A Chandra/ACIS Study of 30 Doradus II. X-Ray Point Sources in The
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Key Information • This Exam Contains 6 Parts, 79 Questions, and 180 Points Total
Reach for the Stars *** Practice Test 2020-2021 Season Answer Key Information • This exam contains 6 parts, 79 questions, and 180 points total. • You may take this test apart. Put your team number on each page. There is not a separate answer page, so write all answers on this exam. • You are permitted the resources specified on the 2021 rules. • Don't worry about significant figures, use 3 or more in your answers. However, be sure your answer is in the correct units. • For calculation questions, any answers within 10% (inclusive) of the answer on the key will be accepted. • Ties will be broken by section score in reverse order (i.e. Section F score is the first tiebreaker, Section A the last). • Written by RiverWalker88. Feel free to PM me if you have any questions, feedback, etc. • Good Luck! Reach for the stars! Reach for the Stars B Team #: Constants and Conversions CONSTANTS Stefan-Boltzmann Constant = σ = 5:67 × 10−8 W=m2K4 Speed of light = c = 3 × 108m/s 30 Mass of the sun = M = 1:99 × 10 kg 5 Radius of the sun = R = 6:96 × 10 km Temperature of the sun = T = 5778K 26 Luminosity of the sun = L = 3:9 × 10 W Absolute Magnitude of the sun = MV = 4.83 UNIT CONVERSIONS 1 AU = 1:5 × 106km 1 ly = 9:46 × 1012km 1 pc = 3:09 × 1013km = 3.26 ly 1 year = 31557600 seconds USEFUL EQUATIONS 2900000 Wien's Law: λ = peak T • T = Temperature (K) • λpeak = Peak Wavelength in Blackbody Spectrum (nanometers) 1 Parallax: d = p • d = Distance (pc) • p = Parallax Angle (arcseconds) Page 2 of 13Page 13 Reach for the Stars B Team #: Part A: Astrophotographical References 9 questions, 18 points total For each of the following, identify the star or deep space object pictured in the image. -
The Exotic Eclipsing Nucleus of the Ring Planetary Nebula Suwt2
The Exotic Eclipsing Nucleus of the Ring Planetary Nebula SuWt 21 K. Exter,2 Howard E. Bond,3,4 K. G. Stassun5,6 B. Smalley,7 P. F. L. Maxted,7 and D. L. Pollacco8 Received ; accepted 1Based in part on observations obtained with the SMARTS Consortium 1.3- and 1.5- m telescopes located at Cerro Tololo Inter-American Observatory, Chile, and with ESO Telescopes at the La Silla Observatory 2Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA. Current address: Institute voor Sterrenkunde, Katholieke Universiteit Leuven, Leuven, Bel- gium; [email protected] 3Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA; [email protected] 4Visiting astronomer, Cerro Tololo Inter-American Observatory, National Optical As- tronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. Guest Observer with the arXiv:1009.1919v1 [astro-ph.SR] 10 Sep 2010 International Ultraviolet Explorer, operated by the Goddard Space Flight Center, National Aeronautics and Space Administration. 5Dept. of Physics and Astronomy, Vanderbilt University, Nashville, TN 32735, USA 6Department of Physics, Fisk University, 1000 17th Ave. N, Nashville, TN 37208, USA 7Astrophysics Group, Chemistry & Physics, Keele University, Staffordshire, ST5 5BG, UK 8Queen’s University Belfast, Belfast, UK –2– ABSTRACT SuWt 2 is a planetary nebula (PN) consisting of a bright ionized thin ring seen nearly edge-on, with much fainter bipolar lobes extending perpendicularly to the ring. It has a bright (12th-mag) central star, too cool to ionize the PN, which we discovered in the early 1990’s to be an eclipsing binary. -
The Low-Mass Populations in OB Associations
The Low-mass Populations in OB Associations Cesar´ Briceno˜ Centro de Investigaciones de Astronom´ıa Thomas Preibisch Max-Planck-Institut fur¨ Radioastronomie William H. Sherry National Optical Astronomy Observatory Eric E. Mamajek Harvard-Smithsonian Center for Astrophysics Robert D. Mathieu University of Wisconsin - Madison Frederick M. Walter Stony Brook University Hans Zinnecker Astrophysikalisches Institut Potsdam Low-mass stars (0:1 . M . 1 M ) in OB associations are key to addressing some of the most fundamental problems in star formation. The low-mass stellar populations of OB associa- tions provide a snapshot of the fossil star-formation record of giant molecular cloud complexes. Large scale surveys have identified hundreds of members of nearby OB associations, and revealed that low-mass stars exist wherever high-mass stars have recently formed. The spatial distribution of low-mass members of OB associations demonstrate the existence of significant substructure (”subgroups”). This ”discretized” sequence of stellar groups is consistent with an origin in short-lived parent molecular clouds within a Giant Molecular Cloud Complex. The low-mass population in each subgroup within an OB association exhibits little evidence for significant age spreads on time scales of ∼ 10 Myr or greater, in agreement with a scenario of rapid star formation and cloud dissipation. The Initial Mass Function (IMF) of the stellar populations in OB associations in the mass range 0:1 . M . 1 M is largely consistent with the field IMF, and most low-mass pre-main sequence stars in the solar vicinity are in OB associations. These findings agree with early suggestions that the majority of stars in the Galaxy were born in OB associations. -
R136: the Core of the Lonizing Cluster of 30 Doradus J
R136: The Core of the lonizing Cluster of 30 Doradus J. Me/nick, ESO Introduction crucial role in the whole story, I will give abrief description of this remarkable object. I first read that R136 contained a supermassive object some time ago in the Sunday edition of the Chilean daily newspaper The 30 Doradus Nebula and R136 EI Mercurio, where it was announced that ... "European astronomers discover the most massive star in the Universe!". The 30 Doradus nebula (thus named because it lies in the Since EI Mercurio is almost always wrang I did not take the Constellation of Doradus) is an outstanding complex of gas, announcement very seriously until the paper by Feitzinger and dust and stars in the Large Magellanic Cloud (LMC), the Co-workers (henceforth the Bochum graup) appeared in nearest galaxy to our own. Beautiful colour photographs of the Astronomy and Astrophysics in 1980. More or less simultane LMC and the 30 Doradus region can be found in the December ously with the publication of these optical observations, a graup 1982 issue of The Messenger. The diameter of 30 Dor is of observers from the University of Wisconsin, headed by J. several hundred parsecs and, although emission nebulae as Cassinelli (henceforth the Wisconsin group) reached the same large or larger than 30 Dor exist in other galaxies, none is found Conclusion on the basis of ultraviolet observations obtained in our own. The visual light emitted by the nebula is produced with the International Ultraviolet Explorer (IUE). almost entirely by hydrogen recombination lines and in orderte . After these papers where published, and since I have been maintain this radiation the equivalent of about 10004stars (the Interested in R136 for a long time, I started to consider the hottest stars known have spectral type 03) are required. -
The R136 Star Cluster Dissected with Hubble Space Telescope/STIS
MNRAS 000, 1–39 (2015) Preprint 29 January 2016 Compiled using MNRAS LATEXstylefilev3.0 The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He ii λ1640 in young star clusters Paul A. Crowther1⋆, S.M. Caballero-Nieves1, K.A. Bostroem2,3,J.Ma´ız Apell´aniz4, F.R.N. Schneider5,6,N.R.Walborn2,C.R.Angus1,7,I.Brott8,A.Bonanos9, A. de Koter10,11,S.E.deMink10,C.J.Evans12,G.Gr¨afener13,A.Herrero14,15, I.D. Howarth16, N. Langer6,D.J.Lennon17,J.Puls18,H.Sana2,11,J.S.Vink13 1Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA 3Department of Physics, University of California, Davis, 1 Shields Ave, Davis CA 95616, USA 4Centro de Astrobiologi´a, CSIC/INTA, Campus ESAC, Apartado Postal 78, E-28 691 Villanueva de la Ca˜nada, Madrid, Spain 5 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK 6 Argelanger-Institut fur¨ Astronomie der Universit¨at Bonn, Auf dem Hugel¨ 71, D-53121 Bonn, Germany 7 Department of Physics, University of Warwick, Gibbet Hill Rd, Coventry CV4 7AL, UK 8 Institute for Astrophysics, Tuerkenschanzstr. 17, AT-1180 Vienna, Austria 9 Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & Vas. Pavlou St, P. Penteli 15236, Greece 10 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, Netherlands 11 Institute of Astronomy, KU Leuven, Celestijnenlaan -
R144 Revealed As a Double-Lined Spectroscopic Binary?
Mon. Not. R. Astron. Soc. 000, 1{6 (2002) Printed 4 October 2018 (MN LATEX style file v2.2) R144 revealed as a double-lined spectroscopic binary? H. Sana,1y T. van Boeckel,1 F. Tramper,1 L.E. Ellerbroek,1 A. de Koter,1;2;3 L. Kaper,1 A.F.J. Moffat,4 O. Schnurr,5 F.R.N. Schneider,6 D.R. Gies7 1 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH, Amsterdam, The Netherlands 2 Utrecht University, Princetonplein 5, 3584CC, Utrecht, The Netherlands 3 Instituut voor Sterrenkunde, Universiteit Leuven, Celestijnenlaan 200 D, 3001, Leuven, Belgium 4 D´epartment de Physique, Universit´ede Montr´ealand Centre de Recherche en Astrophysique du Qu´ebec, C. P. 6128, succ. centre-ville, Montr´eal(Qc) H3C 3J7, Canada 5 Leibniz Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 6 Argelander-Institut f¨urAstronomie, Universit¨atBonn, Auf dem H¨ugel71, 53121 Bonn, Germany 7 Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106, USA Accepted 1988 December 15. Received 1988 December 14; in original form 1988 October 11 ABSTRACT R144 is a WN6h star in the 30 Doradus region. It is suspected to be a binary because of its high luminosity and its strong X-ray flux, but no periodicity could be established so far. Here, we present new X-shooter multi-epoch spectroscopy of R144 obtained at the ESO Very Large Telescope (VLT). We detect variability in position and/or shape of all the spectral lines. -
Dissecting the Core of the Tarantula Nebula with MUSE
Astronomical Science DOI: 10.18727/0722-6691/5053 Dissecting the Core of the Tarantula Nebula with MUSE Paul A. Crowther1 firmed as Lyman continuum leakers (for ute mosaic which encompasses both Norberto Castro2 example, Micheva et al., 2017). the R136 star cluster and R140 (an aggre- Christopher J. Evans3 gate of WR stars to the north). See Fig- Jorick S. Vink4 The Tarantula Nebula is host to hundreds ure 1 for a colour-composite of the cen- Jorge Melnick5 of massive stars that power the strong tral 200 × 160 pc of the Tarantula Nebula Fernando Selman5 Hα nebular emission, comprising main obtained with the Advanced Camera sequence OB stars, evolved blue super- for Surveys (ACS) and the Wide Field giants, red supergiants, luminous blue Camera 3 (WFC3) aboard the HST. The 1 Department of Physics & Astronomy, variables and Wolf-Rayet (WR) stars. The resulting image resolution spanned 0.7 University of Sheffield, United Kingdom proximity of the LMC (50 kpc) permits to 1.1 arcseconds, corresponding to a 2 Department of Astronomy, University of individual massive stars to be observed spatial resolution of 0.22 ± 0.04 pc, pro- Michigan, Ann Arbor, USA under natural seeing conditions (Evans viding a satisfactory extraction of sources 3 UK Astronomy Technology Centre, et al., 2011). The exception is R136, the aside from R136. Four exposures of Royal Observatory, Edinburgh, United dense star cluster at the LMC’s core that 600 s each for each pointing provided a Kingdom necessitates the use of adaptive optics yellow continuum signal-to-noise (S/N) 4 Armagh Observatory, United Kingdom or the Hubble Space Telescope (HST; see ≥ 50 for 600 sources. -
THE MAGELLANIC CLOUDS NEWSLETTER an Electronic Publication Dedicated to the Magellanic Clouds, and Astrophysical Phenomena Therein
THE MAGELLANIC CLOUDS NEWSLETTER An electronic publication dedicated to the Magellanic Clouds, and astrophysical phenomena therein No. 159 — 2 June 2019 http://www.astro.keele.ac.uk/MCnews Editor: Jacco van Loon Figure 1: The Large Magellanic Cloud imaged in [O iii], Hα and [S ii] by the Ciel Austral team at the El Sauce au Chili observatory with a 16cm aperture telescope and a total integration time of over 1000 hours during 2017–2019. This picture was suggested by Sakib Rasool; for more details see http://www.cielaustral.com/galerie/photo95.htm. 1 Editorial Dear Colleagues, It is my pleasure to present you the 159th issue of the Magellanic Clouds Newsletter. I am sure you must have been mesmerized by the cover picture. It is not just stunning but also inspiring. You’re very welcome to e-mail pictures of the Magellanic Clouds or objects in the Magellanic Clouds, that show them in a different light from what we’ve been used to seeing. The Small Magellanic Cloud rises higher in the sky again (and the Antarctic nights are getting longer) so new obser- vations will start to be possible again. Of course radio observations, particle observations and observations from space have never ceased. At radio frequencies, the SKA pathfinders are becoming fully fledged, so watch this space for more great progress. The next issue is planned to be distributed on the 1st of August. Editorially Yours, Jacco van Loon 2 Refereed Journal Papers The resolved distributions of dust mass and temperature in Local Group galaxies Dyas Utomo1, I-Da Chiang2, Adam Leroy1, Karin Sandstrom2 and Jeremy Chastenet2 1Ohio State University, USA 2University of California, San Diego, USA We utilize archival far-infrared maps from the Herschel Space Observatory in four Local Group galaxies (Small and Large Magellanic Clouds, M31, and M33). -
The VLT-FLAMES Tarantula Survey ⋆⋆⋆⋆⋆⋆
UvA-DARE (Digital Academic Repository) The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus Doran, E.I.; Crowther, P.A.; de Koter, A.; Evans, C.J.; McEvoy, C.; Walborn, N.R.; Bastian, N.; Bestenlehner, J.M.; Gräfener, G.; Herrero, A.; Köhler, K.; Maíz Apellániz, J.; Najarro, F.; Puls, J.; Sana, H.; Schneider, F.R.N.; Taylor, W.D.; van Loon, J.Th.; Vink, J.S. DOI 10.1051/0004-6361/201321824 Publication date 2013 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Doran, E. I., Crowther, P. A., de Koter, A., Evans, C. J., McEvoy, C., Walborn, N. R., Bastian, N., Bestenlehner, J. M., Gräfener, G., Herrero, A., Köhler, K., Maíz Apellániz, J., Najarro, F., Puls, J., Sana, H., Schneider, F. R. N., Taylor, W. D., van Loon, J. T., & Vink, J. S. (2013). The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus. Astronomy & Astrophysics, 558, A134. https://doi.org/10.1051/0004- 6361/201321824 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. -
Refereed Publications Selma E De Mink Generated Automatically from NASA ADS Database on 8Th August 2019
Refereed publications Selma E de Mink Generated automatically from NASA ADS database on 8th August 2019. (Papers accepted for publication very recently or submitted that do not yet appear on ADS may be missing.) Publications Statistics Total number of citations 5719 Total number of papers 142 Total number of refereed papers 91 Numberofpaperswithmorethan100citations 14 Numberofpaperswithmorethan50citations 32 Numberofpaperswithmorethan10citations 79 Hirsch factor 37 Refereed Publications 2019 (6 refereed publications) (91) Abdul-Masih, Sana, Sundqvist, Mahy, Menon et al. and 8 further coauthors incl. De Mink (2019), “Clues on the Origin and Evolution of Massive Contact Binaries: Atmosphere Analysis of VFTS 352”, The Astrophysical Journal, Volume 880, Issue 2, article id. 115, 19 pp. (2019)., (90) Vigna-Gómez, Justham, Mandel, De Mink, Podsiadlowski (2019), “Massive Stellar Mergers as Pre- cursors of Hydrogen-rich Pulsational Pair Instability Supernovae”, The Astrophysical Journal Letters, Volume 876, Issue 2, article id. L29, 6 pp. (2019)., (6 citations) (89) Cook, Lee, Adamo, Kim, Chandar et al. and 60 further coauthors incl. De Mink (2019), “Star cluster catalogues for the LEGUS dwarf galaxies”, Monthly Notices of the Royal Astronomical Society, Volume 484, Issue 4, p.4897-4919, (3 citations) (88) Renzo, Zapartas, De Mink, Götberg, Justham et al. and 4 further coauthors (2019), “Massive run- away and walkaway stars. A study of the kinematical imprints of the physical processes governing the evolution and explosion of their binary progenitors”, Astronomy & Astrophysics, Volume 624, id.A66, 28 pp., (16 citations) (87) Kerzendorf, Do, De Mink, Götberg, Milisavljevic et al. and 5 further coauthors (2019), “No sur- viving non-compact stellar companion to Cassiopeia A”, Astronomy & Astrophysics, Volume 623, id.A34, 12 pp., (7 citations) (86) Renzo, De Mink, Lennon, Platais, van der Marel et al. -
The Tarantula Massive Binary Monitoring Project: II. a First SB2
Astronomy & Astrophysics manuscript no. paper c ESO 2016 October 26, 2016 The Tarantula Massive Binary Monitoring project: II. A first SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145 T. Shenar1, N. D. Richardson2, D. P. Sablowski3, R. Hainich1, H. Sana4, A. F. J. Moffat5, H. Todt1, W.-R. Hamann1, L. M. Oskinova1, A. Sander1, F. Tramper6, N. Langer7, A. Z. Bonanos8, S. E. de Mink9, G. Gräfener10, P. A. Crowther11, J. S. Vink10, L. A. Almeida12; 13, A. de Koter4; 9, R. Barbá14, A. Herrero15, and K. Ulaczyk16 1Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany e-mail: [email protected] 2Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA 3Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany 4Institute of Astrophysics, KU Leuven, Celestijnenlaan 200 D, 3001, Leuven, Belgium 5Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, Canada 6European Space Astronomy Centre (ESA/ESAC), PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 7Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany 8IAASARS, National Observatory of Athens, GR-15236 Penteli, Greece 9Anton Pannenkoek Astronomical Institute, University of Amsterdam, 1090 GE Amsterdam, Netherlands 10Armagh Observatory, College Hill, Armagh, BT61 9DG, Northern Ireland, UK 11Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH 12Instituto de Astronomia, Geofísica e Ciências, Rua do Matão 1226, Cidade Universitária São Paulo, SP, Brasil 13Dep. -
A Wind-Eclipsing Binary with a Total Mass 140 M
Open Research Online The Open University’s repository of research publications and other research outputs The Tarantula Massive Binary Monitoring. V. R144: a wind-eclipsing binary with a total mass 140 M Journal Item How to cite: Shenar, T.; Sana, H.; Marchant, P.; Pablo, B.; Richardson, N.; Moffat, A. F. J.; Van Reeth, T.; Barbá, R. H.; Bowman, D. M.; Broos, P.; Crowther, P. A.; Clark, J. S.; de Koter, A.; de Mink, S. E.; Dsilva, K.; Gräfener, G.; Howarth, I. D.; Langer, N.; Mahy, L.; Maíz Apellániz, J.; Pollock, A. M. T.; Schneider, F. R. N.; Townsley, L. and Vink, J. S. (2021). The Tarantula Massive Binary Monitoring. V. R144: a wind-eclipsing binary with a total mass 140 M. Astronomy & Astrophysics, 650, article no. A147. For guidance on citations see FAQs. c 2021 ESO Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1051/0004-6361/202140693 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk A&A 650, A147 (2021) Astronomy https://doi.org/10.1051/0004-6361/202140693 & © ESO 2021 Astrophysics The Tarantula Massive Binary Monitoring ? V. R 144: a wind-eclipsing binary with a total mass &140 M T. Shenar1, H. Sana1, P. Marchant1, B. Pablo2, N. Richardson3, A. F. J. Moffat4, T. Van Reeth1, R. H. Barbá5, D. M. Bowman1, P.