Fast and Accurate Estimation for Astrophysical Problems in Large Databases
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
2004-2005 Annual Report
Anglo-Australian Observatory Annual Report of the Anglo-Australian Telescope Board 1 July 2004 to 30 June 2005 Anglo-Australian Observatory 167 Vimiera Road Eastwood NSW 2122 Australia Postal Address: PO Box 296 Epping NSW 1710 Australia Telephone: (02) 9372 4800 (international) + 61 2 9372 4800 Facsimile: (02) 9372 4880 (international) + 61 2 9372 4880 e-mail: [email protected] Website: http://www.aao.gov.au/ Annual Report Website: http://www.aao.gov.au/annual/ Anglo-Australian Telescope Board Address as above Telephone: (02) 9372 4813 (international) + 61 2 9372 4813 e-mail: [email protected] ABN: 71871323905 © Anglo-Australian Telescope Board 2005 ISSN 1443-8550 Cover: Dome of the UK Schmidt Telescope. Photo courtesy Shaun Amy. Combined H-alpha and Red colour mosaic image of the Vela Supernova remnant taken from several AAO/UK Schmidt Telescope H- alpha survey fields. Image produced by Mike Read and Quentin Parker Cover Design: TTR Print Management Computer Typeset: Anglo-Australian Observatory Picture Credits: The editors would like to thank for their photographs and images throughout this publication Shaun Amy, Stuart Bebb (Physics Photo- graphic Unit, Oxford), Jurek Brzeski, Chris Evans, Kristin Fiegert, David James, Urs Klauser, David Malin, Chris McCowage and Andrew McGrath ii AAO Annual Report 2004–2005 The Honourable Dr Brendan Nelson, MP, Minister for Education, Science and Training Government of the Commonwealth of Australia The Right Honourable Alan Johnson, MP, Secretary of State for Trade and Industry, Government of the United Kingdom of Great Britain and Northern Ireland In accordance with Article 8 of the Agreement between the Australian Government and the Government of the United Kingdom to provide for the establishment and operation of an optical telescope at Siding Spring Mountain in the state of New South Wales, I present herewith a report by the Anglo-Australian Telescope Board for the year from 1 July 2004 to 30 June 2005. -
ASTRONET IR Final Word Doc for Printing with Logo
ASTRONET: Infrastructure Roadmap Update Ian Robson The ASTRONET Science Vision and Infrastructure Roadmap were published in 2007 and 2008 respectively and presented a strategic plan for the development of European Astronomy. A requirement was to have a light-touch update of these midway through the term. The Science Vision was updated in 2013 and the conclusions were fed into the Roadmap update. This was completed following the outcome of the ESA decisions on the latest missions. The community has been involved through a variety of processes and the final version of the update has been endorsed by the ASTRONET Executive. ASTRONET was created by a group of European funding agencies in order to establish a strategic planning mechanism for all of European astronomy . It covers the whole astronomical domain, from the Sun and Solar System to the limits of the observable Universe, and from radioastronomy to gamma-rays and particles, on the ground as well as in space; but also theory and computing, outreach, training and recruitment of the vital human resources. And, importantly, ASTRONET aims to engage all astronomical communities and relevant funding agencies on the new map of Europe. http://www.astronet-eu.org/ ASTRONET has been supported by the EC since 2005 as an ERA-NET . Despite the formidable challenges of establishing such a comprehensive plan, ASTRONET reached that goal with the publication of its Infrastructure Roadmap in November 2008. Building on this remarkable achievement, the present project will proceed to the implementation stage, a very significant new step towards the coordination and integration of European resources in the field. -
Inferring Kilonova Population Properties with a Hierarchical Bayesian Framework I : Non-Detection Methodology and Single-Event Analyses
Draft version July 16, 2021 Typeset using LATEX twocolumn style in AASTeX631 Inferring kilonova population properties with a hierarchical Bayesian framework I : Non-detection methodology and single-event analyses Siddharth R. Mohite,1, 2, ∗ Priyadarshini Rajkumar,3 Shreya Anand,4 David L. Kaplan,1 Michael W. Coughlin,5 Ana Sagues-Carracedo´ ,6 Muhammed Saleem,5 Jolien Creighton,1 Patrick R. Brady,1 Tomas´ Ahumada,7 Mouza Almualla,8 Igor Andreoni,4 Mattia Bulla,9 Matthew J. Graham,4 Mansi M. Kasliwal,4 Stephen Kaye,10 Russ R. Laher,11 Kyung Min Shin,12 David L. Shupe,11 and Leo P. Singer13, 14 1Center for Gravitation, Cosmology and Astrophysics, Department of Physics, University of Wisconsin{Milwaukee, P.O. Box 413, Milwaukee, WI 53201, USA 2Center for Computational Astrophysics, Flatiron Institute, 162 5th Ave, New York, NY 10010, USA 3Department of Physics and Astronomy, Texas Tech University, Lubbock, TX 79409-1051, USA 4Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 5School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA 6The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden 7Department of Astronomy, University of Maryland, College Park, MD 20742, USA 8Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE 9The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden 10Caltech Optical Observatories, California -
J-PLUS: on the Identification of New Cluster
A&A 622, A178 (2019) https://doi.org/10.1051/0004-6361/201731348 Astronomy & © ESO 2019 Astrophysics J-PLUS: On the identification of new cluster members in the double galaxy cluster A2589 and A2593 using PDFs A. Molino1,2, M. V. Costa-Duarte1,3, C. Mendes de Oliveira1, A. J. Cenarro4, G. B. Lima Neto1, E. S. Cypriano1, L. Sodré Jr1, P. Coelho1, M. Chow-Martínez5,6, R. Monteiro-Oliveira7,1, L. Sampedro1,2, D. Cristobal-Hornillos4, J. Varela4, A. Ederoclite4, A. L. Chies-Santos7, W. Schoenell1, T. Ribeiro8, A. Marín-Franch4, C. López-Sanjuan4, J. D. Hernández-Fernández1, A. Cortesi1, H. Vázquez Ramió4, W. Santos Jr1, N. Cibirka1, P. Novais1, E. Pereira1, J. A. Hernández-Jimenez1, Y. Jimenez-Teja9, M. Moles4, N. Benítez2, and R. Dupke9 1 Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão 1226, 05508-090 São Paulo, Brazil e-mail: [email protected] 2 Instituto de Astrofísica de Andalucía. IAA-CSIC. Glorieta de la astronomía s/n, 18008 Granada, Spain 3 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands 4 Centro de Estudios de Física del Cosmos de Aragón, Plaza San Juan 1, 44001 Teruel, Spain 5 Departamento de Astronomía, DCNE, Universidad de Guanajuato, Apdo. Postal 144, CP 36000 Guanajuato, Mexico 6 Instituto de Geología y Geofísica - Centro de Investigaciones Geocientíficas/Universidad Nacional Autónoma de Nicaragua, Managua, Rotonda Universitaria 200 metros al Este, Managua, Nicaragua 7 Departamento de Astronomía, Instituto de Física, Universidade Federal do Rio Grande do Sul, 15051 Porto Alegre RS, Brazil 8 Departamento de Física, Universidade Federal de Sergipe, Av. -
Combining Dark Energy Survey Science Verification Data with Near
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 16 October 2018 (MN LATEX style file v2.2) Combining Dark Energy Survey Science Verification Data with Near Infrared Data from the ESO VISTA Hemisphere Survey Manda Banerji1⋆, S. Jouvel1, H. Lin2, R. G. McMahon3,4, O. Lahav1, F. J. Castander5, F. B. Abdalla1, E. Bertin6, S. E. Bosman3, A. Carnero7,8, M. Carrasco Kind9, L. N. da Costa7,8, D. Gerdes10, J. Gschwend7,8, M. Lima11,8, M. A. G. Maia7,8, A. Merson3, C. Miller10, R. Ogando7,8, P. Pellegrini7,8, S. Reed3, R. Saglia12,C.Sanchez´ 13, S. Allam14,2, J. Annis2, G. Bernstein15, J. Bernstein16, R. Bernstein17, D. Capozzi18, M. Childress19,20, Carlos E. Cunha21, T. M. Davis22,20, D. L. DePoy23, S. Desai24,25, H. T. Diehl2, P. Doel1, J. Findlay3, D. A. Finley2, B. Flaugher2, J. Frieman2, E. Gaztanaga5, K. Glazebrook26, C. Gonzalez-Fern´ andez´ 3, E. Gonzalez-Solares3, K. Honscheid27, M. J. Irwin3, M. J. Jarvis28,29, A. Kim30, S. Koposov3, K. Kuehn31, A. Kupcu-Yoldas3, D. Lagattuta26,20, J. R. Lewis3, C. Lidman31, M. Makler32, J. Marriner2, Jennifer L. Marshall23, R. Miquel13,33, Joseph J. Mohr24,25,12, E. Neilsen2, J. Peoples2, M. Sako15, E. Sanchez34, V. Scarpine2, R. Schindler35, M. Schubnell10, I. Sevilla34, R. Sharp36, M. Soares-Santos2, M. E. C. Swanson37, G. Tarle11, J. Thaler38, D. Tucker2, S. A. Uddin26,20, R. Wechsler21, W. Wester2, F. Yuan38,19, J. Zuntz39 16 October 2018 ABSTRACT We present the combination of optical data from the Science Verification phase of the Dark Energy Survey (DES) with near infrared data from the ESO VISTA Hemisphere Survey (VHS). -
Astro2010: the Astronomy and Astrophysics Decadal Survey
Astro2010: The Astronomy and Astrophysics Decadal Survey Notices of Interest 1. 4 m space telescope for terrestrial planet imaging and wide field astrophysics Point of Contact: Roger Angel, University of Arizona Summary Description: The proposed 4 m telescope combines capabilities for imaging terrestrial exoplanets and for general astrophysics without compromising either. Extremely high contrast imaging at very close inner working angle, as needed for terrestrial planet imaging, is accomplished by the powerful phase induced amplitude apodization method (PIAA) developed by Olivier Guyon. This method promises 10-10 contrast at 2.0 l/D angular separation, i.e. 50 mas for a 4 m telescope at 500 nm wavelength. The telescope primary mirror is unobscured with off-axis figure, as needed to achieve such high contrast. Despite the off-axis primary, the telescope nevertheless provides also a very wide field for general astrophysics. A 3 mirror anastigmat design by Jim Burge delivers a 6 by 24 arcminute field whose mean wavefront error of 12 nm rms, i.e.diffraction limited at 360 nm wavelength. Over the best 10 square arcminutes the rms error is 7 nm, for diffraction limited imaging at 200 nm wavelength. Any of the instruments can be fed by part or all of the field, by means of a flat steering mirror at the exit pupil. To allow for this, the field is curved with a radius equal to the distance from the exit pupil. The entire optical system fits in a 4 m diameter cylinder, 8 m long. Many have considered that only by using two spacecraft, a conventional on-axis telescope and a remote occulter, could high contrast and wide field imaging goals be reconciled. -
Atlas: a High-Cadence All-Sky Survey System
Draft version March 30, 2018 Typeset using LATEX preprint style in AASTeX61 ATLAS: A HIGH-CADENCE ALL-SKY SURVEY SYSTEM J. L. Tonry,1 L. Denneau,1 A. N. Heinze,1 B. Stalder,2 K. W. Smith,3 S. J. Smartt,3 C. W. Stubbs,4 H. J. Weiland,1 and A. Rest5, 6 1Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 2LSST, 950 N. Cherry Ave, Tucson, AZ 85719 3Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, BT7 1NN, UK 4Department of Physics, Harvard University, Cambridge, MA 02138, USA 5Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 6Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA ABSTRACT Technology has advanced to the point that it is possible to image the entire sky every night and process the data in real time. The sky is hardly static: many interesting phenomena occur, including variable stationary objects such as stars or QSOs, transient stationary objects such as supernovae or M dwarf flares, and moving objects such as asteroids and the stars themselves. Funded by NASA, we have designed and built a sky survey system for the purpose of finding dangerous near-Earth asteroids (NEAs). This system, the \Asteroid Terrestrial-impact Last Alert System" (ATLAS), has been optimized to produce the best survey capability per unit cost, and therefore is an efficient and competitive system for finding potentially hazardous asteroids (PHAs) but also for tracking variables and finding transients. While carrying out its NASA mission, ATLAS now discovers more bright (m < 19) supernovae candidates than any ground based survey, frequently detecting very young explosions due to its 2 day cadence. -
Astronet SV for Publication New Cover Final
ASTRONET: Science Vision Update Ian Robson This is the update to the ASTRONET Science Vision for European Astronomy report that was published in 2007. The update is current as of February 2013. One of its key roles is to feed into the ASTRONET Infrastructure Roadmap update that will be published in late 2014. ASTRONET was created by a group of European funding agencies in order to establish a strategic planning mechanism for all of European astronomy . It covers the whole astronomical domain, from the Sun and Solar System to the limits of the observable Universe, and from radioastronomy to gamma-rays and particles, on the ground as well as in space; but also theory and computing, outreach, training and recruitment of the vital human resources. And, importantly, ASTRONET aims to engage all astronomical communities and relevant funding agencies on the new map of Europe. http://www.astronet-eu.org/ ASTRONET has been supported by the EC since 2005 as an ERA-NET. Despite the formidable challenges of establishing such a comprehensive plan, ASTRONET reached that goal with the publication of its Infrastructure Roadmap in November 2008. Building on this remarkable achievement, the present project will proceed to the implementation stage, a very significant new step towards the coordination and integration of European resources in the field. Acknowledgements: I would like to thank all those who contributed to this update of the Science Vision Document, especially those mentioned in Appendix 1. Ian Robson March 2013 ‘It is a pleasure to welcome the publication of this update which builds upon the very successful initial Science Vision. -
THE ALHAMBRA SURVEY: EVOLUTION of GALAXY SPECTRAL SEGREGATION Ll
Draft version August 11, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 THE ALHAMBRA SURVEY: EVOLUTION OF GALAXY SPECTRAL SEGREGATION Ll. Hurtado-Gil1,2, P. Arnalte-Mur1, V. J. Mart´ınez1,3,4, A. Fernandez-Soto´ 2,4, M. Stefanon5, B. Ascaso6,21, C. Lopez-Sanju´ an´ 8, I. Marquez´ 7, M. Povic´7, K. Viironen8, J. A. L. Aguerri9,10, E. Alfaro7, T. Aparicio-Villegas11,7 N. Ben´ıtez7, T. Broadhurst12,13, J. Cabrera-Cano~ 14, F. J. Castander15, J. Cepa9,10, M. Cervino~ 7,9,10, D. Cristobal-Hornillos´ 8, R. M. Gonzalez´ Delgado7, C. Husillos7, L. Infante16, J. Masegosa7, M. Moles8,7, A. Molino17,7, A. del Olmo7, S. Paredes18, J. Perea7, F. Prada7,19,20, J. M. Quintana7 Draft version August 11, 2018 Abstract We study the clustering of galaxies as a function of spectral type and redshift in the range 0:35 < z < 1:1 using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data cover 2.381 2 deg in 7 fields, after applying a detailed angular selection mask, with accurate photometric redshifts [σz < 0:014(1 + z)] down to IAB < 24. From this catalog we draw five fixed number density, redshift-limited bins. We estimate the clustering evolution for two different spectral populations selected using the ALHAMBRA-based photometric templates: quiescent and star-forming galaxies. For each sample, we measure the real-space clustering using the projected correlation function. Our calculations are −1 −1 performed over the range [0:03; 10:0]h Mpc, allowing us to find a steeper trend for rp . -
Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities
Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Space Based, Technological Development, and State of the Profession Activities Ground Based, Space Based, and Technological Development Activities Ground Based and Space Based Activities Ground Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Infrastructure, Technological Development, State of the Profession, and Other Activities Ground Based, Infrastructure, and Technological Development Activities Ground Based, Infrastructure, and State of the Profession Activities Ground Based and Infrastructure Activities Ground Based, Technological Development, and State of the Profession Activities Ground Based and Technological Development Activities Ground Based Projects Space Based, Infrastructure, Technological Development, and State of the Profession Activities Space Based, Infrastructure, Technological Development Activities Space Based and Infrastructure Activities Space Based, Technological Development, and State of the Profession Activities Space Based and Technological Development Activities Space Based and State of the Profession Activities Space Based Projects Infrastructure, Technological Development, and State of the Profession Activities Infrastructure, Technological Development, and Other Activities Infrastructure and Technological Development Activities Infrastructure, State of the Profession, and Other Activities Infrastructure and State of the Profession -
Assessing the Photometric Redshift Precision of the S-PLUS Survey: the Stripe-82 As a Test-Case
MNRAS 000, 000{000 (0000) Preprint 16 July 2019 Compiled using MNRAS LATEX style file v3.0 Assessing the photometric redshift precision of the S-PLUS survey: the Stripe-82 as a test-case. A. Molino1? M. V. Costa-Duarte1, L. Sampedro1, F. R. Herpich1, L. Sodr´eJr.1, C. Mendes de Oliveira1, W. Schoenell2, C. E. Barbosa1, C. Queiroz3, E. V. R. Lima1, L. Azanha1, N. Mu~noz-Elgueta4;5, T. Ribeiro6, A. Kanaan7, J. A. Hernandez-Jimenez8;1, A. Cortesi9, S. Akras10;11, R. Lopes de Oliveira12;11;13, S. Torres-Flores4, C. Lima-Dias4, J. L. Nilo Castellon4, G. Damke4;5, A. Alvarez-Candal11, Y. Jim´enez-Teja11, P. Coelho1, E. Pereira14, A. D. Montero-Dorta15, N. Ben´ıtez16, T. S. Gon¸calves8, L. Santana-Silva8, S. V. Werner1, L. A. Almeida17;1, P. A. A. Lopes8, A. L. Chies-Santos2, E. Telles10, Thom de Souza, R. C.19, D. R. Gon¸calves8, R. S. de Souza18, M. Makler20, V. M. Placco21;22, L. M. I. Nakazono1, R. K. Saito7, R. A. Overzier11;1, L. R. Abramo3 Affiliations can be found after the references. Submitted to MNRAS. ABSTRACT In this paper we present a thorough discussion about the photometric redshift (photo-z) performance of the Southern Photometric Local Universe Survey (S-PLUS). This survey combines a 7 narrow + 5 broad passband filter system, with a typi- cal photometric-depth of r∼21 AB. For this exercise, we utilize the Data Release 1 (DR1), corresponding to 336 deg2 from the Stripe-82 region. We rely on the BPZ2 code to compute our estimates, using a new library of SED models, which includes addi- tional templates for quiescent galaxies. -
Discovering the Unexpected in Astronomical Survey Data
Publications of the Astronomical Society of Australia (PASA), Vol. 34, e007, 10 pages (2017). © Astronomical Society of Australia 2017; published by Cambridge University Press. doi:10.1017/pasa.2016.63 Discovering the Unexpected in Astronomical Survey Data Ray P. Norris1,2 1Western Sydney University, Locked Bag 1797, Penrith South, NSW 1797, Australia 2CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia Email: [email protected] (RECEIVED November 17, 2016; ACCEPTED December 19, 2016) Abstract Most major discoveries in astronomy are unplanned, and result from surveying the Universe in a new way, rather than by testing a hypothesis or conducting an investigation with planned outcomes. For example, of the ten greatest discoveries made by the Hubble Space Telescope, only one was listed in its key science goals. So a telescope that merely achieves its stated science goals is not achieving its potential scientific productivity. Several next-generation astronomical survey telescopes are currently being designed and constructed that will signifi- cantly expand the volume of observational parameter space, and should in principle discover unexpected new phenomena and new types of object. However, the complexity of the telescopes and the large data volumes mean that these discoveries are unlikely to be found by chance. Therefore, it is necessary to plan explicitly for unexpected discoveries in the design and construction. Two types of discovery are recognised: unexpected objects and unexpected phenomena. This paper argues that next-generation astronomical surveys require an explicit process for detecting the unexpected, and proposes an implementation of this process. This implementation addresses both types of discovery, and relies heavily on machine-learning techniques, and also on theory-based simulations that encapsulate our current understanding of the Universe.