DOCSLIB.ORG

Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection UvA-DARE (Digital Academic Repository) Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection Sana, H.; de Bouquin, J.B.; Lacour, S.; Berger, J.-P.; Duvert, G.; Gauchet, L.; Norris, B.; Olofsson, J.; Pickel, D.; Zins, G.; Absil, O.; de Koter, A.; Kratter, K.; Schnurr, O.; Zinnecke, H. DOI 10.1088/0067-0049/215/1/15 Publication date 2014 Published in The Astrophysical Journal. Supplement Series Link to publication Citation for published version (APA): Sana, H., de Bouquin, J. B., Lacour, S., Berger, J-P., Duvert, G., Gauchet, L., Norris, B., Olofsson, J., Pickel, D., Zins, G., Absil, O., de Koter, A., Kratter, K., Schnurr, O., & Zinnecke, H. (2014). Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection. The Astrophysical Journal. Supplement Series, 215(1), 15. https://doi.org/10.1088/0067-0049/215/1/15 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. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:26 Sep 2021 The Astrophysical Journal Supplement Series, 215:15 (35pp), 2014 November doi:10.1088/0067-0049/215/1/15 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. SOUTHERN MASSIVE STARS AT HIGH ANGULAR RESOLUTION: OBSERVATIONAL CAMPAIGN AND COMPANION DETECTION H. Sana1, J.-B. Le Bouquin2,3, S. Lacour4, J.-P. Berger5, G. Duvert2,3, L. Gauchet4, B. Norris6, J. Olofsson7, D. Pickel4, G. Zins2,3,O.Absil8,15, A. de Koter9,10, K. Kratter11,12,16, O. Schnurr13, and H. Zinnecker14 1 European Space Agency/Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected] 2 Universite´ Grenoble Alpes, IPAG, F-38000 Grenoble, France 3 CNRS, IPAG, F-38000 Grenoble, France 4 LESIA, Observatoire de Paris, CNRS, UPMC, Universite´ Paris-Diderot, Paris Sciences et Lettres, 5 Place Jules Janssen, F-92195 Meudon, France 5 European Southern Observatory, Schwarzschild-Str. 2, D-85748 Garching bei Munchen,¨ Germany 6 Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia 7 Max-Planck-Institut fur¨ Astronomie, Koenigstuhl 17, D-69117 Heidelberg, Germany 8 Departement´ d’Astrophysique, Geophysique´ et Oceanographie,´ UniversitedeLi´ ege,` 17 Allee´ du Six Aout,ˆ B-4000 Liege,` Belgium 9 Astrophysical Institute Anton Pannekoek, Universiteit van Amsterdam, Science Park 904, 1098XH Amsterdam, The Netherlands 10 Instituut voor Sterrenkunde, Universiteit Leuven, Celestijnenlaan 200 D, B-3001, Leuven, Belgium 11 JILA, 440 UCB, University of Colorado, Boulder, CO 80309-0440, USA 12 Steward Observatory/Department of Astronomy, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721, USA 13 Leibniz-Institut fur¨ Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany 14 Deutsches SOFIA Instituut, SOFIA Science Center, NASA Ames Research Center, Mail Stop N232-12, Moffett Field, CA 94035, USA Received 2014 February 7; accepted 2014 September 8; published 2014 November 4 ABSTRACT Multiplicity is one of the most fundamental observable properties of massive O-type stars and offers a promising way to discriminate between massive star formation theories. Nevertheless, companions at separations between 1 and 100 milliarcsec (mas) remain mostly unknown due to intrinsic observational limitations. At a typical distance of 2 kpc, this corresponds to projected physical separations of 2–200 AU. The Southern MAssive Stars at High angular resolution survey (smash+) was designed to fill this gap by providing the first systematic interferometric survey of Galactic massive stars. We observed 117 O-type stars with VLTI/PIONIER and 162 O-type stars with NACO/ Sparse Aperture Masking (SAM), probing the separation ranges 1–45 and 30–250 mas and brightness contrasts of ΔH<4 and ΔH<5, respectively. Taking advantage of NACO’s field of view, we further uniformly searched for visual companions in an 8 radius down to ΔH = 8. This paper describes observations and data analysis, reports the discovery of almost 200 new companions in the separation range from 1 mas to 8 and presents a catalog of detections, including the first resolved measurements of over a dozen known long-period spectroscopic binaries. Excluding known runaway stars for which no companions are detected, 96 objects in our main sample (δ<0◦; H<7.5) were observed both with PIONIER and NACO/SAM. The fraction of these stars with at least one resolved companion within 200 mas is 0.53. Accounting for known but unresolved spectroscopic or eclipsing companions, the multiplicity fraction at separation ρ<8 increases to fm = 0.91 ± 0.03. The fraction of luminosity class V stars that have a bound companion reaches 100% at 30 mas while their average number of physically connected companions within 8 is fc = 2.2 ± 0.3. This demonstrates that massive stars form nearly exclusively in multiple systems. The nine non-thermal radio emitters observed by smash+ are all resolved, including the newly discovered pairs HD 168112 and CPD−47◦2963. This lends strong support to the universality of the wind-wind collision scenario to explain the non-thermal emission from O-type stars. Key words: binaries: visual – stars: early-type – stars: imaging – surveys – techniques: high angular resolution – techniques: interferometric Online-only material: color figures 1. INTRODUCTION several massive companions (e.g., Kratter & Matzner 2006; Krumholz 2012). The properties of the binary population, for One of the most striking properties of massive stars is their example, the period and mass ratio distributions, can then high degree of multiplicity. In clusters and associations, 75% serve as a useful diagnostics to discriminate between different of the O-type objects have at least one companion detected formation models. Different massive star formation theories do through either spectroscopy or imaging techniques (Mason indeed have different expectations for multiplicity properties et al. 2009). This rate has not been corrected for observational (for recent reviews, see Zinnecker & Yorke 2007; Tan et al. biases so that the true multiplicity fraction might very well 2014). Unfortunately, observations have so far failed to provide come close to 100%. Typically, the detected companions have a comprehensive view of the O star multiplicity over the a mass one to five times smaller than the primary mass and full separation range relevant for massive star formation and are mostly O and B stars. We can thus postulate that the evolution, leaving us with a strongly biased view toward tight typical end product of massive star formation is not a single (physical separation d<1 AU) and wide (d>103 AU) star but a multiple system, with at least one and possibly companions. Binary detection through spectroscopy is typically limited to 15 F.R.S.—FNRS Research Associate. systems with mass ratios M1/M2 up to 5 to 15 (for double- and 16 Hubble Fellow. single-lined binaries, respectively) and to separations up to a 1 The Astrophysical Journal Supplement Series, 215:15 (35pp), 2014 November Sana et al. few astronomical units (corresponding to periods of about one its small spectral dispersion mode is H = 7.5. The limiting year). Most imaging techniques suffer from a brightness contrast magnitude from the fast guiding systems of the auxiliary versus separation bias (Turner et al. 2008; Sana & Evans 2011), telescopes (STRAP) allowing for a proper injection of the beams which limits the detection of moderate brightness companions into the instruments fibers is V = 11. The practical range of to separations larger than several 0.1 at best. Separations below accessible declinations (δ<0◦) is limited by observability 0.1 have most successfully been probed through various flavors constraints of the auxiliary telescopes in the intermediate and of interferometry, such as speckle, aperture masking, and long large configurations. The Galactic O Star Catalog (GOSC-v2; baseline interferometry, although very few observations have Sota et al. 2008) lists 147 O-type stars fulfilling these criteria. been able to probe the regime of highest contrasts (Δmag > 2) Rejecting the Orion stars that have already been observed by and closest angular separations (ρ<75 milliarcsec (mas); for the VLTI (Grellmann et al. 2013), we are left with 138 possible a review, see Sana & Evans 2011). targets. Of these, 12 are flagged as runaway stars in the GOSC This paper introduces the Southern MAssive Stars at High and are handled separately from the main target list. angular resolution survey (smash+), an interferometric survey Tables 1 and 2 list the properties of stars in our main list of over 100 Galactic O-type stars designed to systematically of targets and in the runaway list. Columns 1 and 2 indicate explore the separation range between 1 and 200 mas. The Sparse whether the object has been observed with PIONIER and Aperture Masking (SAM) mode (Lacour et al. 2011b)ofNACO NACO. Columns 3 and 4 provide the main identifier used in our at the Very Large Telescope (VLT) has allowed us to resolve survey (HD number if available, BD/CPD identifiers otherwise) massive binaries with separations in the range of 30–250 mas and alternative names commonly used in the literature.
Load more

Recommended publications
  • The Effect of the Apsidal Motion on the Light Curve of the Close Binary HD 93205 (O3V+O8V)?
    A&A 397, 921–925 (2003) Astronomy DOI: 10.1051/0004-6361:20021438 & c ESO 2003 Astrophysics The effect of the apsidal motion on the light curve of the close binary HD 93205 (O3V+O8V)? A. M. van Genderen?? Leiden Observatory, Postbus 9513, 2300 RA Leiden, The Netherlands Received 25 June 2002/Accepted 28 August 2002 Abstract. The 1982–1985 photometry (VBLUW system) of the O3V+O8V close binary HD 93205 has been rediscussed be- cause of new insights into its true nature and orbital changes. By comparing this data set with the one obtained by Antokhina et al. (2000) in 1993, and using the same ephemeris to construct the light curve in the phase diagram, the effect of the apsidal motion became obvious: a phase shift between the two light curves and a small change of the shape. A phase-locked light variationintheL passband (containing the higher Balmer lines) is clearly present in the 1982–1985 data set and is presumably due to absorption if the O8 star is seen through cooler inter-binary gas, e.g. the bow-shock between the two colliding winds. Key words. stars: variables: general – stars: binaries: close – stars: early-type – stars: individual: HD 93205 1. Introduction Sect. 2). So far only the observations in the V band relative to the comparison star were published (Papers I, IX). The phase HD 93205 (O3V+O8V) is the earliest known system for which diagrams of the 1982–1985 and 1993 data sets, the latter from an RV is known, of which the first was presented by Conti & Antokhina et al.
    [Show full text]
  • X-Ray Study of Stellar Winds with Suzaku
    X-ray Study of Stellar Winds with Suzaku Yoshiaki Hyodo Department of Physics, Graduate School of Science, Kyoto University Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan [email protected] This thesis was submitted to the Department of Physics, Graduate School of Science, Kyoto University on January 5 2009 in partial fulfillment of the requirements for the degree of Doctor of Philosophy in physics. Abstract Stellar winds from massive stars play an important role for dynamical and chemical evolution of galaxies. To evaluate their effects in a galaxy scale, both the total number and the properties of massive stars should be understood. Most massive stars have soft X-ray emission, while some have additional hard emission. Although it is indicated that the binarity is important, the condition for hard X-ray production has not yet been elucidated. Also, some massive star clusters exhibit diffuse (pc scale) X-ray emission, where stellar winds may be depositing energy to the interstellar space. However, previous studies were not able to clarify the origin of the diffuse emission. It is even unclear whether the emission is physically related to the star cluster or not. The X-ray Imaging Spectrometer (XIS) on board Suzaku has a good energy resolution, a low and stable background, and a large effective area, which are suited for narrow-band surveys and spectroscopy of both point-like and extended X-ray emission. Using the XIS, we performed a very deep survey in the direction of the central region of our Galaxy and pointing observations of three well-known star forming regions in our Galaxy (M 17, the Carina Nebula, and the Arches cluster).
    [Show full text]
  • Observational Evidence for Tidal Interaction in Close Binary Systems, Including Short-Period Extrasolar Planets
    Tidal effects in stars, planets and disks M.-J. Goupil and J.-P. Zahn EAS Publications Series, Vol. ?, 2018 OBSERVATIONAL EVIDENCE FOR TIDAL INTERACTION IN CLOSE BINARY SYSTEMS Tsevi Mazeh1 Abstract. This paper reviews the rich corpus of observational evidence for tidal effects, mostly based on photometric and radial-velocity mea- surements. This is done in a period when the study of binaries is being revolutionized by large-scaled photometric surveys that are detecting many thousands of new binaries and tens of extrasolar planets. We begin by examining the short-term effects, such as ellipsoidal variability and apsidal motion. We next turn to the long-term effects, of which circularization was studied the most: a transition period be- tween circular and eccentric orbits has been derived for eight coeval samples of binaries. The study of synchronization and spin-orbit align- ment is less advanced. As binaries are supposed to reach synchroniza- tion before circularization, one can expect finding eccentric binaries in pseudo-synchronization state, the evidence for which is reviewed. We also discuss synchronization in PMS and young stars, and compare the emerging timescale with the circularization timescale. We next examine the tidal interaction in close binaries that are orbited by a third distant companion, and review the effect of pumping the binary eccentricity by the third star. We elaborate on the impact of the pumped eccentricity on the tidal evolution of close binaries residing in triple systems, which may shrink the binary separation. Finally we consider the extrasolar planets and the observational evidence for tidal interaction with their parent stars.
    [Show full text]
  • Arxiv:1008.3235V2 [Astro-Ph.HE] 30 Aug 2010 .Roth M
    F ermi Large Area Telescope Observation of a Gamma-ray Source at the Position of Eta Carinae A. A. Abdo1,2, M. Ackermann3, M. Ajello3, A. Allafort3, L. Baldini4, J. Ballet5, G. Barbiellini6,7, D. Bastieri8,9, K. Bechtol3, R. Bellazzini4, B. Berenji3, R. D. Blandford3, E. Bonamente10,11, A. W. Borgland3, A. Bouvier3, T. J. Brandt12,13, J. Bregeon4, A. Brez4, M. Brigida14,15, P. Bruel16, R. Buehler3, T. H. Burnett17, G. A. Caliandro18, R. A. Cameron3, P. A. Caraveo19, S. Carrigan9, J. M. Casandjian5, C. Cecchi10,11, O.¨ C¸elik20,21,22, S. Chaty5, A. Chekhtman1,23, C. C. Cheung1,2, J. Chiang3, S. Ciprini11, R. Claus3, J. Cohen-Tanugi24, L. R. Cominsky25, J. Conrad26,27,28, C. D. Dermer1, F. de Palma14,15, S. W. Digel3, E. do Couto e Silva3, P. S. Drell3, R. Dubois3, D. Dumora29,30, C. Favuzzi14,15, S. J. Fegan16, E. C. Ferrara20, M. Frailis31,32, Y. Fukazawa33, P. Fusco14,15, F. Gargano15, N. Gehrels20, S. Germani10,11, N. Giglietto14,15, F. Giordano14,15, G. Godfrey3, I. A. Grenier5, M.-H. Grondin29,30, J. E. Grove1, L. Guillemot34,29,30, S. Guiriec35, D. Hadasch36, Y. Hanabata33, A. K. Harding20, M. Hayashida3, E. Hays20, A. B. Hill37,38, D. Horan16, R. E. Hughes13, R. Itoh33, M. S. Jackson39,27, G. J´ohannesson3, A. S. Johnson3, W. N. Johnson1, T. Kamae3, H. Katagiri33, J. Kataoka40, M. Kerr17, J. Kn¨odlseder12, M. Kuss4, J. Lande3, L. Latronico4, S.-H. Lee3, M. Lemoine-Goumard29,30, M. Livingstone41, M. Llena Garde26,27, F. Longo6,7, F. Loparco14,15, M.
    [Show full text]
  • CANDIDATE X-RAY-EMITTING OB STARS in the CARINA NEBULA IDENTIFIED VIA INFRARED SPECTRAL ENERGY DISTRIBUTIONS Matthew S
    For Publication in the Chandra Carina Complex Project Special Issue of the Astrophysical Journal Supplement Series Preprint typeset using LATEX style emulateapj v. 8/13/10 CANDIDATE X-RAY-EMITTING OB STARS IN THE CARINA NEBULA IDENTIFIED VIA INFRARED SPECTRAL ENERGY DISTRIBUTIONS Matthew S. Povich,1,2 Leisa K. Townsley,1 Patrick S. Broos,1 Marc Gagne,´ 3 Brian L. Babler,4 Remy´ Indebetouw,5 Steven R. Majewski,5 Marilyn R. Meade,4 Konstantin V. Getman,1 Thomas P. Robitaille,6,7 & Richard H. D. Townsend4 For Publication in the Chandra Carina Complex Project Special Issue of the Astrophysical Journal Supplement Series ABSTRACT We report the results of a new survey of massive, OB stars throughout the Carina Nebula using the X-ray point source catalog provided by the Chandra Carina Complex Project (CCCP) in conjunction with infrared (IR) photometry from the Two Micron All-Sky Survey and the Spitzer Space Telescope Vela–Carina survey. Mid-IR photometry is relatively unaffected by extinction, hence it provides strong constraints on the luminosities of OB stars, assuming that their association with the Carina Nebula, and hence their distance, is confirmed. We fit model stellar atmospheres to the optical (UBV)and IR spectral energy distributions (SEDs) of 182 OB stars with known spectral types and measure the bolometric luminosity and extinction for each star. We find that the extinction law measured toward the OB stars has two components: AV = 1–1.5 mag produced by foreground dust with a ratio of total-to-selective absorption RV =3.1 plus a contribution from local dust with RV > 4.0inthe Carina molecular clouds that increases as AV increases.
    [Show full text]
  • The Carina Nebula in X-Rays
    THE CARINA NEBULA IN X-RAYS M. F. Corcoran1 2 , J. Swank2, G. Rawley3 , R. Petre2, J. Schmitt4 , C. Day1 2 RESUMEN New ROSAT PSPC and HRI observations of the Carina Nebula region are used to examine the X-ray emission from the discrete sources as well as the diffuse hot gas in the Carina Nebula near Eta Carina. Most of the diffuse emission comes from gas at a temperature of a few million degrees, but hotter (4 × 107 K) diffuse gas in an 11 pc region around Eta Car is also detected. Eta Car shows a 3 component spectrum with temperatures of 106, 6 × 106 and 4 × 107 K. A 0.1 × 0.2 pc shell of X-ray emitting gas around Eta Car has been resolved by the HRI, and comparison of the Einstein HRI and ROSAT HRI images supports the suggestion that the soft components originate in the shell (which is unresolved by the PSPC) while the hottest gas is produced less than an arcsec from the optical star. Spectra of the bright O stars are characterized by 2 temperature components (107 K and 2 × 106 K) and generally show absorption columns larger than the interstellar column. PSPC and ROSAT HRI observations are used to examine the Lx/Lbol relation for hot stars in the field through the early-B spectral class. ABSTRACT New ROSAT PSPC and HRI observations of the Carina Nebula region are used to examine the X-ray emission from the discrete sources as well as the diffuse hot gas in the Carina Nebula near Eta Carina.
    [Show full text]
  • Gaia, Trumpler 16, and Eta Carinae
    This site uses cookies. By continuing to use this site you agree to our use of cookies. To find out more, see our Privacy and Cookies policy. Gaia, Trumpler 16, and Eta Carinae Kris Davidson1, Greta Helmel2 , and Roberta M. Humphreys1 Published 2018 August 1 • © 2018. The American Astronomical Society. All rights reserved. Research Notes of the AAS, Volume 2, Number 3 1 Minnesota Institute for Astrophysics, 116 Church St. SE, Minneapolis, MN 55455, USA 2 Department of Physics and Astronomy, Macalester College, 1600 Grand Ave. St. Paul, MN 55105, USA Greta Helmel https://orcid.org/0000-0002-6542-2920 Roberta M. Humphreys https://orcid.org/0000-0003-1720-9807 Received 2018 July 24 Accepted 2018 July 26 Published 2018 August 1 Kris Davidson et al 2018 Res. Notes AAS 2 133 https://doi.org/10.3847/2515-5172/aad63c open clusters and associations: individual (Tr 16,) ; parallaxes; stars: distances; stars: individual (eta Car) Export citation and abstract BibTeX RIS The star cluster Tr 16 contains four O3-type members and η Car—an extraordinary concentration of stars with M 50 M⊙. Here we note that Gaia parallaxes reveal a discrepancy in η Car's distance, and also a serious overestimate of cluster membership. For information about η Car, see various authors' reviews in Davidson & Humphreys (2012). We employ Gaia Data Release 2 (Brown et al. 2018; Luri et al. 2018), assuming that the error estimates σi have the characteristics described by those authors. We assembled a list of fifty stars which are said to be members of Tr 16 (Walborn 1973, 1995; Massey & Johnson 1993), all having Gaia parallaxes i with standard errors σi < 0.05 mas (Figure 1).
    [Show full text]
  • A Catalog of Chandra X-Ray Sources in the Carina Nebula
    Re-submitted for the CCCP Special Issue, December 20, 2010 A Catalog of Chandra X-ray Sources in the Carina Nebula Patrick S. Broos1, Leisa K. Townsley1, Eric D. Feigelson1, Konstantin V. Getman1, Gordon P. Garmire1, Thomas Preibisch2, Nathan Smith3, Brian L. Babler4, Simon Hodgkin5, R´emy Indebetouw6, Mike Irwin5, Robert R. King7, Jim Lewis5, Steven R. Majewski,6, Mark J. McCaughrean7;8, Marilyn R Meade4, Hans Zinnecker9 [email protected] ABSTRACT We present a catalog of ∼14,000 X-ray sources observed by the ACIS instrument on the Chandra X-ray Observatory within a 1.42 square degree survey of the Great Nebula in Carina, known as the Chandra Carina Complex Project (CCCP). This study appears in a Special Issue of the ApJS devoted to the CCCP. Here, we describe the data reduction and analysis procedures performed on the X-ray observations, including calibration and cleaning of the X- ray event data, point source detection, and source extraction. The catalog appears to be complete across most of the field to an absorption-corrected total-band luminosity of ∼1030:7 erg s−1 for a typical low-mass pre-main sequence star. Counterparts to the X-ray sources are identified in a variety of visual, near-infrared, and mid-infrared surveys. The X-ray and infrared source properties presented here form the basis of many CCCP studies of the young stellar populations in Carina. Subject headings: ISM: individual objects (Carina Nebula) | open clusters and associations: individual (Tr14, Tr15, Tr16) | stars: formation | stars: pre-main sequence | X-Rays: stars 1Department of Astronomy & Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA 2Universit¨ats-Sternwarte, Ludwig-Maximilians-Universit¨at,Scheinerstr.
    [Show full text]
  • Massive Binaries
    Massive Binaries Nidia Morrell Las Campanas Observatory, OCIW, Chile Contifest, Oct. 2008 – p.1/26 Why do we study massive binaries? Double lined eclipsing systems provide the only way to empirically measure stellar fundamental parameters such as masses and radii throgh the simultaneous analysis of radial velocity and light variations. Massive binaries are special objects for the analysis of pair interactions, wind-wind collisions, etc. Massive binaries have been succesfully used as extragalactic distance idicators: Guinan et al. 1998, Fitzpatrick et al. 2002, Ribas et al. 2002, Harries et al. 2003, Hilditch et al. 2005, Ribas et al. 2005, Bonanos 2008 Contifest, Oct. 2008 – p.2/26 Some questions need to be addressed How massive a star can be? (Oey & Clarke 2005, Figer 2005) Are massive stars always part of multiple systems? (Mason et al. 1998, Turner et al. 2008). Analysis of multiplicity provides clues to the understanding of massive star formation (Zinnecker & Yorke 2007). On the other hand, non detected multiplicity will affect the derivation of stellar parameters and can produce biases in the estimated IMF (Maíz Apellániz & Úbeda 2005) Why do masses derived from evolutionary models often desagree with those calculated via comparison of the spectrum with model atmospheres? Keplearian masses should help to find the origin of the “mass discrepancy” (Herrero et al 1992, Massey et al. 2005) Contifest, Oct. 2008 – p.3/26 Found in massive star forming regions Contifest, Oct. 2008 – p.4/26 HD 93205 Contifest, Oct. 2008 – p.5/26 The most massive binaries NGC3603-A1 (WN6ha) 116 ± 31 + 89 ± 16 M⊙ (Schnurr et al.
    [Show full text]
  • A Radial Velocity Survey of the Carina Nebula's O-Type Stars
    MNRAS 000, 1–20 (2018) Preprint 20 September 2018 Compiled using MNRAS LATEX style file v3.0 A radial velocity survey of the Carina Nebula’s O-type stars Megan M. Kiminki1⋆ and Nathan Smith1 1Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA Accepted 2018 March 14. Received 2018 March 11; in original form 2017 June 17. ABSTRACT We have obtained multi-epoch observations of 31 O-type stars in the Carina Nebula using the CHIRON spectrograph on the CTIO/SMARTS 1.5-m telescope. We measure their radial velocities to 1–2 km s−1 precision and present new or updated orbital solutions for the binary systems HD 92607, HD 93576, HDE 303312, and HDE 305536. We also compile radial ve- locities from the literature for 32 additional O-type and evolved massive stars in the region. The combined data set shows a mean heliocentric radial velocity of 0.6 km s−1. We calculate a velocity dispersion of ≤ 9.1kms−1, consistent with an unbound, substructured OB associ- ation. The Tr 14 cluster shows a marginally significant 5 km s−1 radial velocity offset from its neighbor Tr 16, but there are otherwise no correlations between stellar position and veloc- ity. The O-type stars in Cr 228 and the South Pillars region have a lower velocity dispersion than the region as a whole, supporting a model of distributed massive-star formation rather than migration from the central clusters. We compare our stellar velocities to the Carina Neb- ula’s molecular gas and find that Tr 14 shows a close kinematic association with the Northern Cloud.
    [Show full text]
  • International Astronomical Union Commission 42 BIBLIOGRAPHY
    International Astronomical Union Commission 42 BIBLIOGRAPHY OF CLOSE BINARIES No. 73 Editor-in-Chief: C.D. Scarfe Editors: H. Drechsel D.R. Faulkner V.G. Karetnikov E. Lapasset C. Maceroni Y. Nakamura P.G. Niarchos R.G. Samec M. Wolf Material published by September 15, 2001 BCB issues are available via URL: http://www.sternwarte.uni-erlangen.de/ftp/bcb or via anonymous ftp from: ftp://www.sternwarte.uni-erlangen.de/pub/bcb This issue is also available via URL: http://www.astro.washington.edu/szkody/c42/ The bibliographical entries for Individual Stars and Collections of Data are categorized according to the following coding scheme: 1. Observational data a. Photometry b. Spectroscopy c. Spectrophotometry d. Polarimetry e. Astrometry, interferometry f. Times of minima g. γ-ray data i. Infrared data o. Optical data p. Photographic data r. Radio data u. Ultraviolet data v. Visual estimates x. X-ray data 2. Derived physical data a. Orbital elements b. Absolute dimensions, masses c. New or improved ephemeris, period variations d. Apsidal motion e. Physical properties of stellar atmospheres f. Chemical abundances g. Accretion disks and accretion phenomena 3. Catalogues, discoveries, charts a. Catalogues b. Discoveries of new binaries and novae c. Identification of optical counterparts of X-ray, IR, or radio sources d. Finding charts 4. Observational techniques 5. Theoretical investigations 6. Statistical investigations 7. Miscellaneous a. Abstract b. Addenda or errata Abbreviations AD accretion disk HMXB high-mass X-ray binary QPO quasi-periodic oscillation BH black hole IP intermediate polar RV radial velocity CB close binary LC light curve SB spectroscopic binary CV cataclysmic variable LMXB low-mass X-ray binary WD white dwarf EB eclipsing binary NS neutron star WR Wolf-Rayet star Individual Stars RT And Ekmekci, F., Ak, H.
    [Show full text]
  • Optical Spectroscopy of X-Mega Targets in the Carina Nebula. II. The
    Mon. Not. R. Astron. Soc. 000, 000–000 (2000) Printed 26 October 2018 (MN LATEX style file v1.4) Optical spectroscopy of X-Mega targets in the Carina Nebula. II. The massive double-lined O-type binary HD 93205 ⋆ ⋆ N.I. Morrell1 , R.H. Barb´a1 , V.S. Niemela1†, M.A. Corti1‡, J.F. Albacete Colombo1, G. Rauw2§, M. Corcoran3,4, T. Morel5, J.-F. Bertrand6,7, A.F.J. Moffat6,7, N. St-Louis6,7 1 Facultad de Ciencias Astron´omicas y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA La Plata, Argentina 2 Institut d’Astrophysique et de G´eophysique, Universit´e de Li`ege, 5, Avenue de Cointe, B 4000 Li`ege, Belgium 3 Universities Space Research Association, 7501 Forbes Blvd, Ste 206, Seabrook, MD 20706, USA 4 Laboratory for High Energy Astrophysics, Goddard Space Flight Center, Greenbelt MD 20771, USA 5 Inter-University Center for Astronomy and Astrophysics (IUCAA), Post Bag 4, Ganeshkhind, Pune, 411 007, India. 6 D´epartement de physique, Universit´ede Montr´eal, C.P. 6128, Succursale Centre-ville, Montr´eal, QC, H3C 3J7, Canada 7 Observatoire du Mont M´egantic, Canada Accepted 2000 December 15. Received 2000 December 14; in original form 2000 October 11 ABSTRACT A new high-quality set of orbital parameters for the O-type spectroscopic binary HD 93205 has been obtained combining ´echelle and coud´eCCD observations. The radial velocity orbits derived from the He ii λ4686 A˚ (primary component) and He i λ4471 A˚ (secondary component) absorption lines yield semiamplitudes of 133 ± 2 and 314 ± 2 kms−1 for each binary component, resulting in minimum masses of 31 and 13 M⊙ (q =0.42).
    [Show full text]