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Stsci Newsletter: 1997 Volume 014 Issue 01
January 1997 • Volume 14, Number 1 SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • AURA science and functional awards to Leitherer and Hanisch — pages 1 and 23 • Cycle 7 to be extended — page 5 • Cycle 7 approved Newsletter program listing — pages 7-13 Astronomy with HST Climbing the Starburst Distance Ladder C. Leitherer Massive stars are an important and powerful star formation events in sometimes dominant energy source for galaxies. Even the most luminous star- a galaxy. Their high luminosity, both in forming regions in our Galaxy are tiny light and mechanical energy, makes on a cosmic scale. They are not them detectable up to cosmological dominated by the properties of an distances. Stars ~100 times more entire population but by individual massive than the Sun are one million stars. Therefore stochastic effects times more luminous. Except for stars prevail. Extinction represents a severe of transient brightness, like novae and problem when a reliable census of the supernovae, hot, massive stars are Galactic high-mass star-formation the most luminous stellar objects in history is atempted, especially since the universe. massive stars belong to the extreme Massive stars are, however, Population I, with correspondingly extremely rare: The number of stars small vertical scale heights. Moreover, formed per unit mass interval is the proximity of Galactic regions — roughly proportional to the -2.35 although advantageous for detailed power of mass. We expect to find very studies of individual stars — makes it few massive stars compared to, say, difficult to obtain integrated properties, solar-type stars. This is consistent with such as total emission-line fluxes of observations in our solar neighbor- the ionized gas. -
On the Weak-Wind Problem in Massive Stars: X-Ray Spectra Reveal a Massive Hot Wind in Mu Columbae
East Tennessee State University From the SelectedWorks of Richard Ignace September 10, 2012 On the Weak-Wind Problem in Massive Stars: X- Ray Spectra Reveal a Massive Hot Wind in mu Columbae. David P. Huenemoerder, Massachusetts nI stitute of Technology Lidia M. Oskinova, University of Potsdam Richard Ignace, East Tennessee State University Wayne L. Waldron, Eureka Scientific nI c. Helge Todt, University of Potsdam, et al. Available at: https://works.bepress.com/richard_ignace/61/ The Astrophysical Journal Letters, 756:L34 (5pp), 2012 September 10 doi:10.1088/2041-8205/756/2/L34 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ON THE WEAK-WIND PROBLEM IN MASSIVE STARS: X-RAY SPECTRA REVEAL A MASSIVE HOT WIND IN μ COLUMBAE David P. Huenemoerder1, Lidia M. Oskinova2, Richard Ignace3, Wayne L. Waldron4, Helge Todt2, Kenji Hamaguchi5,6, and Shunji Kitamoto7 1 Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, Cambridge, MA 02139, USA 2 Institute for Physics and Astronomy, University of Potsdam, D-14476 Potsdam, Germany 3 Department of Physics and Astronomy, East Tennessee State University, Johnson City, TN 37614, USA 4 Eureka Scientific Inc., 2452 Dellmer Street, Suite 100, Oakland, CA 94602, USA 5 CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA 6 Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 7 Department of Physics, Rikkyo University, Tokyo 171-8501, Japan Received 2012 June 16; accepted 2012 August 3; published 2012 August 22 ABSTRACT μ Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. -
Filter Performance Comparisons for Some Common Nebulae
Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3. -
Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen William T
Draft version September 6, 2019 Typeset using LATEX preprint2 style in AASTeX63 Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen William T. Reach,1 Le Ngoc Tram,1 Matthew Richter,2 Antoine Gusdorf,3 Curtis DeWitt,1 1Universities Space Research Association, MS 232-11, Moffett Field, CA 94035, USA 2University of California, Davis, CA USA 3Observatoire de Paris, Ecole´ normale sup´erieure, Sorbonne Universit´e,CNRS, LERMA, 75005 Paris, France ABSTRACT Supernovae from core-collapse of massive stars drive shocks into the molecular clouds from which the stars formed. Such shocks affect future star formation from the molecu- lar clouds, and the fast-moving, dense gas with compressed magnetic fields is associated with enhanced cosmic rays. This paper presents new theoretical modeling, using the Paris-Durham shock model, and new observations at high spectral resolution, using the Stratospheric Observatory for Infrared Astronomy (SOFIA), of the H2 S(5) pure rota- tional line from molecular shocks in the supernova remnant IC 443. We generate MHD models for non-steady-state shocks driven by the pressure of the IC 443 blast wave into gas of densities 103 to 105 cm−3. We present the first detailed derivation of the shape of the velocity profile for emission from H2 lines behind such shocks, taking into account the shock age, preshock density, and magnetic field. For preshock densities 103{105 −3 cm , the H2 emission arises from layers that extend 0.01{0.0003 pc behind the shock, respectively. The predicted shifts of line centers, and the line widths, of the H2 lines range from 20{2, and 30{4 km s−1, respectively. -
RATIOS and STAR FORMATION EFFICIENCIES in SUPERGIANT H Ii REGIONS
The Astrophysical Journal, 788:167 (7pp), 2014 June 20 doi:10.1088/0004-637X/788/2/167 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ENHANCEMENT OF CO(3–2)/CO(1–0) RATIOS AND STAR FORMATION EFFICIENCIES IN SUPERGIANT H ii REGIONS Rie E. Miura1,2, Kotaro Kohno3,4, Tomoka Tosaki5, Daniel Espada1,6,7, Akihiko Hirota8, Shinya Komugi1, Sachiko K. Okumura9, Nario Kuno7,8, Kazuyuki Muraoka10, Sachiko Onodera10, Kouichiro Nakanishi1,6,7, Tsuyoshi Sawada1,6, Hiroyuki Kaneko11, Tetsuhiro Minamidani8, Kosuke Fujii1,2, and Ryohei Kawabe1,6 1 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; [email protected] 2 Department of Astronomy, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 133-0033, Japan 3 Institute of Astronomy, School of Science, The University of Tokyo, Osawa, Mitaka, Tokyo 181-0015, Japan 4 Research Center for Early Universe, School of Science, The University of Tokyo, Hongo, Bunkyo, Tokyo 113-0033, Japan 5 Joetsu University of Education, Yamayashiki-machi, Joetsu, Niigata 943-8512, Japan 6 Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura 763-0355, Santiago, Chile 7 Department of Astronomical Science, The Graduate University for Advanced Studies (Sokendai), 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan 8 Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1805, Japan 9 Department of Mathematical and Physical Sciences, Faculty of Science, Japan Woman’s University, Mejirodai 2-8-1, Bunkyo, Tokyo 112-8681, Japan 10 Osaka Prefecture University, -
How to Make $1000 with Your Telescope! – 4 Stargazers' Diary
Fort Worth Astronomical Society (Est. 1949) February 2010 : Astronomical League Member Club Calendar – 2 Opportunities & The Sky this Month – 3 How to Make $1000 with your Telescope! – 4 Astronaut Sally Ride to speak at UTA – 4 Aurgia the Charioteer – 5 Stargazers’ Diary – 6 Bode’s Galaxy by Steve Tuttle 1 February 2010 Sunday Monday Tuesday Wednesday Thursday Friday Saturday 1 2 3 4 5 6 Algol at Minima Last Qtr Moon Æ 5:48 am 11:07 pm Top ten binocular deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2244, NGC 2264, NGC 2301, NGC 2360 Top ten deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2261, NGC 2362, NGC 2392, NGC 2403 7 8 9 10 11 12 13 Algol at Minima Morning sports a Moon at Apogee New Moon Æ super thin crescent (252,612 miles) 8:51 am 7:56 pm Moon 8:00 pm 3RF Star Party Make use of the New Moon Weekend for . better viewing at the Dark Sky Site See Notes Below New Moon New Moon Weekend Weekend 14 15 16 17 18 19 20 Presidents Day 3RF Star Party Valentine’s Day FWAS Traveler’s Guide Meeting to the Planets UTA’s Maverick Clyde Tombaugh Ranger 8 returns Normal Room premiers on Speakers Series discovered Pluto photographs and NatGeo 7pm Sally Ride “Fat Tuesday” Ash Wednesday 80 years ago. impacts Moon. 21 22 23 24 25 26 27 Algol at Minima First Qtr Moon Moon at Perigee Å (222,345 miles) 6:42 pm 12:52 am 4 pm {Low in the NW) Algol at Minima Æ 9:43 pm Challenge binary star for month: 15 Lyncis (Lynx) Challenge deep-sky object for month: IC 443 (Gemini) Notable carbon star for month: BL Orionis (Orion) 28 Notes: Full Moon Look for a very thin waning crescent moon perched just above and slightly right of tiny Mercury on the morning of 10:38 pm Feb. -
A 2D Multiwavelength Study of the Ionized Gas and Stellar Population in the Giant HII Region NGC
Mon. Not. R. Astron. Soc. 000, 1–?? (2010) Printed 28 November 2018 (MN LATEX style file v2.2) A 2D multiwavelength study of the ionized gas and stellar population in the Giant HII Region NGC 588 A. Monreal-Ibero1,2⋆†, M. Relano˜ 3, C. Kehrig2, E. Perez-Montero´ 1, J. M. V´ılchez1, A. Kelz2, M. M. Roth2, O. Streicher2 1Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Glorieta de la Astronom´ıa, s/n, 18008 Granada, Spain 2Astrophysikalisches Institut Potsdam, innoFSPEC Potsdam, An der Sternwarte 16, D-14482, Potsdam, Germany 3Dpto. de F´ısica Te´orica y del Cosmos, Universidad de Granada, Campus Fuentenueva, Granada, Spain revised version ABSTRACT Giant H II regions (GHIIRs) in nearby galaxies are a local sample in which we can study in detail processes in the interaction of gas, dust, and newly formed stars which are analagous to those which occurred in episodes of higher intensity in which much of the current stel- lar population was born. Here, we present an analysis of NGC 588, a GHIIR in M33, based on optical Integral Field Spectroscopy (IFS) data obtained with the PMAS instru- ment at the 3.5 m telescope of Calar Alto Observatory, CAHA, together with Spitzer in- frared images at 8 µm and 24 µm. The extinction distribution measured in the optical shows complex structure, with three maxima which correlate in position with those of the emis- sion at 24 µm and 8 µm. Furthermore, the Hα luminosity absorbed by the dust within the H II region reproduces the structure observed in the 24 µm image, supporting the use of the 24 µm band as a valid tracer of recent star formation. -
A Multispectral Analysis of the Northeastern Shell of IC 443
MNRAS 000,1–13 (2019) Preprint 13 August 2019 Compiled using MNRAS LATEX style file v3.0 A multispectral analysis of the northeastern shell of IC 443 Alexandre Alarie,1;2;3 Laurent Drissen,2;3 1 Instituto de Astronomía, Universidad National Autónoma de México, Apdo. Postal 70264, 04510 Mexico D.F., Mexico 2 Département de physique, de génie physique et d’optique, Université Laval, Québec, QC, G1V 0A6, Canada 3 Centre de Recherche en Astrophysique du Québec 13 August 2019 ABSTRACT We have carried out optical observations of the north-eastern part of the supernova remnant IC 443 using the CFHT imaging spectrograph SITELLE. The observations consist of three multispectral cubes covering an 110 ×110 area allowing the investigation of both the spatial and spectral variation of 9 emission lines : [O II] ll3726+3729, [O III] ll4959,5007, Hb, Ha, [N II] ll6548,6583 and [S II] ll6716,6731. Extinction measurement from the Ha/Hb shows significant variation across the observed region with E(B-V) = 0.8-1.1. Electron density measurements using [S II] lines indicate densities ranging from 100 up to 2500 cm−3. Models computed with the shock modelling code MAPPINGS are presented and compared with the observations. A combination of complete shock model and truncated ones are required in order to explain the observed spectrum. The shock velocities found in IC 443 are between 20 and 150 km s−1 with 75 km s−1 being the most prominent velocity. The pre-shock number density varies from 20 to 60 cm−3. A single set of abundances close to solar values combined with varying shock parameters (shock velocity, pre-shock density and shock age) are sufficient to explain the great variation of lines intensities observed in IC 443. -
From Luminous Hot Stars to Starburst Galaxies
9780521791342pre CUP/CONT July 9, 2008 11:48 Page-i FROM LUMINOUS HOT STARS TO STARBURST GALAXIES Luminous hot stars represent the extreme upper mass end of normal stellar evolution. Before exploding as supernovae, they live out their lives of only a few million years with prodigious outputs of radiation and stellar winds which dramatically affect both their evolution and environments. A detailed introduction to the topic, this book connects the astrophysics of mas- sive stars with the extremes of galaxy evolution represented by starburst phenomena. A thorough discussion of the physical and wind parameters of massive stars is pre- sented, together with considerations of their birth, evolution, and death. Hll galaxies, their connection to starburst galaxies, and the contribution of starburst phenomena to galaxy evolution through superwinds, are explored. The book concludes with the wider cosmological implications, including Population III stars, Lyman break galaxies, and gamma-ray bursts, for each of which massive stars are believed to play a crucial role. This book is ideal for graduate students and researchers in astrophysics who are interested in massive stars and their role in the evolution of galaxies. Peter S. Conti is an Emeritus Professor at the Joint Institute for Laboratory Astro- physics (JILA) and theAstrophysics and Planetary Sciences Department at the University of Colorado. Paul A. Crowther is a Professor of Astrophysics in the Department of Physics and Astronomy at the University of Sheffield. Claus Leitherer is an Astronomer with the Space Telescope Science Institute, Baltimore. 9780521791342pre CUP/CONT July 9, 2008 11:48 Page-ii Cambridge Astrophysics Series Series editors: Andrew King, Douglas Lin, Stephen Maran, Jim Pringle and Martin Ward Titles available in the series 10. -
Narrowband CCD Photometry of Giant HII Regions
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 November 2018 (MN LATEX style file v2.2) Narrowband CCD Photometry of Giant HII Regions Guillermo Bosch 1 ⋆, Elena Terlevich 2 †, Roberto Terlevich 1 ‡ 1 Institute of Astronomy, Madingley Road, Cambridge CB3 0HA 2 INAOE, Puebla, M´exico 1 November 2018 ABSTRACT We have obtained accurate CCD narrow band Hβ and Hα photometry of Giant HII Regions in M 33, NGC 6822 and M 101. Comparison with previous determinations of emission line fluxes show large discrepancies; their probable origins are discussed. Combining our new photometric data with global velocity dispersion (σ) derived from emission line widths we have reviewed the L(Hβ)) − σ relation. A reanalysis of the properties of the GEHRs included in our sample shows that age spread and the su- perposition of components in multiple regions introduce a considerable spread in the regression. Combining the information available in the literature regarding ages of the associated clusters, evolutionary footprints on the interstellar medium, and kinemati- cal properties of the knots that build up the multiple GEHRs, we have found that a subsample - which we refer to as young and single GEHRs - do follow a tight relation in the L − σ plane. Key words: galaxies: individual: NGC6822, M33, M101 – H ii regions – galaxies: star clusters 1 INTRODUCTION tional explanation for this observed kinematical behaviour. Other authors confirmed the existence of a correlation, al- Accurate photometry of Giant HII Regions (GEHRs) is a though they found different slopes for the linear regression. key source of information about the energetics of these large New models were produced to account for the underlying dy- star-forming regions. -
La Porte Des Étoiles Le Journal Des Astronomes Amateurs Du Nord De La France
la porte des étoiles le journal des astronomes amateurs du nord de la France Numéro 39 - hiver 2018 39 À la une Les environs de la grande nébuleuse d’Orion Auteur : F. Lefebvre et D. Fayolle Date : 16/10/2017 Lieu : Saint-Véran (05) GROUPEMENT D’ASTRONOMES Matériel : APN Canon 1000D et AMATEURS COURRIEROIS astrographe Boren-Simon 8'' F2.8 Adresse postale GAAC - Simon Lericque Édito 12 lotissement des Flandres 62128 WANCOURT On avait déjà raconté beaucoup de choses sur Saint-Véran et son Internet observatoire... On pensait même avoir tout dit... On ne voulait pas Site : http://www.astrogaac.fr se répéter... Et pourtant, la mission Astroqueyras 2017 du GAAC Facebook : https://www.facebook.com/GAAC62 a encore repoussé les limites... Imaginez, une fine équipe de 20 E-mail : [email protected] astronomes amateurs venus de l’ensemble des Hauts-de-France (et même au-delà) envahissant pour une semaine le plus bel Les auteurs de ce numéro observatoire astronomique ouvert aux amateurs ; parmi eux, des Philippe Nonckelynck - membre du GAAC contemplateurs, des dessinateurs, des photographes. Les résultats, E-mail : [email protected] fort nombreux, de cette mission historique nous ont poussé à nouveau à prendre la plume pour causer de ce coin de paradis, Simon Lericque - membre du GAAC E-mail : [email protected] de son ciel, de son observatoire et de ses instruments, et surtout de l’ambiance extraordinaire d’une semaine à 3000 mètres sous Yann Picco - membre du GAAC les étoiles... La belle histoire entre le GAAC et Saint-Véran se E-mail : [email protected] poursuit donc avec cet épais numéro de la porte des étoiles.. -
TRANSIT the Newsletter Of
TRANSIT The Newsletter of 05 January 2009 Hubble caught Saturn with the edge-on rings in 1996. Image courtesy Eric Karkoschka (UoA) Front Page Image - Saturn, like the Earth, is tilted on its axis compared to the plane of its orbit, being off vertical by 26.7 degrees. Saturn’s rings are aligned with its equator so that means that roughly twice every orbit of Saturn we on Earth see the rings edge on. We pass through the ring plane in September 2009 but at that time Saturn is on the other side of the Sun, so now is the best time to view Saturn in Leo with the almost disappeared rings when they are inclined at 0.8 degrees to our line of sight. The next ring plane crossing is March 2025 Last meeting : 12 December 2008. “The Large Hadron Collider” by Dr Peter Edwards of Durham University. Dr Edwards proved he was a skilled public communicator when he initially launched into a short history of particle physics – we all understood what he was talking about! After then explaining what the LHC was actually looking for and how their massive detectors work he explained the problems caused by the unfortunate accident when firing up the LHC for the first time. The prognosis for future collisions seems to have a varying date but perhaps the 2010 date is the most likely. We wish Dr Edwards and his LHC colleagues the best of luck in achieving an early target date. Next meeting : 09 January 2009 – Members night. The meeting will start with the Society 2009 AGM and follow on with short talks presented by members of the Society.