DOCSLIB.ORG

An Infrared Study of the Magellanic Clouds Schwering, P.B.W

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
An Infrared Study of the Magellanic Clouds Schwering, P.B.W An infrared study of the Magellanic clouds Schwering, P.B.W. Citation Schwering, P. B. W. (1988, October 19). An infrared study of the Magellanic clouds. Retrieved from https://hdl.handle.net/1887/12856 Version: Corrected Publisher’s Version Licence agreement concerning inclusion of License: doctoral thesis in the Institutional Repository of the University of Leiden Downloaded from: https://hdl.handle.net/1887/12856 Note: To cite this publication please use the final published version (if applicable). AN INFRARED STUDY OF THE MAGELLANIC CLOUDS Piet Schwering Promotiecommissie: Promotor: Prof. Dr. H.J. Habing Co-promotor: Dr. F.F. Israël Referent: Dr. J. Koornneef Overige leden: Prof. Dr. W.B. Burton Prof. Dr. A. Blaauw Prof. Dr. H. van de Laan Prof. Dr. G.K. Miley Prof. Ir. C. van Schooneveld Prof. Dr. W.J. Huiskamp The Infrared Astronomical Satellite (IRAS) was developed and operated by the Nether- lands Agency for Aerospace Programs (NIVR), the U.S. National Aeronautics and Space Administration (NASA) and the U.K. Science and Engineering Research Council (SERC). Gracias a la Vida Gracias a la vida que me ha dado tanto, me dió dos luceros que cuando los abro perfecto distingo lo negro del blanco, en el alto cielo su fonda estrellado, en las multitudes la mujer que yo amo. Gracias a la vida que me ha dada tanto, me dió el corazón que agita su morco cuando miro el fruto del cerebro humano, cuando miro el bueno tan lejos del malo, cuando miro el fonda de tus ojos claros. Violeta Parra Mijn dank aan het leven Mijn dank aan het leven dat me zo véél heeft gegeven, het heeft me twee ogen gegeven zodat ik, wanneer ik ze open perfekt het donkere van het lichte kan onderscheiden, in de hoge hemel de besterde verte, in de menigten de vrouw die ik liefheb. Mijn dank aan het leven dat me zo véél heeft gegeven, het heeft me mijn hart gegeven dat zo heftig klopt als ik de vrucht bekijk van het menselijk brein, als ik de goede mensen zo ver verwijderd zie van de slechte mensen, als ik de diepte zie van jouw heldere ogen. vertaald door Hannie van Loon Contents Chapter I Introduction 1. The earliest observations of the Magellanic Clouds 1 2. Modern observations 2 2.1. The Local Group of Galaxies 2 2.2. The Magellanic Clouds 2 2.3. Atomic, molecular and ionized gas 4 2.4. Abundances and star formation 5 3. Outline of this thesis 6 Chapter II Infrared Observations of the Small Magellanic Cloud Summary 11 1. Introduction 11 2. Observations and data reduction 13 3. The maps of infrared radiation 16 4. The Infrared Source List in the SMC 19 4.1. The Source List 19 4.2. Positions 29 4.3. Flux densities .' 30 5. Identification of Sources v 30 5.1. Stars in the DPM fields 30 5.1.1. Comparison with SAO stars 30 5.1.2. Comparison with Radcliffe SMC-stars 32 5.1.3. Comparison with Late Type Giants 34 5.1.4. Stars: Conclusion 34 5.2. Ha nebulosities in the SMC 34 5.3. Clusters in the SMC 38 5.4. Supernova- remnants in the SMC 39 5.5. Planetary nebulae in the SMC 40 5.6. Dark clouds in the SMC 41 6. Conclusions 41 Appendix A: Additions to the Infrared Source List 44 A.I. Introduction 44 A.2. Observations and data reduction 44 A.3. The maps of infrared radiation 45 A.4. Additions to the Infrared Source List in the SMC 46 A.5. Identification of sources 47 A.5.1. Stars in the fields 47 A.5.1.1. Comparison with SAO stars 47 A.5.1.2. Comparison with Radcliffe SMC-stars 47 A.5.2. Ha nebulosities in the SMC 47 A.5.3. Clusters in the SMC 48 A.5.4. Planetary nebulae in the SMC 48 A.6. Conclusions 48 Chapter jIII Infrared Observations of the Large Magellanic Cloud Summary 51 1. Introduction 51 2. Observations and data reduction 52 3. The maps of infrared radiation 54 4. The Infrared Source List in the LMC 60 5. Identification of Sources 82 5.1. Stars in the DPM fields 82 5.1.1. Comparison with foreground stars 82 5.1.2. Comparison with Radcliffe LMC-stars 82 5.1.3. Comparison with LMC Late Type Giants 89 5.1.4. Stars: Conclusion 97 5.2. Ha nebulosities in the LMC 97 5.3. Globular clusters in the LMC 98 5.4. Supernova remnants in the LMC 98 5.5. Planetary nebulae in the LMC 100 5.6. Dark clouds in the LMC 105 6. Conclusions 105 Appendix A: Additions to the Infrared Source List 107 A.I. Introduction 107 A.2. Observations and data reduction 107 A.3. The maps of infrared radiation 107 A.4. Additions to the Infrared Source List in the LMC 108 A.5. Identification of sources 109 A.5.1. Stars in the Co-added fields 109 A.5.2. Ha nebulosities in the LMC 109 A.5.3. Globular clusters in the LMC 109 A.5.4. Planetary nebulae in the LMC 109 A.6. Conclusions Ill Chapter IV Galactic infrared foreground emission in the direction of the Magellanic Clouds 1. Introduction 115 2. Data presentation and handling 116 2.1. Infrared data 116 2.2. Atomic hydrogen data 118 3. The stellar infrared foreground 120 4. The cirrus infrared foreground 121 4.1. Atomic and molecular hydrogen column densities 122 4.2. Infrared emission 122 4.3. Dust temperatures 124 4.4. Dust column densities 125 4.5. Gas-to-dust ratio 125 4.6. Predicted infrared foreground emission 133 5. The relation between Galactic infrared and atomic hydrogen 135 5.1. Comparison of Galactic infrared-atomic hydrogen relations ... 135 5.2. Variations in the relation between infrared intensity and atomic hydrogen column density 136 6. The Galactic foreground extinction 139 7. Implications of the extinction by foreground dust on Magellanic Clouds studies 141 8. Conclusions 142 Chapter V Overall infrared properties of the Magellanic Clouds 1. Introduction 145 2. Data presentation and data handling 145 3. Integrated infrared properties of the Magellanic Clouds 146 3.1. Flux densities and spectra 146 3.2. Infrared sizes 161 3.3. Luminosities and luminosity ratios 162 4. Large scale infrared structure of the Magellanic Clouds 167 4.1. Infrared morphology 167 4.2. Line-of-sight temperature distribution of the dust 170 4.3. Comparison of infrared radiation with Ha / HI supergiant shells 181 4.4. The density of the Interstellar radiation field 181 5. Comparison of infrared emission with data at other wavelengths . .. 183 5.1. Comparison of infrared with ultraviolet radiation from the LMC 183 5.2. Comparison of infrared radiation with Ha emission 188 5.3. Comparison of infrared with radio continuum radiation 188 6. Conclusions 190 m Chapter VI Properties of dust in the Magellanic Clouds 1. Introduction and data presentation 195 2. Nature of dust emitting at mid-infrared wavelengths 195 2.1. The Clouds' integrated mid-infrared excess emission 196 2.2. The contribution of star-like objects to the mid-infrared excess emission 199 2.2.1. Cool stellar photospheres 199 2.2.2. Dust shells surrounding main sequence stars 200 2.2.3. Late-type stars with thick dust shells (OH/IR stars and Miras) 200 2.2.4. Proto stellar objects or young stars still embedded in dust 201 2.3. The nature of the mid-infrared excess emission 203 2.3.1. Very small grains mixed with large grains in infrared cirrus 203 2.3.2. The distribution of the mid-infrared excess emission ... 204 2.3.3. Conclusion: mid-infrared emission in the Magellanic Clouds 211 3. Amount of emitting dust in the Magellanic Clouds 212 3.1. Dust mass estimated from global emission 212 3.2. Dust mass estimated from line-of-sight temperature distribution 214 3.3. Dust mass estimated from decomposition of line-of-sight temperatures 215 3.4. The cold dust mass 217 3.5. The total dust mass of the Magellanic Clouds 218 3.6. The distribution of warm and cool dust 218 4. Comparison of infrared radiation and dust with atomic hydrogen 223 4.1. Infrared and atomic hydrogen emission 223 4.2. Dust and atomic hydrogen column densities 231 5. Conclusions 232 Chapter VII Dust in the Magellanic Clouds 1. Introduction 235 2. Infrared characteristics of the Magellanic Clouds 235 2.1. Galactic foreground dust 235 2.2. Global infrared properties 236 2.3. The radiation fields in the Magellanic Clouds 239 2.4. Dust properties 239 2.5. The gas-to-dust ratio 240 3. The relation between global and local characteristics 246 4. The Magellanic Clouds compared to other galaxies 246 4.1. Local Group spiral galaxies 246 4.2. Irregular galaxies 250 Appendix On the interpretation of IRAS infrared observations 1. Introduction 253 2. Mechanisms and origin of infrared radiation 253 2.1. Mechanisms of infrared radiation 253 2.2. Origin and sources of infrared radiation 254 3. IRAS in-band intensities, specific intensities and colour corrections 254 4. Dust properties and radiative transfer theory 259 4.1. Dust properties 259 4.2. Radiative transfer 261 5. Dust temperature from infrared observations 265 6. Far-infrared luminosity ' 271 7. Optical depth, dust column density and dust masses 275 8. Multiple dust components contributing to the infrared emission 276 9. Summary 277 Summary 281 Resumen 284 Samenvatting 287 Curriculum vitae 291 Nawoord 293 The Antarctic Pole is not so starry as the Arctic.
Load more

Recommended publications
  • 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. 85 | 1 February 2007 http://www.astro.keele.ac.uk/MCnews Editors: Jacco van Loon and Sne·zana Stanimirovi¶c Editorial Dear Colleagues, It is our pleasure to present the 85th issue of the Magellanic Clouds Newsletter. Two very interesting contributions discuss the tidal e®ects on the Magellanic Clouds, creating the Magellanic Bridge (Harris) and causing tidal heating of the disk of the LMC (Olsen & Massey). Several other contributions shed new light on the late stages of stellar evolution from studies in the Magellanic Clouds There are two job announcements, one for a postdoctoral fellowship and another one for PhD studentships. And you might well be interested in the release of shape, a powerful tool for interpreting position-velocity datacubes. The next issue will be distributed on the 1st of April; the deadline for contributions is the 31st of March. Editorially Yours, Jacco van Loon and Sne·zana Stanimirovi¶c 1 Refereed Journal Papers Con¯rmation of New Planetary Nebulae in the Large Magellanic Cloud Richard A. Shaw1, Warren A. Reid2;3 and Quentin A. Parker2;3 1National Optical Astronomy Observatory 2Department of Physics, Macquarie University, Sydney, NSW 2109, Australia 3Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia We present Hubble Space Telescope (HST) images of new planetary nebulae (PNe) that were discovered in the Reid- Parker AAO/UKST H® survey of the Large Magellanic Cloud. These serendipitous observations from various HST programs yield independent con¯rmations of 6 PNe; one other detected nebula may also be a PN, and one appears to be a region of di®use emission.
    [Show full text]
  • POSTERS SESSION I: Atmospheres of Massive Stars
    Abstracts of Posters 25 POSTERS (Grouped by sessions in alphabetical order by first author) SESSION I: Atmospheres of Massive Stars I-1. Pulsational Seeding of Structure in a Line-Driven Stellar Wind Nurdan Anilmis & Stan Owocki, University of Delaware Massive stars often exhibit signatures of radial or non-radial pulsation, and in principal these can play a key role in seeding structure in their radiatively driven stellar wind. We have been carrying out time-dependent hydrodynamical simulations of such winds with time-variable surface brightness and lower boundary condi- tions that are intended to mimic the forms expected from stellar pulsation. We present sample results for a strong radial pulsation, using also an SEI (Sobolev with Exact Integration) line-transfer code to derive characteristic line-profile signatures of the resulting wind structure. Future work will compare these with observed signatures in a variety of specific stars known to be radial and non-radial pulsators. I-2. Wind and Photospheric Variability in Late-B Supergiants Matt Austin, University College London (UCL); Nevyana Markova, National Astronomical Observatory, Bulgaria; Raman Prinja, UCL There is currently a growing realisation that the time-variable properties of massive stars can have a funda- mental influence in the determination of key parameters. Specifically, the fact that the winds may be highly clumped and structured can lead to significant downward revision in the mass-loss rates of OB stars. While wind clumping is generally well studied in O-type stars, it is by contrast poorly understood in B stars. In this study we present the analysis of optical data of the B8 Iae star HD 199478.
    [Show full text]
  • THE AGB NEWSLETTER an Electronic Publication Dedicated to Asymptotic Giant Branch Stars and Related Phenomena
    THE AGB NEWSLETTER An electronic publication dedicated to Asymptotic Giant Branch stars and related phenomena No. 117 | 1 February 2007 http://www.astro.keele.ac.uk/AGBnews Editors: Jacco van Loon and Albert Zijlstra Editorial Dear Colleagues, It is our pleasure to present you the 117th issue of the AGB Newsletter. Of the 21 refereed journal publications, eight deal directly with Planetary Nebulae | which may have something to do with planets after all, and perhaps with dark energy as well (see the contribution by Gibson & Schild). Don't miss the many job advertisements, both for PhD studentships (Denver, Vienna, Portsmouth) and postdoctoral fellowships (Vienna, Keele). The Food for Thought statement published last month generated some reaction. One of you considered the relation between rotation rate and magnetic activity to be the principal question in relation to AGB stars that needs to be answered. Hence, we make it this month's Food for Thought statement. Reactions to this, or suggestions for other pertinent questions, are very welcome and will be discussed in future issues of the newsletter. The next issue will be distributed on the 1st of March; the deadline for contributions is the 28th of February. Editorially Yours, Jacco van Loon and Albert Zijlstra Food for Thought This month's thought-provoking statement is: The relation between rotation rate and magnetic activity is the principal question in relation to AGB stars that needs to be answered Reactions to this statement or suggestions for next month's statement can be e-mailed to [email protected] (please state whether you wish to remain anonymous) 1 Refereed Journal Papers Magnetic ¯elds in planetary nebulae and post-AGB nebulae.
    [Show full text]
  • The Red Supergiant Content of the Local Group
    The Lives and Death-throes of Massive Stars Proceedings IAU Symposium No. 329, 2017 c 2017 International Astronomical Union J.J.Eldridge,ed. DOI: 00.0000/X000000000000000X The Red Supergiant Content of the Local Group Philip Massey1, Emily Levesque2, Kathryn Neugent1, Kate Evans1,3, Maria Drout4, and Madeleine Beck5 1 Lowell Observatory, 1400 W Mars Hill Road, Flagstaff, AZ 86001 and Dept. Physics & Astronomy, Northern Arizona University, Flagstaff, AZ 86011-6010 email: [email protected], [email protected] 2Dept. Astronomy, University of Washington, Box 351580, Seattle, WA 98195 USA email: [email protected] 3REU participant, 2015; California Institute of Technology, 1200 E, California Blvd, Pasadena, CA 91125 USA email: [email protected] 4Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA email:[email protected] 5REU participant, 2016; Wellesley College, 106 Central Street, Wellesley, MA 02481 USA email: [email protected] Abstract. We summarize here recent work in identifying and characterizing red supergiants (RSGs) in the galaxies of the Local Group. Keywords. stars: early type, supergiants, stars: Wolf-Rayet 1. Introduction In the Olden Days, the term “massive star” was synonymous with “hot [massive] star,” and topics at these conferences were restricted to O-type stars and Wolf-Rayet (WR) stars. Gradually massive star research has expanded to include the red supergiants (RSGs). Stars with initial masses 8 − 30M⊙ will evolve into RSGs, and these are the progenitors of many core-collapse SNe. The amount of mass loss during the RSG phase will affect the subsequent evolution (if any) of these stars, with some evolving back to the blue side of the H-R diagram (HRD), and possibly even becoming WRs (see, e.g., Meynet et al.
    [Show full text]
  • The Luminosities of Cool Supergiants in the Magellanic Clouds, and the Humphreys-Davidson Limit Revisited
    This is a repository copy of The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys-Davidson limit revisited. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/130065/ Version: Accepted Version Article: Davies, B., Crowther, P.A. and Beasor, E.R. (2018) The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys-Davidson limit revisited. Monthly Notices of the Royal Astronomical Society, 478 (3). pp. 3138-3148. ISSN 0035-8711 https://doi.org/10.1093/mnras/sty1302 This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Ben Davies, Paul A Crowther, Emma R Beasor, The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited, Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 3, August 2018, Pages 3138–3148, is available online at: https://doi.org/10.1093/mnras/sty1302 Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version. This is indicated by the licence information on the White Rose Research Online record for the item. 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.
    [Show full text]
  • HV 11423: the Coolest Supergiant in The
    HV 11423: The Coolest Supergiant in the SMC Philip Massey,1,2 Emily M. Levesque,2,3 K. A. G. Olsen,4 Bertrand Plez,5 B. A. Skiff 1 ABSTRACT We call attention to the fact that one of the brightest red supergiants in the SMC has recently changed its spectral type from K0-1 I (December 2004) to M4 I (December 2005) and back to K0-1 I (September 2006). An archival spectrum from the Very Large Telescope reveals that the star was even cooler (M4.5-M5 I) in December 2001. By contrast, the star was observed to be an M0 I in both October 1978 and October 1979. The M4-5 I spectral types is by far the latest type seen for an SMC supergiant, and its temperature in that state places it well beyond the Hayashi limit into a region of the H-R diagram where the star should not be in hydrostatic equilibrium. The star is variable by nearly 2 mag in V , but essentially constant in K. Our modeling of its spectral energy distribution shows that the visual extinction has varied during this time, but that the star has remained essentially constant in bolometric luminosity. We suggest that the star is currently undergoing a period of intense instability, with its effective temperature changing from 4300 K to 3300 K on the time-scale of months. It has one of the highest 12µm fluxes of any RSG in the SMC, and we suggest that the variability at V is due primarily to changes in effective temperature, and secondly, due to changes in the local extinction due to creation and dissipation of circumstellar dust.
    [Show full text]
  • Annual Report 2007 ESO
    ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 presented to the Council by the Director General Prof. Tim de Zeeuw ESO is the pre-eminent intergovernmental science and technology organisation in the field of ground-based astronomy. It is supported by 13 countries: Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Further coun- tries have expressed interest in member- ship. Created in 1962, ESO provides state-of- the-art research facilities to European as- tronomers. In pursuit of this task, ESO’s activities cover a wide spectrum including the design and construction of world- class ground-based observational facili- ties for the member-state scientists, large telescope projects, design of inno- vative scientific instruments, developing new and advanced technologies, further- La Silla. ing European cooperation and carrying out European educational programmes. One of the most exciting features of the In 2007, about 1900 proposals were VLT is the possibility to use it as a giant made for the use of ESO telescopes and ESO operates the La Silla Paranal Ob- optical interferometer (VLT Interferometer more than 700 peer-reviewed papers servatory at several sites in the Atacama or VLTI). This is done by combining the based on data from ESO telescopes were Desert region of Chile. The first site is light from several of the telescopes, al- published. La Silla, a 2 400 m high mountain 600 km lowing astronomers to observe up to north of Santiago de Chile.
    [Show full text]
  • Late-Type Red Supergiants: Too Cool for the Magellanic Clouds?
    Late-Type Red Supergiants: Too Cool for the Magellanic Clouds? Emily M. Levesque1 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 [email protected] Philip Massey1 Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ 86001 [email protected] K. A. G. Olsen Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile [email protected] Bertrand Plez GRAAL, Universite Montpellier II, CNRS, 34095 Montpellier, France [email protected] ABSTRACT We have identified seven red supergiants (RSGs) in the Large Magellanic Cloud (LMC) and four RSGs in the Small Magellanic Cloud (SMC), all of which arXiv:0705.3431v1 [astro-ph] 23 May 2007 have spectral types that are considerably later than the average type observed in their parent galaxy. Using moderate-resolution optical spectrophotometry and the MARCS stellar atmosphere models, we determine their physical properties and place them on the H-R diagram for comparison with the predictions of current stellar evolutionary tracks. The radial velocities of these stars suggest that they are likely all members of the Clouds rather than foreground dwarfs or halo giants. Their locations in the H-R diagram also show us that these stars are cooler than 1Visiting Astronomer, Cerro Tololo Inter-American Observatory (CTIO), National Optical Astronomy Observatory (NOAO), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation (NSF). –2– the current evolutionary tracks allow, appearing to the right of the Hayashi limit, a region in which stars are no longer in hydrodynamic equilibrium.
    [Show full text]
  • The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (As Supergigantes Vermelhas No Aglomerado Estelar Supermassivo Westerlund 1)
    Universidade de S~aoPaulo Instituto de Astronomia, Geof´ısicae Ci^enciasAtmosf´ericas Departamento de Astronomia Aura de las Estrellas Ram´ırezAr´evalo The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (As Supergigantes Vermelhas no Aglomerado Estelar Supermassivo Westerlund 1) S~aoPaulo 2018 Aura de las Estrellas Ram´ırezAr´evalo The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (As Supergigantes Vermelhas no Aglomerado Estelar Supermassivo Westerlund 1) Disserta¸c~aoapresentada ao Departamento de Astronomia do Instituto de Astronomia, Geof´ısica e Ci^enciasAtmosf´ericasda Universidade de S~aoPaulo como requisito parcial para a ob- ten¸c~aodo t´ıtulode Mestre em Ci^encias. Area´ de Concentra¸c~ao:Astronomia Orientador: Prof. Dr. Augusto Damineli Neto Vers~aoCorrigida. O original encontra- se dispon´ıvel na Unidade. S~aoPaulo 2018 To my parents, Eustorgio and Esmeralda, to whom I owe everything. Acknowledgements This dissertation was possible thanks to the support of many people, to whom I owe not only this manuscript and the work behind it, but many years of personal and professional growth. In the first place I thank my parents, Eustorgio and Esmeralda, for all the unconditional love and the sacrifices they have made to make me the woman I am today, for never leaving me alone no matter how far we are, and for all the support they have given me throughout the years, that has allowed me to fulfill my dreams. This accomplishment is theirs. Pap´a y mam´a,este logro es de ustedes. I thank Alex, my companion during this phase, for his love, patience and priceless support especially in those difficult times, when he would cheer me up.
    [Show full text]
  • The Physical Properties of Red Supergiants
    **FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The Physical Properties of Red Supergiants Philip Massey,1 Bertrand Plez,2 Emily M. Levesque,3 K. A. G. Olsen,4 David R. Silva,5 and Geoffrey C. Clayton6 Abstract. Red supergiants (RSGs) are an evolved stage in the life of in- termediate massive stars (< 25M⊙). For many years their location in the H-R diagram was at variance with the evolutionary models. Using the MARCS stel- lar atmospheres, we have determined new effective temperatures and bolometric luminosities for RSGs in the Milky Way, LMC, and SMC, and our work has resulted in much better agreement with the evolutionary models. We have also found evidence of significant visual extinction due to circumstellar dust. Al- though in the Milky Way the RSGs contribute only a small fraction (<1%) of the dust to the interstellar medium (ISM), in starburst galaxies or galaxies at large look-back times, we expect that RSGs may be the main dust source. We are in the process of extending this work now to RSGs of higher and lower metallicities using the galaxies M31 and WLM. 1. Introduction: What Am I Doing Here? I feel I have to explain what I’m doing at a “cool stars” conference, much less giving the opening talk. Most of my work has been concerned with the formation, physical properties, and evolution of massive stars, and for most of my career I’ve stayed over on the “hot” side of the H-R diagram (HRD). Still, as shown in Figure 1 some massive stars spend a significant fraction of their lives as red supergiants (RSGs).
    [Show full text]
  • Spitzer Infrared Spectrograph Point Source Classification in the Small
    MNRAS 451, 3504–3536 (2015) doi:10.1093/mnras/stv1106 Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud Paul M. E. Ruffle,1,2‹ F. Kemper,2† O. C. Jones,1,3 G. C. Sloan,4 K. E. Kraemer,5 Paul M. Woods,6 M. L. Boyer,7 S. Srinivasan,2 V. Antoniou,8 E. Lagadec,9 M. Matsuura,10,11 I. McDonald,1 J. M. Oliveira,12 B. A. Sargent,13 M. Sewiło,14,15 R. Szczerba,16 J. Th. van Loon,12 K. Volk3 and A. A. Zijlstra1 1Jodrell Bank Centre for Astrophysics, The University of Manchester, Alan Turing Building, Oxford Road, Manchester M13 9PL, UK 2Academia Sinica, Institute of Astronomy and Astrophysics, Taipei 10617, Taiwan 3Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 4Department of Astronomy, Cornell University, Ithaca, NY 14853, USA 5Institute for Scientific Research, Boston College, 140 Commonwealth Avenue, Chestnuthill, MA 02467, USA 6Astrophysics Research Centre, School of Mathematics & Physics, Queen’s University Belfast, University Road, Belfast BT7 1NN, UK 7Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 8Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 9Laboratoire Lagrange, Universite´ de Nice - Sophia Antipolis, Observatoire de la Coteˆ d’Azur, CNRS, F-06304 Nice, France 10School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK 11Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 12School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK 13Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 54 Lomb Memorial Drive, Rochester, NY 14623, USA 14Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA 15Department of Physics and Astronomy, Johns Hopkins University, 366 Bloomberg Center, 3400 N.
    [Show full text]
  • A Census of Yellow Supergiants in the SMC: Testing Massive Star Evolutionary Models at Low Metallicities
    NOAO Observing Proposal Standard proposal Panel: For office use. Date: March 27, 2009 Category: Massive Stars A Census of Yellow Supergiants in the SMC: Testing Massive Star Evolutionary Models at Low Metallicities PI: Philip Massey Status: P Affil.: Lowell Observatory 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA Email: [email protected] Phone: 928-233-3264 FAX: 928-774-6296 CoI: Maria Drout Status: U Affil.: University of Iowa CoI: Knut Olsen Status: P Affil.: NOAO CoI: Brian Skiff Status: O Affil.: Lowell Observatory CoI: Norbert Przybilla Status: P Affil.: Univ Erlangen-Nurnberg, Bamberg, Germany CoI: Georges Meynet Status: P Affil.: Geneva Observatory CoI: Andre Maeder Status: P Affil.: Geneva Observatory Abstract of Scientific Justification (will be made publicly available for accepted proposals): We are proposing to determine an accurate census of the yellow (F- and G-type) supergiants in the SMC in order to carry out a new and stringent test of the latest stellar evolutionary models. This region of the H-R diagram is heavily contaminated (80-90%) by foreground dwarfs and halo giants, but our study will use both radial velocities and standard spectral luminosity indicators to establish membership. Our recent study of the yellow supergiants in M31 demonstrated a serious disagreement between the evolutionary time scales for stars in this very short-lived phase. This might be connected to M31’s high ( 2 solar) metallicity and its result on mass-loss during the ∼ × red supergiant phase, or it may be a more generic problem with the models. We therefore propose to conduct a similar test at low metallicity.
    [Show full text]