The Hubble Tarantula Treasury Project
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Gas and Dust in the Magellanic Clouds
Gas and dust in the Magellanic clouds A Thesis Submitted for the Award of the Degree of Doctor of Philosophy in Physics To Mangalore University by Ananta Charan Pradhan Under the Supervision of Prof. Jayant Murthy Indian Institute of Astrophysics Bangalore - 560 034 India April 2011 Declaration of Authorship I hereby declare that the matter contained in this thesis is the result of the inves- tigations carried out by me at Indian Institute of Astrophysics, Bangalore, under the supervision of Professor Jayant Murthy. This work has not been submitted for the award of any degree, diploma, associateship, fellowship, etc. of any university or institute. Signed: Date: ii Certificate This is to certify that the thesis entitled ‘Gas and Dust in the Magellanic clouds’ submitted to the Mangalore University by Mr. Ananta Charan Pradhan for the award of the degree of Doctor of Philosophy in the faculty of Science, is based on the results of the investigations carried out by him under my supervi- sion and guidance, at Indian Institute of Astrophysics. This thesis has not been submitted for the award of any degree, diploma, associateship, fellowship, etc. of any university or institute. Signed: Date: iii Dedicated to my parents ========================================= Sri. Pandab Pradhan and Smt. Kanak Pradhan ========================================= Acknowledgements It has been a pleasure to work under Prof. Jayant Murthy. I am grateful to him for giving me full freedom in research and for his guidance and attention throughout my doctoral work inspite of his hectic schedules. I am indebted to him for his patience in countless reviews and for his contribution of time and energy as my guide in this project. -
Carbon Stars T. Lloyd Evans
J. Astrophys. Astr. (2010) 31, 177–211 Carbon Stars T. Lloyd Evans SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK. e-mail: [email protected] Received 2010 July 19; accepted 2010 October 18 Abstract. In this paper, the present state of knowledge of the carbon stars is discussed. Particular attention is given to issues of classification, evolution, variability, populations in our own and other galaxies, and circumstellar material. Key words. Stars: carbon—stars: evolution—stars: circumstellar matter —galaxies: magellanic clouds. 1. Introduction Carbon stars have been reviewed on several previous occasions, most recently by Wallerstein & Knapp (1998). A conference devoted to this topic was held in 1996 (Wing 2000) and two meetings on AGB stars (Le Bertre et al. 1999; Kerschbaum et al. 2007) also contain much on carbon stars. This review emphasizes develop- ments since 1997, while paying particular attention to connections with earlier work and to some of the important sources of concepts. Recent and ongoing develop- ments include surveys for carbon stars in more of the galaxies of the local group and detailed spectroscopy and infrared photometry for many of them, as well as general surveys such as 2MASS, AKARI and the Sirius near infrared survey of the Magel- lanic Clouds and several dwarf galaxies, the Spitzer-SAGE mid-infrared survey of the Magellanic Clouds and the current Herschel infrared satellite project. Detailed studies of relatively bright galactic examples continue to be made by high-resolution spectroscopy, concentrating on abundance determinations using the red spectral region, and infrared and radio observations which give information on the history of mass loss. -
A FUSE Survey of Interstellar O VI Absorption in the Small Magellanic
Accepted for publication in the Astrophysical Journal A FUSE Survey of Interstellar O VI Absorption in the Small Magellanic Cloud Charles G. Hoopes1, Kenneth R. Sembach1,2, J. Christopher Howk1, Blair D. Savage3, and Alex W. Fullerton1,4 ABSTRACT We present the results of a Far Ultraviolet Spectroscopic Explorer (FUSE) survey of O VI 1031.93 A˚ and 1037.62 A˚ absorption toward 18 OB stars in the Small Magellanic Cloud (SMC). The FUSE data are of very high quality, allowing a detailed study of the coronal temperature gas in the SMC. We find that O VI is ubiquitous in the SMC, with a detection along every sight line. The average value of the O VI column density in the SMC is log < N(O VI)>= 14.53. This value is 1.7 times higher than the average value for the Milky Way halo (perpendicular to the Galactic plane) of log N⊥(O VI)=14.29 found by FUSE, even though the SMC has much lower metallicity than the Galaxy. The column density in the SMC is higher along sight lines that lie close to star-forming regions, in particular NGC 346 in the northern part of the SMC, and to a lesser degree the southwestern complex of H II regions. This correlation with star formation suggests that local processes have an important effect on the distribution of coronal gas in the SMC. If the sight lines within NGC 346 are excluded, the mean column density for the SMC is log N(O VI)= 14.45, only 1.4 times higher than the Milky Way average. -
The Tarantula – Revealed by X-Rays (T-Rex) a Definitive Chandra
TheTarantula{ Revealed byX-rays (T-ReX) A Definitive Chandra Investigation of 30 Doradus Our first impressions of spiral and irregular galaxies are defined by massive star-forming regions (MSFRs), signposts marking spiral arms, bars, and starbursts. They remind us that galaxies really are evolving, churned by the continuous injection of energy and processed material. MSFRs offer us a microcosm of starburst astrophysics, where winds from O and Wolf-Rayet (WR) stars combine with supernovae to carve up the neutral medium from which they formed, both triggering and suppressing new generations of stars. With X-ray observations we see the stars themselves|the engines that shape the larger view of a galaxy|along with the hot, shocked ISM created by massive star feedback, which in turn fills the superbubbles that define starburst clusters (Fig. 1). We propose the 2 Ms Chandra/ACIS-I X-ray Visionary Project T-ReX, an intensive study of 30 Doradus (The Tarantula Nebula) in the LMC, the most powerful MSFR in the Local Group. To date Chandra has invested just 114 ks in this iconic target|proportionally far less than other premier observatories (e.g. HST, VLT, Spitzer, VISTA)|revealing only the most massive stars and large-scale diffuse structures. This very deep observation is essential to engage the great power of Chandra's unparalleled spatial resolution, a unique resource that will remain unmatched for another decade. T-ReX will reveal the X-ray properties of hundreds of 30 Dor's low-metallicity massive stars [1], thousands of lower-mass pre-main sequence (pre-MS) stars that record its star formation history [2], and parsec-scale shocks from winds and supernovae that are shredding its ISM [3,4]. -
The VLT-FLAMES Tarantula Survey
Astronomy & Astrophysics manuscript no. msOrevfinalcorr c ESO 2019 May 8, 2019 The VLT-FLAMES Tarantula Survey XIV. The O-Type Stellar Content of 30 Doradus N. R. Walborn1, H. Sana1,2, S. Sim´on-D´ıaz3,4, J. Ma´ız Apell´aniz5, W. D. Taylor6,7, C. J. Evans7, N. Markova8, D. J. Lennon9, and A. de Koter2,10 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands 3 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 4 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 5 Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18008 Granada, Spain 6 Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 7 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 8 Institute of Astronomy, National Astronomical Observatory, Bulgarian Academy of Sciences, PO Box 136, 4700 Smoljan, Bulgaria 9 European Space Agency, European Space Astronomy Centre, Camino Bajo del Castillo s/n, Urbanizaci´on Villafranca del Castillo, E-28691 Villanueva de la Ca˜nada, Madrid, Spain 10 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium ABSTRACT Detailed spectral classifications are presented for 352 O–B0 stars in the VLT-FLAMES Tarantula Survey ESO Large Programme, of which 213 O-type are judged of sufficiently high quality for further morphological analysis. -
Mapping the Youngest and Most Massive Stars in the Tarantula Nebula with MUSE-NFM
Astronomical Science DOI: 10.18727/0722-6691/5223 Mapping the Youngest and Most Massive Stars in the Tarantula Nebula with MUSE-NFM Norberto Castro 1 Myrs, but in very dramatic ways. The are to unveil the nature of the most mas- Martin M. Roth 1 energy released during their short lives, sive stars, to constrain the role of these Peter M. Weilbacher 1 and their deaths in supernova explosions, parameters in their evolution, and to pro- Genoveva Micheva 1 shape the chemistry and dynamics of vide homogeneous results and landmarks Ana Monreal-Ibero 2, 3 their host galaxies. Ever since the reioni- for the theory. Spectroscopic surveys Andreas Kelz1 sation of the Universe, massive stars have transformed the field in this direc- Sebastian Kamann4 have been significant sources of ionisa- tion, yielding large samples for detailed Michael V. Maseda 5 tion. Nonetheless, the evolution of mas- quantitative studies in the Milky Way (for Martin Wendt 6 sive O- and B-type stars is far from being example, Simón-Díaz et al., 2017) and in and the MUSE collaboration well understood, a lack of knowledge that the nearby Magellanic Clouds (for exam- is even worse for the most massive stars ple, Evans et al., 2011). However, massive (Langer, 2012). These missing pieces in stars are rarer than smaller stars, and 1 Leibniz-Institut für Astrophysik Potsdam, our understanding of the formation and very massive stars (> 70 M☉) are even Germany evolution of massive stars propagate to rarer. The empirical distribution of stars 2 Instituto de Astrofísica de Canarias, other fields in astrophysics. -
The Tarantula Nebula As a Template for Extragalactic Star Forming Regions from VLT/MUSE and HST/STIS
This is a repository copy of The Tarantula Nebula as a template for extragalactic star forming regions from VLT/MUSE and HST/STIS. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/112327/ Version: Accepted Version Proceedings Paper: Crowther, P.A., Caballero-Nieves, S.M., Castro, N. et al. (1 more author) (2016) The Tarantula Nebula as a template for extragalactic star forming regions from VLT/MUSE and HST/STIS. In: Proceedings of the International Astronomical Union. IAUS 329: The Lives and Death-Throes of Massive Stars, 28 Nov - 02 Dec 2016, Auckland, New Zealand. Cambridge University Press , pp. 292-296. https://doi.org/10.1017/S1743921317002484 Reuse Unless indicated otherwise, fulltext items are protected by copyright with all rights reserved. The copyright exception in section 29 of the Copyright, Designs and Patents Act 1988 allows the making of a single copy solely for the purpose of non-commercial research or private study within the limits of fair dealing. The publisher or other rights-holder may allow further reproduction and re-use of this version - refer to the White Rose Research Online record for this item. Where records identify the publisher as the copyright holder, users can verify any specific terms of use on the publisher’s website. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ The lives and death-throes of massive stars Proceedings IAU Symposium No. -
STAR FORMATION (Ch. 19)
STAR FORMATION (Ch. 19) The basics: GRAVITY vs. PRESSURE (heat; but also rotation and magnetic fields can be important) Stages (you don’t have to memorize numbers of stages in textbook or here, just be able to describe the sequence of events) 1. Interstellar cloud—cold (T~10K), large (~1-10pc), massive 3 5 (~10 – 10 Msun), so gravity wins easily over gas pressure (atomic motions—see Fig. 19.2): cloud must break up, or “fragment.” Other inhibitors: rotation, magnetic fields (More Precisely 19-1, p. 503). 2. Collapsing cloud fragment—still cold, size~0.1-0.01pc. This may fragment further, so have multiple stages of fragmentation (see Fig. 19.3). 3. Fragmentation ceases—center of fragment dense enough to become opaque to its own radiation, so it heats up, slowing the collapse. (Previously it was transparent and so could stay cool because radiation escaped easily.) This property makes qualifies the object as a: 4. Protostar—now object has a “surface” because it is opaque; this surface is the photosphere (the layer where the photons can finally escape into space). So a protostar is defined by when the object becomes dense enough to have a photosphere. It appears in the H-R diagram in upper right (large! See Fig. 19.4) Protostar heats up by gravitational contraction and accretion of remaining material (from a disk). But the temperature in center is too low for nuclear reactions at this stage. 5. Continued slow contraction (getting fainter), heating. Protostar moves roughly on a vertical track in the H-R diagram (see Fig. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
Arxiv:1802.01597V1 [Astro-Ph.GA] 5 Feb 2018 Born 1991)
Astronomy & Astrophysics manuscript no. AA_2017_32084 c ESO 2018 February 7, 2018 Mapping the core of the Tarantula Nebula with VLT-MUSE? I. Spectral and nebular content around R136 N. Castro1, P. A. Crowther2, C. J. Evans3, J. Mackey4, N. Castro-Rodriguez5; 6; 7, J. S. Vink8, J. Melnick9 and F. Selman9 1 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA e-mail: [email protected] 2 Department of Physics & Astronomy, University of Sheffield, Hounsfield Road, Sheffield, S3 7RH, UK 3 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK 4 Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin, Ireland 5 GRANTECAN S. A., E-38712, Breña Baja, La Palma, Spain 6 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Spain 7 Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Spain 8 Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, Northern Ireland, UK 9 European Southern Observatory, Alonso de Cordova 3107, Santiago, Chile February 7, 2018 ABSTRACT We introduce VLT-MUSE observations of the central 20 × 20 (30 × 30 pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming region in the Local Group. Spectrophotometry and radial-velocity estimates of the nebular gas (superimposed on the stellar spectra) are provided for 2255 point sources extracted from the MUSE datacubes, and we present estimates of stellar radial velocities for 270 early-type stars (finding an average systemic velocity of 271 ± 41 km s−1). -
Curriculum Vitae of You-Hua Chu
Curriculum Vitae of You-Hua Chu Address and Telephone Number: Institute of Astronomy and Astrophysics, Academia Sinica 11F of Astronomy-Mathematics Building, AS/NTU No.1, Sec. 4, Roosevelt Rd, Taipei 10617 Taiwan, R.O.C. Tel: (886) 02 2366 5300 E-mail address: [email protected] Academic Degrees, Granting Institutions, and Dates Granted: B.S. Physics Dept., National Taiwan University 1975 Ph.D. Astronomy Dept., University of California at Berkeley 1981 Professional Employment History: 2014 Sep - present Director, Institute of Astronomy and Astrophysics, Academia Sinica 2014 Jul - present Distinguished Research Fellow, Institute of Astronomy and Astrophysics, Academia Sinica 2014 Jul - present Professor Emerita, University of Illinois at Urbana-Champaign 2005 Aug - 2011 Jul Chair of Astronomy Dept., University of Illinois at Urbana-Champaign 1997 Aug - 2014 Jun Professor, University of Illinois at Urbana-Champaign 1992 Aug - 1997 Jul Research Associate Professor, University of Illinois at Urbana-Champaign 1987 Jan - 1992 Aug Research Assistant Professor, University of Illinois at Urbana-Champaign 1985 Feb - 1986 Dec Graduate College Scholar, University of Illinois at Urbana-Champaign 1984 Sep - 1985 Jan Lindheimer Fellow, Northwestern University 1982 May - 1984 Jun Postdoctoral Research Associate, University of Wisconsin at Madison 1981 Oct - 1982 May Postdoctoral Research Associate, University of Illinois at Urbana-Champaign 1981 Jun - 1981 Aug Postdoctoral Research Associate, University of California at Berkeley Committees Served: -
The VLT-FLAMES Tarantula Survey? XXIX
A&A 618, A73 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833433 & c ESO 2018 Astrophysics The VLT-FLAMES Tarantula Survey? XXIX. Massive star formation in the local 30 Doradus starburst F. R. N. Schneider1, O. H. Ramírez-Agudelo2, F. Tramper3, J. M. Bestenlehner4,5, N. Castro6, H. Sana7, C. J. Evans2, C. Sabín-Sanjulián8, S. Simón-Díaz9,10, N. Langer11, L. Fossati12, G. Gräfener11, P. A. Crowther5, S. E. de Mink13, A. de Koter13,7, M. Gieles14, A. Herrero9,10, R. G. Izzard14,15, V. Kalari16, R. S. Klessen17, D. J. Lennon3, L. Mahy7, J. Maíz Apellániz18, N. Markova19, J. Th. van Loon20, J. S. Vink21, and N. R. Walborn22,?? 1 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK e-mail: [email protected] 2 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 3 European Space Astronomy Centre, Mission Operations Division, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 4 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 5 Department of Physics and Astronomy, Hicks Building, Hounsfield Road, University of Sheffield, Sheffield S3 7RH, UK 6 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA 7 Institute of Astrophysics, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 8 Departamento de Física y Astronomía, Universidad de La Serena, Avda. Juan Cisternas 1200, Norte, La Serena, Chile 9 Instituto de Astrofísica de Canarias, 38205 La Laguna,