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1. How the StarDICE photometric calibration of standard stars can improve cosmological constraints?

Author

Souverin, T., Neveu, J., Betoule, M., Bongard, S., Blanc, P. E., Tanugi, J. Cohen, Dagoret-Campagne, S., Feinstein, F., Ferrari, M., Hazenberg, F., Juramy, C., Guillou, L. Le, Van Suu, A. Le, Moniez, M., Nuss, E., Plez, B., Regnault, N., Sepulveda, E., and Sommer, K.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The number of type Ia supernova (SNe Ia) observations will grow significantly within the next decade, mainly thanks to the Legacy Survey of Space and Time (LSST) undertaken by the Vera Rubin Observatory in Chile. With this improvement, statistical uncertainties will decrease, and flux calibration will become the main uncertainty for the characterization of dark energy. Currently, the astronomical flux scale is anchored on the numerical models of white dwarf atmospheres from the CALSPEC catalog, and every error on the model can induce a bias over cosmological parameters inference. The StarDICE experiment proposes a new calibration reference that only relies on observations from the optical watt defined by the NIST towards the magnitude of standard stars. It is currently operating at l'Observatoire de Haute-Provence and has been collecting data since the beginning of 2023. To overcome the photometric calibration uncertainty and reach a sub-percent precision, the instrument throughput has been calibrated with a Collimated Beam Projector. It will be monitored on-site with a LED-based artificial star source calibrated with NIST photodiodes. In this proceeding, we will first illustrate how an error in the photometric calibration can impact the SNe Ia distance moduli and thus bias the measurement of cosmological parameters. Then we will present the StarDICE experiment and how we can recalibrate the CALSPEC catalog at the millimagnitude level on the NIST scale with photometric analysis., Comment: 4 pages, 3 figures, contribution to the 2024 Cosmology session of the 58th Rencontres de Moriond

Published
2024

2. StarDICE III: Characterization of the photometric instrument with a Collimated Beam Projector

Author

Souverin, Thierry, Neveu, Jérémy, Betoule, Marc, Bongard, Sébastien, Stubbs, Christopher W., Urbach, Elana, Brownsberger, Sasha, Blanc, Pierre Éric, Tanugi, Johann Cohen, Dagoret-Campagne, Sylvie, Feinstein, Fabrice, Hardin, Delphine, Juramy, Claire, Guillou, Laurent Le, Van Suu, Auguste Le, Moniez, Marc, Plez, Bertrand, Regnault, Nicolas, Sepulveda, Eduardo, Sommer, Kélian, and Collaboration, the LSST Dark Energy Science

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The measurement of type Ia supernovae magnitudes provides cosmological distances, which can be used to constrain dark energy parameters. Large photometric surveys require a substantial improvement in the calibration precision of their photometry to reduce systematic uncertainties in cosmological constraints. The StarDICE experiment is designed to establish accurate broadband flux references for these surveys, aiming for sub-percent precision in magnitude measurements. This requires a precise measurement of the filter bandpasses of both the StarDICE and survey instruments with sub-nanometer accuracy. To that end, we have developed the Collimated Beam Projector (CBP), an optical device capable of calibrating the throughput of an astronomical telescope and of its filters. The CBP is built from a tunable laser source and a reversed telescope to emit a parallel monochromatic light beam that is continuously monitored in flux and wavelength. The CBP output light flux is measured using a large area photodiode, previously calibrated relative to a NIST photodiode. We derive the StarDICE telescope throughput and filter transmissions from the CBP measurements, anchoring it to the absolute calibration provided by the NIST. After analyzing the systematic uncertainties, we achieved sub-nanometer accuracy in determining filter central wavelengths, measured each filter transmission with a precision of 0.5% per 1nm bin, and detected out-of-band leakages at 0.01%. Furthermore, we have synthesized the equivalent transmission for full pupil illumination from four sample positions in the StarDICE telescope mirror, with an accuracy of approximately 0.2nm for central wavelengths and 7mmag for broadband fluxes. We demonstrated our ability to characterize a telescope throughput down to the mmag, and paved the way for future developments, such as a portable CBP version for in-situ transmission monitoring., Comment: 29 pages, 50 figures

Published
2024

3. StarDICE I: sensor calibration bench and absolute photometric calibration of a Sony IMX411 sensor

Author

Betoule, Marc, Antier, Sarah, Bertin, Emmanuel, Blanc, Pierre Éric, Bongard, Sébastien, Tanugi, Johann Cohen, Dagoret-Campagne, Sylvie, Feinstein, Fabrice, Hardin, Delphine, Juramy, Claire, Guillou, Laurent Le, Van Suu, Auguste Le, Moniez, Marc, Neveu, Jérémy, Nuss, Éric, Plez, Bertrand, Regnault, Nicolas, Sepulveda, Eduardo, Sommer, Kélian, Souverin, Thierry, and Wang, Xiao Feng

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Hubble diagram of type-Ia supernovae (SNe-Ia) provides cosmological constraints on the nature of dark energy with an accuracy limited by the flux calibration of currently available spectrophotometric standards. The StarDICE experiment aims at establishing a 5-stage metrology chain from NIST photodiodes to stars, with a targeted accuracy of \SI{1}{mmag} in $griz$ colors. We present the first two stages, resulting in the calibration transfer from NIST photodiodes to a demonstration \SI{150}{Mpixel} CMOS sensor (Sony IMX411ALR as implemented in the QHY411M camera by QHYCCD). As a side-product, we provide full characterization of this camera. A fully automated spectrophotometric bench is built to perform the calibration transfer. The sensor readout electronics is studied using thousands of flat-field images from which we derive stability, high resolution photon transfer curves and estimates of the individual pixel gain. The sensor quantum efficiency is then measured relative to a NIST-calibrated photodiode. Flat-field scans at 16 different wavelengths are used to build maps of the sensor response. We demonstrate statistical uncertainty on quantum efficiency below \SI{0.001}{e^-/\gamma} between \SI{387}{nm} and \SI{950}{nm}. Systematic uncertainties in the bench optics are controlled at the level of \SI{1e-3}{e^-/\gamma}. Uncertainty in the overall normalization of the QE curve is 1\%. Regarding the camera we demonstrate stability in steady state conditions at the level of \SI{32.5}{ppm}. Homogeneity in the response is below \SI{1}{\percent} RMS across the entire sensor area. Quantum efficiency stays above \SI{50}{\percent} in most of the visible range, peaking well above \SI{80}{\percent} between \SI{440}{nm} and \SI{570}{nm}. Differential non-linearities at the level of \SI{1}{\percent} are detected. A simple 2-parameter model is proposed to mitigate the effect., Comment: accepted for publication in A&A, correct author list

Published
2022
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4. Measurement of telescope transmission using a Collimated Beam Projector

Author

Souverin, Thierry, Neveu, Jérémy, Betoule, Marc, Bongard, Sébastien, Brownsberger, Sasha, Cohen-Tanugi, Johann, Dagoret-Campagne, Sylvie, Feinstein, Fabrice, Juramy, Claire, Guillou, Laurent Le, Van Suu, Auguste Le, Blanc, Pierre Eric, Hazenberg, François, Nuss, Eric, Plez, Bertrand, Sepulveda, Eduardo, Sommer, Kélian, Stubbs, Christopher, Regnault, Nicolas, and Urbach, Elana

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The number of type Ia supernova observations will see a significant growth within the next decade, especially thanks to the Legacy Survey of Space and Time undertaken by the Vera Rubin Observatory in Chile. With this rise, the statistical uncertainties will decrease and the flux calibration will become the main uncertainty for the characterization of dark energy. The uncertainty over the telescope transmission is a major systematic when measuring SNe Ia colors. Here we introduce the Collimated Beam Projector (CBP), a device that can measure the transmission of a telescope and its filters. Composed of a tunable monochromatic light source and optics to provide a parallel output beam this device is able to measure with high precision the filter transmissions. In the following, we will show how measuring precisely a telescope transmission can also improve the precision of the dark energy parameters. As an example, we will present the first results of the CBP in the context of the StarDice experiment., Comment: 2 pages, 2 figures, contribution to the 2022 Cosmology session of the 56th Rencontres de Moriond

Published
2022
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5. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author

Abareshi, B., Aguilar, J., Ahlen, S., Alam, Shadab, Alexander, David M., Alfarsy, R., Allen, L., Prieto, C. Allende, Alves, O., Ameel, J., Armengaud, E., Asorey, J., Aviles, Alejandro, Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Beltran, S. F., Benavides, B., BenZvi, S., Berti, A., Besuner, R., Beutler, Florian, Bianchi, D., Blake, C., Blanc, P., Blum, R., Bolton, A., Bose, S., Bramall, D., Brieden, S., Brodzeller, A., Brooks, D., Brownewell, C., Buckley-Geer, E., Cahn, R. N., Cai, Z., Canning, R., Rosell, A. Carnero, Carton, P., Casas, R., Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chuang, C., Circosta, C., Cole, S., Cooper, A. P., da Costa, L., Cousinou, M. -C., Cuceu, A., Davis, T. M., Dawson, K., de la Cruz-Noriega, R., de la Macorra, A., de Mattia, A., Della Costa, J., Demmer, P., Derwent, M., Dey, A., Dey, B., Dhungana, G., Ding, Z., Dobson, C., Doel, P., Donald-McCann, J., Donaldson, J., Douglass, K., Duan, Y., Dunlop, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Enriquez-Vargas, M., Escoffier, S., Evatt, M., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Romero, J. E., Frenk, C. S., Fromenteau, S., Gänsicke, B. T., Garcia-Quintero, C., Garrison, L., Gaztañaga, E., Gerardi, F., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, Alma X., Gonzalez-de-Rivera, G., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Grove, C., Gruen, D., Gutierrez, G., Guy, J., Hahn, C., Harris, S., Herrera, D., Herrera-Alcantar, Hiram K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jelinsky, P., Jiang, L., Jimenez, J., Jing, Y. P., Joyce, R., Jullo, E., Juneau, S., Karaçaylı, N. G., Karamanis, M., Karcher, A., Karim, T., Kehoe, R., Kent, S., Kirkby, D., Kisner, T., Kitaura, F., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, Alex, L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, Ting-Wen, Landriau, M., Lane, S., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Van Suu, A. Le, Levi, Michael E., Li, T. S., Magneville, C., Manera, M., Manser, Christopher J., Marshall, B., McCollam, W., McDonald, P., Meisner, Aaron M., Mezcua, J. Mena-Fernández M., Miller, T., Miquel, R., Montero-Camacho, P., Moon, J., Martini, J. Paul, Meneses-Rizo, J., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, Andrea, Myers, Adam D., Nadathur, S., Najita, J., Napolitano, L., Neilsen, E., Newman, Jeffrey A., Nie, J. D., Ning, Y., Niz, G., Norberg, P., Noriega, Hernán E., O'Brien, T., Obuljen, A., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Pappalardo, D., Peng, X., Percival, W. J., Perruchot, S., Pogge, R., Poppett, C., Porredon, A., Prada, F., Prochaska, J., Pucha, R., Pérez-Fernández, A., Pérez-Ráfols, I., Rabinowitz, D., Raichoor, A., Ramirez-Solano, S., Ramírez-Pérez, César, Ravoux, C., Reil, K., Rezaie, M., Rocher, A., Rockosi, C., Roe, N. A., Roodman, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Safonova, S., Said, K., Saintonge, A., Catonga, Javier Salas, Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E., Schlegel, D., Schmoll, J., Scholte, D., Schubnell, M., Secroun, A., Seo, H., Serrano, S., Sharples, Ray M., Sholl, Michael J., Silber, Joseph Harry, Silva, D. R., Sirk, M., Siudek, M., Smith, A., Sprayberry, D., Staten, R., Stupak, B., Tan, T., Tarlé, Gregory, Tie, Suk Sien, Tojeiro, R., Ureña-López, L. A., Valdes, F., Valenzuela, O., Valluri, M., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, C., Wechsler, R., Wilson, Michael J., Yang, J., Yu, Y., Yuan, S., Yèche, Christophe, Zhang, H., Zhang, K., Zhao, Cheng, Zhou, Rongpu, Zhou, Zhimin, Zou, H., Zou, J., Zou, S., and Zu, Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt{\AA} > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged), Comment: 78 pages, 32 figures, submitted to AJ

Published
2022
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6. Testing the 10 spectrograph units for DESI: approach and results

Author

Perruchot, S., Blanc, P. -E., Guy, J., Guillou, L. Le, Ronayette, S., Régal, X., Castagnoli, G., Van Suu, A. Le, Sepulveda, E., Jullo, E., Cuby, J. -G., Karkar, S., Ghislain, P., Repain, P., Carton, P. -H., Magneville, C., Ealet, A., Escoffier, S., Secroun, A., Honscheid, K., Elliot, A., Jelinsky, P., Brooks, D., Doel, P., Duan, Y., Edelstein, J., Estrada, J. C., Gastañaga, E., Karcher, A., Landriau, M., Levi, M., Martini, P., Palanque-Delabrouille, N., Prada, F., Tarle, G., and Zhang, K.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sqdeg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers 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, IN2P3, Sorbonne Universit\'e and Universit\'e de Paris) and the WINLIGHT Systems company based in Pertuis (France), were in charge of integrating and validating the performance requirements of the ten full spectrographs, equipped with their cryostats, shutters and other mechanisms. We present a summary of our activity which allowed an efficient validation of the systems in a short-time schedule. We detail the main results. We emphasize the benefits of our approach and also its limitations., Comment: 20 pages, 16 figures, in 2020 SPIE Astronomical Telescopes + Instrumentation conference proceedings

Published
2021
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7. Potential asteroid discoveries by the ESA Gaia mission: Results from follow-up observations

Author

Carry, B., Thuillot, W., Spoto, F., David, P., Berthier, J., Tanga, P., Mignard, F., Bouquillon, S., Mendez, R . A., Rivet, J. -P., Van Suu, A. Le, Dell'Oro, A., Fedorets, G., Frezouls, B., Granvik, M., Guiraud, J., Muinonen, K., Panem, C., Pauwels, T., Roux, W., Walmsley, G., Petit, J. -M., Abe, L., azian, V. Ayv, Baillié, K., Baransky, A., Bendjoya, P., Dennefeld, M., Desmars, J., Eggl, S., Godunova, V., Hestroffer, D ., Inasaridze, R., Kashuba, V., Krugly, Y. N., Molotov, I. E., Robert, V., Simon, A., Sokolov, I., Souami, D., Tarady, V., Taris, F., Troianskyi, V., Vasylenko, V., and Vernet, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Since July 2014, the ESA Gaia mission has been surveying the entire sky down to magnitude 20.7 in the visible. In addition to the millions of stars, thousands of Solar System Objects (SSOs) are observed daily. By comparing their positions to those of known objects, a daily processing pipeline filters known objects from potential discoveries. However, owing to Gaia's specific scanning law designed for stars, potential newly discovered moving objects are characterized by very few observations, acquired over a limited time. This aspect was recognized early in the design of the Gaia data processing. A daily processing pipeline dedicated to these candidate discoveries was set up to release calls for observations to a network of ground-based telescopes. Their aim is to acquire follow-up astrometry and to characterize these objects. From the astrometry measured by Gaia, preliminary orbital solutions are determined, allowing to predict the position of these potentially new discovered objects in the sky accounting for the large parallax between Gaia and the Earth (separated by 0.01 au). A specific task within the Gaia Consortium has been responsible for the distribution of requests for follow-up observations of potential Gaia SSO discoveries. Since late 2016, these calls for observations (called alerts) are published daily via a Web interface, freely available to anyone world-wide. Between November 2016 and July 2020, over 1700 alerts have been published, leading to the successful recovery of more than 200 objects. Among those, six have provisional designation assigned with the Gaia observations, the others being previously known objects with poorly characterized orbits, precluding identification at the time of Gaia observations. There is a clear trend for objects with a high inclination to be unidentified, revealing a clear bias in the current census of SSOs against high inclination populations., Comment: Submitted to Astronomy & Astrophysics

Published
2020
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8. Overview of the DESI Legacy Imaging Surveys

Author

Dey, Arjun, Schlegel, David J., Lang, Dustin, Blum, Robert, Burleigh, Kaylan, Fan, Xiaohui, Findlay, Joseph R., Finkbeiner, Doug, Herrera, David, Juneau, Stephanie, Landriau, Martin, Levi, Michael, McGreer, Ian, Meisner, Aaron, Myers, Adam D., Moustakas, John, Nugent, Peter, Patej, Anna, Schlafly, Edward F., Walker, Alistair R., Valdes, Francisco, Weaver, Benjamin A., Zou, Christophe Yeche Hu, Zhou, Xu, Abareshi, Behzad, Abbott, T. M. C., Abolfathi, Bela, Aguilera, C., Alam, Shadab, Allen, Lori, Alvarez, A., Annis, James, Ansarinejad, Behzad, Aubert, Marie, Beechert, Jacqueline, Bell, Eric F., BenZvi, Segev Y., Beutler, Florian, Bielby, Richard M., Bolton, Adam S., Buckley-Geer, Cesar Briceno Elizabeth J., Butler, Karen, Calamida, Annalisa, Carlberg, Raymond G., Carter, Paul, Casas, Ricard, Castander, Francisco J., Choi, Yumi, Comparat, Johan, Cukanovaite, Elena, Delubac, Timothee, DeVries, Kaitlin, Dey, Sharmila, Dhungana, Govinda, Dickinson, Mark, Ding, Zhejie, Donaldson, John B., Duan, Yutong, Duckworth, Christopher J., Eftekharzadeh, Sarah, Eisenstein, Daniel J., Etourneau, Thomas, Fagrelius, Parker A., Farihi, Jay, Fitzpatrick, Mike, Font-Ribera, Andreu, Fulmer, Leah, Gansicke, Boris T., Gaztanaga, Enrique, George, Koshy, Gerdes, David W., Gontcho, Satya Gontcho A, Gorgoni, Claudio, Green, Gregory, Guy, Julien, Harmer, Diane, Hernandez, M., Honscheid, Klaus, Lijuan, Huang, James, David, Jannuzi, Buell T., Jiang, Linhua, Joyce, Richard, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kneib, Jean-Paul, Kueter-Young, Andrea, Lan, Ting-Wen, Lauer, Tod, Guillou, Laurent Le, Van Suu, Auguste Le, Lee, Jae Hyeon, Lesser, Michael, Levasseur, Laurence Perreault, Li, Ting S., Mann, Justin L., Marshall, Bob, Martinez-Vazquez, C. E., Martini, Paul, Bourboux, Helion du Mas des, McManus, Sean, Meier, Tobias Gabriel, Menard, Brice, Metcalfe, Nigel, Munoz-Gutierrez, Andrea, Najita, Joan, Napier, Kevin, Narayan, Gautham, Newman, Jeffrey A., Nie, Jundan, Nord, Brian, Norman, Dara J., Olsen, Knut A. G., Paat, Anthony, Palanque-Delabrouille, Nathalie, Peng, Xiyan, Poppett, Claire L., Poremba, Megan R., Prakash, Abhishek, Rabinowitz, David, Raichoor, Anand, Rezaie, Mehdi, Robertson, A. N., Roe, Natalie A., Ross, Ashley J., Ross, Nicholas P., Rudnick, Gregory, Safonova, Sasha, Saha, Abhijit, Sanchez, F. Javier, Savary, Elodie, Schweiker, Heidi, Scott, Adam, Seo, Hee-Jong, Shan, Huanyuan, Silva, David R., Slepian, Zachary, Soto, Christian, Sprayberry, David, Staten, Ryan, Stillman, Coley M., Stupak, Robert J., Summers, David L., Tie, Suk Sien, Tirado, H., Vargas-Magana, Mariana, Vivas, A. Katherina, Wechsler, Risa H., Williams, Doug, Yang, Jinyi, Yang, Qian, Yapici, Tolga, Zaritsky, Dennis, Zenteno, A., Zhang, Kai, Zhang, Tianmeng, Zhou, Rongpu, and Zhou, Zhimin

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The DESI Legacy Imaging Surveys are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image approximately 14,000 deg^2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12 and 22 micorons) observed by the Wide-field Infrared Survey Explorer (WISE) satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project., Comment: 47 pages, 18 figures; accepted for publication in the Astronomical Journal

Published
2018
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9. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author

DESI Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de la Macorra, Axel, De Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, Van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, MacCrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, McCauley, Jeremy, McDonald, Patrick, McGreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Zu, Ying

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

Published
2016

10. The DESI Experiment Part II: Instrument Design

Author

DESI Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de la Macorra, Axel, De Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, Van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, MacCrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, McCauley, Jeremy, McDonald, Patrick, McGreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Zu, Ying

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.

Published
2016

11. Murchison Widefield Array Limits on Radio Emission from ANTARES Neutrino Events

Author

Croft, S., Kaplan, D. L., Tingay, S. J., Murphy, T., Bell, M. E., Rowlinson, A., Adrian-Martinez, S., Ageron, M., Albert, A., Andre, M., Anton, G., Ardid, M., Aubert, J. -J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Bertin, V., Biagi, S., Bormuth, R., Bouwhuis, M. C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Chiarusi, T., Circella, M., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Dekeyser, I., Deschamps, A., De Bonis, G., Distefano, C., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Bojaddaini, I. El, Elsasser, D., Enzenhofer, A., Fehn, K., Felis, I., Fermani, P., Fusco, L. A., Galata, S., Gay, P., Geisselsoder, S., Geyer, K., Giordano, V., Gleixner, A., Glotin, H., Gracia-Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Hugon, C., James, C. W, de Jong, M., Kadler, M., Kalekin, O., Katz, U., Kiessling, D., Kooijman, P., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mathieu, A., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Nezri, E., Pavalas, G. E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Racca, C., Riccobene, G., Roensch, K., Saldana, M., Samtleben, D. F. E., Sanchez-Losa, A., Sanguineti, M., Sapienza, P., Schmid, J., Schnabel, J., Schussler, F., Seitz, T., Sieger, C., Spurio, M., Steijger, J. J. M., Stolarczyk, T., Taiuti, M., Tamburini, C., Trovato, A., Tselengidou, M., Turpin, D., Tonnis, C., Vallage, B., Vallee, C., Van Elewyck, V., Visser, E., Vivolo, D., Wagner, S., Wilms, J., Zornoza, J. D., Zuniga, J., Klotz, A., Boer, M., Van Suu, A. Le, Akerlof, C., and Zheng, W.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a search, using the Murchison Widefield Array (MWA), for electromagnetic counterparts to two candidate high energy neutrino events detected by the ANTARES neutrino telescope in 2013 November and 2014 March. These events were selected by ANTARES because they are consistent, within 0.4 degrees, with the locations of galaxies within 20 Mpc of Earth. Using MWA archival data at frequencies between 118 and 182 MHz, taken ~20 days prior to, at the same time as, and up to a year after the neutrino triggers, we look for transient or strongly variable radio sources consistent with the neutrino positions. No such counterparts are detected, and we set a 5 sigma upper limit for low-frequency radio emission of ~1E37 erg/s for progenitors at 20 Mpc. If the neutrino sources are instead not in nearby galaxies, but originate in binary neutron star coalescences, our limits place the progenitors at z > 0.2. While it is possible, due to the high background from atmospheric neutrinos, that neither event is astrophysical, the MWA observations are nevertheless among the first to follow up neutrino candidates in the radio, and illustrate the promise of wide-field instruments like MWA to detect electromagnetic counterparts to such events., Comment: 7 pages, 2 figures, accepted for publication in ApJL

Published
2016
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12. Optical and X-ray early follow-up of ANTARES neutrino alerts

Author

Adrian-Martinez, S., Ageron, M., Albert, A., Samarai, I. Al, Andre, M., Anton, G., Ardid, M., Aubert, J. -J., Baret, B., Barrios-Marti, J., Basa, S., Bertin, V., Biagi, S., Bogazzi, C., Bormuth, R., Bou-Cabo, M., Bouwhuis, M. C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Chiarusi, T., Circella, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Dekeyser, I., Deschamps, A., De Bonis, G., Distefano, C., Donzaud, C., Dornic, D., Drouhin, D., Dumas, A., Eberl, T., Elsasser, D., Enzenhofer, A., Fehn, K., Felis, I., Fermani, P., Folger, F., Fusco, L. A., Galata, S., Gay, P., Geißelsoder, S., Geyer, K., Giordano, V., Gleixner, A., Gracia-Ruiz, R., Graf, K., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Herrero, A., Hoßl, J., Hofestadt, J., Hugon, C., James, C. W, de Jong, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kooijman, P., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lambard, G., Lattuada, D., Lefevre, D., Leonora, E., Loucatos, S., Mangano, S., Marcelin, M., Margiotta, A., Martinez-Mora, J. A., Martini, S., Mathieu, A., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Neff, M., Nezri, E., Pavalas, G. E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Racca, C., Riccobene, G., Richter, R., Roensch, K., Rostovtsev, A., Saldana, M., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schmid, J., Schnabel, J., Schulte, S., Schüssler, F., Seitz, T., Sieger, C., Spurio, M., Steijger, J. J. M., Stolarczyk, Th., Sanchez-Losa, A., Taiuti, M., Tamburini, C., Trovato, A., Tselengidou, M., Tonnis, C., Turpin, D., Vallage, B., Vallee, C., Van Elewyck, V., Vecchi, M., Visser, E., Vivolo, D., Wagner, S., Wilms, J., Zornoza, J. D., Zuniga, J., Klotz, A., Boer, M., Van Suu, A. Le, Akerlof, C., Zheng, W., Evans, P., Gehrels, N., Kennea, J., Osborne, J. P., and Coward, D. M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. Even with the recent detection of extraterrestrial high-energy neutrinos by the IceCube experiment, no astrophysical neutrino source has yet been discovered. Transient sources, such as gamma-ray bursts, core-collapse supernovae, or active galactic nuclei are promising candidates. Multi-messenger programs offer a unique opportunity to detect these transient sources. By combining the information provided by the ANTARES neutrino telescope with information coming from other observatories, the probability of detecting a source is enhanced, allowing the possibility of identifying a neutrino progenitor from a single detected event. A method based on optical and X-ray follow-ups of high-energy neutrino alerts has been developed within the ANTARES collaboration. This program, denoted as TAToO, triggers a network of robotic optical telescopes (TAROT and ROTSE) and the Swift-XRT with a delay of only a few seconds after a neutrino detection, and is therefore well-suited to search for fast transient sources. To identify an optical or X-ray counterpart to a neutrino signal, the images provided by the follow-up observations are analysed with dedicated pipelines. A total of 42 alerts with optical and 7 alerts with X-ray images taken with a maximum delay of 24 hours after the neutrino trigger have been analysed. No optical or X-ray counterparts associated to the neutrino triggers have been found, and upper limits on transient source magnitudes have been derived. The probability to reject the gamma-ray burst origin hypothesis has been computed for each alert.

Published
2015
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13. The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica

Author

Abe, L., Gonçalves, I., Agabi, A., Alapini, A., Guillot, T., Mékarnia, D., Rivet, J. -P., Schmider, F. -X., Crouzet, N., Fortney, J., Pont, F., Barbieri, M., Daban, J. -B., Fanteï-Caujolle, Y., Gouvret, C., Bresson, Y., Roussel, A., Bonhomme, S., Robini, A., Dugué, M., Bondoux, E., Péron, S., Petit, P. -Y., Szulágyi, J., Fruth, T., Erikson, A., Rauer, H., Fressin, F., Valbousquet, F., Blanc, P. -E., van Suu, A. Le, and Aigrain, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. The WASP-19 system was observed during 24 nights in May 2010. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and larger than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 +/- 0.5 days, in agreement with the SuperWASP determination of 10.5 +/- 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q'star > 3.10^7. Separately, we find evidence for a secondary eclipse of depth 390 +/- 190 ppm with a 2.0 sigma significance, a phase consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day side brightness temperature of 2690(-220/+150) K, in line with measurements in the z' and K bands. The day side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side, or to direct reflection of stellar light with a maximum geometrical albedo Ag=0.27 +/- 0.13. We also report a low-frequency oscillation well in phase at the planet orbital period, but with a lower-limit amplitude that could not be attributed to the planet phase alone, and possibly contaminated with residual lightcurve trends., Comment: Accepted for publication in Astronomy and Astrophysics, 13 pages, 13 figures

Published
2013
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14. The Positioning System of the ANTARES Neutrino Telescope

Author

Adrián-Martínez, S., Ageron, M., Aguilar, J. A., Samarai, I. Al, Albert, A., André, M., Anghinolfi, M., Anton, G., Anvar, S., Ardid, M., Jesus, A. C. Assis, Astraatmadja, T., Aubert, J. -J., Baret, B., Basa, S., Bertin, V., Biagi, S., Bigi, A., Bigongiari, C., Bogazzi, C., Bou-Cabo, M., Bouhou, B., Bouwhuis, M. C., Brunner, J., Busto, J., Camarena, F., Capone, A., Carloganu, C., Carminati, G., Carr, J., Cecchini, S., Charif, Z., Charvis, Ph., Chiarusi, T., Circella, M., Coniglione, R., Costantini, H., Coyle, P., Curtil, C., De Bonis, G., Decowski, M. P., Dekeyser, I., Deschamps, A., Distefano, C., Donzaud, C., Dornic, D., Dorosti, Q., Drouhin, D., Eberl, T., Emanuele, U., Enzenhöfer, A., Ernenwein, J. -P., Escoffier, S., Fermani, P., Ferri, M., Flaminio, V., Folger, F., Fritsch, U., Fuda, J. -L., Galatá, S., Gay, P., Giacomelli, G., Giordano, V., Gómez-González, J. P., Graf, K., Guillard, G., Halladjian, G., Hallewell, G., van Haren, H., Hartman, J., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Herold, B., Hößl, J., Hsu, C. C., de Jong, M., Kadler, M., Kalekin, O., Kappes, A., Katz, U., Kavatsyuk, O., Keller, P., Kooijman, P., Kopper, C., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lamare, P., Larosa, G., Lattuada, D., Lefévre, D., Van Suu, A. Le, Lim, G., Presti, D. Lo, Loehner, H., Loucatos, S., Mangano, S., Marcelin, M., Margiotta, A., Martínez-Mora, J. A., Meli, A., Montaruli, T., Moscoso, L., Motz, H., Neff, M., Nezri, E., Niess, V., Palioselitis, D., Păvălaş, G. E., Payet, K., Payre, P., Petrovic, J., Piattelli, P., Picot-Clemente, N., Popa, V., Pradier, T., Presani, E., Racca, C., Real, D., Reed, C., Riccobene, G., Richardt, C., Richter, R., Rivière, C., Robert, A., Roensch, K., Rostovtsev, A., Ruiz-Rivas, J., Rujoiu, M., Russo, G. V., Salesa, F., Samtleben, D. F. E., Schöck, F., Schuller, J. -P., Schüssler, F., Seitz, T., Shanidze, R., Simeone, F., Spies, A., Spurio, M., Steijger, J. J. M., Stolarczyk, Th., Sánchez-Losa, A., Taiuti, M., Tamburini, C., Toscano, S., Vallage, B., Van Elewyck, V., Vannoni, G., Vecchi, M., Vernin, P., Wagner, S., Wijnker, G., Wilms, J., de Wolf, E., Yepes, H., Zaborov, D., Zornoza, J. D., and Zúñiga, J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The ANTARES neutrino telescope, located 40km off the coast of Toulon in the Mediterranean Sea at a mooring depth of about 2475m, consists of twelve detection lines equipped typically with 25 storeys. Every storey carries three optical modules that detect Cherenkov light induced by charged secondary particles (typically muons) coming from neutrino interactions. As these lines are flexible structures fixed to the sea bed and held taut by a buoy, sea currents cause the lines to move and the storeys to rotate. The knowledge of the position of the optical modules with a precision better than 10cm is essential for a good reconstruction of particle tracks. In this paper the ANTARES positioning system is described. It consists of an acoustic positioning system, for distance triangulation, and a compass-tiltmeter system, for the measurement of the orientation and inclination of the storeys. Necessary corrections are discussed and the results of the detector alignment procedure are described.

Published
2012
Full Text
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15. Neutrino detection of transient sources with optical follow-up observations

Author

D, D. Dornic, Basa, S., Brunner, J., Busto, J., Klotz, A., Boer, M., Escoffier, S., Vallage, B., Gendre, B., Mazure, A., Atteia, J. L., and Van Suu, A. Le

Subjects
Astrophysics
Abstract

The ANTARES telescope has the opportunity to detect transient neutrino sources, such as gamma-ray bursts (GRBs), core-collapse supernovae (SNe), flares of active galactic nuclei (AGNs)... To enhance the sensitivity to these sources, we are developing a new detection method based on the observation of neutrino bursts followed by an optical detection. The ANTARES Collaboration is implementing a fast on-line event reconstruction with a good angular resolution. These characteristics allow to trigger an optical telescope network in order to identify the nature of the neutrinos (and high energy cosmic-rays) sources. This follow-up can be done with a network of small automatic telescopes and required a small observation time. An optical follow-up of special events, such as neutrino doublets in coincidence in time and space or single neutrino having a very high energy, would not only give access to the nature of the sources but also improve the sensitivity for neutrino detection from SNe or GRBs., Comment: 4 pages, proceeding for the SF2A general assembly June 2008

Published
2008

16. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author

DESI Collaboration, Abareshi, B., Aguilar, J., Ahlen, S., Alam, Shadab, Alexander, David M., Alfarsy, R., Allen, L., Prieto, C. Allende, Alves, O., Ameel, J., Armengaud, E., Asorey, J., Aviles, Alejandro, Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Beltran, S. F., Benavides, B., BenZvi, S., Berti, A., Besuner, R., Beutler, Florian, Bianchi, D., Blake, C., Blanc, P., Blum, R., Bolton, A., Bose, S., Bramall, D., Brieden, S., Brodzeller, A., Brooks, D., Brownewell, C., Buckley-Geer, E., Cahn, R. N., Cai, Z., Canning, R., Capasso, R., Rosell, A. Carnero, Carton, P., Casas, R., Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chuang, C., Circosta, C., Cole, S., Cooper, A. P., Costa, L. Da, Cousinou, M.-C., Cuceu, A., Davis, T. M., Dawson, K., Cruz-Noriega, R. De La, Macorra, A. De La, Mattia, A. De, Costa, J. Della, Demmer, P., Derwent, M., Dey, A., Dey, B., Dhungana, G., Ding, Z., Dobson, C., Doel, P., Donald-McCann, J., Donaldson, J., Douglass, K., Duan, Y., Dunlop, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Enriquez-Vargas, M., Escoffier, S., Evatt, M., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Romero, J. E., Frenk, C. S., Fromenteau, S., Gänsicke, B. T., Garcia-Quintero, C., Garrison, L., Gaztañaga, E., Gerardi, F., Gil-Marín, H., A Gontcho, S. Gontcho, Gonzalez-Morales, Alma X., Gonzalez-De-Rivera, G., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Grove, C., Gruen, D., Gutierrez, G., Guy, J., Hahn, C., Harris, S., Herrera, D., Herrera-Alcantar, Hiram K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jelinsky, P., Jiang, L., Jimenez, J., Jing, Y. P., Joyce, R., Jullo, E., Juneau, S., Karaçaylı, N. G., Karamanis, M., Karcher, A., Karim, T., Kehoe, R., Kent, S., Kirkby, D., Kisner, T., Kitaura, F., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, Alex, L’Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, Ting-Wen, Landriau, M., Lane, S., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Van Suu, A. Le, Levi, Michael E., Li, T. S., Magneville, C., Manera, M., Manser, Christopher J., Marshall, B., Martini, Paul, McCollam, W., McDonald, P., Meisner, Aaron M., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miller, T., Miquel, R., Montero-Camacho, P., Moon, J., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, Andrea, Myers, Adam D., Nadathur, S., Najita, J., Napolitano, L., Neilsen, E., Newman, Jeffrey A., Nie, J. D., Ning, Y., Niz, G., Norberg, P., Noriega, Hernán E., O’Brien, T., Obuljen, A., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Pappalardo, D., PENG, X., Percival, W. J., Perruchot, S., Pogge, R., Poppett, C., Porredon, A., Prada, F., Prochaska, J., Pucha, R., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramirez-Solano, S., Ramírez-Pérez, César, Ravoux, C., Reil, K., Rezaie, M., Rocher, A., Rockosi, C., Roe, N. A., Roodman, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Safonova, S., Said, K., Saintonge, A., Catonga, Javier Salas, Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E., Schlegel, D., Schmoll, J., Scholte, D., Schubnell, M., Secroun, A., Seo, H., Serrano, S., Sharples, Ray M., Sholl, Michael J., Silber, Joseph Harry, Silva, D. R., Sirk, M., Siudek, M., Smith, A., Sprayberry, D., Staten, R., Stupak, B., Tan, T., Tarlé, Gregory, Tie, Suk Sien, Tojeiro, R., Ureña-López, L. A., Valdes, F., Valenzuela, O., Valluri, M., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, C., Wechsler, R., Wilson, Michael J., Yang, J., Yu, Y., Yuan, S., Yèche, Christophe, Zhang, H., Zhang, K., Zhao, Cheng, Zhou, Rongpu, Zhou, Zhimin, Zou, H., Zou, J., Zou, S., Zu, Y., Aguilar, J. [0000-0003-0822-452X], Ahlen, S. [0000-0001-6098-7247], Alam, Shadab [0000-0002-3757-6359], Alexander, David M. [0000-0002-5896-6313], Allen, L. [0000-0002-7789-5119], Prieto, C. Allende [0000-0002-0084-572X], Ameel, J. [0000-0003-3638-2584], Asorey, J. [0000-0002-6211-499X], Bailey, S. [0000-0003-4162-6619], Balaguera-Antolínez, A. [0000-0001-5028-3035], Ballester, O. [0000-0002-7126-5300], Bault, A. [0000-0002-9964-1005], Beltran, S. F. [0000-0001-6324-4019], Berti, A. [0000-0003-3582-6649], Beutler, Florian [0000-0003-0467-5438], Bose, S. [0000-0002-0974-5266], Brieden, S. [0000-0003-3896-9215], Brodzeller, A. [0000-0002-8934-0954], Brooks, D. [0000-0002-8458-5047], Cahn, R. N. [0000-0003-2748-0641], Cai, Z. [0000-0001-8467-6478], Capasso, R. [0000-0002-3083-6840], Rosell, A. Carnero [0000-0003-3044-5150], Castander, F. J. [0000-0001-7316-4573], Cervantes-Cota, J. L. [0000-0002-3057-6786], Chabanier, S. [0000-0002-5692-5243], Chaussidon, E. [0000-0001-8996-4874], Chuang, C. [0000-0002-3882-078X], Cole, S. [0000-0002-5954-7903], Cooper, A. P. [0000-0001-8274-158X], Cuceu, A. [0000-0002-2169-0595], Davis, T. M. [0000-0002-4213-8783], Dawson, K. [0000-0002-0553-3805], Costa, J. Della [0000-0003-0928-2000], Dey, A. [0000-0002-4928-4003], Dey, B. [0000-0002-5665-7912], Dhungana, G. [0000-0002-5402-1216], Ding, Z. [0000-0002-3369-3718], Douglass, K. [0000-0002-9540-546X], Duan, Y. [0000-0002-2611-0895], Eisenstein, D. J. [0000-0002-2929-3121], Escoffier, S. [0000-0002-2847-7498], Fan, X. [0000-0003-3310-0131], Fawcett, V. A. [0000-0003-1251-532X], Ereza, J. [0000-0002-0194-4017], Frenk, C. S. [0000-0002-2338-716X], Gänsicke, B. T. [0000-0002-2761-3005], Garrison, L. [0000-0002-9853-5673], Gaztañaga, E. [0000-0001-9632-0815], Gonzalez-Morales, Alma X. [0000-0003-4089-6924], Gonzalez-de-Rivera, G. [0000-0003-4452-743X], Gonzalez-Perez, V. [0000-0001-9938-2755], Graur, O. [0000-0002-4391-6137], Green, D. [0000-0002-0676-3661], Gruen, D. [0000-0003-3270-7644], Hahn, C. [0000-0003-1197-0902], Herrera, D. [0000-0003-2092-6727], Herrera-Alcantar, Hiram K. [0000-0002-9136-9609], Huterer, D. [0000-0001-6558-0112], Iršič, V. [0000-0002-5445-461X], Ishak, M. [0000-0002-6024-466X], Jiang, L. [0000-0003-4176-6486], Jing, Y. P. [0000-0002-4534-3125], Joyce, R. [0000-0003-0201-5241], Jullo, E. [0000-0002-9253-053X], Juneau, S. [0000-0002-0000-2394], Karaçaylı, N. G. [0000-0001-7336-8912], Karamanis, M. [0000-0001-9489-4612], Karim, T. [0000-0002-5652-8870], Kehoe, R. [0000-0002-7101-697X], Kent, S. [0000-0003-4207-7420], Kirkby, D. [0000-0002-8828-5463], Kisner, T. [0000-0003-3510-7134], Koposov, S. E. [0000-0003-2644-135X], Kovács, A. [0000-0002-5825-579X], Kremin, A. [0000-0001-6356-7424], L’Huillier, B. [0000-0003-2934-6243], Landriau, M. [0000-0003-1838-8528], Lang, D. [0000-0002-1172-0754], Lasker, J. [0000-0003-2999-4873], Guillou, L. Le [0000-0001-7178-8868], Leauthaud, A. [0000-0002-3677-3617], Van Suu, A. Le [0000-0001-5488-783X], Levi, Michael E. [0000-0003-1887-1018], Li, T. S. [0000-0002-9110-6163], Manser, Christopher J. [0000-0003-1543-5405], Martini, Paul [0000-0002-0194-4017], McDonald, P. [0000-0001-8346-8394], Meisner, Aaron M. [0000-0002-1125-7384], Mena-Fernández, J. [0000-0001-9497-7266], Meneses-Rizo, J. [0000-0003-3201-9788], Miquel, R. [0000-0002-6610-4836], Moustakas, J. [0000-0002-2733-4559], Nadathur, S. [0000-0001-9070-3102], Neilsen, E. [0000-0002-7357-0317], Newman, Jeffrey A. [0000-0001-8684-2222], Nie, J. D. [0000-0001-6590-8122], Ning, Y. [0000-0001-9442-1217], Niz, G. [0000-0002-1544-8946], Norberg, P. [0000-0002-5875-0440], Noriega, Hernán E. [0000-0002-3397-3998], Obuljen, A. [0000-0002-9012-6621], Palanque-Delabrouille, N. [0000-0003-3188-784], PENG, X. [0000-0002-3784-830X], Percival, W. J. [0000-0002-0644-5727], Pogge, R. [0000-0003-1435-3053], Porredon, A. [0000-0002-2762-2024], Prada, F. [0000-0001-7145-8674], Prochaska, J. [0000-0002-7738-6875], Pucha, R. [0000-0002-4940-3009], Pérez-Ràfols, I. [0000-0001-6979-0125], Rabinowitz, D. [0000-0003-4961-7653], Raichoor, A. [0000-0001-5999-7923], Rezaie, M. [0000-0001-5589-7116], Rockosi, C. [0000-0002-6667-7028], Roodman, A. [0000-0001-5326-3486], Sabiu, C. G. [0000-0002-5513-5303], Safonova, S. [0000-0002-2240-7421], Said, K. [0000-0002-1809-6325], Saintonge, A. [0000-0003-4357-3450], Samushia, L. [0000-0002-1609-5687], Sanchez, E. [0000-0002-9646-8198], Saulder, C. [0000-0002-0408-5633], Schaan, E. [0000-0002-4619-8927], Schlegel, D. [0000-0002-5042-5088], Secroun, A. [0000-0003-0505-3710], Seo, H. [0000-0002-6588-3508], Sharples, Ray M. [0000-0003-3449-8583], Silber, Joseph Harry [0000-0002-3461-0320], Silva, D. R. [0000-0002-7678-2155], Sprayberry, D. [0000-0001-7583-6441], Tarlé, Gregory [0000-0003-1704-0781], Tie, Suk Sien [0000-0002-5249-1353], Valdes, F. [0000-0001-5567-1301], Valenzuela, O. [0000-0002-0523-5509], Valluri, M. [0000-0002-6257-2341], Verde, L. [0000-0003-2601-8770], Walther, M. [0000-0002-1748-3745], Wang, B. [0000-0003-4877-1659], Wang, M. S. [0000-0002-2652-4043], Wechsler, R. [0000-0003-2229-011X], Yang, J. [0000-0001-5287-4242], Yu, Y. [0000-0002-9359-7170], Yuan, S. [0000-0002-5992-7586], Yèche, Christophe [0000-0001-5146-8533], Zhang, H. [0000-0001-6847-5254], Zhang, K. [0000-0002-9808-3646], Zhao, Cheng [0000-0002-1991-7295], Zhou, Rongpu [0000-0001-5381-4372], Zhou, Zhimin [0000-0002-4135-0977], Zou, H. [0000-0002-6684-3997], Zou, J. [0000-0001-9189-0368], Zou, S. [0000-0002-3983-6484], Zu, Y. [0000-0001-6966-6925], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), 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), 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DESI, HEP, INSPIRE, and Ministerio de Ciencia e Innovación (España)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, redshift 0.6, Settore FIS/05 - Astronomia e Astrofisica, QB Astronomy, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, MCC, Astronomy and Astrophysics, DAS, space, distortions, peak, Laboratory Astrophysics, Instrumentation, Software, and Data, QC Physics, Space and Planetary Science, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], astro-ph.CO, galaxy sample, power-spectrum, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], growth-rate, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

Full list of authors: Abareshi, B.; Aguilar, J.; Ahlen, S.; Alam, Shadab; Alexander, David M.; Alfarsy, R.; Allen, L.; Allende Prieto, C.; Alves, O.; Ameel, J.; Armengaud, E.; Asorey, J.; Aviles, Alejandro; Bailey, S.; Balaguera-Antolinez, A.; Ballester, O.; Baltay, C.; Bault, A.; Beltran, S. F.; Benavides, B.; BenZvi, S.; Berti, A.; Besuner, R.; Beutler, Florian; Bianchi, D.; Blake, C.; Blanc, P.; Blum, R.; Bolton, A.; Bose, S.; Bramall, D.; Brieden, S.; Brodzeller, A.; Brooks, D.; Brownewell, C.; Buckley-Geer, E.; Cahn, R. N.; Cai, Z.; Canning, R.; Capasso, R.; Carnero Rosell, A.; Carton, P.; Casas, R.; Castander, F. J.; Cervantes-Cota, J. L.; Chabanier, S.; Chaussidon, E.; Chuang, C.; Circosta, C.; Cole, S.; Cooper, A. P.; da Costa, L.; Cousinou, M-C; Cuceu, A.; Davis, T. M.; Dawson, K.; De la Cruz-Noriega, R.; de la Macorra, A.; de Mattia, A.; Della Costa, J.; Demmer, P.; Derwent, M.; Dey, A.; Dey, B.; Dhungana, G.; Ding, Z.; Dobson, C.; Doel, P.; Donald-McCann, J.; Donaldson, J.; Douglass, K.; Duan, Y.; Dunlop, P.; Edelstein, J.; Eftekharzadeh, S.; Eisenstein, D. J.; Enriquez-Vargas, M.; Escoffier, S.; Evatt, M.; Fagrelius, P.; Fan, X.; Fanning, K.; Fawcett, V. A.; Ferraro, S.; Ereza, J.; Flaugher, B.; Font-Ribera, A.; Forero-Romero, J. E.; Frenk, C. S.; Fromenteau, S.; Gansicke, B. T.; Garcia-Quintero, C.; Garrison, L.; Gaztanaga, E.; Gerardi, F.; Gil-Marin, H.; Gontcho, S. Gontcho A.; Gonzalez-Morales, Alma X.; Gonzalez-de-Rivera, G.; Gonzalez-Perez, V; Gordon, C.; Graur, O.; Green, D.; Grove, C.; Gruen, D.; Gutierrez, G.; Guy, J.; Hahn, C.; Harris, S.; Herrera, D.; Herrera-Alcantar, Hiram K.; Honscheid, K.; Howlett, C.; Huterer, D.; Irsic, V; Ishak, M.; Jelinsky, P.; Jiang, L.; Jimenez, J.; Jing, Y. P.; Joyce, R.; Jullo, E.; Juneau, S.; Karacayli, N. G.; Karamanis, M.; Karcher, A.; Karim, T.; Kehoe, R.; Kent, S.; Kirkby, D.; Kisner, T.; Kitaura, F.; Koposov, S. E.; Kovacs, A.; Kremin, A.; Krolewski, Alex; L'Huillier, B.; Lahav, O.; Lambert, A.; Lamman, C.; Lan, Ting-Wen; Landriau, M.; Lane, S.; Lang, D.; Lange, J. U.; Lasker, J.; Le Guillou, L.; Leauthaud, A.; Suu, A. Le Van; Levi, Michael E.; Li, T. S.; Magneville, C.; Manera, M.; Manser, Christopher J.; Marshall, B.; Martini, Paul; McCollam, W.; McDonald, P.; Meisner, Aaron M.; Mena-Fernandez, J.; Meneses-Rizo, J.; Mezcua, M.; Miller, T.; Miquel, R.; Montero-Camacho, P.; Moon, J.; Moustakas, J.; Mueller, E.; Munoz-Gutierrez, Andrea; Myers, Adam D.; Nadathur, S.; Najita, J.; Napolitano, L.; Neilsen, E.; Newman, Jeffrey A.; Nie, J. D.; Ning, Y.; Niz, G.; Norberg, P.; Noriega, Hernan E.; O'Brien, T.; Obuljen, A.; Palanque-Delabrouille, N.; Palmese, A.; Zhiwei, P.; Pappalardo, D.; Peng, X.; Percival, W. J.; Perruchot, S.; Pogge, R.; Poppett, C.; Porredon, A.; Prada, F.; Prochaska, J.; Pucha, R.; Perez-Fernandez, A.; Perez-Rafols, I; Rabinowitz, D.; Raichoor, A.; Ramirez-Solano, S.; Ramirez-Perez, Cesar; Ravoux, C.; Reil, K.; Rezaie, M.; Rocher, A.; Rockosi, C.; Roe, N. A.; Roodman, A.; Ross, A. J.; Rossi, G.; Ruggeri, R.; Ruhlmann-Kleider, V; Sabiu, C. G.; Safonova, S.; Said, K.; Saintonge, A.; Catonga, Javier Salas; Samushia, L.; Sanchez, E.; Saulder, C.; Schaan, E.; Schlafly, E.; Schlegel, D.; Schmoll, J.; Scholte, D.; Schubnell, M.; Secroun, A.; Seo, H.; Serrano, S.; Sharples, Ray M.; Sholl, Michael J.; Silber, Joseph Harry; Silva, D. R.; Sirk, M.; Siudek, M.; Smith, A.; Sprayberry, D.; Staten, R.; Stupak, B.; Tan, T.; Tarle, Gregory; Tie, Suk Sien; Tojeiro, R.; Urena-Lopez, L. A.; Valdes, F.; Valenzuela, O.; Valluri, M.; Vargas-Magana, M.; Verde, L.; Walther, M.; Wang, B.; Wang, M. S.; Weaver, B. A.; Weaverdyck, C.; Wechsler, R.; Wilson, Michael J.; Yang, J.; Yu, Y.; Yuan, S.; Yeche, Christophe; Zhang, H.; Zhang, K.; Zhao, Cheng; Zhou, Rongpu; Zhou, Zhimin; Zou, H.; Zou, J.; Zou, S.; Zu, Y.; DESI Collaboration.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The Dark Energy Spectroscopic Instrument (DESI) embarked on an ambitious 5 yr survey in 2021 May to explore the nature of dark energy with spectroscopic measurements of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the baryon acoustic oscillation method to measure distances from the nearby universe to beyond redshift z > 3.5, and employ redshift space distortions to measure the growth of structure and probe potential modifications to general relativity. We describe the significant instrumentation we developed to conduct the DESI survey. This includes: a wide-field, 3fdg2 diameter prime-focus corrector; a focal plane system with 5020 fiber positioners on the 0.812 m diameter, aspheric focal surface; 10 continuous, high-efficiency fiber cable bundles that connect the focal plane to the spectrographs; and 10 identical spectrographs. Each spectrograph employs a pair of dichroics to split the light into three channels that together record the light from 360–980 nm with a spectral resolution that ranges from 2000–5000. We describe the science requirements, their connection to the technical requirements, the management of the project, and interfaces between subsystems. DESI was installed at the 4 m Mayall Telescope at Kitt Peak National Observatory and has achieved all of its performance goals. Some performance highlights include an rms positioner accuracy of better than 0farcs1 and a median signal-to-noise ratio of 7 of the [O ii] doublet at 8 × 10−17 erg s−1 cm−2 in 1000 s for galaxies at z = 1.4–1.6. We conclude with additional highlights from the on-sky validation and commissioning, key successes, and lessons learned. © 2022. The Author(s). Published by the American Astronomical Society., This research is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under contract No. DE-AC02-05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI is provided by the U.S. National Science Foundation, Division of Astronomical Sciences under contract No. AST-0950945 to the NSF's National Optical-Infrared Astronomy Research Laboratory; the Science and Technologies Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising–Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain, and by the DESI Member Institutions: Aix-Marseille University; Argonne National Laboratory; Barcelona-Madrid Regional Participation Group; Brookhaven National Laboratory; Boston University; Brazil Regional Participation Group; Carnegie Mellon University; CEA-IRFU, Saclay; China Participation Group; Cornell University; Durham University; École Polytechnique Fédérale de Lausanne; Eidgenössische Technische Hochschule, Zürich; Fermi National Accelerator Laboratory; Granada-Madrid-Tenerife Regional Participation Group; Harvard University; Kansas State University; Korea Astronomy and Space Science Institute; Korea Institute for Advanced Study; Lawrence Berkeley National Laboratory; Laboratoire de Physique Nucléaire et de Hautes Energies; Ludwig Maximilians University; Max Planck Institute; Mexico Regional Participation Group; New York University; NSF's National Optical-Infrared Astronomy Research Laboratory; Ohio University; Perimeter Institute; Shanghai Jiao Tong University; Siena College; SLAC National Accelerator Laboratory; Southern Methodist University; Swinburne University; The Ohio State University; Universidad de los Andes; University of Arizona; University of Barcelona; University of California, Berkeley; University of California, Irvine; University of California, Santa Cruz; University College London; University of Florida; University of Michigan at Ann Arbor; University of Pennsylvania; University of Pittsburgh; University of Portsmouth; University of Queensland; University of Rochester; University of Toronto; University of Utah; University of Waterloo; University of Wyoming; University of Zurich; UK Regional Participation Group; and Yale University. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

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2022
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17. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author

Abareshi, B., additional, Aguilar, J., additional, Ahlen, S., additional, Alam, Shadab, additional, Alexander, David M., additional, Alfarsy, R., additional, Allen, L., additional, Prieto, C. Allende, additional, Alves, O., additional, Ameel, J., additional, Armengaud, E., additional, Asorey, J., additional, Aviles, Alejandro, additional, Bailey, S., additional, Balaguera-Antolínez, A., additional, Ballester, O., additional, Baltay, C., additional, Bault, A., additional, Beltran, S. F., additional, Benavides, B., additional, BenZvi, S., additional, Berti, A., additional, Besuner, R., additional, Beutler, Florian, additional, Bianchi, D., additional, Blake, C., additional, Blanc, P., additional, Blum, R., additional, Bolton, A., additional, Bose, S., additional, Bramall, D., additional, Brieden, S., additional, Brodzeller, A., additional, Brooks, D., additional, Brownewell, C., additional, Buckley-Geer, E., additional, Cahn, R. N., additional, Cai, Z., additional, Canning, R., additional, Capasso, R., additional, Rosell, A. Carnero, additional, Carton, P., additional, Casas, R., additional, Castander, F. J., additional, Cervantes-Cota, J. L., additional, Chabanier, S., additional, Chaussidon, E., additional, Chuang, C., additional, Circosta, C., additional, Cole, S., additional, Cooper, A. P., additional, Costa, L. da, additional, Cousinou, M.-C., additional, Cuceu, A., additional, Davis, T. M., additional, Dawson, K., additional, Cruz-Noriega, R. de la, additional, Macorra, A. de la, additional, Mattia, A. de, additional, Costa, J. Della, additional, Demmer, P., additional, Derwent, M., additional, Dey, A., additional, Dey, B., additional, Dhungana, G., additional, Ding, Z., additional, Dobson, C., additional, Doel, P., additional, Donald-McCann, J., additional, Donaldson, J., additional, Douglass, K., additional, Duan, Y., additional, Dunlop, P., additional, Edelstein, J., additional, Eftekharzadeh, S., additional, Eisenstein, D. J., additional, Enriquez-Vargas, M., additional, Escoffier, S., additional, Evatt, M., additional, Fagrelius, P., additional, Fan, X., additional, Fanning, K., additional, Fawcett, V. A., additional, Ferraro, S., additional, Ereza, J., additional, Flaugher, B., additional, Font-Ribera, A., additional, Forero-Romero, J. E., additional, Frenk, C. S., additional, Fromenteau, S., additional, Gänsicke, B. T., additional, Garcia-Quintero, C., additional, Garrison, L., additional, Gaztañaga, E., additional, Gerardi, F., additional, Gil-Marín, H., additional, A Gontcho, S. Gontcho, additional, Gonzalez-Morales, Alma X., additional, Gonzalez-de-Rivera, G., additional, Gonzalez-Perez, V., additional, Gordon, C., additional, Graur, O., additional, Green, D., additional, Grove, C., additional, Gruen, D., additional, Gutierrez, G., additional, Guy, J., additional, Hahn, C., additional, Harris, S., additional, Herrera, D., additional, Herrera-Alcantar, Hiram K., additional, Honscheid, K., additional, Howlett, C., additional, Huterer, D., additional, Iršič, V., additional, Ishak, M., additional, Jelinsky, P., additional, Jiang, L., additional, Jimenez, J., additional, Jing, Y. P., additional, Joyce, R., additional, Jullo, E., additional, Juneau, S., additional, Karaçaylı, N. G., additional, Karamanis, M., additional, Karcher, A., additional, Karim, T., additional, Kehoe, R., additional, Kent, S., additional, Kirkby, D., additional, Kisner, T., additional, Kitaura, F., additional, Koposov, S. E., additional, Kovács, A., additional, Kremin, A., additional, Krolewski, Alex, additional, L’Huillier, B., additional, Lahav, O., additional, Lambert, A., additional, Lamman, C., additional, Lan, Ting-Wen, additional, Landriau, M., additional, Lane, S., additional, Lang, D., additional, Lange, J. U., additional, Lasker, J., additional, Guillou, L. Le, additional, Leauthaud, A., additional, Van Suu, A. Le, additional, Levi, Michael E., additional, Li, T. S., additional, Magneville, C., additional, Manera, M., additional, Manser, Christopher J., additional, Marshall, B., additional, Martini, Paul, additional, McCollam, W., additional, McDonald, P., additional, Meisner, Aaron M., additional, Mena-Fernández, J., additional, Meneses-Rizo, J., additional, Mezcua, M., additional, Miller, T., additional, Miquel, R., additional, Montero-Camacho, P., additional, Moon, J., additional, Moustakas, J., additional, Mueller, E., additional, Muñoz-Gutiérrez, Andrea, additional, Myers, Adam D., additional, Nadathur, S., additional, Najita, J., additional, Napolitano, L., additional, Neilsen, E., additional, Newman, Jeffrey A., additional, Nie, J. D., additional, Ning, Y., additional, Niz, G., additional, Norberg, P., additional, Noriega, Hernán E., additional, O’Brien, T., additional, Obuljen, A., additional, Palanque-Delabrouille, N., additional, Palmese, A., additional, Zhiwei, P., additional, Pappalardo, D., additional, PENG, X., additional, Percival, W. J., additional, Perruchot, S., additional, Pogge, R., additional, Poppett, C., additional, Porredon, A., additional, Prada, F., additional, Prochaska, J., additional, Pucha, R., additional, Pérez-Fernández, A., additional, Pérez-Ràfols, I., additional, Rabinowitz, D., additional, Raichoor, A., additional, Ramirez-Solano, S., additional, Ramírez-Pérez, César, additional, Ravoux, C., additional, Reil, K., additional, Rezaie, M., additional, Rocher, A., additional, Rockosi, C., additional, Roe, N. A., additional, Roodman, A., additional, Ross, A. J., additional, Rossi, G., additional, Ruggeri, R., additional, Ruhlmann-Kleider, V., additional, Sabiu, C. G., additional, Safonova, S., additional, Said, K., additional, Saintonge, A., additional, Catonga, Javier Salas, additional, Samushia, L., additional, Sanchez, E., additional, Saulder, C., additional, Schaan, E., additional, Schlafly, E., additional, Schlegel, D., additional, Schmoll, J., additional, Scholte, D., additional, Schubnell, M., additional, Secroun, A., additional, Seo, H., additional, Serrano, S., additional, Sharples, Ray M., additional, Sholl, Michael J., additional, Silber, Joseph Harry, additional, Silva, D. R., additional, Sirk, M., additional, Siudek, M., additional, Smith, A., additional, Sprayberry, D., additional, Staten, R., additional, Stupak, B., additional, Tan, T., additional, Tarlé, Gregory, additional, Tie, Suk Sien, additional, Tojeiro, R., additional, Ureña-López, L. A., additional, Valdes, F., additional, Valenzuela, O., additional, Valluri, M., additional, Vargas-Magaña, M., additional, Verde, L., additional, Walther, M., additional, Wang, B., additional, Wang, M. S., additional, Weaver, B. A., additional, Weaverdyck, C., additional, Wechsler, R., additional, Wilson, Michael J., additional, Yang, J., additional, Yu, Y., additional, Yuan, S., additional, Yèche, Christophe, additional, Zhang, H., additional, Zhang, K., additional, Zhao, Cheng, additional, Zhou, Rongpu, additional, Zhou, Zhimin, additional, Zou, H., additional, Zou, J., additional, Zou, S., additional, and Zu, Y., additional

Published
2022
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18. Transmission of light in deep sea water at the site of the A ntares neutrino telescope

Author

Aguilar, J.A., Albert, A., Amram, P., Anghinolfi, M., Anton, G., Anvar, S., Ardellier-Desages, F.E., Aslanides, E., Aubert, J-J., Azoulay, R., Bailey, D., Basa, S., Battaglieri, M., Becherini, Y., Bellotti, R., Beltramelli, J., Bertin, V., Billault, M., Blaes, R., Blanc, F., Bland, R.W., de Botton, N., Boulesteix, J., Bouwhuis, M.C., Brooks, C.B., Bradbury, S.M., Bruijn, R., Brunner, J., Bugeon, F., Burgio, G.F., Cafagna, F., Calzas, A., Caponetto, L., Carmona, E., Carr, J., Cartwright, S.L., Cecchini, S., Charvis, P., Circella, M., Colnard, C., Compère, C., Croquette, J., Cooper, S., Coyle, P., Cuneo, S., Damy, G., van Dantzig, R., Deschamps, A., Marzo, C. De, Destelle, J.-J., Vita, R. De, Dinkelspiler, B., Dispau, G., Drougou, J.-F., Druillole, F., Engelen, J., Favard, S., Feinstein, F., Ferry, S., Festy, D., Fopma, J., Fuda, J.-L., Gallone, J.-M., Giacomelli, G., Girard, N., Goret, P., Gournay, J.-F., Hallewell, G., Hartmann, B., Heijboer, A., Hello, Y., Hernández-Rey, J.J., Herrouin, G., Hößl, J., Hoffmann, C., Hubbard, J.R., Jaquet, M., de Jong, M., Jouvenot, F., Kappes, A., Karg, T., Karkar, S., Karolak, M., Katz, U., Keller, P., Kooijman, P., Korolkova, E.V., Kouchner, A., Kretschmer, W., Kudryavtsev, V.A., Lafoux, H., Lagier, P., Lamare, P., Languillat, J.-C., Laubier, L., Legou, T., Guen, Y. Le, Provost, H. Le, Van Suu, A. Le, Nigro, L. Lo, Presti, D. Lo, Loucatos, S., Louis, F., Lyashuk, V., Magnier, P., Marcelin, M., Margiotta, A., Maron, C., Massol, A., Mazéas, F., Mazeau, B., Mazure, A., McMillan, J.E., Michel, J.-L., Millot, C., Milovanovic, A., Montanet, F., Montaruli, T., Morel, J.-P., Moscoso, L., Nezri, E., Niess, V., Nooren, G.J., Ogden, P., Olivetto, C., Palanque-Delabrouille, N., Payre, P., Petta, C., Pineau, J.-P., Poinsignon, J., Popa, V., Potheau, R., Pradier, T., Racca, C., Randazzo, N., Real, D., van Rens, B.A.P., Réthoré, F., Ripani, M., Roca-Blay, V., Romeyer, A., Rollin, J.-F., Romita, M., Rose, H.J., Rostovtsev, A., Ruppi, M., Russo, G.V., Sacquin, Y., Saouter, S., Schuller, J.-P., Schuster, W., Sokalski, I., Suvorova, O., Spooner, N.J.C., Spurio, M., Stolarczyk, T., Stubert, D., Taiuti, M., Thompson, L.F., Tilav, S., Usik, A., Valdy, P., Vallage, B., Vaudaine, G., Vernin, P., Virieux, J., Vladimirsky, E., de Vries, G., de Witt Huberts, P., de Wolf, E., Zaborov, D., Zaccone, H., Zakharov, V., Zavatarelli, S., de Zornoza, J.D., and Zúñiga, J.

Published
2005
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19. Overview of the DESI Legacy Imaging Surveys

Author

Dey, Arjun, primary, Schlegel, David J., additional, Lang, Dustin, additional, Blum, Robert, additional, Burleigh, Kaylan, additional, Fan, Xiaohui, additional, Findlay, Joseph R., additional, Finkbeiner, Doug, additional, Herrera, David, additional, Juneau, Stéphanie, additional, Landriau, Martin, additional, Levi, Michael, additional, McGreer, Ian, additional, Meisner, Aaron, additional, Myers, Adam D., additional, Moustakas, John, additional, Nugent, Peter, additional, Patej, Anna, additional, Schlafly, Edward F., additional, Walker, Alistair R., additional, Valdes, Francisco, additional, Weaver, Benjamin A., additional, Yèche, Christophe, additional, Zou, Hu, additional, Zhou, Xu, additional, Abareshi, Behzad, additional, Abbott, T. M. C., additional, Abolfathi, Bela, additional, Aguilera, C., additional, Alam, Shadab, additional, Allen, Lori, additional, Alvarez, A., additional, Annis, James, additional, Ansarinejad, Behzad, additional, Aubert, Marie, additional, Beechert, Jacqueline, additional, Bell, Eric F., additional, BenZvi, Segev Y., additional, Beutler, Florian, additional, Bielby, Richard M., additional, Bolton, Adam S., additional, Briceño, César, additional, Buckley-Geer, Elizabeth J., additional, Butler, Karen, additional, Calamida, Annalisa, additional, Carlberg, Raymond G., additional, Carter, Paul, additional, Casas, Ricard, additional, Castander, Francisco J., additional, Choi, Yumi, additional, Comparat, Johan, additional, Cukanovaite, Elena, additional, Delubac, Timothée, additional, DeVries, Kaitlin, additional, Dey, Sharmila, additional, Dhungana, Govinda, additional, Dickinson, Mark, additional, Ding, Zhejie, additional, Donaldson, John B., additional, Duan, Yutong, additional, Duckworth, Christopher J., additional, Eftekharzadeh, Sarah, additional, Eisenstein, Daniel J., additional, Etourneau, Thomas, additional, Fagrelius, Parker A., additional, Farihi, Jay, additional, Fitzpatrick, Mike, additional, Font-Ribera, Andreu, additional, Fulmer, Leah, additional, Gänsicke, Boris T., additional, Gaztanaga, Enrique, additional, George, Koshy, additional, Gerdes, David W., additional, A Gontcho, Satya Gontcho, additional, Gorgoni, Claudio, additional, Green, Gregory, additional, Guy, Julien, additional, Harmer, Diane, additional, Hernandez, M., additional, Honscheid, Klaus, additional, Huang, Lijuan (Wendy), additional, James, David J., additional, Jannuzi, Buell T., additional, Jiang, Linhua, additional, Joyce, Richard, additional, Karcher, Armin, additional, Karkar, Sonia, additional, Kehoe, Robert, additional, Kneib, Jean-Paul,, additional, Kueter-Young, Andrea, additional, Lan, Ting-Wen, additional, Lauer, Tod R., additional, Guillou, Laurent Le, additional, Van Suu, Auguste Le, additional, Lee, Jae Hyeon, additional, Lesser, Michael, additional, Levasseur, Laurence Perreault, additional, Li, Ting S., additional, Mann, Justin L., additional, Marshall, Robert, additional, Martínez-Vázquez, C. E., additional, Martini, Paul, additional, du Mas des Bourboux, Hélion, additional, McManus, Sean, additional, Meier, Tobias Gabriel, additional, Ménard, Brice, additional, Metcalfe, Nigel, additional, Muñoz-Gutiérrez, Andrea, additional, Najita, Joan, additional, Napier, Kevin, additional, Narayan, Gautham, additional, Newman, Jeffrey A., additional, Nie, Jundan, additional, Nord, Brian, additional, Norman, Dara J., additional, Olsen, Knut A. G., additional, Paat, Anthony, additional, Palanque-Delabrouille, Nathalie, additional, Peng, Xiyan, additional, Poppett, Claire L., additional, Poremba, Megan R., additional, Prakash, Abhishek, additional, Rabinowitz, David, additional, Raichoor, Anand, additional, Rezaie, Mehdi, additional, Robertson, A. N., additional, Roe, Natalie A., additional, Ross, Ashley J., additional, Ross, Nicholas P., additional, Rudnick, Gregory, additional, Safonova, Sasha, additional, Saha, Abhijit, additional, Sánchez, F. Javier, additional, Savary, Elodie, additional, Schweiker, Heidi, additional, Scott, Adam, additional, Seo, Hee-Jong, additional, Shan, Huanyuan, additional, Silva, David R., additional, Slepian, Zachary, additional, Soto, Christian, additional, Sprayberry, David, additional, Staten, Ryan, additional, Stillman, Coley M., additional, Stupak, Robert J., additional, Summers, David L., additional, Tie, Suk Sien, additional, Tirado, H., additional, Vargas-Magaña, Mariana, additional, Vivas, A. Katherina, additional, Wechsler, Risa H., additional, Williams, Doug, additional, Yang, Jinyi, additional, Yang, Qian, additional, Yapici, Tolga, additional, Zaritsky, Dennis, additional, Zenteno, A., additional, Zhang, Kai, additional, Zhang, Tianmeng, additional, Zhou, Rongpu, additional, and Zhou, Zhimin, additional

Published
2019
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20. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author

Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolás G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de La Macorra, Axel, de Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stephanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Paris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Régal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarlè, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magaña, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, Zu, Ying, Korea Astronomy and Space Science Institute (KASI), Okayama University, University of California [Berkeley], University of California, National Optical Astronomy Observatory (NOAO), Instituto de Astrofisica de Canarias (IAC), Fermi National Accelerator Laboratory (Fermilab), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Yale University [New Haven], Ohio State University [Columbus] (OSU), The University of Notre Dame [Sydney], Department of Astronomy, University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Space Sciences Laboratory [Berkeley] (SSL), University of California-University of California, University of Portsmouth, University of British Columbia (UBC), Ecole Polytechnique Fédérale de Lausanne (EPFL), 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), Cerro Tololo Inter-American Observatory, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, 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)-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), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Carreterra Mexico-Toluca, Department of Physics [Durham University], Durham University, Department of Astronomy, The Ohio State University, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Institute for Computational Cosmology (ICC), 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), Universidad Nacional Autónoma de México (UNAM), Department of Applied Physics, Departamento de Fisica Aplicada [Granada], Universidad de Granada (UGR)-Universidad de Granada (UGR), University College of London [London] (UCL), University of Wyoming (UW), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Arizona State University [Tempe] (ASU), Department of Information Engineering, Zhejiang University of Technology, Zhejiang University of Technology, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Departamento de Fisica Teorica, Institute of Cosmology & Gravitation [Portsmouth], Carnegie Mellon University [Pittsburgh] (CMU), NASA Goddard Space Flight Center (GSFC), Korea Institute for Advanced Study (KIAS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), Department of Physics, University of California, University of California [Los Angeles] (UCLA), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Center for Cosmology & AstroParticle Physics, California Institute of Technology (CALTECH), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Department of Physics [Durham], University of New Hampshire (UNH), University of Waterloo [Waterloo], Universität Zürich [Zürich] = University of Zurich (UZH), Department of Astronomy and Space Science [Sejong University], Sejong University, Department of Physics [Oxford], University of Oxford [Oxford], Institute of Plasma Physics, Chinese Academy of Sciences (ASIPP), Department of Physics [Ann Arbor], University of St Andrews [Scotland], University of Science and Technology of China [Hefei] (USTC), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Karlsruhe Institute of Technology (KIT), National University of Defense Technology [China], DESI Collaboration, University of California [Berkeley] (UC Berkeley), University of California (UC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universidad Autónoma de Madrid (UAM), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Universidad de Granada = University of Granada (UGR)-Universidad de Granada = University of Granada (UGR), Harvard University-Smithsonian Institution, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), University of California [Irvine] (UC Irvine), University of Oxford, and Escoffier, Stephanie

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Galaxy Astrophysics
Abstract

DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

Published
2016

21. The ANTARES optical beacon system

Author

Ageron, M., Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Ardellier-Desages, F., Aslanides, E., Aubert, J-J, Auer, R., Barbarito, E., Basa, S., Battaglieri, M., Becherini, Yvonne, Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bradbury, S. M., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Cartwright, S. L., Castel, D., Castorina, E., Cavasinni, V., Cecchini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A-S, Damy, G., van Dantzig, R., De Bonis, G., De Marzo, C., De Vita, R., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Destelle, J-J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J-F, Druillole, F., Durand, D., Ernenwein, J-P, Escoffier, S., Falchini, E., Favard, S., Fehr, F., Feinstein, F., Ferry, S., Fiorello, C., Flaminio, V., Fratini, K., Fuda, J-L, Galeotti, S., Gallone, J-M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Katz, U., Keller, P., Kok, E., Kok, H., Kooijman, P., Kopper, C., Korolkova, E. V., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Kudryavstev, V. A., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Lambard, G., Languillat, J-C, Laschinsky, H., Lavalle, J., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Lefevre, D., Legou, T., Lelaizant, G., Lim, G., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., McMillan, J. E., Megna, R., Melissas, M., Migneco, E., Milovanovic, A., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Musumeci, M., Naumann-Godo, M., Naumann, C., Niess, V., Noble, T., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H., Perez, A., Petta, C., Piattelli, P., Pillet, R., Pineau, J-P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Rose, H. J., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Rusydi, G., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J-P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Terreni, G., Thompson, L. F., Urbano, F., Valdy, P., Valente, V., Vallage, B., Vaudaine, G., Venekamp, G., Verlaat, B., Vernin, P., de Vries-Uiterweerd, G., van Wijk, R., Wijnker, G., Huberts, P. de Witt, Wobbe, G., de Wolf, E., Yao, A-F, Zaborov, D., Zaccone, H., Zornoza, J. D., Zuniga, J., Ageron, M., Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Ardellier-Desages, F., Aslanides, E., Aubert, J-J, Auer, R., Barbarito, E., Basa, S., Battaglieri, M., Becherini, Yvonne, Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bradbury, S. M., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Cartwright, S. L., Castel, D., Castorina, E., Cavasinni, V., Cecchini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A-S, Damy, G., van Dantzig, R., De Bonis, G., De Marzo, C., De Vita, R., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Destelle, J-J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J-F, Druillole, F., Durand, D., Ernenwein, J-P, Escoffier, S., Falchini, E., Favard, S., Fehr, F., Feinstein, F., Ferry, S., Fiorello, C., Flaminio, V., Fratini, K., Fuda, J-L, Galeotti, S., Gallone, J-M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Katz, U., Keller, P., Kok, E., Kok, H., Kooijman, P., Kopper, C., Korolkova, E. V., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Kudryavstev, V. A., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Lambard, G., Languillat, J-C, Laschinsky, H., Lavalle, J., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Lefevre, D., Legou, T., Lelaizant, G., Lim, G., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., McMillan, J. E., Megna, R., Melissas, M., Migneco, E., Milovanovic, A., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Musumeci, M., Naumann-Godo, M., Naumann, C., Niess, V., Noble, T., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H., Perez, A., Petta, C., Piattelli, P., Pillet, R., Pineau, J-P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Rose, H. J., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Rusydi, G., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J-P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Terreni, G., Thompson, L. F., Urbano, F., Valdy, P., Valente, V., Vallage, B., Vaudaine, G., Venekamp, G., Verlaat, B., Vernin, P., de Vries-Uiterweerd, G., van Wijk, R., Wijnker, G., Huberts, P. de Witt, Wobbe, G., de Wolf, E., Yao, A-F, Zaborov, D., Zaccone, H., Zornoza, J. D., and Zuniga, J.

Abstract

ANTARES is a neutrino telescope being deployed in the Mediterranean Sea. It consists of a three-dimensional array of photomultiplier tubes that can detect the Cherenkov light induced by charged particles produced in the interactions of neutrinos with the surrounding medium. High angular resolution can be achieved, in particular, when a muon is produced, provided that the Cherenkov photons are detected with sufficient timing precision. Considerations of the intrinsic time uncertainties stemming from the transit time spread in the photomultiplier tubes and the mechanism of transmission of light in sea water lead to the conclusion that a relative time accuracy of the order of 0.5 ns is desirable. Accordingly, different time calibration systems have been developed for the ANTARES telescope. In this article, a system based on Optical Beacons, a set of external and well-controlled pulsed light sources located throughout the detector, is described. This calibration system takes into account the optical properties of sea water, which is used as the detection volume of the ANTARES telescope. The design, tests, construction and first results of the two types of beacons, LED and laser-based, are presented. (C) 2007 Elsevier B.V. All rights reserved.

Published
2007
Full Text
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22. Studies of a full-scale mechanical prototype line for the ANTARES neutrino telescope and tests of a prototype instrument for deep-sea acoustic measurements

Author

Ageron, M., Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Ardellier-Desages, F., Aslanides, E., Aubert, J. J., Auer, R., Barbarito, E., Basa, S., Battaglieri, M., Bazzotti, M., Becherini, Yvonne, Bethoux, N., Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Castel, D., Castorina, E., Cavasinni, V., Ceechini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Coail, J. Y., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A. -S, Damy, G., van Dantzig, R., DeBonis, G., De Marzo, C., De Vita, R., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Dessa, J. -X, Destelle, J. -J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J-F, Druillole, F., Durand, D., Ernenwein, J. -P, Escoffier, S., Falchini, E., Favard, S., Fehr, F., Feinstein, F., Florello, C., Flaminio, V., Fratini, K., Fuda, J. -L, Galeotti, S., Gallone, J. -M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Guilloux, F., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Katz, U., Keller, P., Kneib, J. P., Kok, E., Kok, H., Kooijman, P., Kopper, C., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Lambard, G., Languillat, J. C., Laschinsky, H., Lavalle, J., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Lefevre, D., Legou, T., Lelaizant, G., Lim, G., Lo Presti, D., Loaec, G., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Mangano, S., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., Megna, R., Melissas, M., Migneco, E., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Motz, H., Musumeci, M., Naumann, C., Naumann-Godo, M., Niess, V., Noble, A., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H. Z., Perez, A., Petta, C., Piattelli, P., Pillet, R., Pineau, J. -P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., Regnier, M., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Rusydi, G., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J. -P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Tasca, L., Terreni, G., Urbano, F., Valdy, P., Valente, V., Vallage, B., Vaudaine, G., Venekamp, G., Verlaat, B., Vernin, P., van Wijk, R., Wijnker, G., Wobbe, G., de Wolf, E., Yao, A. -F, Zaborov, D., Zaccone, H., Zornoza, J. D., Zuniga, J., Ageron, M., Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Ardellier-Desages, F., Aslanides, E., Aubert, J. J., Auer, R., Barbarito, E., Basa, S., Battaglieri, M., Bazzotti, M., Becherini, Yvonne, Bethoux, N., Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Castel, D., Castorina, E., Cavasinni, V., Ceechini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Coail, J. Y., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A. -S, Damy, G., van Dantzig, R., DeBonis, G., De Marzo, C., De Vita, R., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Dessa, J. -X, Destelle, J. -J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J-F, Druillole, F., Durand, D., Ernenwein, J. -P, Escoffier, S., Falchini, E., Favard, S., Fehr, F., Feinstein, F., Florello, C., Flaminio, V., Fratini, K., Fuda, J. -L, Galeotti, S., Gallone, J. -M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Guilloux, F., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Katz, U., Keller, P., Kneib, J. P., Kok, E., Kok, H., Kooijman, P., Kopper, C., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Lambard, G., Languillat, J. C., Laschinsky, H., Lavalle, J., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Lefevre, D., Legou, T., Lelaizant, G., Lim, G., Lo Presti, D., Loaec, G., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Mangano, S., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., Megna, R., Melissas, M., Migneco, E., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Motz, H., Musumeci, M., Naumann, C., Naumann-Godo, M., Niess, V., Noble, A., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H. Z., Perez, A., Petta, C., Piattelli, P., Pillet, R., Pineau, J. -P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., Regnier, M., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Rusydi, G., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J. -P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Tasca, L., Terreni, G., Urbano, F., Valdy, P., Valente, V., Vallage, B., Vaudaine, G., Venekamp, G., Verlaat, B., Vernin, P., van Wijk, R., Wijnker, G., Wobbe, G., de Wolf, E., Yao, A. -F, Zaborov, D., Zaccone, H., Zornoza, J. D., and Zuniga, J.

Abstract

full-scale mechanical prototype line was deployed to a depth of 2500 m to test the leak tightness of the electronics containers and the pressure-resistant properties of an electromechanical cable under evaluation for use in the ANTARES deep-sea neutrino telescope. During a month-long immersion study, line parameter data were taken using miniature autonomous data loggers and shore-based optical time domain reflectometry. Details of the mechanical prototype line, the electromechanical cable and data acquisition are presented. Data taken during the immersion study revealed deficiencies in the pressure resistance of the electromechanical cable terminations at the entry points to the electronics containers. The improvements to the termination, which have been integrated into subsequent detection lines, are discussed. The line also allowed deep-sea acoustic measurements with a prototype hydrophone system. The technical setup of this system is described, and the first results of the data analysis are presented. (c) 2007 Elsevier B.V. All rights reserved.

Published
2007
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23. First results of the instrumentation line for the deep-sea ANTARES neutrino telescope

Author

Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Aslanides, E., Aubert, J. -J, Barbarito, E., Basa, S., Battaglieri, M., Becherini, Yvonne, Bellotti, R., Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bradbury, S. M., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Cartwright, S. L., Castel, D., Castorina, E., Cavasinni, V., Cecchini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A. -S, Damy, G., van Dantzig, R., De Marzo, C., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Dessages-Ardellier, F., Destelle, J. -J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J. -F, Druillole, F., Durand, D., Ernenwein, J. -P, Escoffier, S., Falchini, E., Favard, S., Feinstein, F., Ferry, S., Festy, D., Fiorello, C., Flaminio, V., Galeotti, S., Gallone, J. -M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Karkar, S., Katz, U., Keller, P., Kok, H., Kooijman, P., Kopper, C., Korolkova, E. V., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Kudryavstev, V. A., Lachartre, D., Lafoux, H., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Languillat, J. C., Laschinsky, H., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Legou, T., Lim, G., Lo Nigro, L., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., McMillan, J. E., Megna, R., Melissas, M., Migneco, E., Milovanovic, A., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Musumeci, M., Naumann, C., Naumann-Godo, M., Niess, V., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H., Petta, C., Piattelli, P., Pineau, J. -P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Romita, M., Rose, H. J., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J. -P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Stubert, D., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Terreni, G., Thompson, L. F., Valdy, P., Valente, V., Vallage, B., Venekamp, G., Verlaat, B., Vernin, P., de Vita, R., de Vries, G., van Wijk, R., Huberts, P. de Witt, Wobbe, G., de Wolf, E., Yao, A. -F, Zaborov, D., Zaccone, H., Zornoza, J. D., Zuniga, J., Aguilar, J. A., Albert, A., Ameli, F., Anghinolfi, M., Anton, G., Anvar, S., Aslanides, E., Aubert, J. -J, Barbarito, E., Basa, S., Battaglieri, M., Becherini, Yvonne, Bellotti, R., Beltramelli, J., Bertin, V., Bigi, A., Billault, M., Blaes, R., de Botton, N., Bouwhuis, M. C., Bradbury, S. M., Bruijn, R., Brunner, J., Burgio, G. F., Busto, J., Cafagna, F., Caillat, L., Calzas, A., Capone, A., Caponetto, L., Carmona, E., Carr, J., Cartwright, S. L., Castel, D., Castorina, E., Cavasinni, V., Cecchini, S., Ceres, A., Charvis, P., Chauchot, P., Chiarusi, T., Circella, M., Colnard, C., Compere, C., Coniglione, R., Cottini, N., Coyle, P., Cuneo, S., Cussatlegras, A. -S, Damy, G., van Dantzig, R., De Marzo, C., Dekeyser, I., Delagnes, E., Denans, D., Deschamps, A., Dessages-Ardellier, F., Destelle, J. -J, Dinkespieler, B., Distefano, C., Donzaud, C., Drogou, J. -F, Druillole, F., Durand, D., Ernenwein, J. -P, Escoffier, S., Falchini, E., Favard, S., Feinstein, F., Ferry, S., Festy, D., Fiorello, C., Flaminio, V., Galeotti, S., Gallone, J. -M, Giacomelli, G., Girard, N., Gojak, C., Goret, Ph., Graf, K., Hallewell, G., Harakeh, M. N., Hartmann, B., Heijboer, A., Heine, E., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hoffman, C., Hogenbirk, J., Hubbard, J. R., Jaquet, M., Jaspers, M., de Jong, M., Jouvenot, F., Kalantar-Nayestanaki, N., Kappes, A., Karg, T., Karkar, S., Katz, U., Keller, P., Kok, H., Kooijman, P., Kopper, C., Korolkova, E. V., Kouchner, A., Kretschmer, W., Kruijer, A., Kuch, S., Kudryavstev, V. A., Lachartre, D., Lafoux, H., Lagier, P., Lahmann, R., Lamanna, G., Lamare, P., Languillat, J. C., Laschinsky, H., Le Guen, Y., Le Provost, H., Van Suu, A. Le, Legou, T., Lim, G., Lo Nigro, L., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Lyashuk, V., Marcelin, M., Margiotta, A., Masullo, R., Mazeas, F., Mazure, A., McMillan, J. E., Megna, R., Melissas, M., Migneco, E., Milovanovic, A., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Musumeci, M., Naumann, C., Naumann-Godo, M., Niess, V., Olivetto, C., Ostasch, R., Palanque-Delabrouille, N., Payre, P., Peek, H., Petta, C., Piattelli, P., Pineau, J. -P, Poinsignon, J., Popa, V., Pradier, T., Racca, C., Randazzo, N., van Randwijk, J., Real, D., van Rens, B., Rethore, F., Rewiersma, P., Riccobene, G., Rigaud, V., Ripani, M., Roca, V., Roda, C., Rolin, J. F., Romita, M., Rose, H. J., Rostovtsev, A., Roux, J., Ruppi, M., Russo, G. V., Salesa, F., Salomon, K., Sapienza, P., Schmitt, F., Schuller, J. -P, Shanidze, R., Sokalski, I., Spona, T., Spurio, M., van der Steenhoven, G., Stolarczyk, T., Streeb, K., Stubert, D., Sulak, L., Taiuti, M., Tamburini, C., Tao, C., Terreni, G., Thompson, L. F., Valdy, P., Valente, V., Vallage, B., Venekamp, G., Verlaat, B., Vernin, P., de Vita, R., de Vries, G., van Wijk, R., Huberts, P. de Witt, Wobbe, G., de Wolf, E., Yao, A. -F, Zaborov, D., Zaccone, H., Zornoza, J. D., and Zuniga, J.

Abstract

In 2005, the ANTARES Collaboration deployed and operated at a depth of 2500 m a so-called Mini Instrumentation Line equipped with Optical Modules (MILOM) at the ANTARES site. The various data acquired during the continuous operation from April to December 2005 of the MILOM confirm the satisfactory performance of the Optical Modules, their front-end electronics and readout system. as well as the calibration devices of the detector. The in situ measurement of the Optical Module time response yields a resolution better than 0.5 ns. The performance of the acoustic positioning system, which enables the spatial reconstruction of the ANTARES detector with a precision of about 10 cm, is verified. These results demonstrate that with the full ANTARES neutrino telescope the design angular resolution of better than 0.3 degrees can be realistically achieved.

Published
2006
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25. Transmission of light in deep sea water at the site of the Antares neutrino telescope

Author

Aguilar, J.A., primary, Albert, A., additional, Amram, P., additional, Anghinolfi, M., additional, Anton, G., additional, Anvar, S., additional, Ardellier-Desages, F.E., additional, Aslanides, E., additional, Aubert, J-J., additional, Azoulay, R., additional, Bailey, D., additional, Basa, S., additional, Battaglieri, M., additional, Becherini, Y., additional, Bellotti, R., additional, Beltramelli, J., additional, Bertin, V., additional, Billault, M., additional, Blaes, R., additional, Blanc, F., additional, Bland, R.W., additional, de Botton, N., additional, Boulesteix, J., additional, Bouwhuis, M.C., additional, Brooks, C.B., additional, Bradbury, S.M., additional, Bruijn, R., additional, Brunner, J., additional, Bugeon, F., additional, Burgio, G.F., additional, Cafagna, F., additional, Calzas, A., additional, Caponetto, L., additional, Carmona, E., additional, Carr, J., additional, Cartwright, S.L., additional, Cecchini, S., additional, Charvis, P., additional, Circella, M., additional, Colnard, C., additional, Compère, C., additional, Croquette, J., additional, Cooper, S., additional, Coyle, P., additional, Cuneo, S., additional, Damy, G., additional, van Dantzig, R., additional, Deschamps, A., additional, Marzo, C. De, additional, Destelle, J.-J., additional, Vita, R. De, additional, Dinkelspiler, B., additional, Dispau, G., additional, Drougou, J.-F., additional, Druillole, F., additional, Engelen, J., additional, Favard, S., additional, Feinstein, F., additional, Ferry, S., additional, Festy, D., additional, Fopma, J., additional, Fuda, J.-L., additional, Gallone, J.-M., additional, Giacomelli, G., additional, Girard, N., additional, Goret, P., additional, Gournay, J.-F., additional, Hallewell, G., additional, Hartmann, B., additional, Heijboer, A., additional, Hello, Y., additional, Hernández-Rey, J.J., additional, Herrouin, G., additional, Hößl, J., additional, Hoffmann, C., additional, Hubbard, J.R., additional, Jaquet, M., additional, de Jong, M., additional, Jouvenot, F., additional, Kappes, A., additional, Karg, T., additional, Karkar, S., additional, Karolak, M., additional, Katz, U., additional, Keller, P., additional, Kooijman, P., additional, Korolkova, E.V., additional, Kouchner, A., additional, Kretschmer, W., additional, Kudryavtsev, V.A., additional, Lafoux, H., additional, Lagier, P., additional, Lamare, P., additional, Languillat, J.-C., additional, Laubier, L., additional, Legou, T., additional, Guen, Y. Le, additional, Provost, H. Le, additional, Van Suu, A. Le, additional, Nigro, L. Lo, additional, Presti, D. Lo, additional, Loucatos, S., additional, Louis, F., additional, Lyashuk, V., additional, Magnier, P., additional, Marcelin, M., additional, Margiotta, A., additional, Maron, C., additional, Massol, A., additional, Mazéas, F., additional, Mazeau, B., additional, Mazure, A., additional, McMillan, J.E., additional, Michel, J.-L., additional, Millot, C., additional, Milovanovic, A., additional, Montanet, F., additional, Montaruli, T., additional, Morel, J.-P., additional, Moscoso, L., additional, Nezri, E., additional, Niess, V., additional, Nooren, G.J., additional, Ogden, P., additional, Olivetto, C., additional, Palanque-Delabrouille, N., additional, Payre, P., additional, Petta, C., additional, Pineau, J.-P., additional, Poinsignon, J., additional, Popa, V., additional, Potheau, R., additional, Pradier, T., additional, Racca, C., additional, Randazzo, N., additional, Real, D., additional, van Rens, B.A.P., additional, Réthoré, F., additional, Ripani, M., additional, Roca-Blay, V., additional, Romeyer, A., additional, Rollin, J.-F., additional, Romita, M., additional, Rose, H.J., additional, Rostovtsev, A., additional, Ruppi, M., additional, Russo, G.V., additional, Sacquin, Y., additional, Saouter, S., additional, Schuller, J.-P., additional, Schuster, W., additional, Sokalski, I., additional, Suvorova, O., additional, Spooner, N.J.C., additional, Spurio, M., additional, Stolarczyk, T., additional, Stubert, D., additional, Taiuti, M., additional, Thompson, L.F., additional, Tilav, S., additional, Usik, A., additional, Valdy, P., additional, Vallage, B., additional, Vaudaine, G., additional, Vernin, P., additional, Virieux, J., additional, Vladimirsky, E., additional, de Vries, G., additional, de Witt Huberts, P., additional, de Wolf, E., additional, Zaborov, D., additional, Zaccone, H., additional, Zakharov, V., additional, Zavatarelli, S., additional, de Zornoza, J.D., additional, and Zúñiga, J., additional

Published
2005
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