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Interstellar Extinction in Orion. Variation of the Strength of the UV
MNRAS 000, 1–9 (2017) Preprint 9 July 2018 Compiled using MNRAS LATEX style file v3.0 Interstellar extinction in Orion. Variation of the strength of the UV bump across the complex. Leire Beitia-Antero,1⋆ Ana I. G´omez de Castro,1† 1AEGORA Research Group, Universidad Complutense de Madrid, Facultad de CC. Matem´aticas, Plaza de Ciencias 3, E-28040 Madrid Accepted XXX. Received YYY; in original form ZZZ ABSTRACT There is growing observational evidence of dust coagulation in the dense filaments within molecular clouds. Infrared observations show that the dust grains size distri- bution gets shallower and the relative fraction of small to large dust grains decreases as the local density increases. Ultraviolet (UV) observations show that the strength of the 2175 A˚ feature, the so-called UV bump, also decreases with cloud density. In this work, we apply the technique developed for the Taurus study to the Orion molecular cloud and confirm that the UV bump decreases over the densest cores of the cloud as well as in the heavily UV irradiated λ Orionis shell. The study has been extended to the Rosette cloud with uncertain results given the distance (1.3 kpc). Key words: ISM: dust, extinction 1 INTRODUCTION feature of the extinction curve, the so-called UV bump. The UV bump is, by far, the strongest spectral feature in the ex- The Interstellar Medium (ISM) is a complex ensemble of tinction curve but its source remains uncertain (see e.g. the gas, large molecules and dust coupled through the action of review by Draine (2003)). -
Cassiopeia a January2008
CASSIOPEIA A JANUARY2008 Cassiopeia A is the youngest (about 300 years old) known supernova Su Mo Tu We Th Fr Sa remnant in the Milky Way. Astronomers have used Chandra’s long ob - 01 02 03 04 05 servations of this remnant to make a map of the acceleration of elec - trons in this supernova remnant. The analysis shows that the electrons 06 07 08 09 10 11 12 are being accelerated to almost the maximum theoretical limit in some 13 14 15 16 17 18 19 parts of Cassiopeia A (Cas A) in what can be thought of as a “relativistic pinball machine.” Protons and ions, which make up the bulk of cosmic 20 21 22 23 24 25 26 rays, are expected to be accelerated in a similar way to the electrons. The Cas A observations thus provide strong evidence that supernova 27 28 29 30 31 remnants are key sites for energizing cosmic rays. 3C442A FEBRUARY2008 X -ray data from NASA’s Chandra X -ray Observatory and radio obser - Su Mo Tu We Th Fr Sa vations from the NSF’s Very Large Array show that a role reversal is 01 02 taking place in the middle of 3C442A - a system with two merging gal - 03 04 05 06 07 08 09 axies in the center. Chandra detects hot gas (blue) that has been push - ing aside the radio -bright gas (orange). This is the opposite of what 10 11 12 13 14 15 16 is typically found in these systems when jets from the supermassive black hole in the center create cavities in the hot gas surrounding the 17 18 19 20 21 22 23 galaxy. -
Theoretical Limits of Star Sensor Accuracy †
sensors Article Theoretical Limits of Star Sensor Accuracy † Marcio A. A. Fialho 1,* and Daniele Mortari 2 1 Divisão de Eletrônica Aeroespacial (DIDEA), National Institute for Space Research (INPE), Av. dos Astronautas, 1758, São José dos Campos, SP 12227, Brazil 2 Aerospace Engineering, Texas A&M University, College Station, TX 77843, USA; [email protected] * Correspondence: marcio.fi[email protected]; Tel.: +55-12-3208-6145 † This paper is a revised and extended version of a work previously published as a doctoral thesis chapter. Received: 17 October 2019; Accepted: 25 November 2019; Published: 5 December 2019 Abstract: To achieve mass, power and cost reduction, there is a trend to reduce the volume of many instruments aboard spacecraft, especially for small spacecraft (cubesats or nanosats) with very limited mass, volume and power budgets. With the current trend of miniaturizing spacecraft instruments one could naturally ask if is there a physical limit to this process for star sensors. This paper shows that there is a fundamental limit on star sensor accuracy, which depends on stellar distribution, star sensor dimensions and exposure time. An estimate of this limit is given for our location in the galaxy. Keywords: star sensors; stellar distribution; photometry; astrometry; star catalogs; fundamental limits 1. Introduction Much progress in a variety of fields in science and technology could be accomplished thanks to the miniaturization obtained in microelectronics in the recent decades. One of the most remarkable examples is the prediction by Gordon Moore that the computational power would increase exponentially, an empirical observation that became known as Moore’s law [1–4]. -
The Spitzer Space Telescope and the IR Astronomy Imaging Chain
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different from optical astronomy sources) 2) Object (usually the same as the source in astronomy) 3) Collector (Spitzer Space Telescope) 4) Sensor (IR detector) 5) Processing 6) Display 7) Analysis 8) Storage ... but steps 3) and 4) are a bit more difficult! Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 2/38 The infrared imaging chain Longer wavelength – need a bigger telescope to get the same resolution or put up with lower resolution Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 3/38 Emission of IR radiation Warm objects emit lots of thermal infrared as well as reflecting it Including telescopes, people, and the Earth – so collection of IR radiation with a telescope is more complicated than an optical telescope Optical image of Spitzer Space Telescope launch: brighter regions are those which reflect more light IR image of Spitzer launch: brighter regions are those which emit more heat Infrared wavelength depends on temperature of object Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 4/38 Atmospheric absorption The atmosphere blocks most infrared radiation Need a telescope in space to view the IR properly Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 5/38 -
Young Stellar Object Candidates Toward the Orion Region Selected from GALEX (Research Note)
A&A 572, A89 (2014) Astronomy DOI: 10.1051/0004-6361/201424629 & c ESO 2014 Astrophysics Young stellar object candidates toward the Orion region selected from GALEX (Research Note) Nestor Sanchez, Ana Inés Gómez de Castro, Fátima Lopez-Martinez, and Javier López-Santiago S. D. Astronomía y Geodesia, Fac. CC. Matemáticas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: [email protected] Received 18 July 2014 / Accepted 28 October 2014 ABSTRACT We analyze 359 ultraviolet tiles from the All Sky Imaging Survey of the space mission GALEX covering roughly 400 square degrees toward the Orion star-forming region. There are a total of 1 555 174 ultraviolet sources that were cross-matched with other catalogs (2MASS, UCAC4, SDSS, DENIS, CMC15, and WISE) to produce a list of 290 717 reliable sources with a wide range of photometric information. Using different color selection criteria, we identify 111 young stellar object candidates showing both ultraviolet and infrared excesses, of which 81 are new identifications. We discuss the spatial distribution, the spectral energy distributions, and other physical properties of these stars. Their properties are, in general, compatible with those expected for T Tauri stars. This population of TTS candidates is widely dispersed around the Orion molecular cloud. Key words. stars: low-mass – stars: pre-main sequence – stars: variables: T Tauri, Herbig Ae/Be – ultraviolet: stars 1. Introduction and magnetic stellar activity (Edwards et al. 1994; Muzerolle et al. 1998). As spectroscopic observations are time consuming The current paradigm for low-mass star formation catego- and are sometimes restricted to bright objects, a good strategy is rizes young stellar objects (YSOs) into four general classes: to perform spectroscopic follow-ups only for the most reliable Class 0 sources are faint central protostars surrounded by a YSO candidates selected using photometric methods. -
Sky-Watcher Skyliner-300P Flextube Auto Sky-Watcher’S Latest Dobsonian Telescope Can Track the Stars So That the Views Through Its Huge Aperture Stay in the Eyepiece
AUGUST 09 FIRST LIGHT: AN IN-DEPTH LOOK AT THIS MONTH'S HOTTEST NEW PRODUCT SKY-waTCHER Skyliner-300P FlexTube Auto Sky-Watcher’s latest Dobsonian telescope can track the stars so that the views through its huge aperture stay in the eyepiece. Paul Money takes a look VITAL STATS hen John Dobson MDF rocker base here, like the plug it into a power pack, neither created the telescope setup of some other Dobsonians. of which are supplied. > PRICE £1,099 design that bears his This is no doubt to ensure that the The Skyliner’s 1,500mm of > APERTURE 305mm (12 inches) name, he would scarcely have 300P’s axis motors stay accurately focal length collapses down to > FOCAL LENGTH 1,500mm; f/5 imagined how it would evolve installed. Instead, you just lift the just under a metre thanks to its > OpTICAL DESIGN Newtonian thanks to Sky-Watcher. First, tube assembly onto the rocker telescopically extending trusses, reflector > FINDER 9x50 straight-through the company came up with the base and the main job’s done. All making it extremely portable for > EYEPIECES 25mm, 10mm; FlexTube collapsible truss tube, that’s left is the 9x50 straight- such a large instrument. We were 1.25-inch fit which greatly improved through finderscope to assemble impressed to find no collimation > FOCUSER Crayford; 1.25- & 2-inch fit portability. Now it has added and the hand controller to install. issues, even after repeated setups. > MOUNT Motorised Dobsonian auto-tracking motors to the The 300P comes with two And with its tracking motors, we > WEIGHT 40kg FlexTube design, taking the eyepieces, a 25mm and 10mm could take decent images of the > SUPPLIER Optical Vision Dobsonian on its next great 1.25-inch fit that give 60x and Moon and planets, despite the > www.opticalvision.co.uk leap forward. -
Gao-21-306, Nasa
United States Government Accountability Office Report to Congressional Committees May 2021 NASA Assessments of Major Projects GAO-21-306 May 2021 NASA Assessments of Major Projects Highlights of GAO-21-306, a report to congressional committees Why GAO Did This Study What GAO Found This report provides a snapshot of how The National Aeronautics and Space Administration’s (NASA) portfolio of major well NASA is planning and executing projects in the development stage of the acquisition process continues to its major projects, which are those with experience cost increases and schedule delays. This marks the fifth year in a row costs of over $250 million. NASA plans that cumulative cost and schedule performance deteriorated (see figure). The to invest at least $69 billion in its major cumulative cost growth is currently $9.6 billion, driven by nine projects; however, projects to continue exploring Earth $7.1 billion of this cost growth stems from two projects—the James Webb Space and the solar system. Telescope and the Space Launch System. These two projects account for about Congressional conferees included a half of the cumulative schedule delays. The portfolio also continues to grow, with provision for GAO to prepare status more projects expected to reach development in the next year. reports on selected large-scale NASA programs, projects, and activities. This Cumulative Cost and Schedule Performance for NASA’s Major Projects in Development is GAO’s 13th annual assessment. This report assesses (1) the cost and schedule performance of NASA’s major projects, including the effects of COVID-19; and (2) the development and maturity of technologies and progress in achieving design stability. -
A Guide to Smartphone Astrophotography National Aeronautics and Space Administration
National Aeronautics and Space Administration A Guide to Smartphone Astrophotography National Aeronautics and Space Administration A Guide to Smartphone Astrophotography A Guide to Smartphone Astrophotography Dr. Sten Odenwald NASA Space Science Education Consortium Goddard Space Flight Center Greenbelt, Maryland Cover designs and editing by Abbey Interrante Cover illustrations Front: Aurora (Elizabeth Macdonald), moon (Spencer Collins), star trails (Donald Noor), Orion nebula (Christian Harris), solar eclipse (Christopher Jones), Milky Way (Shun-Chia Yang), satellite streaks (Stanislav Kaniansky),sunspot (Michael Seeboerger-Weichselbaum),sun dogs (Billy Heather). Back: Milky Way (Gabriel Clark) Two front cover designs are provided with this book. To conserve toner, begin document printing with the second cover. This product is supported by NASA under cooperative agreement number NNH15ZDA004C. [1] Table of Contents Introduction.................................................................................................................................................... 5 How to use this book ..................................................................................................................................... 9 1.0 Light Pollution ....................................................................................................................................... 12 2.0 Cameras ................................................................................................................................................ -
Experiments on the Differential Vlbi Measurements with the Former Russian Deep Space Network
EXPERIMENTS ON THE DIFFERENTIAL VLBI MEASUREMENTS WITH THE FORMER RUSSIAN DEEP SPACE NETWORK Igor E. Molotov(1,2,3) (1)Bear Lakes Radio Astronomy Station of Central (Pulkovo) Astronomical Observatory, Pulkovskoye chosse 65/1, Saint-Petersburg, 196140, Russia , E-mail: [email protected] (2)Keldysh Institute of Applied Mathematics, Miusskaja sq. 4, 125047 Moscow, Russia (3)Central Research Institute for Machine Building, 4 Pionerskaya Street, Korolev, 141070, Russia ABSTRACT The differential VLBI technique (delta-VLBI) is applied transforms the signals into video frequencies, which for measuring spacecraft position with accuracy up to 1 then are sampled with 1- or 2-bit quantization, formatted in any standard VLBI format (Mk-4, S2, K-4, mas. This procedure allows to link the sky position of object with the position of close ICRF quasar on the Mk-2) and recorded on magnetic tapes or PC-disks celestial sphere. Few delta-VLBI measurements can together with precise clock using VLBI terminal. All frequency transformations are connected with atomic urgently improve the knowledge of object trajectory in the times of critical maneuvers. frequency standard. The tapes/disks from all radio telescopes of VLBI array are collected at data The Russian Deep Space Network that was based on processing center, where the data are cross-correlated. three large antennas: 70 m in Evpatoria (Ukraine) and The processing is aimed to measure the time delay of Ussuriysk (Far East), and 64 m in Bear Lakes (near emitted wavefront arrival to receiving antennas, and Moscow) arranged the trial delta-VLBI experiments frequency of interference (fringe rate), that contain the with help of four scientific institutions. -
The Blue Planet Report from Stellafane Perspective on Apollo How to Gain and Retain New Members
Published by the Astronomical League Vol. 71, No. 4 September 2019 THE BLUE PLANET REPORT FROM STELLAFANE 7.20.69 5 PERSPECTIVE ON APOLLO YEARS APOLLO 11 HOW TO GAIN AND RETAIN NEW MEMBERS mic Hunter h Cos h 4 er’s 5 t h Win 6 7h +30° AURIG A +30° Fast Facts TAURUS Orion +20° χ1 χ2 +20° GE MIN I ated winter nights are domin ο1 Mid ξ ν 2 ORIO N ο tion Orion. This +10° by the constella 1 a π Meiss λ 2 μ π +10° 2 φ1 attended by his φ 3 unter, α γ π cosmic h Bellatrix 4 Betelgeuse π d ω Canis Major an ψ ρ π5 hunting dogs, π6 0° intaka aurus the M78 δ M , follows T 0° ε and Minor Alnitak Alnilam What’s Your Pleasure? ζ h σ η vens eac EROS ross the hea MONOC M43 M42 Bull ac θ τ ι υ ess pursuit. β –10° night in endl Saiph Rigel –10° κ The showpiece of the ANI S C LEPU S ERIDANU S ion MAJOR constellation is the Or ORION (Constellation) –20° wn here), –20° Nebula (M42,sho ion 5 hr; Location: Right Ascens a region of nebulosity ° north 4h Declination 5 5h 6h 7h 2 square degrees th just 1,300 a: 594 and starbir Are 3 4 5 6 0 1 2 0 -2 -1 he Hunter 2 Symbol: T 0 t-years away that is M42 (Orion Nebula); C ligh Notable Objects: a la); NG C 2024 laked eye as a tary nebu e M78 (plane visible to the n n la) d. -
Web Suppliers of Telescope Building Parts and Materials
Appendix I Web Suppliers of Telescope Building Parts and Materials No endorsement or recommendation is provided or implied. The organizations listed are here because they were found in other such lists or advertisements or were personally known to someone. Those for whom e-mail addresses were available were notified that they would be listed. Those for whom there were no e-mail addresses or whose e-mail was not deliverable were sent regular letters with the same information. If there was no response to notification, the listing was removed. Quite a few listed organizations submitted additions or changes to their list of products. References to items specific to astrophotography and to Dobsonians were, for the most part, avoided. Likewise, references to subjects other than building telescopes, such as star charts, were avoided. If you are searching for some particular item or for something that will serve for a particular item you are advised to look under a variety of related categories. There is very little standardization of nomenclature in telescope design. For exam- ple, “used” usually means “buys and sells used parts and complete scopes.” Rings and mounting rings probably are overlapping categories. Diagonals, mirrors, and secondary mirrors probably all mean the same thing. Some of the listed organizations produce or distribute items useful to us telescope makers but with a much wider/different selection of clients. In dealing with them it would be useful if you are particularly clear as to the intended use. Some produce items for other industries and are set up to supply materials in large quantities. -
Simulated JWST Data Sets for Multispectral and Hyperspectral Image Fusion Claire Guilloteau, Thomas Oberlin, Olivier Berné, Émilie Habart, Nicolas Dobigeon
Simulated JWST data sets for multispectral and hyperspectral image fusion Claire Guilloteau, Thomas Oberlin, Olivier Berné, Émilie Habart, Nicolas Dobigeon To cite this version: Claire Guilloteau, Thomas Oberlin, Olivier Berné, Émilie Habart, Nicolas Dobigeon. Simulated JWST data sets for multispectral and hyperspectral image fusion. Astronomical Journal, American Astro- nomical Society, 2020, 160 (1), pp.0. 10.3847/1538-3881/ab9301. hal-02886110 HAL Id: hal-02886110 https://hal.archives-ouvertes.fr/hal-02886110 Submitted on 1 Jul 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Open Archive Toulouse Archive Ouverte OATAO is an open access repository that collects the work of Toulouse researchers and makes it freely available over the web where possible This is a publisher’s version published in: https://oatao.univ-toulouse.fr/26226 Official URL : https://doi.org/10.3847/1538-3881/ab9301 To cite this version: Guilloteau, Claire and Oberlin, Thomas and Berné, Olivier and Habart, Émilie and Dobigeon, Nicolas Simulated JWST data sets for multispectral and hyperspectral image fusion. (2020) The Astronomical Journal, 160 (1). ISSN 0004-6256. Any correspondence concerning this service should be sent to the repository administrator: [email protected] The Astronomical Journal, 160:28 (13pp), 2020 July https://doi.org/10.3847/1538-3881/ab9301 © 2020.