergio G. Leon-Saval, Joss Bland-Hawthorn, Tim A. Birks, Peter Gillingham, Jean-Gabriel Cuby, Simon Ellis, Roger Haynes, Christopher Q. Trinh, Hans-Gerd Löhmannsröben, Stuart D. Ryder, Jon Lawrence, The University of Sydney, Leibniz-Institut für Astrophysik Potsdam (AIP), Universität Potsdam, Australian Astronomical Observatory, 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), University of Bath [Bath], University of Sydney, the Australian Research Council, the Particle Physics and Astronomy Research Council (UK), the Science and Technology Facilities Committee (UK), the Australian Research Council, the Anglo-Australian Observatory, the Konjunkturpaket II (Germany) and the Laboratoire d'Astrophysique Marseille, University of Potsdam = Universität Potsdam, 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)
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Brightness ,Atmospheric chemistry ,Extraterrestrial Environment ,Infrared Rays ,media_common.quotation_subject ,Astronomy ,Astrophysics::High Energy Astrophysical Phenomena ,Night sky ,General Physics and Astronomy ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,7. Clean energy ,Astronomical filter ,General Biochemistry, Genetics and Molecular Biology ,010309 optics ,Optical physics ,0103 physical sciences ,Emission spectrum ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,Photons ,Multidisciplinary ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Spectrum Analysis ,Astronomical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Optical Devices ,General Chemistry ,Galaxies ,Galaxy ,Redshift ,Starlight ,Atmospheric optics ,Sky ,Astronomy and astrophysics ,Institut für Chemie ,Astrophysics - Instrumentation and Methods for Astrophysics ,Telescopes - Abstract
A long-standing and profound problem in astronomy is the difficulty in obtaining deep near-infrared observations due to the extreme brightness and variability of the night sky at these wavelengths. A solution to this problem is crucial if we are to obtain the deepest possible observations of the early Universe since redshifted starlight from distant galaxies appears at these wavelengths. The atmospheric emission between 1000 nm and 1800 nm arises almost entirely from a forest of extremely bright, very narrow hydroxyl emission lines that varies on timescales of minutes. The astronomical community has long envisaged the prospect of selectively removing these lines, while retaining high throughput between the lines. Here we demonstrate such a filter for the first time, presenting results from the first on-sky tests. Its use on current 8m telescopes and future 30m telescopes will open up many new research avenues in the years to come., Comment: 15 pages, 5 figures. Nature Communications. Published 06 December 2011
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- 2011
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44. Modeling highly aspherical optical surfaces using a new polynomial formalism into Zemax
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M. Gray, Jean-Gabriel Cuby, Sandrine Pascal, Sébastien Vivès, D. Le Mignant, A. Secroun, and Marc Ferrari
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symbols.namesake ,Formalism (philosophy of mathematics) ,Mathematical definition ,Zernike polynomials ,Optical surface ,ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION ,symbols ,Calculus ,High order ,Zemax ,Bernstein polynomial ,Computational science ,Mathematics - Abstract
We developed a new mathematical formalism to model highly aspherical optical surfaces opening the possibility to explore innovative optical designs. This formalism is based on Bernstein polynomials allowing to describe from low to high order deformations of the optical surface. It has been implemented into Zemax making use of the User-Defined Surface (UDS-DLL) Zemax capability. In this case, the mathematical definition of the surface is imported into Zemax then allowing to apply classical optimization and analysis functionalities. This paper presents the UDS-DLL tool based on Bernstein polynomials together with an initial optical analysis performed to evaluate the gain obtained in using such a new formalism.
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- 2011
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45. Stellar metallicities beyond the Local Group: the potential of J-band spectroscopy with extremely large telescopes
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Gérard Rousset, Rolf-Peter Kudritzki, M. Puech, Donald F. Figer, Ben Davies, M. D. Lehnert, Jean-Gabriel Cuby, Yunming Yang, Simon L. Morris, Chris Evans, UK Astronomy Technology Centre, Royal Observatory Edinburgh (UKATC), Rochester Institute of Technology, Institute for Astronomy, University of Hawaii, 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), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-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), National Astronomical Observatoires-CAS, 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, University of Durham, South Road, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Royal Observatory Edinburgh (ROE), University of Edinburgh, European Southern Observatory (ESO), Sciences pour l'environnement (SPE), Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Durham University, ANR-06-BLAN-0191,MAUI,The High Redshift Universe & the Mass Assembly of Galaxies: towards a French leadership in the ELT era.(2006), Beaussier, Catherine, 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), Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP), 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.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Metallicity ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,Spectral line ,[SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Red supergiant ,Spectroscopy ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Local Group ,Astronomy and Astrophysics ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Red-giant branch ,Stars ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Supergiant ,Astrophysics - Instrumentation and Methods for Astrophysics ,[PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present simulated J-band spectroscopy of red giants and supergiants with a 42m European Extremely Large Telescope (E-ELT), using tools developed toward the EAGLE Phase A instrument study. The simulated spectra are used to demonstrate the validity of the 1.15-1.22 micron region to recover accurate stellar metallicities from Solar and metal-poor (one tenth Solar) spectral templates. From tests at spectral resolving powers of four and ten thousand, we require continuum signal-to-noise ratios in excess of 50 (per two-pixel resolution element) to recover the input metallicity to within 0.1 dex. We highlight the potential of direct estimates of stellar metallicites (over the range -1, Comment: Accepted by A&A, 13 pages
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- 2011
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46. Using the Bullet Cluster as a Gravitational Telescope to Study z~7 Lyman Break Galaxies
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Douglas Clowe, Massimo Stiavelli, Benjamin Clément, Tommaso Treu, Christine Jones, Anthony H. Gonzalez, Dennis Zaritsky, Marusa Bradac, Jean-Gabriel Cuby, and Nicholas Hall
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Field (physics) ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy ,law.invention ,Telescope ,Gravitation ,Space and Planetary Science ,law ,0103 physical sciences ,Magnitude (astronomy) ,Cluster (physics) ,010303 astronomy & astrophysics ,Wide Field Camera 3 ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Luminosity function (astronomy) - Abstract
We use imaging obtained with the Hubble Space Telescope Wide Field Camera 3 to search for z_850 dropouts at z~7 and J_110 dropouts at z~9 lensed by the Bullet Cluster. In total we find 10 z_850 dropouts in our 8.27 arcmin^2 field. Using magnification maps from a combined weak and strong lensing mass reconstruction of the Bullet Cluster and correcting for estimated completeness levels, we calculate the surface density and luminosity function of our z_850 dropouts as a function of intrinsic (accounting for magnification) magnitude. We find results consistent with published blank field surveys, despite using much shallower data, and demonstrate the effectiveness of cluster surveys in the search for z~7 galaxies., Comment: 12 pages, 2 tables, 9 figures. Accepted for publication in ApJ. V3: two new figures, improved calculation of intrinsic counts, better organization, added references; main results did not change significantly
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- 2011
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47. The bright end of the z ~ 7 UV Luminosity Function from a wide and deep HAWK-I survey
- Author
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Jean-Gabriel Cuby, S. Salimbeni, Andrea Grazian, Filippo Mannucci, Fabrizio Fiore, Alan Moorwood, Benjamin Clément, Emanuele Giallongo, Alvio Renzini, L. Pentericci, Eros Vanzella, Mario Nonino, D. Paris, Adriano Fontana, Nicola Menci, Marco Castellano, K. Boutsia, Rychard Bouwens, Mauro Giavalisco, Vincenzo Testa, S. Gallozzi, Mark Dickinson, Piero Rosati, Stefano Cristiani, Roberto Maiolino, and Paola Santini
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Number density ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Cosmic variance ,01 natural sciences ,Galaxy ,Luminosity ,Space and Planetary Science ,0103 physical sciences ,Magnitude (astronomy) ,010303 astronomy & astrophysics ,Reionization ,Luminosity function (astronomy) ,Photometric redshift ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
(Abridged) We present here the second half of an ESO Large Programme, which exploits the unique combination of area and sensitivity provided in the near-IR by the camera Hawk-I at the VLT. We have obtained - 30 observing hours with Hawk-I in the Y-band of two high galactic latitude fields. We combined the Y-band data with deep J and K Hawk-I observations, and with FORS1/FORS2 U, B, V, R, I, and Z observations to select z-drop galaxies having Z - Y > 1, no optical detection and flat Y - J and Y - K colour terms. We detect 8 high-quality candidates in the magnitude range Y = 25.5 - 26.5 that we add to the z-drop candidates selected in two Hawk-I pointings over the GOODS-South field. We use this full sample of 15 objects found in -161 arcmin^2 of our survey to constrain the average physical properties and the evolution of the number density of z ~ 7 LBGs. A stacking analysis yields a best-fit SED with photometric redshift z= 6.85 +0.20 -0.15 and an E(B-V)=0.05 +0.15 -0.05. We compute a binned estimate of the z ~ 7 LF and explore the effects of photometric scatter and model uncertainties on the statistical constraints. After accounting for the expected incompleteness through MonteCarlo simulations, we strengthen our previous finding that a Schechter luminosity function constant from z=6 to z=7 is ruled out at a >99% confidence level, even including the effects of cosmic variance. For galaxies brighter than M_1500= -19.0, we derive a luminosity density rho_UV = 1.5^{+2.1}{-0.8} x 10^25 erg/s/Hz/Mpc^3, implying a decrease by a factor 3.5 from z=6 to z=6.8. We find that, under standard assumptions, the emission rate of ionizing photons coming from UV bright galaxies is lower by at least a factor of two than the value required for reionization. Finally, we exploit deep Hawk-I J and K band observations to derive an upper limit on the number density of M1500, Comment: 12 pages, 8 figures. Accepted for publication in Astronomy & Astrophysics
- Published
- 2010
48. The circumstellar environment of the YSO TMR-1 and a revisit to the candidate very low-mass object TMR-1C
- Author
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Monika G. Petr-Gotzens, Jean-Gabriel Cuby, Michael D. Smith, Michael Sterzik, 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
Infrared ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,Substellar object ,010306 general physics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Physics ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Star formation ,Near-infrared spectroscopy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Event (particle physics) - Abstract
TMR-1 (IRAS~04361+2547) is a class~I proto-stellar source located in the nearby Taurus star-forming region. Its circumstellar environment is characterized by extended dust emission with complex structures and conspicuous filaments. A faint companion, called TMR-1C, located near the proto-star had been detected in previous studies, but its nature as a very young substellar object remained inconclusive. To improve the constraints on the nature of TMR-1C, and to investigate the process of very low-mass star formation in the TMR-1 system we use very sensitive infrared imaging observations as well as NIR spectroscopy. We construct the SED of TMR-1C over a much larger wavelength range as had been possible in previous work and compare it with models of extincted background stars, young sub-stellar objects, and very low-mass stars with circumstellar disk and envelope emission. We also search for additional low-luminosity objects in the immediate environment of the TMR-1, study the surrounding NIR dust morphology, and analyse the emission line spectrum of a filamentary structure in the physical context of a bow-shock model. We find that the observed SED of TMR-1C is inconsistent with an extincted background star, nor can be fitted with available models for a young extremely low-mass (80deg. Moreover, we detect an additional very faint source, which we call TMR-1D, and that shows a quite striking symmetry in position with TMR-1C. TMR-1C and TMR-1D may have been formed from a common triggered star-formation event, caused by... (abstract abridged), 15 pages, 11 figures, accepted for publication in A&A
- Published
- 2010
- Full Text
- View/download PDF
49. Toward high-dynamic active mirrors for LGS refocusing systems
- Author
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Marc Ferrari, Jean-Gabriel Cuby, Fabrice Madec, Sébastien Vivès, Emmanuel Hugot, and David Le Mignant
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Physics ,Laser guide star ,Optics ,business.industry ,Aperture ,Astrophysics::Instrumentation and Methods for Astrophysics ,Sodium layer ,Curved mirror ,Active optics ,Wavefront sensor ,business ,Focus variation ,Adaptive optics - Abstract
In the frame of the E-ELT-EAGLE instrument phase A studies, we designed a convex VCM able to compensate for the focus variation on the Laser Guide Star (LGS) wavefront sensor, due to the elevation of the telescope and the fixed sodium layer altitude. We present an original optical design including this active convex mirror, providing a large sag variation on a spherical surface with a 120mm clear aperture, with an optical quality better than lambda/5 RMS up to 820μm of sag and better than lambda/4 RMS up to 1000μm of sag. Finite element analysis (FEA) allowed an optimisation of the mirror's variable thickness distribution to compensate for geometrical and material non linearity. Preliminary study of the pre-stressing has also been performed by FEA, showing that a permanent deformation remains after removal of the loads. Results and comparison with the FEA are presented in the article of F.Madec et al (AS10-7736-119, this conference), with an emphasis on the system approach.
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- 2010
- Full Text
- View/download PDF
50. EAGLE MOAO system conceptual design and related technologies
- Author
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M. Cohen, Philippe Laporte, Richard M. Myers, Damien Gratadour, William Taylor, Gérard Rousset, Simon L. Morris, Chris Evans, P. Parr-Burman, D. Le Mignant, F. Assemat, Eric Gendron, T. Fusco, H. Schnetler, Mathieu Puech, Nigel Dipper, Fabrice Vidal, Tim Morris, Jean-Gabriel Cuby, P. Jagourel, M. D. Lehnert, Clélia Robert, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Groupement d'Intérêt Scientifique du Partenariat Haute résolution Angulaire Sol-Espace (GIS PHASE ), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Duke University [Durham], ONERA, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, United Kingdom Astronomy Technology Ctr, 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
Physics ,business.industry ,media_common.quotation_subject ,Astronomy ,Encircled energy ,Deformable mirror ,Stars ,Optics ,Apparent magnitude ,Laser guide star ,Sky ,business ,Adaptive optics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Spectrograph ,media_common - Abstract
International audience; EAGLE is the multi-object spatially-resolved near-IR spectrograph instrument concept for the E-ELT, relying on a distributed Adaptive Optics, so-called Multi Object Adaptive Optics. This paper presents the results of a phase A study. Using 84×84 actuator deformable mirrors, the performed analysis demonstrates that 6 laser guide stars (on an outer ring of 7.2' diameter) and up to 5 natural guide stars of magnitude R < 17, picked-up in a 7.3' diameter patrol field of view, allow us to obtain an overall performance in terms of Ensquared Energy of 35% in a 75×75mas2 resolution element at H band whatever the target direction in the centred 5' science field for median seeing conditions. In terms of sky coverage, the probability to find the 5 natural guide stars is close to 90% at galactic latitudes |b| ~ 60 deg. Several MOAO demonstration activities are also on-going.
- Published
- 2010
- Full Text
- View/download PDF
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