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Your search keyword '"Liliana Figueroa"' showing total 6 results
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6 results on '"Liliana Figueroa"'

1. The Trans-Neptunian Automated Occultation Survey (TAOS II)

Author

Jennifer L. Karr, Timothy Norton, J. H. Castro-Chacón, Shiang-Yu Wang, Kem H Cook, You-Hua Chu, Wen Ping Chen, M. Reyes-Ruiz, Matthew J. Lehner, Liliana Figueroa, Andrew Szentgyorgyi, Jj Kavelaars, Z. W. Zhang, Benjamin Hernandez, John C. Geary, Wei-Ling Yen, Charles Alcock, Chung-Kai Huang, and F. Alvarez Santana

Subjects
010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, Astronomy, Astronomy and Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Occultation, Geology, 0105 earth and related environmental sciences
Abstract

TAOS II is a next-generation occultation survey with the goal of measuring the size distribution of the small end of the Kuiper Belt (objects with diameters 0.5–30 km). Such objects have magnitudes r > 30, and are thus undetectable by direct imaging. The project will operate three telescopes at San Pedro Mártir Observatory in Baja California, México. Each telescope will be equipped with a custom-built camera comprised of a focal-plane array of CMOS imagers. The cameras will be capable of reading out image data from 10,000 stars at a cadence of 20 Hz. The telescopes will monitor the same set of stars simultaneously to search for coincident occultation detections, thus minimising the false-positive rate. This talk described the project, and reported on the progress of the development of the survey infrastructure.

Published
2017
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2. Primary and secondary mirror manufacturing for COLIBRI ground follow-up telescope of the SVOM mission

Author

Kjetil Dohlen, Didier Dubreuil, F. A. Uribe, S. Cuevas Cardona, C. Meessen, S. Basa, J. Boy, B. Cordier, D. Corre, Emmanuel Hugot, P. Gallais, F. Quirós, J. Platzer, Alan M. Watson, H. Valentin, Jorge Fuentes-Fernández, Liliana Figueroa, W. H. Lee, J-L. Atteia, A. Le Van Suu, Rosalía Langarica Lebre, P. E. Blanc, E. Jimenez-Bailon, O. Boulade, E. Cadena, J. Floriot, J. F. Le Borgne, A. F. Simon, F. Dolon, R. Mathon, Samuel Ronayette, Marc Ferrari, M. Ageron, E. Pallier, J. L. Ochoa, Damien Dornic, Michel Marcos, P. Ambert, and A. Klotz

Subjects
Telescope, Computer science, law, Primary (astronomy), Astrophysics::High Energy Astrophysical Phenomena, Celestial coordinate system, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Secondary mirror, law.invention
Abstract

COLIBRI is one of the two robotic ground follow-up telescopes for the SVOM (Space Variable Object Monitor) mission dedicated to the study of gamma-ray bursts, allowing determination of precise celestial coordinates of the detected bursts. COLIBRI telescope is a two-mirror Ritchey-Chretien telescope whose concave primary and convex secondary mirrors have diameters of 1325mm and 485mm respectively. The mirrors are currently manufactured at LAM (Laboratoire d’Astrophysique de Marseille). In this article, the advancement of the work is presented. We also give a global overview and status of the COLIBRI project.

Published
2018
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3. End-to-end simulations for COLIBRI, ground follow-up telescope for the SVOM mission

Author

Samuel Ronayette, E. Pallier, D. Turpin, E. Cadena, S. Basa, Jorge Fuentes-Fernández, Liliana Figueroa, D. Corre, Michel Marcos, J. Floriot, J. L. Ochoa, P. E. Blanc, J-L. Atteia, Alejandro Farah, F. Quirós, J. F. Le Borgne, R. Mathon, F. Dolon, A. Klotz, W. H. Lee, E. Jimenez-Bailon, O. Boulade, Fernando Ángeles, A. Le Van Suu, J. Platzer, B. Cordier, H. Valentin, S. D. Vergani, Alan M. Watson, Didier Dubreuil, S. Cuevas Cardona, Damien Dornic, P. Gallais, J. Boy, M. Ageron, P. Ambert, R. Langarica Lebre, C. Meessen, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010308 nuclear & particles physics, Computer science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Python (programming language), 01 natural sciences, Redshift, law.invention, Telescope, Open source, End-to-end principle, law, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Gamma-ray burst, 010303 astronomy & astrophysics, computer, Astrophysics::Galaxy Astrophysics, computer.programming_language, Photometric redshift
Abstract

International audience; We present an overview of the development of the end-to-end simulations programs developed for COLIBRI (Catching OpticaL and Infrared BRIght), a 1.3m robotic follow-up telescope of the forthcoming SVOM (Space Variable Object Monitor) mission dedicated to the detection and study of gamma-ray bursts (GRBs). The overview contains a description of the Exposure Time Calculator, Image Simulator and photometric redshift code developed in order to assess the performance of COLIBRI. They are open source Python packages and were developed to be easily adaptable to any optical/ Near-Infrared imaging telescopes. We present the scientific performances of COLIBRI, which allows detecting about 95% of the current GRB dataset. Based on a sample of 500 simulated GRBs, a new Bayesian photometric redshift code predicts a relative photometric redshift accuracy of about 5% from redshift 3 to 7.

Published
2018
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4. Status of the Transneptunian Automated Occultation Survey (TAOS II)

Author

Andrew Szentgyorgyi, Charles Alcock, Shiang-Yu Wang, Dae-Won Kim, Z. W. Zhang, John C. Geary, Matthew J. Lehner, You-Hua Chu, Kem H. Cook, Joel Castro, Wen Ping Chen, Liliana Figueroa, Chung Kai Huang, Mauricio Reyes-Ruiz, Timothy Norton, and Wei Ling Yen

Subjects
Physics, Solar System, Astronomy, Astrophysics, 01 natural sciences, Occultation, law.invention, 010309 optics, Telescope, Stars, Robotic telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics
Abstract

The Transneptunian Automated Occultation Survey (TAOS II) will a im to detect occultations of stars by small( 1 km diameter) objects in the Kuiper Belt and beyond. Such events a re very rare ( < 10 3 events per star peryear) and short in duration ( 200 ms), so many stars must be monitored at a high readout cadenc e. TAOS IIwill operate three 1.3 meter telescopes at the Observatorio Astro no mico Nacional at San Pedro Ma rtir in BajaCalifornia, Me xico. With a 2.3 square degree eld of view and a high spe ed camera comprising CMOS imagers,the survey will monitor 10,000 stars simultaneously with all three tele scopes at a readout cadence of 20 Hz.Construction of the site began in the fall of 2013.Keywords: telescope array, high-speed imaging, TAOS 1. INTRODUCTION The size distribution of Kuiper Belt Objects has been accurately mea sured down to diameters of D & 15 km. 1{7 A measurement of the size distribution of even smaller objects (dow n to D & 0:5 km) is needed because itwould help constrain models of the dynamical evolution of the Solar Sy stem

Published
2016
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5. DDOTI: the deca-degree optical transient imager

Author

Michel Boer, Eleonora Troja, Alexander Kutyrev, José A. de Diego, Carlos Román-Zúñiga, Nathaniel R. Butler, Pierre Thierry, Jaime Ruíz-Diáz-Soto, Alan M. Watson, F. Quirós, Alain Klotz, William H. Lee, Neil Gehrels, Stéphane Basa, M. Reyes-Ruiz, Pierre-Eric Blanc, Yilen Gómez Maqueo Chew, Silvio J. Tinoco, Liliana Figueroa, Fernando Ángeles, and Alejandro Farah

Subjects
Physics, Equatorial mount, FOS: Physical sciences, Astronomy, Field of view, Gamma-ray astronomy, 01 natural sciences, law.invention, Telescope, law, Limiting magnitude, 0103 physical sciences, Hot Jupiter, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

DDOTI will be a wide-field robotic imager consisting of six 28-cm telescopes with prime focus CCDs mounted on a common equatorial mount. Each telescope will have a field of view of 12 square degrees, will have 2 arcsec pixels, and will reach a 10-sigma limiting magnitude in 60 seconds of r = 18.7 in dark time and r = 18.0 in bright time. The set of six will provide an instantaneous field of view of about 72 square degrees. DDOTI uses commercial components almost entirely. The first DDOTI will be installed at the Observatorio Astron\'omico Nacional in Sierra San Pedro Mart\'ir, Baja California, M\'exico in early 2017. The main science goals of DDOTI are the localization of the optical transients associated with GRBs detected by the GBM instrument on the Fermi satellite and with gravitational-wave transients. DDOTI will also be used for studies of AGN and YSO variability and to determine the occurrence of hot Jupiters. The principal advantage of DDOTI compared to other similar projects is cost: a single DDOTI installation costs only about US$500,000. This makes it possible to contemplate a global network of DDOTI installations. Such geographic diversity would give earlier access and a higher localization rate. We are actively exploring this option., Comment: To appear in the proceedings of SPIE conference 9910 "Observatory Operations: Strategies, Processes, and Systems VI". 12 pages

Published
2016
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6. COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

Author

Jaime Ruíz-Diáz-Soto, O. Chapa, Alan M. Watson, Rosa L. Becerra-Godínez, Alejandro Farah, Luis C. Alvarez Nuñez, Fernando Ángeles, Carlos Román-Zúñiga, Salvador Cuevas Cardona, Carlos Tejada, Fernando Quiróz, Rosalía Langarica Lebre, Jorge Fuentes-Fernández, Liliana Figueroa, and Silvio J. Tinoco

Subjects
Physics, Diffraction, 010504 meteorology & atmospheric sciences, Field (physics), Image quality, media_common.quotation_subject, Astronomy, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, law, Sky, 0103 physical sciences, Adaptive optics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, media_common
Abstract

COATLI will provide 0.3 arcsec FWHM images from 550 to 900 nm over a large fraction of the sky. It consists of a robotic 50-cm telescope with a diffraction-limited fast-guiding imager. Since the telescope is small, fast guiding will provide diffraction-limited image quality over a field of at least 1 arcmin and with coverage of a large fraction of the sky, even in relatively poor seeing. The COATLI telescope will be installed at the at the Observatorio Astron\'omico Nacional in Sierra San Pedro M\'artir, M\'exico, during 2016 and the diffraction-limited imager will follow in 2017., Comment: To appear in the proceedings of SPIE conference 9908 "Ground-based and Airborne Instrumentation for Astronomy VI". 9 pages

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