Ten Challenges of Producing an Astronomical Gigapixel Image Best Practices Practices Best
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Through a Technical Lens
THROUGH A TECHNICAL LENS CRAIG MARTIN Figure 1. Front cover: Moon [Signature Page] THROUGH A TECHNICAL LENS A Design Thesis Submitted to the Department of Architecture and Landscape Architecture of North Dakota State University. By, Craig Michael Martin In Partial Fulfillment of the Requirements for the Degree of Master of Architecture. Primary Thesis Advisor Thesis Committee Chair May 2013 Fargo | North Dakota 2-3 TABLE OF CONTENTS Table of Figures 4-9 Thesis Abstract 11 Problem Statement 13 Statement of Intent 14-15 Narrative 17-18 A User/Client Description 19 Major Project Elements 21 Site Information 22-26 Project Emphasis 27 Plan for Proceeding 28-29 Previous Studio Experience 30-31 Theoretical Research 32-41 Typological Case Studies 42-73 Historical Context 74-81 Project Goals 82-83 Site Analysis 84-95 Climate Data 96-107 Programmatic Requirements 108-111 Design Process 112-129 Final Design 130-151 Presentation Display 152-153 References 154-157 Personal Information 159 [Table of Contents] List OF FIGURES Figure 1. Moon ESO: Chekalin 2011 1 Figure 2. Paranal Telescope ESO: Hudepohl 2012 10 Figure 3. Camera Lens Delirium 2012 16 Figure 4. Nebula 1 ESO: Chekalin 2011 18 Figure 4a. Nebula 2 ESO: Chekalin 2011 18 Figure 4b. Nebula 3 ESO: Chekalin 2011 18 Figure 5. Beartooth Pass Craig Martin 2012 20 Figure 6. Beartooth Pass 2 Craig Martin 2012 22 Figure 7. Macro Map Google 2012 22 Figure 8. Micro Map Craig Martin 2012 22 Figure 9. Beartooth Pass 3 Craig Martin 2012 24 Figure 10. Dark Sky Map Grosvold 2011 26 Figure 11. -
M33 Tutorial Making Color Images
M33 Tutorial Making Color Images Travis A. Rector University of Alaska Anchorage and NOAO Department of Physics and Astronomy 3211 Providence Dr., Anchorage, AK USA email: [email protected] Introduction A Note from the Author The purpose of this tutorial is to demonstrate how color images of astronomical objects can be generated from the original FITS data files. The techniques described herein are used to create many of the astronomical images you see from profes- sional observatories such as the Hubble Space Telescope, Kitt Peak, Gemini and The WIYN 0.9-meter Telescope Spitzer. In this tutorial we will make an image of M33, the Triangulum Galaxy. M33 is a spectacular face-on spiral galaxy that is relatively nearby. It is assumed that you are familiar with the prerequisites listed below. If you have problems with the tutorial itself please feel free to contact the author at the email address above. Nomenclature: FITS stands for Flexible Image Prerequisites Transport System. It is the stan- dard format for storing astronomi- To participate in this tutorial, you will need a basic understanding of the follow- cal data. ing concepts and software: • FITS datafiles • Adobe Photoshop or Photoshop Elements • The layering metaphor Description of the Data The datasets of M33 used in this tutorial were obtained with the WIYN 0.9-meter Decoding file names telescope on Kitt Peak, which is located about 40 miles west of Tucson, Arizona. The FITS files are 2048 x 2048 pixels, and about 16 Mb in size each. Datasets in The FITS filenames consist of the name of the object, an underscore, the broadband UBVRI and narrowband Ha filters are available. -
50 Years of Existence of the European Southern Observatory (ESO) 30 Years of Swiss Membership with the ESO
Federal Department for Economic Affairs, Education and Research EAER State Secretariat for Education, Research and Innovation SERI 50 years of existence of the European Southern Observatory (ESO) 30 years of Swiss membership with the ESO The European Southern Observatory (ESO) was founded in Paris on 5 October 1962. Exactly half a century later, on 5 October 2012, Switzerland organised a com- memoration ceremony at the University of Bern to mark ESO’s 50 years of existence and 30 years of Swiss membership with the ESO. This article provides a brief summary of the history and milestones of Swiss member- ship with the ESO as well as an overview of the most important achievements and challenges. Switzerland’s route to ESO membership Nearly twenty years after the ESO was founded, the time was ripe for Switzerland to apply for membership with the ESO. The driving forces on the academic side included the Universi- ty of Geneva and the University of Basel, which wanted to gain access to the most advanced astronomical research available. In 1980, the Federal Council submitted its Dispatch on Swiss membership with the ESO to the Federal Assembly. In 1981, the Federal Assembly adopted a federal decree endorsing Swiss membership with the ESO. In 1982, the Swiss Confederation filed the official documents for ESO membership in Paris. In 1982, Switzerland paid the initial membership fee and, in 1983, the first year’s member- ship contributions. High points of Swiss participation In 1987, the Federal Council issued a federal decree on Swiss participation in the ESO’s Very Large Telescope (VLT) to be built at the Paranal Observatory in the Chilean Atacama Desert. -
Strong Detection of the CMB Lensing × Galaxy Weak Lensing Cross
Astronomy & Astrophysics manuscript no. main_file ©ESO 2020 November 24, 2020 Strong detection of the CMB lensing × galaxy weak lensing cross-correlation from ACT-DR4, Planck Legacy and KiDS-1000 Naomi Clare Robertson1; 2; 3,?, David Alonso3, Joachim Harnois-Déraps4; 5, Omar Darwish6, Arun Kannawadi7, Alexandra Amon8, Marika Asgari5, Maciej Bilicki9, Erminia Calabrese10, Steve K. Choi11; 12, Mark J. Devlin13, Jo Dunkley7; 14, Andrej Dvornik15, Thomas Erben16, Simone Ferraro17; 18, Maria Cristina Fortuna19 Benjamin Giblin5, Dongwon Han20, Catherine Heymans5; 16, Hendrik Hildebrandt15 J. Colin Hill21; 22, Matt Hilton23; 24, Shuay-Pwu P. Ho25, Henk Hoekstra19, Johannes Hubmayr26, Jack Hughes27, Benjamin Joachimi28, Shahab Joudaki3; 29, Kenda Knowles23, Konrad Kuijken19, Mathew S. Madhavacheril30, Kavilan Moodley23; 24, Lance Miller3, Toshiya Namikawa6, Federico Nati31, Michael D. Niemack11; 12, Lyman A. Page14, Bruce Partridge32, Emmanuel Schaan17; 18, Alessandro Schillaci33, Peter Schneider16, Neelima Sehgal20, Blake D. Sherwin6; 2, Cristóbal Sifón34, Suzanne T. Staggs14, Tilman Tröster5, Alexander van Engelen35, Edwin Valentijn36, Edward J. Wollack37, Angus H. Wright15, Zhilei Xu13; 38 (Affiliations can be found after the references) Received XXXX; accepted YYYY ABSTRACT We measure the cross-correlation between galaxy weak lensing data from the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave background (CMB) lensing data from the Atacama Cosmology Telescope (ACT, DR4) and the Planck Legacy survey. We use two samples of source galaxies, -
Outreach Products Integrated Under Virtual Observatories and IDIS
Europlanet N4 Outreach Products integrated under Virtual Observatories and IDIS Pedro Russo (Max Planck Institute for Solar System Research) [email protected] Virtual Observatories European Virtual Observatory The EURO-VO project is open to all European astronomical data centres. Partners include ESO, the European Space Agency, and six national funding agencies, with their respective VO nodes: INAF, Italy; INSU, France; INTA, Spain; NOVA, Netherlands; PPARC, UK; RDS, Germany. Data Centre Alliance Alliance of European data centres Physical storage Publish data, metadata and services Facility Centre Centralised registry for resources, standards and certification mechanisms Support for VO technology Dissemination and scientific program Technology Centre research and development projects on the advancement of VO technology, systems and tools in response to scientific and community requirements http://www.euro-vo.org/ Virtual Observatories International Virtual Observatory Alliance Facilitate the international coordination and collaboration necessary for the development and deployment of the tools, systems and organizational structures necessary to enable the international utilization of astronomical archives as an Virtual Repository 2 integrated and interoperating virtual observatory. ! Data Format Standards ! Metadata Standards Figure 1: The International Virtual Observatory Alliance partners. http://www.ivoa.net/ Astrophysical Virtual Observatory A major European component of the Virtual Observatory is the Astrophysical Virtual Observatory (http://www.euro-vo.org) that started in November 2001 as a three- year Phase A project, funded by the European Commission (FP5) and six organizations (ESO, ESA, AstroGrid, CNRS (CDS, TERAPIX), University Louis Pasteur and the Jodrell Bank Observatory) with a total of 5 M!. A Science Working Group was established in 2002 to provide scientific advice to the AVO Project and to promote the implementation of selected science cases through demonstrations. -
La Silla Paranal Observatory Observatory
European Southern La Silla Paranal Observatory Observatory HARPS Secondary Guiding Poster 7739-171 Gerardo Ihle1, Ismo Kastinen1, Gaspare Lo Curto1, Alex Segovia1, Peter Sinclaire1, Raffaele Tomelleri2 [email protected], [email protected], [email protected] Introduction Design and Fabrication HARPS, the High Accuracy Radial velocity Planet Searcher at the ESO La Silla 3.6m telescope, is The design and fabrication of the unit was done by Tomelleri s.r.l., Villafranca, Italy following defined dedicated to the discovery of exosolar planets and high resolution spectroscopy. specifications and requirements. The unit was installed on top of the HARPS adaptor flange. The current precision in the measurement of the radial velocity of stars down to 60 cm/sec in the long term, has permitted to discover the majority of the “super Earth” type of extra solar planets up to date. Several factors enter in the radial velocity error budget, among these is the guiding accuracy, which has direct influence on the light injection into the spectrograph’s fiber. Guiding is actually done by corrections directly sent to the telescope with frequencies in the range of 0.2 Hz-0.05 Hz, depending on the brightness of the target. Due to mechanical limitations of the telescope there is an expected relaxation time of approximately 2 sec. The final objective of this modification is to reach radial velocities precision of 30 cm/sec with HARPS, that will allow the detection of Earth mass planets in close-in orbits. Fig. 5a Details Fig. 5 Tip Tilt table. The table movement is done by means of three voice coil actuators, with a resolution of 0.1 microns, controlled by an amplifier included in a GALIL- Fig. -
Esocast Episode 29: Running a Desert Town 00:00 [Visuals Start
ESOcast Episode 29: Running a Desert Town 00:00 [Visuals start] Images: [Narrator] 1. The Atacama Desert in northern Chile — one of the driest and most hostile environments in the Plain desert world. Under the blazing Sun, only a few species of animals and plants have evolved to survive. Yet, this is where the European Southern Observatory operates its Very Large Telescope. Running this technological oasis in the barren desert, Paranal seen from distance and making it a comfortable place for people to live, poses many challenges. 00:42 ESOcast intro 2. This is the ESOcast! Cutting-edge science and life ESOcast introduction behind the scenes of ESO, the European Southern Observatory. Exploring the ultimate frontier with our host Dr J, a.k.a. Dr Joe Liske. 00:59 [Dr J] Dr J in studio, on screen: 3. Hello and welcome to the ESOcast. Paranal observatory Cerro Paranal, in the heart of the Atacama Desert, is one of the world’s best sites for observing the night sky. Paranal observatory But operating an observatory with more than 100 staff in such a remote and isolated place poses a real logistical challenge; it’s like running a desert town. 1:25 [Narrator] 4. Everything that is needed to make this Mars-like Water truck landscape a haven for people has to be brought in from far away. The most essential delivery to the arid desert is water. The observatory needs up to 70 000 litres of water each day, and literally every drop has to be brought in from the town of Antofagasta, which lies about 120 kilometres away. -
ESO's Hidden Treasures Competition
Astronomical News References Figure 2. The partici- pants at the workshop Masciadri, E. 2008, The Messenger, 134, 53 on site testing atmos- pheric data in Valparaiso, Chile arrayed by the har- Links bour. 1 Workshop web page: http://site2010.sai.msu.ru/ 2 Workshop web page: http://www.dfa.uv.cl/sitetestingdata/ 3 IAU Site Testing Instruments Working Group: http://www.ctio.noao.edu/science/iauSite/ 4 Sharing of site testing data: http://project.tmt.org/~aotarola/ST ESO’s Hidden Treasures Competition Olivier Hainaut1 Over the past two and a half years ESO The ESO Science Archive stores all the Oana Sandu1 has boosted its production of outreach data acquired on Paranal, and most of Lars Lindberg Christensen1 images, both in terms of quantity and the data obtained on La Silla since the quality, so as to become one of the best late 1990s. This archive constitutes a sources of astronomical images. In goldmine commonly used for science 1 ESO achieving this goal, the whole work flow projects (e.g., Haines et al., 2006), and for from the initial production process, technical studies (e.g., Patat et al., 2011). through to publication and promotion has But besides their scientific value, the ESO’s Hidden Treasures astropho- been optimised and strengthened. The imaging datasets in the archive also have tography competition gave amateur final outputs have been made easier to great outreach potential. astronomers the opportunity to search re-use in other products or channels by ESO’s Science Archive for a well- our partners. ESO has a small team of professional hidden cosmic gem. -
Stsci Newsletter: 2011 Volume 028 Issue 02
National Aeronautics and Space Administration Interacting Galaxies UGC 1810 and UGC 1813 Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) 2011 VOL 28 ISSUE 02 NEWSLETTER Space Telescope Science Institute We received a total of 1,007 proposals, after accounting for duplications Hubble Cycle 19 and withdrawals. Review process Proposal Selection Members of the international astronomical community review Hubble propos- als. Grouped in panels organized by science category, each panel has one or more “mirror” panels to enable transfer of proposals in order to avoid conflicts. In Cycle 19, the panels were divided into the categories of Planets, Stars, Stellar Rachel Somerville, [email protected], Claus Leitherer, [email protected], & Brett Populations and Interstellar Medium (ISM), Galaxies, Active Galactic Nuclei and Blacker, [email protected] the Inter-Galactic Medium (AGN/IGM), and Cosmology, for a total of 14 panels. One of these panels reviewed Regular Guest Observer, Archival, Theory, and Chronology SNAP proposals. The panel chairs also serve as members of the Time Allocation Committee hen the Cycle 19 Call for Proposals was released in December 2010, (TAC), which reviews Large and Archival Legacy proposals. In addition, there Hubble had already seen a full cycle of operation with the newly are three at-large TAC members, whose broad expertise allows them to review installed and repaired instruments calibrated and characterized. W proposals as needed, and to advise panels if the panelists feel they do not have The Advanced Camera for Surveys (ACS), Cosmic Origins Spectrograph (COS), the expertise to review a certain proposal. Fine Guidance Sensor (FGS), Space Telescope Imaging Spectrograph (STIS), and The process of selecting the panelists begins with the selection of the TAC Chair, Wide Field Camera 3 (WFC3) were all close to nominal operation and were avail- about six months prior to the proposal deadline. -
Glossary of Terms Absorption Line a Dark Line at a Particular Wavelength Superimposed Upon a Bright, Continuous Spectrum
Glossary of terms absorption line A dark line at a particular wavelength superimposed upon a bright, continuous spectrum. Such a spectral line can be formed when electromag- netic radiation, while travelling on its way to an observer, meets a substance; if that substance can absorb energy at that particular wavelength then the observer sees an absorption line. Compare with emission line. accretion disk A disk of gas or dust orbiting a massive object such as a star, a stellar-mass black hole or an active galactic nucleus. An accretion disk plays an important role in the formation of a planetary system around a young star. An accretion disk around a supermassive black hole is thought to be the key mecha- nism powering an active galactic nucleus. active galactic nucleus (agn) A compact region at the center of a galaxy that emits vast amounts of electromagnetic radiation and fast-moving jets of particles; an agn can outshine the rest of the galaxy despite being hardly larger in volume than the Solar System. Various classes of agn exist, including quasars and Seyfert galaxies, but in each case the energy is believed to be generated as matter accretes onto a supermassive black hole. adaptive optics A technique used by large ground-based optical telescopes to remove the blurring affects caused by Earth’s atmosphere. Light from a guide star is used as a calibration source; a complicated system of software and hardware then deforms a small mirror to correct for atmospheric distortions. The mirror shape changes more quickly than the atmosphere itself fluctuates. -
Determining the Atmospheric Wind Patterns and Cloud Development of Titan Jenny Nguyen-Ly1, Tersi Arias-Young1, Jonat
Determining the Atmospheric Wind Patterns and Cloud Development of Titan 1 1 2 Jenny Nguyen-Ly , Tersi Arias-Young , Jonathan Mitchell 1 Department of Atmospheric and Oceanic Sciences, University of California, Los Angeles, Maths Science Building, 520 Portola Plaza, Los Angeles, CA 90095 2 Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Geology Building, 595 Charles Young Dr, East, Los Angeles, CA 90095 Abstract: The general public does not think much when they see clouds in the sky. While clouds are a constant part of the everyday life on Earth, they are also a continual phenomenon found on multiple planets and moons beyond Earth. Clouds are simply an endless source of knowledge in regards to their surroundings. Just their shapes, sizes, and movements alone hold more details than one can possibly imagine. They are a tell-tale sign of what is inside the atmosphere for a planet and its climate and weather. When clouds change in number, form, or location, this is an indication of something happening in terms of climate. This is a basis for research on the clouds of Titan, a moon orbiting around Saturn. Learning about the movement of clouds on Titan gives scientists more insight into this moon, and ultimately an improved understanding of the solar system. Moreover, knowledge about the cloud development and trends on Titan could be applied to our own understanding of our planet’s atmosphere too. To accomplish such a task, a comprehensive analysis of the online NASA Planetary Data Systems (PDS) Image Atlas Archive is needed. The Cassini-Huygens mission’s recorded images of Titan lie in this archive. -
NGTS — Uncovering New Worlds with Ultra-Precise Photometry
Astronomical Science DOI: 10.18727/0722-6691/5208 NGTS — Uncovering New Worlds with Ultra-Precise Photometry Daniel Bayliss1 9 Instituto de Astronomía, Universidad the astounding diversity of these worlds, Peter Wheatley 1 Católica del Norte, Antofagasta, Chile many of which have no analogues in our Richard West 1 10 Department of Physics, and Kavli own Solar System. The Next Generation Don Pollacco 1 Institute for Astrophysics and Space Transit Survey1 (NGTS; Wheatley et al., David R. Anderson 1 Research, Massachusetts Institute 2018) is at the forefront of this effort, David Armstrong 1 of Technology, Cambridge, USA finding and characterising transiting Edward Bryant 1 exoplanets around bright stars. Heather Cegla 1 Benjamin Cooke 1 The Next Generation Transit Survey Boris Gänsicke 1 (NGTS) is a state-of-the-art photometric The NGTS facility Samuel Gill 1 facility located at ESO’s Paranal Obser- James Jackman 1 vatory. NGTS is able to reach a preci- The NGTS facility is a set of twelve fully Tom Loudon 1 sion of 150 ppm in 30 minutes, making robotic and automated 20-cm telescopes James McCormac 1 it the most precise ground-based pho- located at the Paranal Observatory in Jack Acton 2 tometric system in the world. This preci- Chile (see Figure 1). Housed in a single Matthew R. Burleigh 2 sion has led to the discovery of a rare roll-off roof enclosure just under 2 km Sarah Casewell2 exoplanet in the “Neptune Desert” from the VLT, NGTS was built at Paranal Michael Goad 2 (NGTS-4b), the shortest-period hot Observatory to take advantage of the Beth Henderson 2 Jupiter ever discovered (NGTS-10b), site’s excellent photometric conditions.