MASS and TEMPERATURE of the TWA 7 DEBRIS DISK Brenda C
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Arxiv:1305.7264V2 [Astro-Ph.EP] 21 Apr 2014 Spain
Draft version September 18, 2018 Preprint typeset using LATEX style emulateapj v. 08/22/09 THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE YEARS Timothy D. Brandt1, Masayuki Kuzuhara2, Michael W. McElwain3, Joshua E. Schlieder4, John P. Wisniewski5, Edwin L. Turner1,6, J. Carson7,4, T. Matsuo8, B. Biller4, M. Bonnefoy4, C. Dressing9, M. Janson1, G. R. Knapp1, A. Moro-Mart´ın10, C. Thalmann11, T. Kudo12, N. Kusakabe13, J. Hashimoto13,5, L. Abe14, W. Brandner4, T. Currie15, S. Egner12, M. Feldt4, T. Golota12, M. Goto16, C. A. Grady3,17, O. Guyon12, Y. Hayano12, M. Hayashi18, S. Hayashi12, T. Henning4, K. W. Hodapp19, M. Ishii12, M. Iye13, R. Kandori13, J. Kwon13,22, K. Mede18, S. Miyama20, J.-I. Morino13, T. Nishimura12, T.-S. Pyo12, E. Serabyn21, T. Suenaga22, H. Suto13, R. Suzuki13, M. Takami23, Y. Takahashi18, N. Takato12, H. Terada12, D. Tomono12, M. Watanabe24, T. Yamada25, H. Takami12, T. Usuda12, M. Tamura13,18 Draft version September 18, 2018 ABSTRACT We present results from the first three years of observations of moving group targets in the SEEDS high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of ∼105 at 100 and ∼106 beyond 200 around 63 proposed members of nearby kinematic moving groups. We review each of the kinematic associations to which our targets belong, concluding that five, β Pictoris (∼20 Myr), AB Doradus (∼100 Myr), Columba (∼30 Myr), Tucana-Horogium (∼30 Myr), and TW Hydrae (∼10 Myr), are sufficiently well-defined to constrain the ages of individual targets. -
EXPLORING TERRESTRIAL PLANET FORMATION in the TW HYDRAE ASSOCIATION Frank J
The Astrophysical Journal, 631:1170–1179, 2005 October 1 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. EXPLORING TERRESTRIAL PLANET FORMATION IN THE TW HYDRAE ASSOCIATION Frank J. Low and Paul S. Smith Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; fl[email protected], [email protected] Michael Werner and Christine Chen1,2 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109; [email protected] Vanessa Krause Division of Physics, Mathematics, and Astronomy, California Institute of Technology, 770 South Wilson Avenue, MS 103-33, Pasadena, CA 91125; [email protected] Michael Jura Department of Physics and Astronomy, Knudsen Hall, University of California, Los Angeles, Los Angeles, CA 90095; [email protected] and Dean C. Hines Space Science Institute, 3100 Marine Street, Suite A353, Boulder, CO 80303 Received 2005 April 5; accepted 2005 June 9 ABSTRACT Spitzer Space Telescope infrared measurements are presented for 24 members of the TW Hya association (TWA). High signal-to-noise ratio 24 m photometry is presented for all these stars, including 20 stars that were not detected by IRAS. Among these 20 stars, only a single object, TWA 7, shows excess emission at 24 m at the level of only 40% above the star’s photosphere. TWA 7 also exhibits a strong 70 m excess that is a factor of 40 brighter than the stellar photosphere at this wavelength. At 70 m, an excess of similar magnitude is detected for TWA 13, although no 24 m excess was detected for this binary. -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
The Metallicity of the Hd 98800 System
The Astrophysical Journal, 698:660–665, 2009 June 10 doi:10.1088/0004-637X/698/1/660 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE METALLICITY OF THE HD 98800 SYSTEM Tanmoy Laskar1,2, David R. Soderblom2, Jeff A. Valenti2, and John R. Stauffer3 1 Department of Physics, Cavendish Laboratory, University of Cambridge, JJ Thomson Avenue, Cambridge CB3 0HE, UK; [email protected] 2 Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA; [email protected], [email protected] 3 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA; [email protected] Received 2008 November 10; accepted 2009 April 2; published 2009 May 22 ABSTRACT Pre-main-sequence (PMS) binaries and multiples enable critical tests of stellar models if masses, metallicities, and luminosities of the component stars are known. We have analyzed high-resolution, high signal-to-noise echelle spectra of the quadruple-star system HD 98800 and using spectrum synthesis computed fits to the composite spectrum for a full range of plausible stellar parameters for the components. We consistently find that subsolar metallicity yields fits with lower χ 2 values, with an overall best fit of [M/H] =−0.20 ± 0.10. This metallicity appears to be consistent with PMS evolutionary tracks for the measured masses and luminosities of the components of HD 98800 but additional constraints on the system and modeling are needed. Key words: stars: abundances – stars: individual (HD 98800) – stars: pre-main sequence Online-only material: color figure 1. THE HD 98800 SYSTEM significantly, primarily because of the different ways the models treat convection. -
Parallactic Distances to Nearby Young Association Stars
Parallactic Distances to Nearby Young Association Stars Alycia Weinberger Carnegie Institution Dept. of Terrestrial Magnetism Planetary Formation Timescales Star- Massive, Planetesimal formation gas-rich dominated to solid disk disk Dust / planet formation dominated disk Gas Removal Giant planets form Terrestrial Astronomer’s planets t0 form 106 yrs 107 yrs 108 yrs 109 yrs CAI / Moon Late Heavy Current age of Chondrule forming Bombardment the Sun: Formation Impact (30+ Myr) (600 Myr) 4.5x109 yrs. Alycia Weinberger 2009 TW Hya With HST 0.5 - 2 µm 500 AU 1.1 µm 1.6 µm “True” Color 0.5 µm Roberge et al. 2005 Debes et al. submitted TW Hya is a classical T Tauri star with lots of gas and dust. What is its age? Other Disks in TWA? 4 accreting, optically thick disks TW Hya – disk, accreting (IRAS) Hen 3-600 – disk, accreting (IRAS) TWA 30 – disk, accreting 2M1207 – BD disk, accreting 7 transitional / debris disks HD 98800 – disk, not accreting (IRAS) HR 4796A – debris, not accreting (IRAS) TWA 7 – debris, not accreting 2M1139 – BD disk, not accreting SSPM1102 – BD disk, not accreting TWA 31 – disk, not accreting TWA 32 – disk, not accreting ~14 stars with no detected disks Bi-modal distribution of dust? (e.g. Weinberger et al., AJ, 2004; Low et al. 2005; Riaz et al. 2008; Plavchan et al. 2009, Schneider et al. 2012) TW Hya is a Puzzle •!At a fairly old age, TW Hya still has a massive disk •!Something is making a partial “gap” in the disk at 80AU •!Very small grains are coexisting with very large grains throughout the disk A planet can account for all of these, except perhaps the first! What is the age of TW Hya anyway? TWA Age Canonically ~10 Myr TW Hya (and only 3 other TWA stars marked by ) have Hipparcos parallactic distances (Adapted from Webb et al. -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
A Tejútrendszer Szerkezete Tóth L
A Tejútrendszer szerkezete Tóth L. Viktor XML to PDF by RenderX XEP XSL-FO F ormatter, visit us at http://www.renderx.com/ A Tejútrendszer szerkezete Tóth L. Viktor Szerzői jog © 2013 Eötvös Loránd Tudományegyetem E könyv kutatási és oktatási célokra szabadon használható. Bármilyen formában való sokszorosítása a jogtulajdonos írásos engedélyéhez kötött. Készült a TÁMOP-4.1.2.A/1-11/1-2011-0073 számú, „E-learning természettudományos tartalomfejlesztés az ELTE TTK-n” című projekt keretében. Konzorciumvezető: Eötvös Loránd Tudományegyetem, konzorciumi tagok: ELTE TTK Hallgatói Alapítvány, ITStudy Hungary Számítástechnikai Oktató- és Kutatóközpont Kft. XML to PDF by RenderX XEP XSL-FO F ormatter, visit us at http://www.renderx.com/ Tartalom Előszó ........................................................................................................................................ vii A Tejútrendszer korai kutatásának néhány érdekessége ...................................................................... viii Referenciák és további olvasnivaló: .......................................................................................... xi 1. A Tejútrendszer alapvonásai ......................................................................................................... 1 1.1 Alapvető paraméterek ....................................................................................................... 1 1.2 Alrendszerek .................................................................................................................... 3 1.2.1. -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C. -
A Moving Cluster Distance to the Exoplanet 2M1207 B in the TW Hya
accepted to Astrophysical Journal, 18 July 2005 A Moving Cluster Distance to the Exoplanet 2M1207 B in the TW Hya Association Eric E. Mamajek1 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS-42, Cambridge, MA 02138 [email protected] ABSTRACT A candidate extrasolar planet companion to the young brown dwarf 2MASSW J1207334-393254 (2M1207) was recently discovered by Chauvin et al. They find that 2M1207 B’s temperature and luminosity are consistent with being a young, ∼5 MJup planet. The 2M1207 system is purported to be a member of the TW Hya association (TWA), and situated ∼70 pc away. Using a revised space mo- tion vector for TWA, and improved proper motion for 2M1207, I use the moving cluster method to estimate the distance to the 2M1207 system and other TWA members. The derived distance for 2M1207 (53 ± 6 pc) forces the brown dwarf and planet to be half as luminous as previously thought. The inferred masses for 2M 1207 A and B decrease to ∼21 MJup and ∼3-4MJup, respectively, with the mass of B being well below the observed tip of the planetary mass function and the theoretical deuterium-burning limit. After removing probable Lower arXiv:astro-ph/0507416v1 18 Jul 2005 Centaurus-Crux (LCC) members from the TWA sample, as well as the prob- able non-member TWA 22, the remaining TWA members are found to have distances of 49 ± 3 (s.e.m.) ± 12(1σ) pc, and an internal 1D velocity dispersion of +0.3 −1 0.8−0.2 km s . There is weak evidence that the TWA is expanding, and the data are consistent with a lower limit on the expansion age of 10 Myr (95% confidence). -
NICMOS Observations of the Pre-Main-Sequence Planetary
The Astrophysical Journal, 520:L45±L48, 1999 July 20 q 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. NICMOS OBSERVATIONS OF THE PRE±MAIN-SEQUENCE PLANETARY DEBRIS SYSTEM HD 988001 Frank J. Low, Dean C. Hines, and Glenn Schneider Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; ¯[email protected], [email protected], [email protected] Received 1999 April 19; accepted 1999 May 19; published 1999 June 21 ABSTRACT Spectral energy distributions (SEDs) from 0.4 to 4.7 mm are presented for the two principal stellar components of HD 98800, A and B. The third major component, an extensive planetary debris system (PDS), emits greater than 20% of the luminosity of star B in a blackbody SED at164 5 5 K extending from mid-IR to millimeter wavelengths. At 0.95 mm, a preliminary upper limit of less than 0.06 is obtained for the ratio of re¯ected light to the total from star B. This result limits the albedo of the PDS to less than 0.3. Values are presented for the temperature, luminosity, and radius of each major systemic component. Remarkable similarities are found between the PDS and the interplanetary debris system around the Sun as it could have appeared a few million years after its formation. Subject headings: binaries: visual Ð circumstellar matter Ð infrared: stars Ð stars: individual (HD 98800) Ð stars: pre±main-sequence 1. INTRODUCTION that all other resolved PDSs scatter and emit about equally. However, based on our predicted inner diameter of less than Long known as a visual double with less than 10 separation, 10 AU and small cross-sectional area for the PDS, we cannot HD 98800 (SAO 179815; IRAS P1119522430) was found by be con®dent of separating the re¯ected light from direct IRAS to contain the brightest planetary debris system (PDS) in starlight. -
Extrasolar Kuiper Belt Dust Disks 465
Moro-Martín et al.: Extrasolar Kuiper Belt Dust Disks 465 Extrasolar Kuiper Belt Dust Disks Amaya Moro-Martín Princeton University Mark C. Wyatt University of Cambridge Renu Malhotra and David E. Trilling University of Arizona The dust disks observed around mature stars are evidence that plantesimals are present in these systems on spatial scales that are similar to that of the asteroids and the Kuiper belt ob- jects (KBOs) in the solar system. These dust disks (a.k.a. “debris disks”) present a wide range of sizes, morphologies, and properties. It is inferred that their dust mass declines with time as the dust-producing planetesimals get depleted, and that this decline can be punctuated by large spikes that are produced as a result of individual collisional events. The lack of solid-state fea- tures indicate that, generally, the dust in these disks have sizes >10 µm, but exceptionally, strong silicate features in some disks suggest the presence of large quantities of small grains, thought to be the result of recent collisions. Spatially resolved observations of debris disks show a di- versity of structural features, such as inner cavities, warps, offsets, brightness asymmetries, spirals, rings, and clumps. There is growing evidence that, in some cases, these structures are the result of the dynamical perturbations of a massive planet. Our solar system also harbors a debris disk and some of its properties resemble those of extrasolar debris disks. From the cratering record, we can infer that its dust mass has decayed with time, and that there was at least one major “spike” in the past during the late heavy bombardment.