BRAS Newsletter August 2013
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Spectroscopy of the Candidate Luminous Blue Variable at the Center
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 06 (08.03.4; 08.05.1; 08.05.3; 08.09.2; 08.13.2; 08.22.3) ASTROPHYSICS Spectroscopy of the candidate luminous blue variable at the center of the ring nebula G79.29+0.46 R.H.M. Voors1,2⋆, T.R. Geballe3, L.B.F.M. Waters4,5, F. Najarro6, and H.J.G.L.M. Lamers1,2 1 Astronomical Institute, University of Utrecht, Princetonplein 5, 3508 TA Utrecht, The Netherlands 2 SRON Laboratory for Space Research, Sorbonnelaan 2, NL-3584 CA Utrecht, The Netherlands 3 Gemini Observatory, 670 N. A’ohoku Place, Hilo, Hawaii 96720, USA 4 Astronomical Institute ’Anton Pannekoek’, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Nether- lands 5 SRON Laboratory for Space Research, P.O. Box 800, NL-9700 AV Groningen, The Netherlands 6 CSIC Instituto de Estructura de la Materia, Dpto. Fisica Molecular, C/Serrano 121, E-28006 Madrid, Spain Received date: 23 March 2000; accepted date Abstract. We report optical and near-infrared spectra of Luminous Blue Variable (LBV) stage (Conti 1984), these the central star of the radio source G79.29+0.46, a can- stars lose a large amount of mass in a short time interval didate luminous blue variable. The spectra contain nu- (e.g. Chiosi & Maeder 1986). The identifying characteris- merous narrow (FWHM < 100 kms−1) emission lines of tics of an LBV in addition to its blue colors are (1) a mass −5 −1 which the low-lying hydrogen lines are the strongest, and loss rate of (∼ 10 M⊙ yr ), (2) a low wind velocity of resemble spectra of other LBVc’s and B[e] supergiants. -
Discovery of a Pulsar Wind Nebula Candidate in the Cygnus Loop
Discovery of a Pulsar Wind Nebula Candidate in the Cygnus Loop 2 3 S Satoru Katsuda" Hiroshi Tsunemi , Koji Mori , Hiroyuki Uchida" Robert Petre , Shin'ya 1 Yamada , and Thru Tamagawa' ABSTRACT We report on a discovery of a diffuse nebula containing a pointlike source in the southern blowout region of the Cygnus Loop supernova remnant, based on Suzaku and XMM-Newton observations. The X-ray spectra from the nebula and the pointlike source are well represented by an absorbed power-law model with photon indices of 2.2±0.1 and 1.6±0.2, respectively. The photon indices as well as the flux ratio of F nebula/ F po;.,li" ~ 4 lead us to propose that the system is a pulsar wind nebula, although pulsations have not yet been detected. If we attribute its origin to the Cygnus Loop supernova, then the 0.5- 8 keY luminosity of the nebula is computed to be 2.1xlo"' (d/MOpc)2ergss-" where d is the distance to the Loop. This implies a spin-down loss-energy E ~ 2.6 X 1035 (d/MOpc)2ergss-'. The location of the neutron star candidate, ~2° away from the geometric center of the Loop, implies a high transverse velocity of ~ 1850(8/2D ) (d/540pc) (t/lOkyr)- ' kms-" assuming the currently accepted age of the Cygnus Loop. Subject headings: ISM: individual objects (Cygnus Loop) - ISM: supernova remnants - pulsars: general - stars: neutron - stars: winds, outflows - X-rays: ISM 'RlKEN (The Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, Sailama 351-0198 2Department of EaTth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Thyonaka, Osaka, 60-0043, Japan SDepartment of Applied Physics, Faculty of Engineering, University of Miyazaki, 1-1 Gakuen Klbana-dai Nishi, Miyazaki, 889-2192, Japan ' Department of PhysiCS, Kyoto University, Kitashirakawa-oiwake-clto, Sakyo, Kyoto 606-8502, J apan 'NASA Goddard Space Flight Center, Code 662, Greenbelt MD 20771 - 2 - 1. -
XMM-Newton Observation of the Northeastern Limb of the Cygnus Loop Supernova Remnant
XMM-Newton Observation of the Northeastern Limb of the Cygnus Loop Supernova Remnant Norbert Nemes Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka, Osaka 560-0043, Japan 04 February 2005 Osaka University Abstract We have observed the northeastern limb of the Cygnus Loop supernova remnant with the XMM-Newton observatory, as part of a 7-pointing campaign to map the remnant across its diameter. We performed medium sensitivity spatially resolved X-ray spectroscopy on the data in the 0.3-3.0 keV energy range, and for the first time we have detected C emission lines in our spectra. The background subtracted spectra were fitted with a single temperature absorbed non-equilibrium (VNEI) model. We created color maps and plotted the radial variation of the different parameters. We found that the heavy element abundances were depleted, but increase toward the edge of the remnant, exhibiting a jump structure near the northeastern edge of the field of view. The depletion suggests that the plasma in this region represents the shock heated ISM rather than the ejecta, while the radial increase of the elemental abundances seems to support the cavity explosion origin. The temperature decreases in the radial direction from 0:3keV to about 0:2keV , however, this ∼ ∼ decrease is not monotonic. There is a low temperature region in the part of the field of view closest to the center of the remnant, which is characterized by low abundances and high NH values. Another low temperature region characterized by low NH values but where the heavy element abundances suddenly jump to high values was found at the northeastern edge of the field of view. -
Observing List
day month year Epoch 2000 local clock time: 23.98 Observing List for 23 7 2019 RA DEC alt az Constellation object mag A mag B Separation description hr min deg min 20 50 Andromeda Gamma Andromedae (*266) 2.3 5.5 9.8 yellow & blue green double star 2 3.9 42 19 28 69 Andromeda Pi Andromedae 4.4 8.6 35.9 bright white & faint blue 0 36.9 33 43 30 55 Andromeda STF 79 (Struve) 6 7 7.8 bluish pair 1 0.1 44 42 16 52 Andromeda 59 Andromedae 6.5 7 16.6 neat pair, both greenish blue 2 10.9 39 2 45 67 Andromeda NGC 7662 (The Blue Snowball) planetary nebula, fairly bright & slightly elongated 23 25.9 42 32.1 31 60 Andromeda M31 (Andromeda Galaxy) large sprial arm galaxy like the Milky Way 0 42.7 41 16 31 61 Andromeda M32 satellite galaxy of Andromeda Galaxy 0 42.7 40 52 32 60 Andromeda M110 (NGC205) satellite galaxy of Andromeda Galaxy 0 40.4 41 41 17 55 Andromeda NGC752 large open cluster of 60 stars 1 57.8 37 41 17 48 Andromeda NGC891 edge on galaxy, needle-like in appearance 2 22.6 42 21 45 69 Andromeda NGC7640 elongated galaxy with mottled halo 23 22.1 40 51 46 57 Andromeda NGC7686 open cluster of 20 stars 23 30.2 49 8 30 121 Aquarius 55 Aquarii, Zeta 4.3 4.5 2.1 close, elegant pair of yellow stars 22 28.8 0 -1 12 120 Aquarius 94 Aquarii 5.3 7.3 12.7 pale rose & emerald 23 19.1 -13 28 32 152 Aquarius M72 globular cluster 20 53.5 -12 32 31 151 Aquarius M73 Y-shaped asterism of 4 stars 20 59 -12 38 16 117 Aquarius NGC7606 Galaxy 23 19.1 -8 29 32 149 Aquarius NGC7009 Saturn Neb planetary nebula, large & bright pale green oval 21 4.2 -11 21.8 38 135 -
Miniature Exoplanet Radial Velocity Array I: Design, Commissioning, and Early Photometric Results
Miniature Exoplanet Radial Velocity Array I: design, commissioning, and early photometric results Jonathan J. Swift Steven R. Gibson Michael Bottom Brian Lin John A. Johnson Ming Zhao Jason T. Wright Paul Gardner Nate McCrady Emilio Falco Robert A. Wittenmyer Stephen Criswell Peter Plavchan Chantanelle Nava Reed Riddle Connor Robinson Philip S. Muirhead David H. Sliski Erich Herzig Richard Hedrick Justin Myles Kevin Ivarsen Cullen H. Blake Annie Hjelstrom Jason Eastman Jon de Vera Thomas G. Beatty Andrew Szentgyorgyi Stuart I. Barnes Downloaded From: http://astronomicaltelescopes.spiedigitallibrary.org/ on 05/21/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Journal of Astronomical Telescopes, Instruments, and Systems 1(2), 027002 (Apr–Jun 2015) Miniature Exoplanet Radial Velocity Array I: design, commissioning, and early photometric results Jonathan J. Swift,a,*,† Michael Bottom,a John A. Johnson,b Jason T. Wright,c Nate McCrady,d Robert A. Wittenmyer,e Peter Plavchan,f Reed Riddle,a Philip S. Muirhead,g Erich Herzig,a Justin Myles,h Cullen H. Blake,i Jason Eastman,b Thomas G. Beatty,c Stuart I. Barnes,j,‡ Steven R. Gibson,k,§ Brian Lin,a Ming Zhao,c Paul Gardner,a Emilio Falco,l Stephen Criswell,l Chantanelle Nava,d Connor Robinson,d David H. Sliski,i Richard Hedrick,m Kevin Ivarsen,m Annie Hjelstrom,n Jon de Vera,n and Andrew Szentgyorgyil aCalifornia Institute of Technology, Departments of Astronomy and Planetary Science, 1200 E. California Boulevard, Pasadena, California 91125, United States bHarvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, United States cThe Pennsylvania State University, Department of Astronomy and Astrophysics, Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, University Park, Pennsylvania 16802, United States dUniversity of Montana, Department of Physics and Astronomy, 32 Campus Drive, No. -
Multiple Star Systems Observed with Corot and Kepler
Multiple star systems observed with CoRoT and Kepler John Southworth Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK Abstract. The CoRoT and Kepler satellites were the first space platforms designed to perform high-precision photometry for a large number of stars. Multiple systems dis- play a wide variety of photometric variability, making them natural benefactors of these missions. I review the work arising from CoRoT and Kepler observations of multiple sys- tems, with particular emphasis on eclipsing binaries containing giant stars, pulsators, triple eclipses and/or low-mass stars. Many more results remain untapped in the data archives of these missions, and the future holds the promise of K2, TESS and PLATO. 1 Introduction The CoRoT and Kepler satellites represent the first generation of astronomical space missions capable of large-scale photometric surveys. The large quantity – and exquisite quality – of the data they pro- vided is in the process of revolutionising stellar and planetary astrophysics. In this review I highlight the immense variety of the scientific results from these concurrent missions, as well as the context provided by their precursors and implications for their successors. CoRoT was led by CNES and ESA, launched on 2006/12/27,and retired in June 2013 after an irre- trievable computer failure in November 2012. It performed 24 observing runs, each lasting between 21 and 152days, with a field of viewof 2×1.3◦ ×1.3◦, obtaining light curves of 163000 stars [42]. Kepler was a NASA mission, launched on 2009/03/07and suffering a critical pointing failure on 2013/05/11. It observed the same 105deg2 sky area for its full mission duration, obtaining high-precision light curves of approximately 191000 stars. -
SEPTEMBER 2014 OT H E D Ebn V E R S E R V ESEPTEMBERR 2014
THE DENVER OBSERVER SEPTEMBER 2014 OT h e D eBn v e r S E R V ESEPTEMBERR 2014 FROM THE INSIDE LOOKING OUT Calendar Taken on July 25th in San Luis State Park near the Great Sand Dunes in Colorado, Jeff made this image of the Milky Way during an overnight camping stop on the way to Santa Fe, NM. It was taken with a Canon 2............................. First quarter moon 60D camera, an EFS 15-85 lens, using an iOptron SkyTracker. It is a single frame, with no stacking or dark/ 8.......................................... Full moon bias frames, at ISO 1600 for two minutes. Visible in this south-facing photograph is Sagittarius, and the 14............ Aldebaran 1.4˚ south of moon Dark Horse Nebula inside of the Milky Way. He processed the image in Adobe Lightroom. Image © Jeff Tropeano 15............................ Last quarter moon 22........................... Autumnal Equinox 24........................................ New moon Inside the Observer SEPTEMBER SKIES by Dennis Cochran ygnus the Swan dives onto center stage this other famous deep-sky object is the Veil Nebula, President’s Message....................... 2 C month, almost overhead. Leading the descent also known as the Cygnus Loop, a supernova rem- is the nose of the swan, the star known as nant so large that its separate arcs were known Society Directory.......................... 2 Albireo, a beautiful multi-colored double. One and named before it was found to be one wide Schedule of Events......................... 2 wonders if Albireo has any planets from which to wisp that came out of a single star. The Veil is see the pair up-close. -
The Midnight Sky: Familiar Notes on the Stars and Planets, Edward Durkin, July 15, 1869 a Good Way to Start – Find North
The expression "dog days" refers to the period from July 3 through Aug. 11 when our brightest night star, SIRIUS (aka the dog star), rises in conjunction* with the sun. Conjunction, in astronomy, is defined as the apparent meeting or passing of two celestial bodies. TAAS Fabulous Fifty A program for those new to astronomy Friday Evening, July 20, 2018, 8:00 pm All TAAS and other new and not so new astronomers are welcome. What is the TAAS Fabulous 50 Program? It is a set of 4 meetings spread across a calendar year in which a beginner to astronomy learns to locate 50 of the most prominent night sky objects visible to the naked eye. These include stars, constellations, asterisms, and Messier objects. Methodology 1. Meeting dates for each season in year 2018 Winter Jan 19 Spring Apr 20 Summer Jul 20 Fall Oct 19 2. Locate the brightest and easiest to observe stars and associated constellations 3. Add new prominent constellations for each season Tonight’s Schedule 8:00 pm – We meet inside for a slide presentation overview of the Summer sky. 8:40 pm – View night sky outside The Midnight Sky: Familiar Notes on the Stars and Planets, Edward Durkin, July 15, 1869 A Good Way to Start – Find North Polaris North Star Polaris is about the 50th brightest star. It appears isolated making it easy to identify. Circumpolar Stars Polaris Horizon Line Albuquerque -- 35° N Circumpolar Stars Capella the Goat Star AS THE WORLD TURNS The Circle of Perpetual Apparition for Albuquerque Deneb 1 URSA MINOR 2 3 2 URSA MAJOR & Vega BIG DIPPER 1 3 Draco 4 Camelopardalis 6 4 Deneb 5 CASSIOPEIA 5 6 Cepheus Capella the Goat Star 2 3 1 Draco Ursa Minor Ursa Major 6 Camelopardalis 4 Cassiopeia 5 Cepheus Clock and Calendar A single map of the stars can show the places of the stars at different hours and months of the year in consequence of the earth’s two primary movements: Daily Clock The rotation of the earth on it's own axis amounts to 360 degrees in 24 hours, or 15 degrees per hour (360/24). -
Ghost Hunt Challenge 2020
Virtual Ghost Hunt Challenge 10/21 /2020 (Sorry we can meet in person this year or give out awards but try doing this challenge on your own.) Participant’s Name _________________________ Categories for the competition: Manual Telescope Electronically Aided Telescope Binocular Astrophotography (best photo) (if you expect to compete in more than one category please fill-out a sheet for each) ** There are four objects on this list that may be beyond the reach of beginning astronomers or basic telescopes. Therefore, we have marked these objects with an * and provided alternate replacements for you just below the designated entry. We will use the primary objects to break a tie if that’s needed. Page 1 TAS Ghost Hunt Challenge - Page 2 Time # Designation Type Con. RA Dec. Mag. Size Common Name Observed Facing West – 7:30 8:30 p.m. 1 M17 EN Sgr 18h21’ -16˚11’ 6.0 40’x30’ Omega Nebula 2 M16 EN Ser 18h19’ -13˚47 6.0 17’ by 14’ Ghost Puppet Nebula 3 M10 GC Oph 16h58’ -04˚08’ 6.6 20’ 4 M12 GC Oph 16h48’ -01˚59’ 6.7 16’ 5 M51 Gal CVn 13h30’ 47h05’’ 8.0 13.8’x11.8’ Whirlpool Facing West - 8:30 – 9:00 p.m. 6 M101 GAL UMa 14h03’ 54˚15’ 7.9 24x22.9’ 7 NGC 6572 PN Oph 18h12’ 06˚51’ 7.3 16”x13” Emerald Eye 8 NGC 6426 GC Oph 17h46’ 03˚10’ 11.0 4.2’ 9 NGC 6633 OC Oph 18h28’ 06˚31’ 4.6 20’ Tweedledum 10 IC 4756 OC Ser 18h40’ 05˚28” 4.6 39’ Tweedledee 11 M26 OC Sct 18h46’ -09˚22’ 8.0 7.0’ 12 NGC 6712 GC Sct 18h54’ -08˚41’ 8.1 9.8’ 13 M13 GC Her 16h42’ 36˚25’ 5.8 20’ Great Hercules Cluster 14 NGC 6709 OC Aql 18h52’ 10˚21’ 6.7 14’ Flying Unicorn 15 M71 GC Sge 19h55’ 18˚50’ 8.2 7’ 16 M27 PN Vul 20h00’ 22˚43’ 7.3 8’x6’ Dumbbell Nebula 17 M56 GC Lyr 19h17’ 30˚13 8.3 9’ 18 M57 PN Lyr 18h54’ 33˚03’ 8.8 1.4’x1.1’ Ring Nebula 19 M92 GC Her 17h18’ 43˚07’ 6.44 14’ 20 M72 GC Aqr 20h54’ -12˚32’ 9.2 6’ Facing West - 9 – 10 p.m. -
Biosignatures Search in Habitable Planets
galaxies Review Biosignatures Search in Habitable Planets Riccardo Claudi 1,* and Eleonora Alei 1,2 1 INAF-Astronomical Observatory of Padova, Vicolo Osservatorio, 5, 35122 Padova, Italy 2 Physics and Astronomy Department, Padova University, 35131 Padova, Italy * Correspondence: [email protected] Received: 2 August 2019; Accepted: 25 September 2019; Published: 29 September 2019 Abstract: The search for life has had a new enthusiastic restart in the last two decades thanks to the large number of new worlds discovered. The about 4100 exoplanets found so far, show a large diversity of planets, from hot giants to rocky planets orbiting small and cold stars. Most of them are very different from those of the Solar System and one of the striking case is that of the super-Earths, rocky planets with masses ranging between 1 and 10 M⊕ with dimensions up to twice those of Earth. In the right environment, these planets could be the cradle of alien life that could modify the chemical composition of their atmospheres. So, the search for life signatures requires as the first step the knowledge of planet atmospheres, the main objective of future exoplanetary space explorations. Indeed, the quest for the determination of the chemical composition of those planetary atmospheres rises also more general interest than that given by the mere directory of the atmospheric compounds. It opens out to the more general speculation on what such detection might tell us about the presence of life on those planets. As, for now, we have only one example of life in the universe, we are bound to study terrestrial organisms to assess possibilities of life on other planets and guide our search for possible extinct or extant life on other planetary bodies. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
A Handbook of Double Stars, with a Catalogue of Twelve Hundred
The original of this bool< is in the Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924064295326 3 1924 064 295 326 Production Note Cornell University Library pro- duced this volume to replace the irreparably deteriorated original. It was scanned using Xerox soft- ware and equipment at 600 dots per inch resolution and com- pressed prior to storage using CCITT Group 4 compression. The digital data were used to create Cornell's replacement volume on paper that meets the ANSI Stand- ard Z39. 48-1984. The production of this volume was supported in part by the Commission on Pres- ervation and Access and the Xerox Corporation. Digital file copy- right by Cornell University Library 1991. HANDBOOK DOUBLE STARS. <-v6f'. — A HANDBOOK OF DOUBLE STARS, WITH A CATALOGUE OF TWELVE HUNDRED DOUBLE STARS AND EXTENSIVE LISTS OF MEASURES. With additional Notes bringing the Measures up to 1879, FOR THE USE OF AMATEURS. EDWD. CROSSLEY, F.R.A.S.; JOSEPH GLEDHILL, F.R.A.S., AND^^iMES Mt^'^I^SON, M.A., F.R.A.S. "The subject has already proved so extensive, and still ptomises so rich a harvest to those who are inclined to be diligent in the pursuit, that I cannot help inviting every lover of astronomy to join with me in observations that must inevitably lead to new discoveries." Sir Wm. Herschel. *' Stellae fixac, quae in ccelo conspiciuntur, sunt aut soles simplices, qualis sol noster, aut systemata ex binis vel interdum pluribus solibus peculiari nexu physico inter se junccis composita.