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