Author: "Gemini Observatory" / Publication Year Range: Last 50 years - Searchworks@Jio Institute Digital Library Search Results

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139 results on '"Gemini Observatory"'

1. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

Author: Gemini Observatory, National Science Foundation (US), National Research Council of Canada, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brasil), Korea Astronomy and Space Science Institute, European Southern Observatory, National Aeronautics and Space Administration (US), German Research Foundation, European Commission, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andrew S., Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, Gemini Observatory, National Science Foundation (US), National Research Council of Canada, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brasil), Korea Astronomy and Space Science Institute, European Southern Observatory, National Aeronautics and Space Administration (US), German Research Foundation, European Commission, Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andrew S., Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, and Wechsler, Risa
Abstract: The See Change survey was designed to make z > 1 cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope (HST) spanning the redshift range z = 1.13-1.75, discovering 57 likely transients and 27 likely SNe Ia at z ~ 0.8-2.3. As in similar previous surveys, this proved to be a highly efficient use of HST for supernova observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star formation rates. We find that the resulting number of SNe Ia per orbit is a factor of ~8 higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and supernova discoveries. Novel features include fully blinded supernova searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 mag of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper. * Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under programs 13677, 14327.
Published: 2021

2. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author: Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., Buddelmeijer, H., Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., and Buddelmeijer, H.
Abstract: The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.© 2018. The American Astronomical Society.
Published: 2018

3. A Massively Parallel Simulation Code for AEOS and Astronomical Adaptive Optics

Author: ASSOCIATION OF UNIVERSITIES FOR RESEARCH IN ASTRONOMY-GEMINI HILO HI GEMINI OBSERVATORY, Ellerbroek, Brent, ASSOCIATION OF UNIVERSITIES FOR RESEARCH IN ASTRONOMY-GEMINI HILO HI GEMINI OBSERVATORY, and Ellerbroek, Brent
Abstract: This is the second and final status report for a project to port an existing parallel adaptive optics (AO) simulation code to the Huinalu cluster at the Maui High Performance Computing Center, and to upgrade the simulation to provide an improved modeling capability for both the AEOS AO system and the astronomical AO systems proposed for future extremely large telescopes (ELTs). The functional elements of the simulation include the basic AO components, disturbances, and control algorithms necessary for scalar wave diffraction modeling of ground-based natural guide star (NGS) AO, laser guide star (LGS) AO, and multi-conjugate AO (MCAO) imaging systems, as illustrated in figure 1 below.
Published: 2004

4. Entering into the Wide Field Adaptive Optics Era in the Northern Hemisphere

Author: Gaetano Sivo, John Blakeslee, Jennifer Lotz, Henry Roe, Morten Andersen, Julia Scharwächter, David Palmer, Scot Kleinman, Andy Adamson, Paul Hirst, Eduardo Marin, Laure Catala, Marcos van Dam, Goodsell, Stephen J., Natalie Provost, Ruben Diaz, Inger Jorgensen, Hwihyun Kim, Marie Lemoine-Busserolle, Celia Blain, Mark Chun, Mark Ammons, Julian Christou, Charlotte Bond, Suresh Sivanandam, Paolo Turri, Peter Wizinowich, Carlos Correia, Benoit Neichel, Jean-Pierre Véran, Simone Esposito, Masen Lamb, Thierry Fusco, François Rigaut, Eric Steinbring, Laboratoire de Traitement et Transport de l'Information (L2TI), Université Paris 13 (UP13)-Institut Galilée-Université Sorbonne Paris Cité (USPC), National Research Council of Canada (NRC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Lawrence Livermore National Laboratory (LLNL), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Université Paris-Sud - Paris 11 (UP11)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Flat Wavefronts, Gemini Observatory, University of Hawai'i [Hilo], 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), W.M. Keck Observatory, University of Coimbra, University of Coimbra [Portugal] (UC), NRC Herzberg Institute of Astrophysics, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut Galilée-Université Paris 13 (UP13)-Université Sorbonne Paris Cité (USPC), École normale supérieure - Paris (ENS Paris), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), and Neichel, Benoit
Subjects: [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [PHYS.ASTR.SR] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; Gemini Observatory plans to revitalize its AO facility at Gemini North for the benefit of the US and international user community, including a funded MCAO system now in development. Our Strategic Plan calls for the development of a GLAO system enabled by an Adaptive Secondary Mirror. We discuss our plans, progress, and funding outlook.
Published: 2019

5. Gemini North Adaptive Optics (GNAO): an MCAO system for Gemini North towards Conceptual Design

Author: Gaetano Sivo, David Palmer, Julia Scharwächter, Morten Andersen, Natalie Provost, Eduardo Marin, Marcos van Dam, Brian Chinn, Emmanuel Chirre, Charles Cavedoni, Thomas Schneider, Stacy Kang, Paul Hirst, William Rambold, Angelic Ebbers, Pedro Gigoux, Laure Catala, Thomas Hayward, John Blakeslee, Henry Roe, Jennifer Lotz, Scot Kleinman, Manuel Lazo, Celia Blain, Suresh Sivanandam, Anja Feldmeier-Krause, Mark Ammons, Chadwick Trujillo, Chris Packham, Franck Marchis, Julian Christou, James Jee, John Bally, Mike Pierce, Thomas Puzia, Paolo Turri, Hwihyun Kim, Meg Schwamb, Trent Dupuy, Ruben Diaz, Rodrigo Carrasco, Benoit Neichel, Carlos Correia, Eric Steinbring, François Rigaut, Jean-Pierre Véran, Mark Chun, Masen Lamb, Scott Chapman, Simone Esposito, Thierry Fusco, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Gemini North Observatory, Flat Wavefronts, Gemini Observatory, Northern Operations Center, Gemini Observatory, Tucson, University of Toronto [Scarborough, Canada], University of Chicago, Lawrence Livermore National Laboratory (LLNL), Northern Arizona University [Flagstaff], The University of Texas at San Antonio (UTSA), Search for Extraterrestrial Intelligence Institute (SETI), Large Binocular Telescope Observatory [Tucson] (LBTO), Younsei University, Seoul, South Korea, University of Colorado [Boulder], University of Wyoming (UW), PONTIFICA UNIVERSIDAD CATOLICA DE CHILE SANTIAGO DE CHILE CHL, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), University of California [Berkeley], University of California, 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), W.M. Keck Observatory, NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Australian National University (ANU), Institute for astronomy [Hilo, Hawaï], University of Hawai'i [Hilo], Dalhousie University [Halifax], INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Pontificia Universidad Católica de Chile (UC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of Toronto at Scarborough, University of California [Berkeley] (UC Berkeley), and University of California (UC)
Subjects: [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], Adaptive Optics, Gemini Observatory, Multi-conjugate adaptive optics, High Angular Resolution, GNAO, GeMS
Abstract: International audience; Gemini Observatory has been awarded from the National Science Foundation a major fund to build a new state-of-the-art Multi Conjugate Adaptive Optics facility for Gemini North on Maunakea called GNAO. The current Telephone: 1+56 51 2205 642 baseline system will use two lasers each split in two to create an artificial constellation of four laser guide star to measure the distortions caused by the atmosphere. At least two deformable mirror conjugated to 0km and the main altitude layer above Maunakea will be used to correct these distortions. The facility will be designed to feed future instrumentation, initially a near infrared imager and potentially a visiting 4-arm multi object adaptive optics IFU spectrograph. 1 In this paper I will present the main characteristics of this exciting facility, its promises and its challenges. I will also present its conceptual design and results of trade studies conducted within the team and the Gemini Adaptive Optics Working Group. The expected first light is for October 2024.
Published: 2019

6. The discovery and nature of the optical transient CSS100217:102913+404220

Author: Christensen, E. [Gemini Observatory, La Serena (Chile)]
Published: 2011
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7. Real-time implementation of an LQG tip-tilt controller for regular science observation on GeMS

Author: Caroline Kulcsár, Cristian Moreno, Vincent Garrel, Vanessa Montes, Pedro Gigoux, Benoit Neichel, Chad Trujillo, Jean-Marc Conan, Rémy Juvénal, Jeff Donahue, Marcos A. van Dam, Gaetano Sivo, Rodrigo Carrasco, Henri-François Raynaud, Lucie Leboulleux, Cyril Petit, Eduardo Marin, William Rambold, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Laboratoire Charles Fabry / Spim, Laboratoire Charles Fabry (LCF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), W.M. Keck Observatory, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire Charles Fabry / Imagerie et Information, Institut d'Optique Graduate School (IOGS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Gemini Observatory, University of Hawai'i [Hilo], Flat Wavefronts, 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), SPIE, Enrico Marchetti, Laird M. Close, and Jean-Pierre Véran
Subjects: Optimal Control, Linear-quadratic-Gaussian control, 01 natural sciences, [SPI.AUTO]Engineering Sciences [physics]/Automatic, 010309 optics, Control theory, 0103 physical sciences, Gemini Planet Imager, LQG, 010303 astronomy & astrophysics, GeMS, ComputingMilieux_MISCELLANEOUS, Simulation, Physics, Spectral density, Natural frequency, Kalman filter, Optimal control, Multi-Conjugated Adaptive Optics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Autoregressive model, Integrator, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Adaptive Optics, Vibrations Rejection, Kalman Filter
Abstract: International audience; AO systems aim at detecting and correcting for optical distortions induced by atmospheric turbulences. They are also extremely sensitive to extraneous sources of perturbation such as vibrations, which degrade the performance. The Gemini South telescope has currently two main AO systems: the Gemini Multi Conjugated AO System GeMS and the Gemini Planet Imager GPI. GeMS is operational and regularly used for science observation delivering close to diffraction limit resolution over a large field of view (85×85 arcsec2). Performance limitation due to the use of an integrator for tip-tilt control is here explored. In particular, this type of controller does not allow for the mitigation of vibrations with an arbitrary natural frequency. We have thus implemented a tip-tilt Linear Quadratic Gaussian (LQG) controller with different underlying perturbation models: (i) a sum of autoregressive models of order 2 identified from an estimated power spectrum density (s-AR2) of the perturbation,1 already tested on CANARY2 and routinely used on SPHERE;3 (ii) cascaded ARMA models of order 2 identified using prediction error minimization (c-PEM) as proposed in.4, 5 Both s-AR2 and c-PEM were parameterized to produce tip or tilt state-space models up to order 20 and 30 respectively. We discuss the parallelized implementation in the real time computer and the expected performance. On-sky tests are scheduled during the November 2016 run or the January 2017 run.
Published: 2016
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8. On-sky validation of an optimal LQG control with vibration mitigation: from the CANARY Multi-Object Adaptive Optics demonstrator to the Gemini Multi-Conjugated Adaptive Optics facility

Author: Sivo, Gaetano, Kulcsár, Caroline, Conan, Jean-Marc, Raynaud, Henri-François, Gendron, Eric, Basden, Alastair G., Gratadour, Damien, Morris, Tim J., Petit, Cyril, Meimon, Serge, Rousset, Gérard, Garrel, Vincent, Neichel, Benoit, Van Dam, Marcos, Marin, Eduardo, Carrasco, Rodrigo, Schirmer, Mischa, Rambold, William, Moreno, Cristian, Montes, Vanessa, Hardie, Kayla, Trujillo, Chadwick, Gemini Observatory, Southern Operations Center, International Occultation Timing Association (IOTA), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre for Advanced Instrumentation, Department of Physics, Durham University (CfAI), 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), Flat Wavefronts, Gemini Observatory, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Laboratoire Charles Fabry / Spim, Laboratoire Charles Fabry (LCF), Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Centre for Advanced Instrumentation, Durham University, W.M. Keck Observatory, Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SPI.AUTO]Engineering Sciences [physics]/Automatic
Abstract: International audience; Adaptive optics provides real time correction of wavefront perturbations on ground-based telescopes and allow to reach the diffraction limit performances. Optimizing control and performance is a key issue for ever more demanding instruments on ever larger telescopes affected not only by atmospheric turbulence, but also by vibrations, windshake and tracking errors. Linear Quadratic Gaussian control achieves optimal correction when provided with a temporal model of the disturbance. We present in this paper the first on-sky results of a Kalman filter based LQG control with vibration mitigation on the CANARY instrument at the Nasmyth platform of the 4.2-m William Herschel Telescope (La Palma, Spain). The results demonstrate a clear improvement of performance for full LQG compared with standard integrator control, and assess the additional improvement brought by vibration filtering with a tip-tilt model identified from on-sky data (by 10 points of Strehl ratio), thus validating the strategy retained on the instrument SPHERE (eXtreme-AO system for extra-solar planets detection and characterization) at the VLT. The MOAO on-sky pathfinder CANARY features two AO configurations that have both been tested: single- conjugated AO and multi-object AO with NGS and NGS Rayleigh LGS, together with vibration mitigation on tip and tilt modes. We finally present the ongoing development done to commission such a control law on a regular Sodium laser Multi-Conjuagated Adaptive Optics (MCAO) system GeMS at the 8-m Gemini South Telescope. This implementation does not require new hardware and is already available in the real-time computer.
Published: 2015

9. Gemini Planet Imager Observational Calibrations I: Overview of the GPI Data Reduction Pipeline

Author: Markus Hartung, Jean-Baptiste Ruffio, Patrick Ingraham, Christian Marois, James R. Graham, David Lafrenière, Mathilde Beaulieu, David Palmer, Naru Sadakuni, Fredrik T. Rantakyrö, Michael P. Fitzgerald, Abhijith Rajan, Jason J. Wang, Sandrine Thomas, Jeffrey Chilcote, Pascale Hibon, Anand Sivaramakrishnan, James E. Larkin, Alexandra Z. Greenbaum, Laurent Pueyo, Max Millar-Blanchaer, Jennifer Patience, Marshall D. Perrin, Stephen J. Goodsell, Schuyler Wolff, Robert J. De Rosa, Jean-François Lavigne, Dmitry Savransky, Zachary H. Draper, Kimberly Ward-Duong, Rémi Soummer, Franck Marchis, Jérôme Maire, Sloane J. Wiktorowicz, Bruce Macintosh, Quinn Konopacky, Kathleen Labrie, René Doyon, Space Telescope Science Institute (STScI), Dunlap Institute for Astronomy and Astrophysics, Univ. of Toronto (Canada), Kavli Institute for Particle Astrophysics and Cosmology, Stanford Univ. (United States), Center for Radiophysics and Space Research, Cornell University (CRSR), Department of Physics and Astronomy, University of Toronto, Johns Hopkins University (JHU), SETI Institute (United States), Univ. of California, Berkeley (United States), Department of Physics and Astronomy, University of Victoria, Gemini Observatory, Southern Operations Center, National Research Council of Canada (NRC), Arizona State University, University of California, Los Angeles (UCLA), Univ. de Montreal (Canada), Lawrence Livermore National Laboratory (LLNL), Gemini Observatory, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), ABB, Inc. (Canada), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), NASA Ames Research Center (ARC), and University of California, Santa Cruz (UCSC)
Subjects: High contrast imaging, 010504 meteorology & atmospheric sciences, Infrared, Computer science, Pipeline (computing), Astronomy, Polarimetry, FOS: Physical sciences, 01 natural sciences, Integral Field Spectroscopy, Integral field spectrograph, Software, Spectrographs, Computer graphics (images), Scientific analysis, 0103 physical sciences, Gemini Planet Imager, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Pipelines, Earth and Planetary Astrophysics (astro-ph.EP), Data reduction, business.industry, Reduction systems, Open source software, Data handling, Exoplanet, Polarization modes, Extrasolar planets, Calibration, Exo-planets, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Polarimeters, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Gemini Planet Imager (GPI) has as its science instrument an infrared integral field spectrograph/polarimeter (IFS). Integral field spectrographs are scientificially powerful but require sophisticated data reduction systems. For GPI to achieve its scientific goals of exoplanet and disk characterization, IFS data must be reconstructed into high quality astrometrically and photometrically accurate datacubes in both spectral and polarization modes, via flexible software that is usable by the broad Gemini community. The data reduction pipeline developed by the GPI instrument team to meet these needs is now publicly available following GPI's commissioning. This paper, the first of a series, provides a broad overview of GPI data reduction, summarizes key steps, and presents the overall software framework and implementation. Subsequent papers describe in more detail the algorithms necessary for calibrating GPI data. The GPI data reduction pipeline is open source, available from planetimager.org, and will continue to be enhanced throughout the life of the instrument. It implements an extensive suite of task primitives that can be assembled into reduction recipes to produce calibrated datasets ready for scientific analysis. Angular, spectral, and polarimetric differential imaging are supported. Graphical tools automate the production and editing of recipes, an integrated calibration database manages reference files, and an interactive data viewer customized for high contrast imaging allows for exploration and manipulation of data., Ground-Based and Airborne Instrumentation for Astronomy V, June 22-26, 2014, Series: Proceedings of SPIE; no. 9147
Published: 2014
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10. Active Luminous Blue Variables in the Large Magellanic Cloud

Author: Angeloni, Rodolfo [Gemini Observatory, Colina El Pino, Casilla 603, La Serena (Chile)]
Published: 2017
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11. Fading AGN Candidates: AGN Histories and Outflow Signatures

Author: Schirmer, Mischa [Gemini Observatory, La Serena (Chile)]
Published: 2017
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12. OPTICAL SPECTROSCOPY OF THE HIGH-MASS γ-RAY BINARY 1FGL J1018.6−5856: A PROBABLE NEUTRON STAR PRIMARY

Author: Salinas, Ricardo [Gemini Observatory, Casilla 603, La Serena (Chile)]
Published: 2015
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13. HST/STIS ULTRAVIOLET SPECTROSCOPY OF THE COMPONENTS OF THE MASSIVE TRIPLE STAR δ ORI A

Author: Chené, André-Nicolas [Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720 (United States)]
Published: 2015
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14. Discovery and characteristics of the rapidly rotating active asteroid (62412) 2000 SY178 in the main belt

Author: Trujillo, Chadwick [Gemini Observatory, 670 North A‘ohoku Place, Hilo, HI 96720 (United States)]
Published: 2015
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15. THE SUBARU HIGH-z QUASAR SURVEY: DISCOVERY OF FAINT z ∼ 6 QUASARS

Author: Hibon, Pascale [Gemini Observatory, La Serena (Chile)]
Published: 2015
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16. Spectroscopic study of extended star clusters in dwarf galaxy NGC 6822

Author: Miller, Bryan [Gemini Observatory, Casilla 603, La Serena (Chile)]
Published: 2014
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17. Investigating the origin of the spectral line profiles of the Hot Wolf–Rayet Star WR 2

Author: Christoph Baranec, Evelyne Alecian, Paul A. Crowther, Étienne Artigau, Olivier Schnurr, André-Nicolas Chené, C. Ziegler, Gregg A. Wade, Nicole St-Louis, A. F. J. Moffat, Nicholas M. Law, Noel D. Richardson, Reed Riddle, Gemma Rate, Gemini Observatory, Northern Operations Center, Département de Physique [Montréal], Université de Montréal [Montréal], School of engineering sciences, University of Southampton, Leibniz-Institut für Astrophysik Potsdam (AIP), Department of Physics and Astronomy [Sheffield], University of Sheffield [Sheffield], Royal Military College of Canada, Department of Physics, Ritter Observatory, University of Toledo, Institute for Astronomy, University of Hawai'i at Manoa, Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Montréal (UdeM), Ritter planetarium and Brooks Observatory, University of Toledo, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])
Subjects: Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Absorption spectroscopy, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, Spectral line, Magnetic field, Wolf–Rayet star, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS
Abstract: The hot WN star WR2 (HD6327) has been claimed to have many singular characteristics. To explain its unusually rounded and relatively weak emission line profiles, it has been proposed that WR2 is rotating close to break-up with a magnetically confined wind. Alternatively, the line profiles could be explained by the dilution of WR2's spectrum by that of a companion. In this paper, we present a study of WR2 using near-infrared AO imaging and optical spectroscopy and polarimetry. Our spectra reveal the presence of weak photospheric absorption lines from a ~B2.5-4V companion, which however contributes only ~5-10% to the total light, suggesting that the companion is a background object. Therefore, its flux cannot be causing any significant dilution of the WR star's emission lines. The absence of intrinsic linear continuum polarization from WR2 does not support the proposed fast rotation. Our Stokes V spectrum was not of sufficient quality to test the presence of a moderately strong organized magnetic field but our new modelling indicates that to confine the wind the putative magnetic field must be significantly stronger than was previously suggested sufficiently strong as to make its presence implausible., 12 pages, 9 figures
Published: 2019
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18. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries

Author: Risa H. Wechsler, Henk Hoekstra, Hans Böhringer, Zachary Raha, S. Dixon, Daniel Stern, Greg Aldering, X. Huang, J. Meyers, J. Nordin, Mark Brodwin, Susana E. Deustua, Rene Fassbender, E. Rozo, Dragan Huterer, Michael D. Gladders, Ravi Gupta, Rahman Amanullah, J. S. Santos, Mike Yen, Greta Chappell, Alex G. Kim, A. S. Fruchter, A. L. Spadafora, Tracy Webb, Isobel Hook, David Rubin, Hendrik Hildebrandt, Miles Currie, Eli S. Rykoff, Caroline Sofiatti, Brian Hayden, Ariel Goobar, Clare Saunders, Nao Suzuki, Steven Williams, Saul Perlmutter, Kyle Boone, Peter Eisenhardt, Chris Lidman, Anthony H. Gonzalez, Johan Richard, Parker Fagrelius, Kyle Luther, M. James Jee, Piero Rosati, Carlos Cunha, Adam Muzzin, Reynald Pain, A. Stanford, Kyle Barbary, Pilar Ruiz-Lapuente, Eric V. Linder, Gillian Wilson, Marek Kowalski, Gemini Observatory, National Science Foundation (US), National Research Council of Canada, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brasil), Korea Astronomy and Space Science Institute, European Southern Observatory, National Aeronautics and Space Administration (US), German Research Foundation, European Commission, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Supernova Cosmology Project, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, NO, Photometry (optics), 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Galaxy cluster, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Type Ia supernovae, Type La Supernovae, Astronomy and Astrophysics, Redshift, Supernova, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 21 pags., 12 figs., 4 tabs., The See Change survey was designed to make z > 1 cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope (HST) spanning the redshift range z = 1.13-1.75, discovering 57 likely transients and 27 likely SNe Ia at z ~ 0.8-2.3. As in similar previous surveys, this proved to be a highly efficient use of HST for supernova observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star formation rates. We find that the resulting number of SNe Ia per orbit is a factor of ~8 higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and supernova discoveries. Novel features include fully blinded supernova searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 mag of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper. * Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under programs 13677, 14327., Based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Based on observations collected at the Table 4. European Organisation for Astronomical Research in the Southern Hemisphere under ESO program(s) 294.A-5025(A), 095.A-0830(A, B, C), 096.A-0926(B, C), 097.A-0442(A, B, C), and 0100.A-0851(A). G.W. acknowledges support from the National Science Foundation through grant AST-1517863, by HST program numbers GO-13677/14327.01 and GO-15294, and by grant No. 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). G.A. and R.G. acknowledge support from HST program NASA HST-GO14163.002-A, and by grant No. NNH16AC25I issued through NASA ADAP. M. J. J. acknowledges support for the current research from the National Research Foundation (NRF) of Korea under the programs 2017R1A2B2004644 and 2020R1A4A2002885. H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). Support for program numbers GO-13677/14327.01 and GO-15294 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work was also partially supported by the Office of Science, Office of High Energy Physics, of the U.S. Department of Energy, under contract no. DE-AC02-05CH11231. Facilities: Hubble Space Telescope, Keck:I (LRIS), Keck:I (MOSFIRE), VLT, Gemini, GTC, Subaru. Software: astropy (Astropy Collaboration 2013), DrizzlePac (Gonzaga et al. 2012), iPython (Pérez & Granger 2007), Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2011), SEP (Barbary 2016), scikit-learn (Pedregosa et al. 2011), SciPy
Published: 2021
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19. ICE AND DUST IN THE PRESTELLAR DARK CLOUD LYNDS 183: PREPLANETARY MATTER AT THE LOWEST TEMPERATURES

Author: Adamson, A. [Gemini Observatory, Southern Operations Center, Casilla 603, La Serena (Chile)]
Published: 2013
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20. STELLAR POPULATIONS AND EVOLUTION OF EARLY-TYPE CLUSTER GALAXIES: CONSTRAINTS FROM OPTICAL IMAGING AND SPECTROSCOPY OF z = 0.5-0.9 GALAXY CLUSTERS

Author: Chiboucas, Kristin [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2013
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21. THE AFTERGLOW AND ULIRG HOST GALAXY OF THE DARK SHORT GRB 120804A

Author: Roth, K. [Gemini Observatory, 670 North Aohoku Place, Hilo, HI 96720 (United States)]
Published: 2013
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22. RED AND DEAD: THE PROGENITOR OF SN 2012aw IN M95

Author: Stephens, A [Gemini Observatory, 670 North Aohoku Place, Hilo, HI 96720 (United States)]
Published: 2012
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23. TWO EXTRAORDINARY SUBSTELLAR BINARIES AT THE T/Y TRANSITION AND THE Y-BAND FLUXES OF THE COOLEST BROWN DWARFS {sup ,}

Author: Leggett, S. [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2012
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24. 2007 TY430: A COLD CLASSICAL KUIPER BELT TYPE BINARY IN THE PLUTINO POPULATION

Author: Trujillo, Chadwick [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2012
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25. THE SPECTROSCOPIC CLASSIFICATION AND EXPLOSION PROPERTIES OF SN 2009nz ASSOCIATED WITH GRB 091127 AT z = 0.490

Author: Roth, K [Gemini Observatory, 670 N. Aohoku Place Hilo, HI 96720 (United States)]
Published: 2011
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26. A SOUTHERN SKY AND GALACTIC PLANE SURVEY FOR BRIGHT KUIPER BELT OBJECTS

Author: Trujillo, Chadwick [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2011
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27. HIGH-RESOLUTION MID-INFRARED IMAGING OF THE CIRCUMSTELLAR DISKS OF HERBIG Ae/Be STARS

Author: Fisher, R [Gemini Observatory Northern Operations Center, Hilo, HI 96720 (United States)]
Published: 2011
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28. STAR CLUSTERS AS TRACERS OF INTERACTIONS IN STEPHAN'S QUINTET (HICKSON COMPACT GROUP 92)

Author: Trancho, G [Gemini Observatory, Casilla 603, La Serena (Chile)]
Published: 2011
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29. JET PROPULSION OF WIND EJECTA FROM A MAJOR FLARE IN THE BLACK HOLE MICROQUASAR SS433

Author: Hirst, Paul [Gemini Observatory, 670 North A'ohoku Place, University Park, Hilo, HI 96720 (United States)]
Published: 2011
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30. THE ULTIMATE LIGHT CURVE OF SN 1998bw/GRB 980425

Author: Candia, Pablo [Gemini Observatory, Casilla 603, La Serena (Chile)]
Published: 2011
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31. ORBITAL SOLUTIONS FOR TWO YOUNG, LOW-MASS SPECTROSCOPIC BINARIES IN OPHIUCHUS

Author: Rodgers, B [Gemini Observatory, Gemini South, AURA/Chile, P.O. Box 26732, Tucson, AZ 85726 (United States)]
Published: 2011
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32. INVESTIGATING THE COSMIC-RAY IONIZATION RATE NEAR THE SUPERNOVA REMNANT IC 443 THROUGH H{sup +}{sub 3} OBSERVATIONS

Author: Geballe, T [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2010
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33. AN AROMATIC INVENTORY OF THE LOCAL VOLUME

Author: Lee, H [Gemini Observatory, Southern Operations Center, Casilla 603, La Serena (Chile)]
Published: 2010
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34. CONSTRAINING THE ENVIRONMENT OF CH{sup +} FORMATION WITH CH{sup +}{sub 3} OBSERVATIONS

Author: Geballe, T [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2010
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35. DASCH DISCOVERY OF LARGE AMPLITUDE {approx}10-100 YEAR VARIABILITY IN K GIANTS

Author: Laycock, Silas [Gemini Observatory, 670 North Aohoku Place, Hilo, HI 96720 (United States)]
Published: 2010
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36. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4

Author: Leindert Boogaard, Lutz Wisotzki, Valentin Mauerhofer, Roland Bacon, Joop Schaye, J. Kerutt, Wolfram Kollatschny, Tanya Urrutia, Michael V. Maseda, Kasper B. Schmidt, Thierry Contini, Simon Conseil, Guillaume Mahler, Edmund Christian Herenz, Floriane Leclercq, Johan Richard, Mirko Krumpe, Jorryt Matthee, Anna Feltre, Themiya Nanayakkara, Leibniz Institute for Astrophysics Potsdam (AIP), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics - instrumentation and methods for astrophysics, Electron density, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics - astrophysics of galaxies, Astrophysics, Photoionization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Methods: observational, 0103 physical sciences, Galaxy formation and evolution, Emission spectrum, Techniques: imaging spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Galaxies: high-redshift, Astronomy and Astrophysics, Galaxy, Redshift, ISM: lines and bands, Galaxies: ISM, Space and Planetary Science, Ultraviolet: galaxies
Abstract: [Abbreviated] Rest-frame UV emission lines probe physical parameters of the emitting star-forming galaxies and their environments. The strongest main UV line, Ly$\alpha$, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly$\alpha$ emission becomes increasingly challenging at $z \gtrsim 6$ when the neutral hydrogen fraction of the CGM and IGM increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies' physical properties and their Ly$\alpha$ emission. The sample of 2052 emission line sources with $1.5 < z < 6.4$ was selected through untargeted source detection in three-dimensional MUSE data cubes. We searched optimally extracted 1D spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly$\alpha$) UV emission lines increases with survey depth, and that the UV emission line strength often correlate with the strength of Ciii]. We measured the velocity offsets of resonant emission lines with respect to systemic tracers as well as the electron density and the gas-phase abundance. Lastly, using "PhotoIonization Model Probability Density Functions" we find that the UV line emitters generally have ionization parameter log10(U) $\approx$ -2.5 and metal mass fractions that scatter around Z $\approx$ 10$^{-2}$, that is Z $\approx$ 0.66Z$\odot$. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper., Comment: Accepted by A&A. Contains 54 pages, 21 figures, and appendices. Catalogs described in Tables B.1 and C.1 will be made available with published paper
Published: 2021
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37. RADIAL DISTRIBUTION OF X-RAY POINT SOURCES NEAR THE GALACTIC CENTER

Author: Laycock, Silas [Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2009
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38. SPATIAL VARIATIONS OF DUST ABUNDANCES ACROSS THE LARGE MAGELLANIC CLOUD

Author: Volk, Kevin [Gemini Observatory, Northern Operations Center, 670 N. Aohuku Place, Hilo, HI 96720 (United States)]
Published: 2009
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39. CHANDRA DISCOVERY OF AN INTERMEDIATE POLAR IN BAADE'S WINDOW

Author: Laycock, Silas [Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720 (United States)]
Published: 2009
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40. Review of PSF reconstruction methods and application to post-processing

Author: Olivier Beltramo-Martin, R. Fetick, Carlos Correia, Sebastian Kamann, Thierry Fusco, Sam Ragland, Giulian Fiorentino, Benoit Neichel, Laura Schreiber, A. Marasco, Peter Wizinowich, Trent J. Dupuy, Laurent Jolissaint, Davide Massari, 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), W.M. Keck Observatory, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Space ODT - Optical Deblurring Technologies, Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), University of Applied Sciences of Western Switzerland, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), INAF - Osservatorio Astrofisico di Arcetri (OAA), INAF - Osservatorio Astronomico di Bologna (OABO), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], and ANR-18-CE31-0018,WOLF,Analyseurs de surface d'onde à filtrage de Fourier pour les optiques adaptatives des télescopes géants(2018)
Subjects: Kinematics, 010504 meteorology & atmospheric sciences, Computer science, Astronomy, Deconvolution, computer.software_genre, 01 natural sciences, 3D modeling, [SPI]Engineering Sciences [physics], Galactic astronomy, 0103 physical sciences, Data storage, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Data processing, business.industry, Reconstruction method, PSF - Point Spread Functions, Calibration, Data mining, business, Adaptive optics, computer
Abstract: International audience; Determining the PSF remains a key challenge for post adaptive-optics (AO) observations regarding the spatial, temporal and spectral variabilities of the AO PSF, as well as itx complex structure. This paper aims to provide a non-exhaustive but classified list of techniques and references that address this issue of PSF determination, with a particular scope on PSF reconstruction, or more generally pupil-plane-based approaches. We have compiled a large amount of references to synthesize the main messages and kept them at a top level. We also present applications of PSF reconstruction/models to post-processing, more especially PSF-fitting and deconvolution for which there is a fast progress in the community.
Published: 2020
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41. Multiband GPI Imaging of the HR 4796A Debris Disk

Author: Alycia J. Weinberger, Robert J. De Rosa, Abhijith Rajan, Katherine B. Follette, Timothy J. Rodigas, Gael M. Roudier, Maxwell A. Millar-Blanchaer, Jessica A. Arnold, Paul Kalas, Kimberly Ward-Duong, Jason J. Wang, David J. Wilner, Zachary H. Draper, Glenn Schneider, Pascale Hibon, Elodie Choquet, Jeffrey Chilcote, Thomas M. Esposito, Schuyler Wolff, Franck Marchis, Juan Sebastián Bruzzone, Johan Mazoyer, Gaspard Duchêne, Pauline Arriaga, Marshall D. Perrin, Charles A. Poteet, Justin Hom, Bin Ren, Laurent Pueyo, Christine Chen, Rémi Soummer, Fredrik T. Rantakyrö, Dean C. Hines, Christopher C. Stark, Michael P. Fitzgerald, Vanessa P. Bailey, Jennifer Patience, Julien Milli, Brenda C. Matthews, Space Telescope Science Institute (STSci), Johns Hopkins University (JHU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Arizona State University [Tempe] (ASU), Department of Physics and Astronomy [UCLA, Los Angeles], University of California [Los Angeles] (UCLA), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Carnegie Institution for Science [Washington], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Physics and Astronomy Department, The University of Western Ontario (UWO), University of Western Ontario (UWO), Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, 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), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), University of Victoria [Canada] (UVIC), Physics and Astronomy Department, Amherst College, Search for Extraterrestrial Intelligence Institute (SETI), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Department of Terrestrial Magnetism [Carnegie Institution], Steward Observatory, University of Arizona, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Carnegie Institution for Science, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Harvard University-Smithsonian Institution
Subjects: 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, 01 natural sciences, Measure (mathematics), symbols.namesake, Debris disks, 0103 physical sciences, Gemini Planet Imager, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, Scattering, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Markov chain Monte Carlo, Function (mathematics), Circumstellar matter, Computational physics, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, symbols, SPHERES, Astrophysics::Earth and Planetary Astrophysics, Planetary system formation, Coronagraphic imaging, Astrophysics - Earth and Planetary Astrophysics
Abstract: We have obtained Gemini Planet Imager (GPI) J-, H-, K1-, and K2-Spec observations of the iconic debris ring around the young, main-sequence star HR 4796A. We applied several point-spread function (PSF) subtraction techniques to the observations (Mask-and-Interpolate, RDI-NMF, RDI-KLIP, and ADI-KLIP) to measure the geometric parameters and the scattering phase function for the disk. To understand the systematic errors associated with PSF subtraction, we also forward-modeled the observations using a Markov Chain Monte Carlo framework and a simple model for the disk. We found that measurements of the disk geometric parameters were robust, with all of our analyses yielding consistent results; however, measurements of the scattering phase function were challenging to reconstruct from PSF-subtracted images, despite extensive testing. As a result, we estimated the scattering phase function using disk modeling. We searched for a dependence of the scattering phase function with respect to the GPI filters but found none. We compared the H-band scattering phase function with that measured by Hubble Space Telescope STIS at visual wavelengths and discovered a blue color at small scattering angles and a red color at large scattering angles, consistent with predictions and laboratory measurements of large grains. Finally, we successfully modeled the SPHERE H2 HR 4796A scattered phase function using a distribution of hollow spheres composed of silicates, carbon, and metallic iron., 34 pages, 30 figures, accepted in ApJ
Published: 2020
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42. Chemodynamics of green pea galaxies - I. Outflows and turbulence driving the escape of ionizing photons and chemical enrichment

Author: Ricardo Amorín, V. Firpo, Enrique Pérez-Montero, R. Chávez, A. Jaskot, Mónica V. Cardaci, Guillermo F. Hägele, L. M. Hogarth, José M. Vílchez, European Research Council, Ministerio de Economía y Competitividad (España), European Commission, Gemini Observatory, and National Science Foundation (US)
Subjects: Gemini Observatory, reionization [Cosmology], DWARF [GALAXIES], Galaxies: abundances, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], Hospitality, Internship, 0103 physical sciences, ABUNDANCES [GALAXIES], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, EVOLUTION [GALAXIES], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, STARBURST [GALAXIES], Galaxies: dwarf, 010308 nuclear & particles physics, business.industry, Galaxies: kinematics and dynamics, Galaxies: evolution, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Cosmology: reionization, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Christian ministry, Astrophysics - High Energy Astrophysical Phenomena, business, ) REIONIZATION [(COSMOLOGY], Galaxies: starburst, KINEMATICS AND DYNAMICS [GALAXIES]
Abstract: We investigate the ionized gas kinematics, physical properties, and chemical abundances of Sloan Digital Sky Survey J142947, a Green Pea galaxy at redshift z∼ 0.17 with strong, double-peak Ly α emission and indirect evidence of Lyman continuum (LyC) leakage. Using high-dispersion spectroscopy, we perform a multicomponent analysis of emission-line profiles. Our model consistently fits all lines as a narrow component with intrinsic velocity dispersion σ ∼ 40 km s-1, and two broader blue-shifted components with σ ∼ 90 and ∼ 250 km s-1. We find electron densities and temperatures, ionization conditions, and direct O/H and N/O abundances for each component. A highly ionized, metal-poor, young and compact starburst dominates narrow emission, showing evidence of hard radiation fields and elevated N/O. The blue-shifted broader components are consistent with highly turbulent, possibly clumpy ionized gas at the base of a strong photoionized outflow, which accounts for ≳50 per cent of the integrated emission-line fluxes. The outflow is dense and metal-enriched compared to the H ii regions, with expansion velocities larger than those obtained from UV interstellar absorption lines under standard assumptions. Some of these metals may be able to escape, with outflows loading factors comparable to those found in high-z galaxies of similar SFR/Area. Our findings depict a two-stage starburst picture; hard radiation fields from young star clusters illuminate a turbulent and clumpy ISM that has been eroded by SNe feedback. Whilst UV data suggest an extended Ly α halo with high average H i column density, LyC photons could only escape from SDSS J142947 through low H i density channels or filaments in the ISM approaching density-bounded conditions, traced by outflowing gas. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society, This study is based on observations made with the William Hersche Telescope operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias. We thank the anonymous referee for her/his helpful report. We would like to express our gratitude to David and Bridget Jacob for their support through the Astronomy Summer Internship Programme at University of Cambridge. Their generous funding made this project possible. LH thanks the hospitality of the Kavli Institute for Cosmology Cambridge during her Internship and subsequent visits. We would also like to thank Dr. A. Saintonge for her guidance during the compiliation of this paper. RA is also grateful to Roberto Maiolino and Polychronis Papaderos for useful discussions on this project. RA thanks the support of DIDULS (project 030503072341) and the ERC Advance Grant ‘QUENCH’. JVM and EPM acknowledge the support by the Spanish MINECO project Estallidos 6 AYA2016- 79724-C4, and by the Spanish Science Ministry ‘Centro de Excelencia Severo Ochoa Program’ under grant SEV-2017-0709. Supported by the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership of Argentina, Brazil, Canada, Chile, the Republic of Korea, and the United States of America.
Published: 2020

43. Ground Layer Adaptive Optics Point Spread Function reconstruction for MUSE Wide Field mode observations

Author: Fusco, Thierry, Bacon, Roland, Kamann, Sebastian, Conseil, S., Neichel, Benoit, Correia, Carlos, Beltramo-Martin, Olivier, Vernet, Joel, Kolb, Johann, Madec, Pierre-Yves, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), 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), and European Southern Observatory (ESO)
Subjects: [PHYS]Physics [physics], [SPI]Engineering Sciences [physics]
Abstract: International audience; Context. This paper describes a simple, efficient and most importantly fully operational Point Spread Function (PSF) reconstruction approach for Laser assisted Ground Layer Adaptive Optics (GLAO) in the frame of the MUSE Wide Field Mode. Aims. Based on clear astrophysical requirements derived by the MUSE team and using the current ESO Adaptive Optics Facility functionalities an operational PSF Reconstruction (PSFR) algorithm has been developed and tested in simulations and using on-sky data. Methods. The PSFR approach is based on a Fourier description of the GLAO correction on which the specific instrumental effects of MUSE Wide Field Mode (pixel size, internal aberrations ...) have been added. It has been first thorough validated with full end-to-end simulations. Sensitivity to the main atmospheric and AO system parameters has been analyzed and the code has been re-optimised to account for this analysis. Finally the optimized algorithm has been tested and commissioned using more than one year of on-sky MUSE data Results. We demonstrate with on-sky data analysis that our algorithm meets all the requirements imposed by the MUSE scientists: an accuracy better than a few percent on the critical PSF parameters including Full Width Half Maximum and global PSF shape through the kurtosis parameter of a Moffat function. Conclusions. The PSFR algorithm is publicly available and is used routinely to assess the MUSE image quality for each observation and can be included in any post processing activity which requires a knowledge of the PSF.
Published: 2020
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44. The triaxial ellipsoid size, density, and rotational pole of asteroid (16) Psyche from Keck and Gemini AO observations 2004–2015

Author: William J. Merline, Peter Tamblyn, Katherine de Kleer, Clark R. Chapman, Julian C. Christou, Christophe Dumas, B. Enke, Vishnu Reddy, Benoit Carry, Jack D. Drummond, Al Conrad, Imke de Pater, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), W.M. Keck Observatory, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Gemini Observatory, University of Hawai'i [Hilo], Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)
Subjects: [PHYS]Physics [physics], Physics, Planetesimal, 010504 meteorology & atmospheric sciences, Spacecraft, business.industry, Ecliptic, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, law.invention, Telescope, Space and Planetary Science, Asteroid, law, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Adaptive optics, business, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Principal axis theorem
Abstract: We analyze a comprehensive set of our adaptive optics (AO) images taken at the 10 m W. M. Keck telescope and the 8 m Gemini telescope to derive values for the size, shape, and rotational pole of asteroid (16) Psyche. Our fit of a large number of AO images, spanning 14 years and covering a range of viewing geometries, allows a well-constrained model that yields small uncertainties in all measured and derived parameters, including triaxial ellipsoid dimensions, rotational pole, volume, and density. We find a best fit set of triaxial ellipsoid diameters of (a,b,c) = (274 ± 9, 231 ± 7, 176 ± 7) km, with an average diameter of 223 ± 7 km. Continuing the literature review of Carry (2012), we find a new mass for Psyche of 2.43 ± 0.35 × 1019 kg that, with the volume from our size, leads to a density estimate 4.16 ± 0.64 g/cm3. The largest contribution to the uncertainty in the density, however, still comes from the uncertainty in the mass, not our volume. Psyche’s M classification, combined with its high radar albedo, suggests at least a surface metallic composition. If Psyche is composed of pure nickel-iron, the density we derive implies a macro-porosity of 47%, suggesting that it may be an exposed, disrupted, and reassembled core of a Vesta-like planetesimal. The rotational pole position (critical for planning spacecraft mission operations) that we find is consistent with others, but with a reduced uncertainty: [RA;Dec]=[32°;+5°] or Ecliptic [λ; δ]=[ 32 ∘ ; − 8 ∘ ] with an uncertainty radius of 3°. Our results provide independent measurements of fundamental parameters for this M-type asteroid, and demonstrate that the parameters are well determined by all techniques, including setting the prime meridian over the longest principal axis. The 5.00 year orbital period of Psyche produces only four distinct opposition geometries, suggesting that observations before the arrival of Psyche Mission in 2030 should perhaps emphasize observations away from opposition, although the penalty then would be that the asteroid will be fainter and further than at opposition.
Published: 2018
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45. H-He collision-induced satellite in the Lyman alpha profile of DBA white dwarf stars

Author: Grégoire Guillon, John F. Kielkopf, Roberto Linguerri, Majdi Hochlaf, Siyi Xu, Ivan Hubeny, Muneerah Mogren Al Mogren, N. F. Allard, Bilel Mehnen, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Louisville], University of Louisville, Gemini Observatory, parent, Laboratoire Interdisciplinaire Carnot de Bourgogne [Dijon] (LICB), Université de Bourgogne (UB)-Université de Technologie de Belfort-Montbeliard (UTBM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Instrumentation, Simulation et Informatique Scientifique (COSYS-LISIS), Université Gustave Eiffel, King Saud University [Riyadh] (KSU), and University of Arizona
Subjects: ATOMIC DATA, LINE: PROFILE, Ab initio, chemistry.chemical_element, BASIS-SET, LINE, EXCITED-STATE, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Physics - Atomic Physics, WHITE DWARF, 0103 physical sciences, Radiative transfer, ABSORPTION, Astrophysics::Solar and Stellar Astrophysics, AB-INITIO CALCULATION, Physics::Atomic Physics, ELECTRONIC-TRANSITION MOMENT, 010306 general physics, STARS: ATMOSPHERE, 010303 astronomy & astrophysics, Helium, Line (formation), POTENTIAL-ENERGY CURVE, Physics, [PHYS]Physics [physics], BALMER-ALPHA, White dwarf, Astronomy and Astrophysics, MOLECULAR DATA, Potential energy, Dipole, chemistry, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, ATOMIC PROCESS, SHAPE, [PHYS.PHYS.PHYS-CHEM-PH]Physics [physics]/Physics [physics]/Chemical Physics [physics.chem-ph], Atomic physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The spectra of helium-dominated white dwarf stars with hydrogen in their atmosphere present a distinctive broad feature centered around 1160~\AA\/ in the blue wing of the Lyman-$\alpha$ line. It is extremely apparent in WD 1425+540 recently observed with HST COS. With new theoretical line profiles based on ab initio atomic interaction potentials we show that this feature is a signature of a collision-induced satellite due to an asymptotically forbidden transition. This quasi-molecular spectral satellite is crucial to understanding the asymmetrical shape of Lyman-$\alpha$ seen in this and other white dwarf spectra. Our previous work predicting this absorption feature was limited by molecular potentials that were not adequate to follow the atomic interactions with spectroscopic precision to the asymptotic limit of large separation. A new set of potential energy curves and electronic dipole transition moments for the lowest electronic states of the H--He system were developed to account accurately for the behavior of the atomic interactions at all distances, from the chemical regime within 1~\AA\/ out to where the radiating H atoms are not significantly perturbed by their neighbors. We use a general unified theory of collision-broadened atomic spectral lines to describe a rigorous treatment of hydrogen Lyman-$\alpha$ with these potentials and present a new study of its broadening by radiative collisions of hydrogen and neutral helium. These results enable ab initio modeling of radiative transport in DBA white dwarf atmospheres., Comment: 9 pages, 7 figures
Published: 2020
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46. ORIGIN: Blind detection of faint emission line galaxies in MUSE datacubes

Author: Simon Conseil, David Mary, Antony Schutz, Roland Bacon, Laure Piqueras, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Universitat de València (UV), Universidad de Los Andes, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: FOS: Physical sciences, 02 engineering and technology, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Data cube, Integral field spectrograph, galaxies: high-redshift, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Discrete cosine transform, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Ground truth, methods: statistical, 020206 networking & telecommunications, Astronomy and Astrophysics, Hubble Ultra-Deep Field, Multi Unit Spectroscopic Explorer, methods: data analysis, Redshift, Maxima and minima, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: One of the major science cases of the MUSE integral field spectrograph is the detection of Lyman-alpha emitters at high redshifts. The on-going and planned deep fields observations will allow for one large sample of these sources. An efficient tool to perform blind detection of faint emitters in MUSE datacubes is a prerequisite of such an endeavor. Several line detection algorithms exist but their performance during the deepest MUSE exposures is hard to quantify, in particular with respect to their actual false detection rate, or purity. {The aim of this work is to design and validate} an algorithm that efficiently detects faint spatial-spectral emission signatures, while allowing for a stable false detection rate over the data cube and providing in the same time an automated and reliable estimation of the purity. Results on simulated data cubes providing ground truth show that the method reaches its aims in terms of purity and completeness. When applied to the deep 30-hour exposure MUSE datacube in the Hubble Ultra Deep Field, the algorithms allows for the confirmed detection of 133 intermediate redshifts galaxies and 248 Lyman Alpha Emitters, including 86 sources with no HST counterpart. The algorithm fulfills its aims in terms of detection power and reliability. It is consequently implemented as a Python package whose code and documentation are available on GitHub and readthedocs., Comment: Accepted to Astronomy & Astrophysics
Published: 2020
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47. The Origin of [C ii] 158 μ m Emission toward the H ii Region Complex S235

Author: A. M. Sobolev, Z. Makai, M. R. Samal, Annie Zavagno, Maria S. Kirsanova, Pascal Tremblin, Morten Andersen, D. Russeil, Matteo Luisi, L. D. Anderson, Volker Ossenkopf-Okada, Nicola Schneider, West Virginia University [Morgantown], Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), 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), Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO), Universität zu Köln, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), Ural State University, 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), Universität zu Köln = University of Cologne, and ANR-16-CE92-0035,GENESIS,GENeration et Evolution des Structures du milieu InterStellaire(2016)
Subjects: ISM [INFRARED], H II region, H II REGIONS, 010504 meteorology & atmospheric sciences, Hydrogen, Infrared, chemistry.chemical_element, FOS: Physical sciences, Astrophysics, Lambda, 01 natural sciences, Ionization, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Green Bank Telescope, Astronomy and Astrophysics, PHOTOMETRIC [TECHNIQUES], Astrophysics - Astrophysics of Galaxies, Galaxy, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ISM [RADIO CONTINUUM]
Abstract: Although the 2P3/2-2P1/2 transition of [CII] at 158um is known to be an excellent tracer of active star formation, we still do not have a complete understanding of where within star formation regions the emission originates. Here, we use SOFIA upGREAT observations of [CII] emission toward the HII region complex Sh2-235 (S235) to better understand in detail the origin of [CII] emission. We complement these data with a fully-sampled Green Bank Telescope radio recombination line map tracing the ionized hydrogen gas. About half of the total [CII] emission associated with S235 is spatially coincident with ionized hydrogen gas, although spectroscopic analysis shows little evidence that this emission is coming from the ionized hydrogen volume. Velocity-integrated [CII] intensity is strongly correlated with WISE 12um intensity across the entire complex, indicating that both trace ultra-violet radiation fields. The 22um and radio continuum intensities are only correlated with [CII] intensity in the ionized hydrogen portion of the S235 region and the correlations between the [CII] and molecular gas tracers are poor across the region. We find similar results for emission averaged over a sample of external galaxies, although the strength of the correlations is weaker. Therefore, although many tracers are correlated with the strength of [CII] emission, only WISE 12um emission is correlated on small-scales of the individual HII region S235 and also has a decent correlation at the scale of entire galaxies. Future studies of a larger sample of Galactic HII regions would help to determine whether these results are truly representative., Comment: Accepted to ApJ
Published: 2019
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48. An Exo-Kuiper Belt and An Extended Halo around HD 191089 in Scattered Light

Author: Pauline Arriaga, Bin Ren, Sloane Wiktorowicz, Alexandra Z. Greenbaum, Rémi Soummer, Arthur Vigan, Christophe Pinte, Robert J. De Rosa, Inseok Song, Laurent Pueyo, Jean-Baptiste Ruffio, Johan Mazoyer, Fredrik T. Rantakyrö, Juan Sebastián Bruzzone, Thomas M. Esposito, Tara Cotten, Patrick Ingraham, Travis Barman, Christopher C. Stark, Sandrine Thomas, J. Kent Wallace, Magaret Moerchen, Jeffrey Chilcote, Julien Rameau, Franck Marchis, Adam C. Schneider, Megan Ansdell, Malena Rice, Christian Marois, Li-Wei Hung, Stanimir Metchev, Lisa Poyneer, Bruce Macintosh, Charles A. Poteet, S. Mark Ammons, René Doyon, James E. Larkin, Kimberly Ward-Duong, Tushar Mittal, Pascale Hibon, Gaspard Duchene, Michael P. Fitzgerald, Quinn Konopacky, Maxwell A. Millar-Blanchaer, Glenn Schneider, Joanna Bulger, Jérôme Maire, Mamadou N'Diaye, Katherine B. Follette, Rebecca Oppenheimer, J. Brendan Hagan, James R. Graham, Eric L. Nielsen, Marie Ygouf, Christine Chen, Paul Kalas, Jennifer Patience, Abhijith Rajan, Marshall D. Perrin, Stephen J. Goodsell, Schuyler Wolff, Anand Sivaramakrishnan, Dean C. Hines, Vanessa P. Bailey, Dmitry Savransky, Elodie Choquet, D. M. Palmer, John H. Debes, Jason J. Wang, Francois Menard, Dominic M. Ryan, Colin Norman, Benjamin L. Gerard, Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Department of Mathematics and Statistics [Baltimore], Loyola University [Maryland, Baltimore], Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), 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), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Space Telescope Science Institute (STSci), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Yale University [New Haven], Steward Observatory, University of Arizona, Lawrence Livermore National Laboratory (LLNL), Department of Physics and Astronomy [UCLA, Los Angeles], University of California [Los Angeles] (UCLA), Lunar and Planetary Laboratory [Tucson] (LPL), University of Western Ontario (UWO), Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), University of Notre Dame [Indiana] (UND), University of Georgia [USA], Institut de Recherche sur les Exoplanètes (iREX), Université de Montréal [Montréal], Amherst College, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), University of Victoria [Canada] (UVIC), National Research Council of Canada (NRC), Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Natural Sounds and Night Skies Division, Large Synoptic Survey Telescope (LSST), Search for Extraterrestrial Intelligence Institute (SETI), University of California [San Diego] (UC San Diego), University of California, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University [Stanford], Department of Physics and Astronomy [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Department of Earth and Planetary Science [UC Berkeley] (EPS), American Geophysical Union, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), American Museum of Natural History (AMNH), Arizona State University [Tempe] (ASU), School of Physics and Astronomy [Clayton], Monash University [Clayton], Department of Astronomy [Ithaca], Cornell University, Department of Astronomy and Astrophysics [UCSC Santa Cruz], University of California [Santa Cruz] (UCSC), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Infrared Processing and Analysis Center (IPAC), 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), NASA-California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Montréal (UdeM), Stanford University, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), University of California (UC), American Geophysical Union [Washington], Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), and Universiteit Leiden
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Phase (waves), FOS: Physical sciences, techniques: image processing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ring (chemistry), stars: individual (HD 191089), 01 natural sciences, Power law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, Range (particle radiation), Scattering, protoplanetary disks, Astronomy and Astrophysics, stars: imaging, Astrophysics - Solar and Stellar Astrophysics, radiative transfer, 13. Climate action, Space and Planetary Science, Halo, Astrophysics::Earth and Planetary Astrophysics, Intensity (heat transfer), Astrophysics - Earth and Planetary Astrophysics
Abstract: We have obtained Hubble Space Telescope STIS and NICMOS, and Gemini/GPI scattered light images of the HD 191089 debris disk. We identify two spatial components: a ring resembling Kuiper Belt in radial extent (FWHM: ${\sim}$25 au, centered at ${\sim}$46 au), and a halo extending to ${\sim}$640 au. We find that the halo is significantly bluer than the ring, consistent with the scenario that the ring serves as the "birth ring" for the smaller dust in the halo. We measure the scattering phase functions in the 30{\deg}-150{\deg} scattering angle range and find the halo dust is both more forward- and backward-scattering than the ring dust. We measure a surface density power law index of -0.68${\pm}$0.04 for the halo, which indicates the slow-down of the radial outward motion of the dust. Using radiative transfer modeling, we attempt to simultaneously reproduce the (visible) total and (near-infrared) polarized intensity images of the birth ring. Our modeling leads to mutually inconsistent results, indicating that more complex models, such as the inclusion of more realistic aggregate particles, are needed., Comment: 29 pages, 18 figures, ApJ accepted
Published: 2019
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49. Massive stars in the young cluster VVV CL074

Author: J. C. Bouret, A.-N. Chené, Jose H. Groh, S. Ramírez Alegría, J. Borissova, Fabrice Martins, Dante Minniti, Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), 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), Instituto de fisica y astronomia, Universidad de Valparaiso [Chile], Millennium Institute of Astrophysics, Trinity College Dublin, Universidad de Antofagasta, Universidad Andrés Bello [Santiago] (UNAB), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Instituto de Fisica y Astronomia [Valparaiso], Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Population, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Quintuplet cluster, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, stars: evolution, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Galactic Center, Astronomy and Astrophysics, open clusters and associations: general, Astrophysics - Astrophysics of Galaxies, Galaxy, stars: massive, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters
Abstract: We obtained K-band spectroscopy of the brightest members of the cluster VVV CL074 in order to identify the massive star population. We also determined the stellar properties of the cluster's massive stars to better quantify the evolutionary sequences linking different types of massive stars. We collected integral field spectroscopy of selected fields in the cluster VVV CL074 with SINFONI on the ESO/VLT. We performed a spectral classification based on the K-band spectra and comparison to infrared spectral atlases. We determined the stellar parameters of the massive stars from analysis with atmosphere models computed with the code CMFGEN. We uncover a population of 25 early-type (OB and Wolf-Rayet) stars, 19 being newly discovered by our observations out of which 15 are likely cluster members. The cluster's spectrophotometric distance is 10.2+/-1.6 kpc, placing it close to the intersection of the galactic bar and the Norma arm, beyond the galactic center. This makes VVV CL074 one the farthest young massive clusters identified so far. Among the massive stars population, three objects are Wolf-Rayet stars, the remaining are O and B stars. From the Hertzsprung-Russell diagram we find that most stars have an age between 3 and 6 Myr according to the Geneva evolutionary tracks. WN8 and WC8-9 stars are the descendants of stars with initial masses between 40 and 60 Msun. The massive star population of VVV CL074 is very similar to that of the cluster DBS2003-179 and to a lesser extent to that of the Quintuplet cluster, indicating the same age. The central cluster of the Galaxy is ~3 Myr older. From the comparison of the massive stars populations in these four clusters, one concludes that galactic stars with an initial mass in the range 40 to 60 Msun likely go through a WN8-9 phase., Comment: 14 pages, 8 figures. Accepted in Astronomy & Astrophysics
Published: 2019
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50. Observations of Didymos: Past Results and Future Plans

Author: Thomas, C., Rivkin, Andrew S., Pravec, P., Scheirich, Peter, Carry, Benoît, de Léon, J., Green, S., Howell, Ellen S., Knight, M. M., Licandro, Javier, Moskovitz, Nicholas A., Osip, David J., Snodgrass, Colin, Thomas-Osip, Joanna E., Northern Arizona University, Flagstaff, Applied Physics Laboratory, Johns Hopkins University, Ondrejov Observatory, Charlottesville, VA, United States, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astéroïdes, comètes, météores et éphémérides (ACME), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Instituto de Astrofísica de Canarias (IAC), Open University, Department of Planetary Sciences, Lunar and Planetary Laboratory, University of Arizona (LPL), University of Maryland [College Park], University of Maryland System, Lowell Observatory, Flagstaff, NRL, Washington, and Gemini Observatory, Southern Operations Center
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; The binary near-Earth asteroid (65803) Didymos is the target for the two components of the Asteroid Impact and Deflection Assessment (AIDA) mission. The NASA DART (Double Asteroid Redirection Test) mission is scheduled to impact the Didymos secondary during its apparition in 2022. ESA's proposed Hera mission will arrive years later to obtain in situ observations of the system following the DART impact. One key scientific goal of AIDA is to measure and characterize the deflection caused by the impact. A combination of spacecraft and ground and space based optical and radar observations in 2022 will provide the required data for AIDA to meet its top-level mission goals.
Published: 2018

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