DOCSLIB.ORG

A Rotating Aperture Mask for Small Telescopes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
A Rotating Aperture Mask for Small Telescopes A ROTATING APERTURE MASK FOR SMALL TELESCOPES A Thesis presented to the Faculty of California Polytechnic State University, San Luis Obispo In Partial Fulfillment of the Requirements for the Degree Master of Science in Mechanical Engineering by Edward Leo Foley November 2019 © 2019 Edward Leo Foley ALL RIGHTS RESERVED ii COMMITTEE MEMBERSHIP TITLE: A Rotating Aperture Mask for Small Telescopes AUTHOR: Edward Leo Foley DATE SUBMITTED: November 2019 COMMITTEE CHAIR: John Ridgely, Ph.D. Professor of Mechanical Engineering COMMITTEE MEMBER: Russell Genet, Ph.D. Research Scholar in Residence COMMITTEE MEMBER: William R. Murray, Ph.D. Professor of Mechanical Engineering COMMITTEE MEMBER: Jane Zhang, Ph.D. Professor of Electrical Engineering iii ABSTRACT A Rotating Aperture Mask for Small Telescopes Edward Leo Foley Observing the dynamic interaction between stars and their close stellar neighbors is key to establishing the stars’ orbits, masses, and other properties. Our ability to visually discriminate nearby stars is limited by the power of our telescopes, posing a challenge to astronomers at small observatories that contribute to binary star surveys. Masks placed at the telescope aperture promise to augment the resolving power of telescopes of all sizes, but many of these masks must be manually and repetitively reoriented about the optical axis to achieve their full benefits. This paper introduces a design concept for a mask rotation mechanism that can be adapted to telescopes of different types and proportions, focusing on an implementation for a Celestron C11 Schmidt–Cassegrain optical tube assembly. Mask concepts were first evaluated using diffraction simulation programs, later manufactured, and finally tested on close double stars using a C11. An electronic rotation mechanism was designed, produced, and evaluated. Results show that applying a properly shaped and oriented mask to a C11 enhances contrast in images of double star systems relative to images captured with the unmasked telescope, and they show that the rotation mechanism accurately and repeatably places masks at target orientations with minimal manual effort. Detail drawings of the mask rotation mechanism and code for the software interface are included. iv ACKNOWLEDGMENTS This thesis is submitted as the product of hard work from many different contributors. I would like to extend my sincere thanks to Dr. Russell Genet for reigniting my love of astronomy through his contagious mix of passion, curiosity, and geniality. He fully supported me throughout my odyssey to complete this project by offering vital direction and encouragement, not to mention connecting me with other astronomers and co-authoring an earlier paper published in the Journal of Double Star Observations. He graciously hosted me at the Orion Observatory and allowed me to use one of his telescopes for crucial optical and mechanical tests. I deeply appreciate the collaborative and positive research environment he fostered—not just for me and this project but also for others and their own scientific pursuits. I am very grateful to thesis committee chair Dr. John Ridgely for the guidance he offered me and the patience he exhibited throughout this project. I also sincerely thank my committee members, Drs. William Murray and Jane Zhang, for attending my defense and sharing constructive feedback on a draft of this paper. I am indebted to Dr. Neil Zimmerman of Princeton University for his counsel and for kindly contributing an optimized mask design for the Celestron C11 telescope. This paper and the conclusions drawn within it benefitted greatly from his efforts, just like the astronomers who might fruitfully use his bowtie mask in double star observations. I am grateful to Jimmy Ray for running the first practical tests of the Gaussian donut mask on a telescope; and to Donald Loveland, who diligently evaluated and documented the performance of two mask designs on several pairs of double stars. v I thank Kevin Jantz for his machining assistance and feedback on early drawings. I also appreciate the efforts of Nick Bonafede, Marc Goupil, and Bodin Rojanachaichanin, who lent some of their time to review my engineering documentation. I must recognize Keenan Reimer, who helped me get to and from campus in the home stretch of the project. I also thank Luke Williams, who delivered the Orion Observatory’s C11 to my house for an afternoon of important mechanical tests. I extend gratitude to David Rowe, who kindly shared with me his Atmospheric Seeing Distortion simulator and adapted it to work with arbitrary aperture shapes in support of this project. I thank the professors and administrators at Cal Poly for actively applying the University’s “Learn by Doing” mantra and for granting a mechanical engineering student the opportunity to enroll in courses within the fields of computer science, computer vision, image processing, digital control systems, and optics. The lessons from this unusual palette of subjects were fundamental in my acquiring an inside-out understanding of a unique project. I give thanks to the many housemates, coworkers, grad lab occupants, and friends who cheered me on through this endeavor. Finally, I thank my parents, Bill and Lori; my brother, Matt; and all my relatives for their love and encouragement. Hopefully their reading these sentences answers their long-standing and oft-repeated question of whether my thesis is done yet. vi TABLE OF CONTENTS Page LIST OF TABLES ......................................................................................................... XIII LIST OF FIGURES ....................................................................................................... XVI CHAPTER 1. INTRODUCTION .................................................................................................. 1 1.1 Statement of problem .................................................................................. 1 1.2 Resolution and contrast targets ................................................................... 5 1.3 Existing approaches .................................................................................... 8 1.3.1 Color filters ..................................................................................... 8 1.3.2 Occulting bars ................................................................................. 9 1.3.3 Lyot coronagraphs ......................................................................... 11 1.3.4 Apodizing masks ........................................................................... 12 1.4 Selection of method .................................................................................. 22 2. SIMULATING SHAPED APERTURES ............................................................. 23 2.1 Optics summary ........................................................................................ 23 2.2 Diffraction simulation ............................................................................... 24 2.2.1 Diffraction simulation using MATLAB ........................................ 24 2.2.2 Diffraction simulation using Maskulator ...................................... 25 2.3 Displaying power spectra .......................................................................... 27 3. APERTURE MASKS FOR THE CELESTRON C11 OPTICAL TUBE ASSEMBLY ......................................................................................................... 29 vii 3.1 The Celestron C11 optical tube assembly ................................................. 29 3.2 Effect of central obstruction on diffraction pattern................................... 30 3.3 Past attempts to mask a central obstruction .............................................. 34 3.4 New mask candidates ................................................................................ 40 3.4.1 Gaussian donut mask..................................................................... 40 3.4.2 Multi-Gaussian mask .................................................................... 46 3.4.3 Concentric ring mask .................................................................... 47 3.4.4 Bowtie mask .................................................................................. 49 3.5 Mask selection .......................................................................................... 52 3.6 Enforcing structural connectivity .............................................................. 53 3.6.1 Structural accommodations for bowtie mask ................................ 53 3.6.2 Structural accommodations for Gaussian donut mask .................. 55 4. MASK ROTATION MECHANISM FOR THE CELESTRON C11 OPTICAL TUBE ASSEMBLY ............................................................................ 58 4.1 Need for rotation mechanism .................................................................... 58 4.2 Mechanical design considerations ............................................................ 60 4.3 Early designs ............................................................................................. 62 4.3.1 Virtual axis design ......................................................................... 62 4.3.2 Lazy Susan design ......................................................................... 66 4.4 Final design ............................................................................................... 69 4.4.1 Establishing a fixed axis ................................................................ 69 4.4.2 Strategies for powering rotation ...................................................
Load more

Recommended publications
  • Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 Through 2009
    Vol. 6 No. 3 July 1, 2010 Journal of Double Star Observations Page 180 Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 through 2009 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: Using a 10” Newtonian and a fast CCD camera, recordings of double and multiple stars were made at high frame rates with a notebook computer. From superpositions of “lucky images”, measurements of 139 systems were obtained and compared with literature data. B/w and color images of some noteworthy systems are also presented. mented double stars, as will be described in the next Introduction section. Generally, I used a red filter to cope with By using the technique of “lucky imaging”, seeing chromatic aberration of the Barlow lens, as well as to effects can strongly be reduced, and not only the reso- reduce the atmospheric spectrum. For systems with lution of a given telescope can be pushed to its limits, pronounced color contrast, I also made recordings but also the accuracy of position measurements can be with near-IR, green and blue filters in order to pro- better than this by about one order of magnitude. This duce composite images. This setup was the same as I has already been demonstrated in earlier papers in used with telescopes under the southern sky, and as I this journal [1-3]. Standard deviations of separation have described previously [1-3]. Exposure times varied measurements of less than +/- 0.05 msec were rou- between 0.5 msec and 100 msec, depending on the tinely obtained with telescopes of 40 or 50 cm aper- star brightness, and on the seeing.
    [Show full text]
  • Liverpool Telescope 2: a New Robotic Facility for Rapid Transient Follow-Up
    Noname manuscript No. (will be inserted by the editor) Liverpool Telescope 2: a new robotic facility for rapid transient follow-up C.M. Copperwheat · I.A. Steele · R.M. Barnsley · S.D. Bates · D. Bersier · M.F. Bode · D. Carter · N.R. Clay · C.A. Collins · M.J. Darnley · C.J. Davis · C.M. Gutierrez · D.J. Harman · P.A. James · J.H. Knapen · S. Kobayashi · J.M. Marchant · P.A. Mazzali · C.J. Mottram · C.G. Mundell · A. Newsam · A. Oscoz · E. Palle · A. Piascik · R. Rebolo · R.J. Smith Received: date / Accepted: date Abstract The Liverpool Telescope is one of the world’s premier facilities for time domain astronomy. The time domain landscape is set to radically change in the coming decade, with synoptic all-sky surveys such as LSST providing huge numbers of transient detections on a nightly basis; transient detections across the electromagnetic spectrum from other major facilities such as SVOM, SKA and CTA; and the era of ‘multi-messenger astronomy’, wherein astro- physical events are detected via non-electromagnetic means, such as neutrino or gravitational wave emission. We describe here our plans for the Liverpool Telescope 2: a new robotic telescope designed to capitalise on this new era of time domain astronomy. LT2 will be a 4-metre class facility co-located with the Liverpool Telescope at the Observatorio del Roque de Los Muchachos on the Canary island of La Palma. The telescope will be designed for extremely C.M. Copperwheat · I.A. Steele · R.M. Barnsley · S.D. Bates · D. Bersier · M.F. Bode · D.
    [Show full text]
  • The GAPS Programme with HARPS-N@ TNG V. A
    Astronomy & Astrophysics manuscript no. xo2_system_arx c ESO 2018 October 19, 2018 The GAPS Programme with HARPS-N@TNG V. A comprehensive analysis of the XO-2 stellar and planetary systems ⋆ M. Damasso1, 2, K. Biazzo3, A.S. Bonomo1, S. Desidera4, A.F. Lanza3, V. Nascimbeni4, 5, M. Esposito6, 7, G. Scandariato3, A. Sozzetti1, R. Cosentino3, 8, R. Gratton4, L. Malavolta5, 9, M. Rainer10, D. Gandolfi3, 11, E. Poretti10, R. Zanmar Sanchez3, I. Ribas12, N. Santos13, 14, 15,L.Affer16, G. Andreuzzi8, M. Barbieri4, L. R. Bedin4, S. Benatti4, A. Bernagozzi2, E. Bertolini2, M. Bonavita4, F. Borsa10, L. Borsato5, W. Boschin8, P. Calcidese2, A. Carbognani2, D. Cenadelli2, J.M. Christille2, 17, R.U. Claudi4, E. Covino18, A. Cunial5, P. Giacobbe1, V. Granata5, A. Harutyunyan8, M. G. Lattanzi1, G. Leto3, M. Libralato4, 5, G. Lodato19, V. Lorenzi8, L. Mancini20, A.F. Martinez Fiorenzano8, F. Marzari4, 5, S. Masiero4, 5, G. Micela16, E. Molinari8, 21, M. Molinaro22, U. Munari4, S. Murabito6, 7, I. Pagano3, M. Pedani8, G. Piotto4, 5, A. Rosenberg6, 7, R. Silvotti1, J. Southworth23 1 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025, Pino Torinese, Italy. E-mail: [email protected] 2 Osservatorio Astronomico della Regione Autonoma Valle d’Aosta, Fraz. Lignan 39, I-11020, Nus (Aosta), Italy 3 INAF – Osservatorio Astrofisico di Catania, Via S.Sofia 78, I-95123, Catania, Italy 4 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122, Padova, Italy 5 Dip. di Fisica e Astronomia Galileo Galilei – Università di Padova, Vicolo dell’Osservatorio 2, I-35122, Padova, Italy 6 Instituto de Astrofísica de Canarias, C/Via Láctea S/N, E-38200 La Laguna, Tenerife, Spain 7 Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 8 Fundación Galileo Galilei - INAF, Rambla José Ana Fernandez Pérez 7, E-38712 Breña Baja, TF - Spain 9 Obs.
    [Show full text]
  • Eligibility Regnum Prefix Titles Dog Name Suffix Titles Breed Owner(S
    Eligibility Regnum Prefix Titles Dog Name Suffix Titles Breed Owner(s) Novice DN05790903 Marquee Katy Malone CD RN Border Collie Linda Falk Novice DN11600401 Desert Star's Midnight Comet CD PCD BN RAE CGCA CGCU TKN Canaan Dog Denise A Gordon Novice DN13412601 HC Blue CD HSAds HIAs HXAds HXBd Border Collie Margaret Duezabou Novice DN14971401 CH Windypine's Autumn Colors CD BN Australian Shepherd Beverley Shaw/April Lessig/Hope Peavey/Deborah Peavey Novice DN16408102 Outlands Hazardous Material CD BN RA CGCA Cardigan Welsh Corgi Robert N LaBerge/Gail A LaBerge/Lucille Stefanik Novice DN16491802 Hjalt Simply Timeless CD BN RE CGCA Shetland Sheepdog Janet West/Patricia Gustafson Novice DN16870002 CH Versace V. Moned CD RAE NA NAJ OF THDX CGC TKN Belgian Tervuren Pat Matejek/Pat Morgan Novice DN17058004 Buhrmans Gorman Brice CD BN RN NA OAJ Shetland Sheepdog Michelle Richards/Christopher Richards Novice DN17382101 Angelica The River Sings CD BN NA NAJ NF Shetland Sheepdog Ms. Jeanne B Stephens Novice DN17407705 MACH2 PACH Quinto CD RN MXC MJC MXPB MJP3 MJPB PAX Border Collie Carol Siegfried/Michael Siegfried Novice DN18066303 Ryladd Sunny-Giftie Gowkie CD NAP NJP Shetland Sheepdog Ellen Brown Novice DN18262306 GCHS CH Barwoods Gor-Don Adrianna CD BN RA Shetland Sheepdog Susan Ancheta/Dennis Ancheta Novice DN19966608 Mommys Frog Dog Day Day Daisy CD RN Pembroke Welsh Corgi Dr. Thomas Alan Tatham Novice DN20052901 CH Stonerhaven Silver Bells CD BN RAE AX AXJ OF CGCA CGCU TKI Shetland Sheepdog Christina R Stoner/Robert Stoner Novice DN20281403
    [Show full text]
  • Extrasolar Planets and Their Host Stars
    Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it.
    [Show full text]
  • Ianuarie 2016 Nebuloasa NGC 6960
    151 Vega ianuarie 2016 Nebuloasa NGC 6960 Astroclubul Foto: Lucian Hudin Bucureşti 151 Vega Cuprins ianuarie 2016 Foto copertă Nebuloasa NGC 6960 Lucian Hudin Atik 383L+ monocrom EQ6, ED100 f/9, expuneri 3 Întâmplări Astronomice de Iarnă de Adrian Bruno Șonka 16x10min în H-alpha și 12x15min în OIII. 4 Observarea Astronomică a Soarelui de Alexandru Burda Redactori Adrian Bruno Șonka Alexandru Burda 5 Constelații Dispărute de Elisabeta Petrescu Redactor Șef 7 Pasionat de Astronomie cu Lucian Hudin Elisabeta Petrescu 12 Galerie de Imagini - Cometa C/2013 US10 ISSN 1584 - 6563 23 Calendarul Astronomic și Harta Cerului [email protected] Vega- ianuarie 2016 Astroclubul București Întâmplări Astronomice de Iarnă Adrian Bruno Șonka Ați observat că în ultimul timp cometele nu mai arată bine vizual? Majoritatea, chiar dacă în poze au mănunchiuri de cozi ionice și cozi de praf care se în- tind pe zeci de grade, se văd prin ocular doar ca niște pete rotunde. Motivul este, desigur, sensibiliatea mică a ochiului în comparație cu cea camerelor ccd, nefiind de fapt vina cometelor. În ianuarie și februarie încă mai putem vedea pe cer cometa C/2013 US10 Catalina, care va fi circumpolară. O puteți urmări prin telescoape pe măsură ce străbate constelațiile Ursa Major până pe 21 ianuar, Draco (între 21 ș 26 ianuarie) și Camelopardalis (după 31 ianuarie). Între 28 ianuarie și 4 februarie cometa se va afla la mai puțin de 10° de steaua Polară, separația aparentă min- imă (de 8,4°) producându-se pe 2 februarie. Catalina se va apropia aparent și de o altă stea mai strălucitoare, în perioada următoare: pe 24 ianuarie, ora 2, se va afla la numai 2,8° de steaua k Draconis (magnitudinea 3,8).
    [Show full text]
  • Stars, Galaxies, and Beyond, 2012
    Stars, Galaxies, and Beyond Summary of notes and materials related to University of Washington astronomy courses: ASTR 322 The Contents of Our Galaxy (Winter 2012, Professor Paula Szkody=PXS) & ASTR 323 Extragalactic Astronomy And Cosmology (Spring 2012, Professor Željko Ivezić=ZXI). Summary by Michael C. McGoodwin=MCM. Content last updated 6/29/2012 Rotated image of the Whirlpool Galaxy M51 (NGC 5194)1 from Hubble Space Telescope HST, with Companion Galaxy NGC 5195 (upper left), located in constellation Canes Venatici, January 2005. Galaxy is at 9.6 Megaparsec (Mpc)= 31.3x106 ly, width 9.6 arcmin, area ~27 square kiloparsecs (kpc2) 1 NGC = New General Catalog, http://en.wikipedia.org/wiki/New_General_Catalogue 2 http://hubblesite.org/newscenter/archive/releases/2005/12/image/a/ Page 1 of 249 Astrophysics_ASTR322_323_MCM_2012.docx 29 Jun 2012 Table of Contents Introduction ..................................................................................................................................................................... 3 Useful Symbols, Abbreviations and Web Links .................................................................................................................. 4 Basic Physical Quantities for the Sun and the Earth ........................................................................................................ 6 Basic Astronomical Terms, Concepts, and Tools (Chapter 1) ............................................................................................. 9 Distance Measures ......................................................................................................................................................
    [Show full text]
  • Mitsky Bino Adv AL Mul Date Time Con RA Dec Name Other Name
    Mitsky Bino Adv AL Mul Date Time Con RA Dec Name Other Name Double DS DS DS Stars And 0:04:36 +42d06m00s Otto Struve 514 Y And 0:08:24 +29d05m00s Alpha And Y And 0:10:00 +46d23m00s Struve 3 Y And 0:16:24 +43d36m00s h1947 Y And 0:16:42 +36d38m00s Struve 19 And 0:18:30 +26d08m00s Struve 24 Y And 0:18:42 +33d43m00s Pi And Y And 0:18:42 +34d47m00s 26 And Y And 0:20:54 +32d56m00s AC1 And 0:30:06 +29d45m00s 28 AND And 0:31:00 +34d05m00s STF 33 And 0:32:36 +23d11m00s BU 1310 And 0:32:48 +28d16m00s STT 14 And 0:35:12 +36d49m00s STF 40 Struve 40 Y And 0:36:54 +33d43m00s 29-Pi Andromeda 12/11/2014 20:53 And 0:36:54 +33d43m00s PI AND H 5 17 Y And 0:38:36 +40d59m00s STF 44 And 0:39:18 +30d51m00s DELTA AND Y And 0:39:18 +30d52m00s Beta And Y 12/11/2014 21:01 And 0:40:18 +24d03m00s STF 47 Struve 47 Y Y And 0:44:24 +33d37m00s STF 55 And 0:46:24 +30d56m00s STF 1 And 0:54:42 +39d10m00s STF 72 And 0:55:00 +23d38m00s 36 And Y And 0:56:48 +38d30m00s MU AND And 0:57:12 +23d25m00s Eta And Y And 0:59:30 +44d43m00s ES 155 And 1:00:00 +44d43m00s STF 79 Struve 79 Y And 1:02:48 +47d42m00s HJ 2010 And 1:02:54 +41d21m00s 39 AND And 1:07:48 +46d51m00s BU 397 And 1:08:54 +45d12m00s HJ 2018 And 1:09:42 +38d07m00s HO 214 And 1:17:48 +49d00m00s STF 102 And 1:18:48 +37d22m00s STF 108 Struve 108 Y And 1:18:54 +39d57m00s STT29 And 1:20:48 +46d20m00s STF 112 And 1:27:24 +41d05m00s HO 7 And 1:27:36 +45d24m00s OMEGA AND And 1:38:42 +38d39m00s BU 1166 And 1:39:06 +41d04m00s STF 140 And 1:40:24 +34:20 STF 133 Struve 133 Y And 1:40:36 +40d34m00s TAU AND And 1:45:00 +43d42m00s
    [Show full text]
  • Cycle 17 Abstract Catalog (Based on Phase I Submissions) Generated On: Fri May 30 08:50:52 EDT 2008
    Cycle 17 Abstract catalog (based on Phase I submissions) Generated on: Fri May 30 08:50:52 EDT 2008 Proposal Category: GO Scientific Category: UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE ID: 11554 Title: Luminosity Profiles of Extremely Massive Clusters in NGC 7252 PI: Nate Bastian PI Institution: University of Cambridge The galactic merger remnant NGC 7252 represents one of the most extreme post- starburst environments in the local universe. During the disk-disk merger (~400 Myr ago) this galaxy produced the largest young massive star cluster population known, including two clusters above 10^7 Msun, a factor of 100 more massive than typical globular clusters in the Milky Way. We propose ACS-HRC observations of 3 fields in NGC 7252 in order to explore the detailed properties, i.e. luminosity profiles, of these massive star clusters. These observations will be able to test massive cluster formation mechanisms (e.g. the cluster merger scenario) as well as the possible tidal erosion and truncation of the outer regions of the clusters by the galactic tidal field. These observations will compliment our large on-going study using archival HST data, of star cluster profiles outside the Local Group. The cluster population in NGC 7252 will extend our sample in cluster mass by an order of magnitude. ====================================================================== Proposal Category: GO Scientific Category: COOL STARS ID: 11555 Title: Transition Region and Chromospheric Activity on Low Metallicity Arcturus Moving Group "Alien" Dwarfs PI: Alexander Brown PI Institution: University of Colorado at Boulder How does low metallicity affect the heating and resultant temperature structure of the chromospheres, transition regions, and coronae of old solar- like dwarf stars? The Arcturus Moving Group is very likely a remnant of the merger of a dwarf galaxy with the Milky Way Galaxy in the distant (~ 7- 8 Gyr) past.
    [Show full text]
  • Water in Star-Forming Regions: Physics and Chemistry from Clouds to Disks As Probed by Herschel Spectroscopy E.F
    Astronomy & Astrophysics manuscript no. wish_final_Jan2021 ©ESO 2021 February 5, 2021 Water in star-forming regions: Physics and chemistry from clouds to disks as probed by Herschel spectroscopy E.F. van Dishoeck1; 2, L.E. Kristensen3, J.C. Mottram4, A.O. Benz5, E.A. Bergin6, P. Caselli2, F. Herpin7, M.R. Hogerheijde1; 21, D. Johnstone8; 9, R. Liseau10, B. Nisini11, M. Tafalla12, F.F.S. van der Tak13; 14, F. Wyrowski15, A. Baudry7, M. Benedettini16, P. Bjerkeli10, G.A. Blake17, J. Braine7, S. Bruderer2; 5, S. Cabrit18, J. Cernicharo19, Y. Choi13; 20, A. Coutens7, Th. de Graauw1; 13, C. Dominik21, D. Fedele22, M. Fich23, A. Fuente12, K. Furuya24, J.R. Goicoechea19, D. Harsono1, F.P. Helmich13; 14, G.J. Herczeg25, T. Jacq7, A. Karska26, M. Kaufman27, E. Keto28, T. Lamberts29, B. Larsson30, S. Leurini15; 31, D.C. Lis32, G. Melnick28, D. Neufeld33, L. Pagani18, M. Persson10, R. Shipman13, V. Taquet22, T.A. van Kempen34, C. Walsh35, S.F. Wampfler36, U. Yıldız32, and the WISH team (Affiliations can be found after the references) Received 1 August 2020; Accepted 14 December 2020 ABSTRACT Context. Water is a key molecule in the physics and chemistry of star and planet formation, but it is difficult to observe from Earth. The Herschel Space Observatory provided unprecedented sensitivity as well as spatial and spectral resolution to study water. The Water In Star-forming regions with Herschel (WISH) key program was designed to observe water in a wide range of environments and provide a legacy data set to address its physics and chemistry. Aims. The aim of WISH is to determine which physical components are traced by the gas-phase water lines observed with Herschel and to quantify the excitation conditions and water abundances in each of these components.
    [Show full text]
  • Publications for Timothy Bedding 2021 2020 2019
    Publications for Timothy Bedding 2021 B., Hogg, D. (2020). Forward Modeling the Orbits of Yu, J., Hekker, S., Bedding, T., Stello, D., Huber, D., Gizon, L., Companions to Pulsating Stars from Their Light Travel Time Khanna, S., Bi, S. (2021). Asteroseismology of luminous red Variations. Astronomical Journal, 159(5), 202. <a giants with Kepler - II. Dependence of mass-loss on pulsations href="http://dx.doi.org/10.3847/1538-3881/ab7d38">[More and radiation. Monthly Notices of the Royal Astronomical Information]</a> Society, 501(4), 5135-5148. <a Li, G., Van Reeth, T., Bedding, T., Murphy, S., Antoci, V., href="http://dx.doi.org/10.1093/mnras/staa3970">[More Ouazzani, R., Barbara, N. (2020). Gravity-mode period Information]</a> spacings and near-core rotation rates of 611 ? Doradus stars Murphy, S., Barbara, N., Hey, D., Bedding, T., Fulcher, B. with Kepler. Monthly Notices of the Royal Astronomical (2021). Finding binaries from phase modulation of pulsating Society, 491(3), 3586-3605. <a stars with Kepler �VI. Orbits for 10 new binaries with href="http://dx.doi.org/10.1093/mnras/stz2906">[More mischaracterized primaries. Monthly Notices of the Royal Information]</a> Astronomical Society, 493(4), 5382-5388. <a Mart�nez, R., Gaudi, B., Rodriguez, J., Zhou, G., Labadie- href="http://dx.doi.org/10.1093/mnras/staa562">[More Bartz, J., Quinn, S., Penev, K., Tan, T., Latham, D., Paredes, L., Information]</a> Bedding, T., et al (2020). KELT-25 b and KELT-26 b: A Hot Li, Y., Bedding, T., Stello, D., Sharma, S., Huber, D., Murphy, Jupiter and a Substellar Companion Transiting Young A Stars S.
    [Show full text]
  • The Observer of the Twin City Amateur Astronomers
    THE OBSERVER OF THE TWIN CITY AMATEUR ASTRONOMERS Volume 40, Number 12 December 2015 INSIDE THIS ISSUE: Editor’s Choice: Image of the Month……..……………….1 A Note from President Weiland..…………………..……….2 Calendar of Celestial Events – December 2015..…....3 New & Renewing Members/Dues Blues…………..…….3 Subscribing to Our E-Mail Lists………………………….……3 This Month’s Phases of the Moon……..……………...…..4 President’s Message (continued)……………………..…….4 Holiday Gathering at Wenning Residence………….…..4 Minutes of November 24th BoD Meeting………………..5 Minutes of 11/24 NCRAL 2016 Planning Meeting……5 E/PO for November 2015…………………………………….…6 Public Observing Sessions for 2016……………….……….6 AstroBits…………………………………………………………..……7 Observations of Moon, Venus, Mars, & Jupiter………9 NCRAL 2016 Coming April 29/30………………………….…9 The Milky Way Riches of Deneb and Sadr…………….10 TCAA on Facebook and Twitter…………………………….11 Cartoon of the Month…………………………………….…...12 Becoming an Amateur Astronomer………………………12 Universe Sampler II Telescope Course Coming……..14 HowTimeFlies……………………………………………………….15 TCAA History Board Retrieved…………………………..….15 Board Seeks Award Nominations………………………….16 EDITOR’S CHOICE: IMAGE OF THE MONTH – IC 1318 TCAA Treasurer’s Report: November 2015………..….16 Editor’s note: Tim Stone produced the above Image of the Month for December. It shows the Sadr region of Cygnus known to astronomers as IC 1318, The Butterfly Nebula. It is the diffuse nebular region surrounding Sadr or Gamma Cygni. Sadr lies in the center of the Cygnus cross. IC 1318 is the first image successfully taken with the new 16” telescope in PSO. Tim writes, “On November 8, 2015, at Prairie Sky Observatory, Bob Finnigan and I acquired the “first light” image with the new 16” Harmer Wynne telescope from AG Optical Systems, IC 1318 in Cygnus.
    [Show full text]