Effective Aperture 3.6–4.9 M) 4.7 M 186″ Segmented, MMT (6×1.8 M) F

Total Page:16

File Type:pdf, Size:1020Kb

Effective Aperture 3.6–4.9 M) 4.7 M 186″ Segmented, MMT (6×1.8 M) F Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 10.4 m 409″ Segmented, Gran Telescopio Roque de los Muchachos 2006/9 36 Canarias (GTC) Obs., Canary Islands, Spain 10 m 394″ Segmented, Keck 1 Mauna Kea Observatories, 1993 36 Hawaii, USA 10 m 394″ Segmented, Keck 2 Mauna Kea Observatories, 1996 36 Hawaii, USA 9.8 m 386″ Segmented, Southern African South African Astronomical 2005 91 Large Telescope Obs., Northern Cape, South (SALT) Africa 9.2 m 362″ Segmented, Hobby-Eberly McDonald Observatory, 1997 91 Telescope (HET) Texas, USA (11 m × 9.8 m mirror) 8.4 m×2 330″×2 Multiple Large Binocular Mount Graham 2004 (can use mirror, 2 Telescope (LBT) Internationals Obs., Phased- Arizona array optics for combined 11.9 m[2]) 8.2 m 323″ Single Subaru (JNLT) Mauna Kea Observatories, 1999 Hawaii, USA 8.2 m 323″ Single VLT UT1 (Antu) Paranal Observatory, 1998 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT2 (Kueyen) Paranal Observatory, 1999 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT3 (Melipal) Paranal Observatory, 2000 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT4 (Yepun) Paranal Observatory, 2001 Antofagasta Region, Chile 8.1 m 318″ Single Gemini North Mauna Kea Observatories, 1999 (Gillett) Hawaii, USA 8.1 m 318″ Single Gemini South Cerro Pachón (CTIO), 2001 Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 1 Las Campanas Obs., 2000 (Walter Baade) Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 2 Las Campanas Obs., 2002 (Landon Clay) Coquimbo Region, Chile 6.5 m 256″ Single MMT (1 x 6.5 M1) F. L. Whipple Obs., Arizona, 2000 USA 6 m 238″ Single BTA-6 Special Astrophysical Obs., 1975 Karachay–Cherkessia, Russia 6 m 236″ Liquid Large Zenith Maple Ridge, British 2003 Telescope (LZT) Columbia, Canada Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 5.08 m 200″ Single Hale Telescope Palomar Observatory, 1948 (200 inch) California, USA 4.9 m– 193″ Segmented, LAMOST (6.67 m Beijing Astronomical Obs., 2008 3.6 m[5] (37 + 24) × 6.05 m + 5.72 m Xinglong, China × 4.40 m corrector; effective aperture 3.6–4.9 m) 4.7 m 186″ Segmented, MMT (6×1.8 m) F. L. Whipple Obs., Arizona, 1979– (6×1.8 m) 6 original optics USA 1998 4.3 m 169″ Single Discovery Lowell Observatory, Happy 2012 Channel Jack, Arizona Telescope 4.2 m 165″ Single William Herschel Roque de los Muchachos 1987 Telescope Obs., Canary Islands, Spain 4.1 m 161″ Single SOAR Cerro Pachón (CTIO), 2002 Coquimbo Region, Chile 4.1 m 161″ Single VISTA Paranal Observatory, 2009 Antofagasta Region, Chile 4 m 157″ Single Victor M. Blanco Cerro Tololo Inter- 1976 Telescope American Obs., Coquimbo Region, Chile 3.89 m 154″ Single Anglo-Australian Australian Astronomical 1975 Telescope (AAT) Obs., New South Wales, Australia 4 m 149.5″ Single Nicholas U. Kitt Peak National Obs., 1973 Mayall 4m Arizona, USA 3.67 m 145″ Single 3.67m AEOS Air Force Maui Optical 1996 Telescope (AEOS) Station, Hawaii, USA 3.58 m 142″ Single New Technology La Silla Observatory, 1989 Telescope (NTT) Coquimbo Region, Chile 3.58 m 141″ Single Canada-France- Mauna Kea Observatories, 1979 Hawaii Telescope Hawaii, USA (CFHT) 3.58 m 141″ Single Telescopio Roque de los Muchachos 1997 Nazionale Galileo Obs., Canary Islands, Spain (TNG) 3.57 m 140″ Single ESO 3.6 m La Silla Observatory, 1977 Telescope Coquimbo Region, Chile 3.5 m 138″ Single MPI-CAHA 3.5 m Calar Alto Obs., Almería, 1984 Spain 3.5 m 138″ Single Space White Sands Missile Range, 2011 Surveillance New Mexico, USA Telescope Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 3.5 m 138″ Single USAF Starfire 3.5 Starfire Optical Range, New 1994 m Mexico, USA 3.5 m 138″ Single WIYN Telescope Kitt Peak National Obs., 1994 Arizona, USA 3.48 m 137″ Single Astrophysical Apache Point Obs., New 1994 Research Mexico, USA Consortium (ARC) 3.05 m 120″ Single Shane Telescope Lick Observatory, 1959 California, USA 3.0 m 120″ Single NASA Infrared Mauna Kea Observatory, 1979 Telescope Facility Hawaii, USA 3 m 118″ Liquid NASA-LMT retired NASA Orbital Debris Obs., 1995– New Mexico, USA 2002 2.72 m 107" Single Harlan J. Smith McDonald Observatory, 1969 Telescope Texas, USA 2.65 m 104" Liquid UBC-Laval LMT Vancouver, British 1992– Columbia, Canada 2.64 m 104" Single Shajn 2.6m Crimean Astrophysical 1961 Obs., Ukraine 2.61 m 102.8" Single VLT Survey Paranal Observatory, 2007 Telescope (VST) Antofagasta Region, Chile 2.6 m 102" Single BAO 2.6 Byurakan Astrophysical 1976 Obs., Mt. Aragatz, Armenia 2.56 m 101" Single Nordic Optical ORM, Canary Islands, Spain 1988 Telescope (NOT) 2.54 m 100" Single Isaac Newton ORM, Canary Islands, Spain 1984 Telescope (INT) (RGO, England, UK until '79) 2.54 m 100" Single Irenee du Pont Las Campanas Observatory, 1976 Telescope Coquimbo Region, Chile 2.54 m 100" Single Hooker 100-Inch Mt. Wilson Observatory, 1917 Telescope California, USA 2.5 m 98.4" Single SOFIA Boeing 747SP (mobile, 2007 USA) 2.5 m 98.4" Single Sloan DSS Apache Point Observatory, 1997 New Mexico, USA 2.4 m 94.5" Single Hiltner Telescope MDM Observatory (Kitt 1986 Peak), Arizona, USA 2.4 m 94.5" Single Thailand National Chalermprakhiat 2012 Telescope (TNT) Astronomical Observatory Commemorating King Bhumibhol's 7th Birthday Anniversary, Thailand 2.4 m 94.5" Single Lijiang Yunnan Astronomical 2008 Observatory, China Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 2.4 m 94.5" Single Hubble (HST) Low Earth orbit 1990 2.4 m 94.5" Single 2.4-meter SINGLE Magdalena Ridge 2006/2 Telescope Observatory, New Mexico, 008 USA 2.4 m 94.5" Single Automated Lick Observatory, 2010 Planet Finder California, USA 2.34 m 92.1" Single Vainu Bappu Vainu Bappu Observatory, 1986 India 2.3 m 90.6" Single Aristarchos National Observatory of 2004 Athens, Mt. Helmos, Greece 2.3 m 90.6" Single IR WIRO 2.3 Wyoming Infrared 1977 Observatory, Wyoming, USA 2.3 m 90.6" Single ANU 2.3m ATT Siding Spring Observatory, 1984 New South Wales, Australia 2.3 m 90.6" Single Bok Telescope Kitt Peak National 1969 (90-inch) Observatory, Arizona, USA 2.24 m 88.2" Single University of Mauna Kea Observatories, 1970 Hawaii 2.2 m Hawaii, USA (UH88) 2.2 m 86.6" Single MPIA-ESO (ESO- La Silla Observatory, 1984[8] MPI) Coquimbo Region, Chile 2.2 m 86.6" Single MPIA-CAHA 2.2m Calar Alto Observatory, 1979 Almería, Spain 2.16 m 85" Single Xinglong 2.16m Xinglong, China 1989 2.15 m 84.6" Single Jorge Sahade Leoncito Astronomical 1987 2.15m Complex, San Juan Province, Argentina 2.12 m 83.5" Single INAOE 2.12 Guillermo Haro 1987 (OAGH) Observatory, Sonora, Mexico 2.12 m 83.5" Single UNAM 2.12 National Astronomical 1979 Observatory, Baja California, Mexico 2.1 m 82.7" Single Kitt Peak 2.1- Kitt Peak National 1964 meter Observatory, Arizona, USA 2.08 m 81.9" Single Otto Struve McDonald Observatory, 1939 Telescope Texas, USA 2.06 m 81.1" Single T13 Automated Fairborn Observatory, 2003 Spectroscopic Arizona, USA Telescope 2.01 m 79.1" Single Himalayan Indian Astronomical 2000 Chandra Observatory, India Telescope (HCT) Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 2 m 78.7" Single Alfred Jensch Karl Schwarzschild 1960 Teleskop Observatory, Germany 2 m 78.7" Single Carl Zeiss Jena Shamakhi Astrophysical 1966 Obs., Azerbaijan 2 m 78.7" Single Ondřejov 2-m Ondřejov Observatory, 1967 Czech 2 m 78.7" Single Ritchey-Chretien- Rozhen Observatory, 1984 Coude (RCC) Bulgaria 2 m 78.7" Single Carl Zeiss Jena Main Ukraine Obs., Ukraine 2 m 78.7" Single Bernard Lyot Pic du Midi Obs., France 1980 Telescope 2 m 78.7" Single Liverpool ORM, Canary Islands, Spain 2003 Telescope 2 m 78.7" Single Faulkes Telescope Haleakala Observatory, 2003[1 North Hawaii, USA 8] 2 m 78.7" Single Faulkes Telescope Siding Spring Observatory, 2001 South New South Wales, Australia 2 m 78.7" Single IR MAGNUM Haleakala Observatory, 2001– Hawaii, USA 2008 125 cm 49.21" Fixed lens, Great Paris Paris 1900 Exposition 1900 scrapped. Exhibition Disman Aimed via a Telescope of 1900 tled 2m reflecting 1900 siderostat 102 cm 40" Largest in Yerkes Williams Bay, Wisconsin, 1897 current Observatory USA operation. 98 cm 39.37" Single Swedish 1-m La Palma, Spain 2002 element Solar Telescope, non- ORM achromatic objective combined with reflective Adaptive optics and a Schupmann corrector. 91 cm 36" James Lick Mount Hamilton, 1888 telescope, Lick California, USA Observatory 83 cm + 32.67" + Double Grande Lunette, Meudon, France 1891 62 cm 24.40" telescope Paris Observatory Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 80 cm + 31.5" + Double Großer Refraktor, Potsdam, Deutsches 1899 50 cm 29.5" telescope Astrophysical Kaiserreich Observatory Potsdam 77 cm 30.3″ Biscoffschei Grande Lunette, Nice, France 1886 m funded Nice Observatory, since 1988 Côte d'Azur Observatory 76 cm 30" Brashear William Thaw Pittsburgh, Pennsylvania, 1914 made, Telescope, USA photographic Allegheny Observatory, University of Pittsburgh 76 cm 30" Destroyed Pulkovo Saint Petersburg, Russian 1885 during WWII, observatory Empire only lens (made by Alvan Clark & Sons) survives. 71 cm 28" 28-inch Grubb Greenwich, London, Great 1894 Refractor, Royal Britain Greenwich Observatory .
Recommended publications
  • Edwin Powell Hubble Papers: Finding Aid
    http://oac.cdlib.org/findaid/ark:/13030/tf7b69n8rd Online items available Edwin Powell Hubble Papers: Finding Aid Processed by Ronald S. Brashear, completed December 12, 1997; machine-readable finding aid created by Xiuzhi Zhou and updated by Diann Benti in June 2017. The Huntington Library, Art Collections, and Botanical Gardens Manuscripts Department 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2191 Email: [email protected] URL: http://www.huntington.org © 1998 The Huntington Library. All rights reserved. Edwin Powell Hubble Papers: mssHUB 1-1098 1 Finding Aid Overview of the Collection Title: Edwin Powell Hubble Papers Dates (inclusive): 1900-1989 Collection Number: mssHUB 1-1098 Creator: Hubble, Edwin, 1889-1953. Extent: 1300 pieces, plus ephemera in 34 boxes Repository: The Huntington Library, Art Collections, and Botanical Gardens. Manuscripts Department 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2191 Email: [email protected] URL: http://www.huntington.org Abstract: This collection contains the papers of Edwin P. Hubble (1889-1953), an astronomer at the Mount Wilson Observatory near Pasadena, California. as well as the diaries and biographical memoirs of his wife, Grace Burke Hubble. Language: English. Access Open to qualified researchers by prior application through the Reader Services Department. For more information, contact Reader Services. Publication Rights The Huntington Library does not require that researchers request permission to quote from or publish images of this material, nor does it charge fees for such activities. The responsibility for identifying the copyright holder, if there is one, and obtaining necessary permissions rests with the researcher. Preferred Citation [Identification of item].
    [Show full text]
  • Spring Semester 2021 (F21) 1 January 2021 Until 30 June 2021
    Centro Astronomico´ Hispano-Aleman´ (CAHA) Call for proposals at the Calar Alto 2.2 & 3.5 meter telescopes Spring semester 2021 (F21) 1 January 2021 until 30 June 2021 DEADLINE: October 15th, 2020 23h59m59s (CEST) at the latest Earliest date for submission: September 17th, 2020 Calar Alto, September 16th, 2020. Contact: [email protected] Contents 1 Applications for observing time at Calar Alto4 1.1 General information...........................4 1.2 Spanish open time at the CAHA 2.2- and 3.5-m telescopes......4 1.3 Proposals from PIs in Europe but out of Spain.............4 1.4 Proposals from non-European PIs...................4 1.5 Visitor and service observing modes..................5 1.5.1 Visitor mode..........................5 1.5.2 Service mode..........................5 1.6 Ongoing surveys............................6 1.6.1 On the 3.5-m telescope.....................6 1.6.2 On the 2.2-m telescope.....................6 2 Important to notice6 2.1 No visits during the COVID-19 pandemic...............6 2.2 CAFE´ ..................................7 2.3 PANIC..................................7 3 How to write a proposal7 3.1 Calar Alto instrument pages......................8 3.1.1 Instruments offered on the 3.5-m telescope..........8 3.1.2 Instruments offered on the 2.2-m telescope..........8 3.2 Science categories of proposals.....................9 3.3 Types of proposal............................9 3.3.1 Re-submitted applications...................9 3.3.2 PhD thesis projects....................... 10 3.3.3 Long term or large projects................... 10 3.3.4 Testing new instruments.................... 10 3.3.5 Visitor instruments....................... 11 3.3.6 Multiple-instrument proposals................
    [Show full text]
  • Telescopes and Binoculars
    Continuing Education Course Approved by the American Board of Opticianry Telescopes and Binoculars National Academy of Opticianry 8401 Corporate Drive #605 Landover, MD 20785 800-229-4828 phone 301-577-3880 fax www.nao.org Copyright© 2015 by the National Academy of Opticianry. All rights reserved. No part of this text may be reproduced without permission in writing from the publisher. 2 National Academy of Opticianry PREFACE: This continuing education course was prepared under the auspices of the National Academy of Opticianry and is designed to be convenient, cost effective and practical for the Optician. The skills and knowledge required to practice the profession of Opticianry will continue to change in the future as advances in technology are applied to the eye care specialty. Higher rates of obsolescence will result in an increased tempo of change as well as knowledge to meet these changes. The National Academy of Opticianry recognizes the need to provide a Continuing Education Program for all Opticians. This course has been developed as a part of the overall program to enable Opticians to develop and improve their technical knowledge and skills in their chosen profession. The National Academy of Opticianry INSTRUCTIONS: Read and study the material. After you feel that you understand the material thoroughly take the test following the instructions given at the beginning of the test. Upon completion of the test, mail the answer sheet to the National Academy of Opticianry, 8401 Corporate Drive, Suite 605, Landover, Maryland 20785 or fax it to 301-577-3880. Be sure you complete the evaluation form on the answer sheet.
    [Show full text]
  • University of Hawaii Telescopes at Mauna Kea Observatory
    UNIVERSITY OF HAWAII TELESCOPES AT MAUNA KEA OBSERVATORY USER MANUAL Fourth Edition, April 1996 Last modi®ed, June 1997 Contents 1 INTRODUCTION 1 1.1 General : ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 1 1.2 About this Manual :: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 1 1.3 Observing TimeÐPolicy and Procedures : :::: ::: :::: ::: :::: ::: :::: ::: :::: : 1 1.3.1 Students and Assistants :: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 3 1.3.2 Information before Arrival : ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 3 1.3.3 Colloquia :: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 3 1.3.4 Reports to the Director ::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 3 1.3.5 Publications and Acknowledgments ::: ::: :::: ::: :::: ::: :::: ::: :::: : 3 1.4 Newsletter :: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 4 1.5 Information for Visiting Observers : ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 4 1.5.1 Transportation from Hilo to Hale Pohaku and Mauna Kea Observatory :: :::: ::: :::: : 4 1.6 AccommodationÐThe Mid-level Facility, Hale Pohaku :::: ::: :::: ::: :::: ::: :::: : 8 1.6.1 Telephone Service : :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 8 1.6.2 Mail Service : ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 8 1.6.3 Library :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 8 2 VISITING OBSERVER EQUIPMENT 11 2.1 Packing Goods for Shipping :::: ::: :::: ::: :::: ::: :::: ::: :::: ::: :::: : 11 2.2 Transport ::: :::: ::: :::: ::: :::: :::
    [Show full text]
  • The Giant Magellan Telescope. Status
    The Giant Magellan Telescope. Status By Dr. Mauricio Pilleux Head of Administration (Chile) GMTO Corporation [email protected] April 17, 2019 Observatories in Chile: The beginnings … a successful experiment Cerro Tololo Interamerican Observatory AURA, 1962 Magellan telescopes, 2000 Las Campanas Carnegie Institution of Washington, 1968 La Silla ESO, 1969 2 Observatories in Chile: “Second stage” Very Large Telescope (VLT) Cerro Paranal, ESO, 1999 Gemini South Cerro Pachón, 2002 (AURA) ALMA NRAO-ESO-NAOJ, 2013 3 Observatories in Chile: “Stage 3.0” – big, big, big Giant Magellan Telescope (GMT) Cerro Las Campanas, 2023 (GMTO Corporation) European- Extremely Large Telescope (EELT) Cerro Armazones, 2026 (ESO) Large Synoptic Survey Telescope (LSST) Cerro Pachón, 2022 (NSF/AURA-DOE/SLAC) 4 What next? Size (physical) GMT TMT EELT LSST Main Author – Presentation Title Observatories in Chile: Where? ALMA CCAT* Nanten 2 ASTE Paranal Vista ACT 2 3 E-ELT* TAO* Apex CTA* Las Campanas GMT* Polar Bear Simons Obs. La Silla 1 Tololo SOAR Gemini LSST* 6 Giant Magellan Telescope (GMT): Will be the largest in the world in 2022 25 meters in diameter “Price”: US$1340 million First light: 2023 Enclosure is 62 m high Groundbreaking research in: . Exoplanets and their atmospheres . Dark matter . Distant objects . Unknown unknowns 7 Just how tall is the GMT? 46 meters 8 Giant Magellan Telescope (GMT): The world’s largest optical telescope Korea Sao Paulo, Brazil Texas A&M Arizona New partners are welcome! Main Author – Presentation Title 9 Central mirror casting
    [Show full text]
  • Researchers Hunting Exoplanets with Superconducting Arrays
    Cryocoolers, a Brief Overview .............................. 8 NASA Preps Four Telescope Missions .............. 37 Lake Shore Celebrates 50 Years ....................... 22 ICCRT Recap ..................................................... 38 Recovering Cold Energy and Waste Heat ............ 32 3-D Printing from Aqueous Materials .................. 40 Exoplanet Hunt with ADR-Cooled Superconducting Detector Arrays | 34 Volume 34 Number 3 Researchers Hunting Exoplanets with Superconducting Arrays The key to revealing the exoplanets tucked away around the universe may just be locked up in the advancement of Microwave Kinetic Inductance Detectors (MKIDs), an array of superconducting de- tectors made from platinum sillicide and housed in a cryostat at 100 mK. An astronomy team led by Dr. Benjamin Mazin at the University of California Santa Barbara is using MKID arrays for research on two telescopes, the Hale telescope at Palomar Observatory near San Diego and the Subaru telescope located at the Maunakea Observatory on Hawaii. Mazin began work on MKIDs nearly two decades ago while working under Dr. Jonas Zmuidzinas at Caltech, who co-pioneered the detectors for cosmic microwave background astronomy with Dr. Henry LeDuc at JPL. A look inside the DARKNESS cryostat. Image: Mazin Mazin has since adapted and ad- vanced the technology for the direct im- aging of exoplanets. With direct imaging, telescopes detect light from the planet itself, recording either the self-luminous thermal infrared light that young—and still hot—planets give off, or reflected light from a star that bounces off a planet and then towards the detector. Researchers have previously relied on indirect methods to search for exo- planets, including the radial velocity technique that looks at the spectrum of a star as it’s pushed and pulled by its planetary companions; and transit pho- tometry, where a dip in the brightness of a star is detected as planets cross in front The astronomy team working with Dr.
    [Show full text]
  • The JWST/Nircam Coronagraph: Mask Design and Fabrication
    The JWST/NIRCam coronagraph: mask design and fabrication John E. Krista, Kunjithapatham Balasubramaniana, Charles A. Beichmana, Pierre M. Echternacha, Joseph J. Greena, Kurt M. Liewera, Richard E. Mullera, Eugene Serabyna, Stuart B. Shaklana, John T. Traugera, Daniel W. Wilsona, Scott D. Hornerb, Yalan Maob, Stephen F. Somersteinb, Gopal Vasudevanb, Douglas M. Kellyc, Marcia J. Riekec aJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasasdena, CA, USA 91109; bLockheed Martin Advanced Technology Center, Palo Alto, CA, USA 94303; cUniversity of Arizona, Tucson, AZ, USA 85721 ABSTRACT The NIRCam instrument on the James Webb Space Telescope will provide coronagraphic imaging from λ=1-5 µm of high contrast sources such as extrasolar planets and circumstellar disks. A Lyot coronagraph with a variety of circular and wedge-shaped occulting masks and matching Lyot pupil stops will be implemented. The occulters approximate grayscale transmission profiles using halftone binary patterns comprising wavelength-sized metal dots on anti-reflection coated sapphire substrates. The mask patterns are being created in the Micro Devices Laboratory at the Jet Propulsion Laboratory using electron beam lithography. Samples of these occulters have been successfully evaluated in a coronagraphic testbed. In a separate process, the complex apertures that form the Lyot stops will be deposited onto optical wedges. The NIRCam coronagraph flight components are expected to be completed this year. Keywords: NIRCam, JWST, James Webb Space Telescope, coronagraph 1. INTRODUCTION 1.1 The planet/star contrast problem Observations of extrasolar planet formation (e.g. protoplanetary disks) and planetary systems are hampered by the large contrast differences between these targets and their much brighter stars.
    [Show full text]
  • Exoplanet Community Report
    JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probe­class missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2
    [Show full text]
  • Large Telescopes and Why We Need Them Transcript
    Large telescopes and why we need them Transcript Date: Wednesday, 9 May 2012 - 1:00PM Location: Museum of London 9 May 2012 Large Telescopes And Why we Need Them Professor Carolin Crawford Astronomy is a comparatively passive science, in that we can’t engage in laboratory experiments to investigate how the Universe works. To study any cosmic object outside of our Solar System, we can only work with the light it emits that happens to fall on Earth. How much we can interpret and understand about the Universe around us depends on how well we can collect and analyse that light. This talk is about the first part of that problem: how we improve the collection of light. The key problem for astronomers is that all stars, nebulae and galaxies are so very far away that they appear both very small, and very faint - some so much so that they can’t be seen without the help of a telescope. Its role is simply to collect more light than the unaided eye can, making astronomical sources appear both bigger and brighter, or even just to make most of them visible in the first place. A new generation of electronic detectors have made observations with the eye redundant. We now have cameras to record the images directly, or once it has been split into its constituent wavelengths by spectrographs. Even though there are a whole host of ingenious and complex instruments that enable us to record and analyse the light, they are still only able to work with the light they receive in the first place.
    [Show full text]
  • Demonstration of Vortex Coronagraph Concepts for On-Axis Telescopes on the Palomar Stellar Double Coronagraph
    Demonstration of vortex coronagraph concepts for on-axis telescopes on the Palomar Stellar Double Coronagraph Dimitri Maweta, Chris Sheltonb, James Wallaceb, Michael Bottomc, Jonas Kuhnb, Bertrand Mennessonb, Rick Burrussb, Randy Bartosb, Laurent Pueyod, Alexis Carlottie, and Eugene Serabynb aEuropean Southern Observatory, Alonso de C´ordova 3107, Vitacura, Casilla 19001, Chile; bJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA; cCalifornia Institute of Technology, Pasadena, CA 91106, USA; dSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; eInstitut de Plan´etologieet d'Astrophysique de Grenoble (IPAG), University Joseph Fourier, CNRS, BP 53, 38041, Grenoble, France; ABSTRACT Here we present preliminary results of the integration of two recently proposed vortex coronagraph (VC) concepts for on-axis telescopes on the Stellar Double Coronagraph (SDC) bench behind PALM-3000, the extreme adaptive optics system of the 200-inch Hale telescope of Palomar observatory. The multi-stage vortex coronagraph (MSVC) uses the ability of the vortex to move light in and out of apertures through multiple VC in series to restore the nominal attenuation capability of the charge 2 vortex regardless of the aperture obscurations. The ring-apodized vortex coronagraph (RAVC) is a one-stage apodizer exploiting the VC Lyot-plane amplitude distribution in order to perfectly null the diffraction from any central obscuration size, and for any vortex topological charge. The RAVC is thus a simple concept that makes the VC immune to diffraction effects of the secondary mirror. It combines a vortex phase mask in the image plane with a single pupil-based amplitude ring apodizer, tailor-made to exploit the unique convolution properties of the VC at the Lyot-stop plane.
    [Show full text]
  • Arxiv:2009.11049V2 [Astro-Ph.IM] 24 Sep 2020
    Research in Astronomy and Astrophysics manuscript no. (LATEX: ms2020-0197.tex; printed on September 25, 2020; 1:02) The estimate of sensitivity for large infrared telescopes based on measured sky brightness and atmospheric extinction Zhi-Jun Zhao1,4, Hai-Jing Zhou1, Yu-Chen Zhang2, Yun Ling3 and Fang-Yu Xu∗2 1 School of Physics, Henan Normal University,Xinxiang 453007, China; xu [email protected]; [email protected] 2 Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China; 3 Kunming Institute of Physics, Kunming 650216, China; 4 Henan Key Laboratory of Infrared Materials & Spectrum Measures and Applications, Xinxiang 453007, China Received 20xx month day; accepted 20xx month day Abstract : In order to evaluate the ground-based infrared telescope sensitivity affected by the noise from the atmosphere, instruments and detectors, we construct a sensitivity model that can calculate limiting magnitudes and signal-to-noise ratio (S/N). The model is tested with tentative measurements of M′-band sky brightness and atmospheric extinction obtained at the Ali and Daocheng sites. We find that the noise caused by an excellent scientific detector and instruments at 135◦C can be ignored compared to the M′-band sky background noise. − Thus, when S/N =3 and total exposure time is 1 second for 10 m telescopes, the magnitude limited by the atmosphere is 13.01m at Ali and 12.96m at Daocheng. Even under less-than- − arXiv:2009.11049v2 [astro-ph.IM] 24 Sep 2020 ideal circumstances, i.e., the readout noise of a deep cryogenic detector is less than 200e and the instruments are cooled to below 87.2◦C, the above magnitudes decrease by 0.056m − at most.
    [Show full text]
  • Minutes Regular Meeting Mauna Kea Management Board Wednesday
    University of Hawai‘i at Hilo 640 N. A‘ohoku Place, Room 203, Hilo, Hawai‘i 96720 Telephone: (808) 933-0734 Fax: (808) 933-3208 Mailing Address: 200 W. Kawili Street, Hilo, Hawai‘i 96720 Minutes Regular Meeting Mauna Kea Management Board Wednesday, May 19, 2010 ʻImiloa Astronomy Center Moana Hoku Hall 600 ʻImiloa Place Hilo, Hawaii 96720 Attending MKMB: Chair Barry Taniguchi, 2nd Vice Chair/Secretary Ron Terry, John Cross, Lisa Hadway, Herring Kalua, and Christian Veillet BOR: Dennis Hirota and Eric Martinson Kahu Kū Mauna: Ed Stevens OMKM: Stephanie Nagata and Dawn Pamarang Others: Robert Albarson, Jim Albertini, Laura Aquino, Dean Au, Madeline Balo-Keawe, Sean Bassle- Kukonu, David Byrne, Rob Christensen, Gregory Chun, Nan Chun, Vaughn Cook, Sandra Dawson, Donn delaCruz, Gerald DeMello, Richard Dods, Suzanne Frayser, Paul Gillett, MRC Greenwood, Richard Ha, Katherine Hall, Cory Harden, Inge Heyer, Clyde Higashi, Nelson Ho, Arthur Hoke, Jacqui Hoover, Stewart Hunter, Stew Hussey, Leslie Isemoto, Mark Ishii, Paul Kagawa, Mike Kaleikini, Ka’iu Kimura, Kyle Kinoshita, Ron Koehler, Randy Kurohara, Susan Law, Tim Law, Karina Leasure, Jonathan Lee, Pete Lindsey, George Martin, Tani Matsubara, Jeff Melrose, Jon Miyata, Delbert Nishimoto, Eugene Nishimura, James Nixon, Cynthia Nomura, Alton Nosaka, Derek Oshita, Tom Peek, Koa Rice, Helen Rogers, Skylark Rossetti, Gary Sanders, Ian Sandison, Bill Stormont, Leonard Tanaka, Rose Tseng, Ross Watson II, Josh Williams, Ross Wilson, Greg Wines, Harry Yada, Mason Yamaki, Miles Yoshioka I. CALL TO ORDER Chair Taniguchi called the meeting of the Mauna Kea Management Board (MKMB) to order at 9:03 a.m. II. APPROVAL OF MINUTES Upon motion by Herring Kalua and seconded by Ron Terry the minutes of the April 21, 2010 meeting of the MKMB were unanimously approved.
    [Show full text]