Space Images in the Keystone “600 Set” and “1200 Set”
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Galileo and the Telescope
Galileo and the Telescope A Discussion of Galileo Galilei and the Beginning of Modern Observational Astronomy ___________________________ Billy Teets, Ph.D. Acting Director and Outreach Astronomer, Vanderbilt University Dyer Observatory Tuesday, October 20, 2020 Image Credit: Giuseppe Bertini General Outline • Telescopes/Galileo’s Telescopes • Observations of the Moon • Observations of Jupiter • Observations of Other Planets • The Milky Way • Sunspots Brief History of the Telescope – Hans Lippershey • Dutch Spectacle Maker • Invention credited to Hans Lippershey (c. 1608 - refracting telescope) • Late 1608 – Dutch gov’t: “ a device by means of which all things at a very great distance can be seen as if they were nearby” • Is said he observed two children playing with lenses • Patent not awarded Image Source: Wikipedia Galileo and the Telescope • Created his own – 3x magnification. • Similar to what was peddled in Europe. • Learned magnification depended on the ratio of lens focal lengths. • Had to learn to grind his own lenses. Image Source: Britannica.com Image Source: Wikipedia Refracting Telescopes Bend Light Refracting Telescopes Chromatic Aberration Chromatic aberration limits ability to distinguish details Dealing with Chromatic Aberration - Stop Down Aperture Galileo used cardboard rings to limit aperture – Results were dimmer views but less chromatic aberration Galileo and the Telescope • Created his own (3x, 8-9x, 20x, etc.) • Noted by many for its military advantages August 1609 Galileo and the Telescope • First observed the -
Mission to Jupiter
This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines. -
Comet Lemmon, Now in STEREO 25 April 2013, by David Dickinson
Comet Lemmon, Now in STEREO 25 April 2013, by David Dickinson heads northward through the constellation Pisces. NASA's twin Solar TErrestrial RElations Observatory (STEREO) spacecraft often catch sungrazing comets as they observe the Sun. Known as STEREO A (Ahead) & STEREO B (Behind), these observatories are positioned in Earth leading and trailing orbits. This provides researchers with full 360 degree coverage of the Sun. Launched in 2006, STEREO also gives us a unique perspective to spy incoming sungrazing comets. Recently, STEREO also caught Comet 2011 L4 PanSTARRS and the Earth as the pair slid into view. Another solar observing spacecraft, the European Space Agencies' SOlar Heliospheric Observatory (SOHO) has been a prolific comet discoverer. Amateur comet sleuths often catch new Kreutz group sungrazers in the act. Thus far, SOHO has Animation of Comet 2012 F6 Lemmon as seen from discovered over 2400 comets since its launch in NASA’s STEREO Ahead spacecraft. Credit: 1995. SOHO won't see PanSTARRS or Lemmon in NASA/GSFC; animation created by Robert Kaufman its LASCO C3 camera but will catch a glimpse of Comet 2012 S1 ISON as it nears the Sun late this coming November. An icy interloper was in the sights of a NASA Like SOHO and NASA's Solar Dynamics spacecraft this past weekend. Comet 2012 F6 Observatory, data from the twin STEREO Lemmon passed through the field of view of spacecraft is available for daily perusal on their NASA's HI2A camera as seen from its solar website. We first saw this past weekend's observing STEREO Ahead spacecraft. As seen in animation of Comet Lemmon passing through the animation above put together by Robert STEREO's field of view on the Yahoo Kaufman, Comet Lemmon is now displaying a fine STEREOHunters message board. -
Building Nustar's Mirrors
20 | ASK MAGAZINE | STORY Title BY BUILDING NUSTAR’S MIRRORS Intro Many NASA projects involve designing and building one-of-a-kind spacecraft and instruments. Created for particular, unique missions, they are custom-made, more like works of technological art than manufactured objects. Occasionally, a mission calls for two identical satellites (STEREO, the Solar Terrestrial Relations Observatory, for instance). Sometimes multiple parts of an instrument are nearly identical: the eighteen hexagonal beryllium mirror segments that will form the James Webb Space Telescope’s mirror are one example. But none of this is mass production or anything close to it. nn GuisrCh/ASA N:tide CrothoP N:tide GuisrCh/ASA nn Niko Stergiou, a contractor at Goddard Space Flight Center, helped manufacture the 9,000 mirror segments that make up the optics unit in the NuSTAR mission. ASK MAGAZINE | 21 BY WILLIAM W. ZHANG The mirror segments my group has built for NuSTAR, the the interior surface and a bakeout, dries into a smooth and clean Nuclear Spectroscopic Telescope Array, are not mass produced surface, very much like glazed ceramic tiles. Finally we had to either, but we make them on a scale that may be unique at NASA: map the temperatures inside each oven to ensure they would we created more than 20,000 mirror segments over a period of two provide a uniform heating environment so the glass sheets years. In other words, we’re talking about some middle ground could slump in a controlled and gradual way. Any “wrinkles” between one-of-a-kind custom work and industrial production. -
Observational Artifacts of Nustar: Ghost-Rays and Stray-Light
Observational Artifacts of NuSTAR: Ghost-rays and Stray-light Kristin K. Madsena, Finn E. Christensenb, William W. Craigc, Karl W. Forstera, Brian W. Grefenstettea, Fiona A. Harrisona, Hiromasa Miyasakaa, and Vikram Ranaa aCalifornia Institute of Technology, 1200 E. California Blvd, Pasadena, USA bDTU Space, National Space Institute, Technical University of Denmark, Elektronvej 327, DK-2800 Lyngby, Denmark cSpace Sciences Laboratory, University of California, Berkeley, CA 94720, USA ABSTRACT The Nuclear Spectroscopic Telescope Array (NuSTAR), launched in June 2012, flies two conical approximation Wolter-I mirrors at the end of a 10.15 m mast. The optics are coated with multilayers of Pt/C and W/Si that operate from 3{80 keV. Since the optical path is not shrouded, aperture stops are used to limit the field of view from background and sources outside the field of view. However, there is still a sliver of sky (∼1.0{4.0◦) where photons may bypass the optics altogether and fall directly on the detector array. We term these photons Stray-light. Additionally, there are also photons that do not undergo the focused double reflections in the optics and we term these Ghost Rays. We present detailed analysis and characterization of these two components and discuss how they impact observations. Finally, we discuss how they could have been prevented and should be in future observatories. Keywords: NuSTAR, Optics, Satellite 1. INTRODUCTION 1 arXiv:1711.02719v1 [astro-ph.IM] 7 Nov 2017 The Nuclear Spectroscopic Telescope Array (NuSTAR), launched in June 2012, is a focusing X-ray observatory operating in the energy range 3{80 keV. -
The Kew Photoheliograph
THE KEW PHOTOHELIOGRAPH PEDRO RÉ http://pedroreastrophotography.com/ The Kew Photoheliograph (Figure 1) was the first telescope specifically designed for solar photography. It was commissioned in 1854 and named after the Kew Observatory where it has housed. The Photoheliograph was designed by Warren De la Rue (1815-1889) (Figure 2) for the London Royal Society in 1857 and made by Andrew Ross (1798-1859). It was mainly used for daily photography of the Sun at the Kew Observatory and the Royal Observatory of Greenwich. It was also transported to Rivabellosa in Northern Spain where it was used to photograph the Total eclipse of the Sun on July 18th, 1860. Figure 1- The Kew Photoheliograph. The first solar photographs were obtained by Hippolyte Fizeau and Leon Focault in 1844. The first photographs of the partial phase of a total solar eclipse and of the solar spectrum were also obtained in the 1840s. In 1849 Hervé Faye made an important communication to the Frech Academy of Sciences proposing the continuous photographic survey of the Sun: If a solar image is formed in the daguerrotype plate ... the same measurements can be repeated later on and compared with contemporaneous ones ... The same procedure may be applied to the determination of the heliocentric sunspot co-ordinates ... On April 24, 1854 John Herschel wrote to Edward Sabine: I consider it an object of very considerable importance to secure at some observatory, and indeed at more than one, in different localities, daily photographic representations of the sun, with a view to keep up a consecutive and perfectly faithful record of the history of the spots. -
1 AA Issue 4 Final Print Version 10 Dec 07.Pub
g{x TÇà|ÖâtÜ|tÇ TáàÜÉÇÉÅxÜ Journal of the Society for the History of Astronomy Issue 4 January 2008 ISSN 1740-3677 The cover illustration The Oxford heliometer ontinuing the anniversary theme of previous covers of The Antiquarian Astronomer, this issue shows an engraving of the Oxford heliometer1. Ordered from the instrument maker A & G Repsold, C Hamburg, Germany, in 1841, the heliometer began work 160 years ago, in 1848. It was the only large example of this type of instrument installed at an observatory in Britain. The heliometer (more correctly a divided-objective-lens micrometer) was conceived by Ole Römer (1644-1710), and improved by the optician, John Dollond (1706-1761). His design used an objective lens bisected across the diameter, each part having the same focal length, and served by one eyepiece. Mounted in a frame, each semi-lens could be moved along its diameter using a fine screw-thread. The displacement between the two images gives a very precise measure of the angular separation of the stars under observa- tion, or the apparent diameter of the Sun or planet. Significant work using a heliometer was not achieved until a 6-inch instrument was delivered to the Königsberg Observatory in 1829. Designed by Joseph Fraun- hofer (1787-1826), this heliometer was used by Friedrich Bessel (1784-1846) to measure the parallax of the star 61 Cygni - the first accurate measure of the distance to the stars. Against this background of German success in using the heliometer, the trustees of the Radcliffe Observatory, Oxford, England, opted to acquire an example with a 7½-inch diameter objective lens. -
Kew Observatory and the Evolution of Victorian Science, 1840–1910
introduction Kew Observatory, Victorian Science, and the “Observatory Sciences” One more recent instance of the operations of this Society in this respect I may mention, in addition to those I have slightly enumerated. I mean the important accession to the means of this Society of a fixed position, a place for deposit, regula- tion, and comparison of instruments, and for many more purposes than I could name, perhaps even more than are yet contemplated, in the Observatory at Kew. Address by Lord Francis Egerton to British Association for the Advancement of Science, June 1842 When in 1842 Lord Egerton, president of the British Association for the Advancement of Science (BAAS), announced the association’s acquisition of Kew Observatory (figure I.1), he heralded the inaugura- tion of what would become one of the major institutions of nineteenth- century British—indeed international—science. Originally built as a pri- vate observatory for King George III and long in a moribund state, after 1842 the Kew building would, as Egerton predicted, become a multi- functional observatory, put to more purposes than were even imagined in 1842. It became distinguished in several sciences: geomagnetism, me- teorology, solar astronomy, and standardization—the latter term being used in this book to refer to testing scientific instruments and develop- ing prototypes of instruments to be used elsewhere, as well as establish- ing and refining constants and standards of measurement. Many of the major figures in the physical sciences of the nineteenth century were in some way involved with Kew Observatory. For the first twenty months of the twentieth century, Kew was the site of the National Physical Labora- 3 © 2018 University of Pittsburgh Press. -
Little Books on Art General Editor: Cyril Davenport
L I TTL E B O O K S O N A R T GENERAL EDITOR : CY RIL DAVENPORT COR OT L I T T L E BO O K S O N A R T 1 01 2s 6d. n et Demy 6 0. S U B J E C T S I K N MINIATU RES . AL CE COR RA B DWA D ALMA CK OOKPLATES . E R R E H B WA T G E K A . L E RT. RS R AR T H B W T OMAN . AL ERS H MRS . A W Y T E ARTS OF JAPAN . C M S L E W R V N P T JE ELLE Y . C . DA E OR R R MRS . H . N N CH IST IN A T. JE ER R RS H N N R A T M . OU LADY IN . JE ER HR M B H N N C ISTIAN SY OLISM . JE ER W B ADLEY ILLUMINATED MSS . J . R R W ENAMELS . M S . NELSON DA SON R G N MEw FURNITU E . E A A R T I S T S R GEO GE PA TON OMNEY. R S R I N DU ER. L. JESS E ALLE IM REYNOLDS . J . S E W I R K TCH Y A S . D S E LE TT M SS E . PPN E H K IPT N HO R . P . K . S O T R R RAN CE Y ELL-GILL U NE . F S T RR H R H GAN MEw OGA T . -
The Highenergy Sun at High Sensitivity: a Nustar Solar Guest
The High-Energy Sun at High Sensitivity: a NuSTAR Solar Guest Investigation Program A concept paper submitted to the Space Studies Board Heliophysics Decadal Survey by David M. Smith, Säm Krucker, Gordon Hurford, Hugh Hudson, Stephen White, Fiona Harrison (NuSTAR PI), and Daniel Stern (NuSTAR Project Scientist) Figure 1: Artist©s conception of the NuSTAR spacecraft Introduction and Overview Understanding the origin, propagation and fate of non-thermal electrons is an important topic in solar and space physics: it is these particles that present a danger for interplanetary probes and astronauts, and also these particles that carry diagnostic information that can teach us about acceleration processes elsewhere in the heliosphere and throughout the universe. Such non-thermal electrons can be detected via their X-ray or gamma-ray emission, their radio emission, or directly in situ in interplanetary space. To date, the state of the art in solar hard x-ray imaging has been the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), a NASA Small Explorer satellite launched in 2002, which uses an indirect imaging method (rotating modulation collimators) for hard x-ray imaging. This technique can provide high angular resolution, but it is limited in dynamic range and in sensitivity to small events, due to high background. High-energy imaging of the active Sun is technically easiest in the soft x-ray band (see, for example, the detailed and dynamic images returned by the soft x- ray imager on Hinode, as well as the corresponding telescopes on Yohkoh and GOES), but these x-rays are generally emitted by lower-energy thermal plasmas. -
E F L E C T I O N S a Man Not Known to Sleep E
s u m m e r . q u a r t e r / j u n e . 2 0 1 4 r e f l e c t i o n s a man not known to sleep E. E. Barnard on Mount Wilson According to Allan Sandage, Edward Emerson Barnard was “the last of the great visual observers and the first of the long line of photo- graphic atlas makers with wide-angle telescopes.” William Sheehan, Barnard’s biographer, wrote that he deserves special recognition as “one of the most versatile astronomers of the 19th century, perhaps the last to master the entire field of observational astronomy, and a marvelous visual and photographic observer as well.” Yet Barnard is little known today outside of astronomical circles. Barnard worked on Mount Wilson for about 8 months in 1905. He at mount wilson observatory in 1905 From left: H. L. Miller, Charles G. Abbot, George Ellery Hale, Leonard Ingersoll, Ferdinand Ellerman, was on leave from Yerkes Observatory, along with a Yerkes telescope. Walter S. Adams, Edward Emerson Barnard, Charles Backus. Only Hale, This brief period yielded 40 of the 50 fields of Barnard’s magnificent Adams, Ellerman, and Backus were permanent staff members. star atlas — An Atlas of Selected Regions of the Milky Way — published in 1927. The Milky Way atlas represents the first use of a photographic observations of the night sky and became fascinated with comets, telescope, an unusual instrument sponsored by (and named after) which he began hunting on a methodical basis. Finding that a patron Catherine Wolfe Bruce. -
Low Altitude Solar Magnetic Reconnection, Type III Solar Radio Bursts, and X-Ray Emissions Received: 11 January 2015 I
www.nature.com/scientificreports OPEN Low Altitude Solar Magnetic Reconnection, Type III Solar Radio Bursts, and X-ray Emissions Received: 11 January 2015 I. H. Cairns 1, V. V. Lobzin1,23, A. Donea2, S. J. Tingay3, P. I. McCauley1, D. Oberoi4, R. T. Accepted: 18 December 2017 Dufn1,3,5, M. J. Reiner6,7, N. Hurley-Walker3, N. A. Kudryavtseva 3,8, D. B. Melrose1, J. C. Published: xx xx xxxx Harding1, G. Bernardi9,10,11, J. D. Bowman12, R. J. Cappallo13, B. E. Corey13, A. Deshpande14, D. Emrich 3, R. Goeke15, B. J. Hazelton16, M. Johnston-Hollitt17,3, D. L. Kaplan18, J. C. Kasper10, E. Kratzenberg13, C. J. Lonsdale13, M. J. Lynch3, S. R. McWhirter13, D. A. Mitchell19,3, M. F. Morales16, E. Morgan15, S. M. Ord3,10, T. Prabu14, A. Roshi20, N. Udaya Shankar14, K. S. Srivani15, R. Subrahmanyan14,20, R. B. Wayth 3,21, M. Waterson3,22, R. L. Webster19,21, A. R. Whitney13, A. Williams 3 & C. L. Williams15 Type III solar radio bursts are the Sun’s most intense and frequent nonthermal radio emissions. They involve two critical problems in astrophysics, plasma physics, and space physics: how collective processes produce nonthermal radiation and how magnetic reconnection occurs and changes magnetic energy into kinetic energy. Here magnetic reconnection events are identifed defnitively in Solar Dynamics Observatory UV-EUV data, with strong upward and downward pairs of jets, current sheets, and cusp-like geometries on top of time-varying magnetic loops, and strong outfows along pairs of open magnetic feld lines. Type III bursts imaged by the Murchison Widefeld Array and detected by the Learmonth radiospectrograph and STEREO B spacecraft are demonstrated to be in very good temporal and spatial coincidence with specifc reconnection events and with bursts of X-rays detected by the RHESSI spacecraft.