Publications Ralph Neuhäuser 1. Refereed
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Jupiter Analogues and Planets of Acave Stars
Jupiter analogues and planets of ac2ve stars. RV searches at MPIA Heidelberg Mar2n Kürster with Maren Mohler-Fischer (1) Jupiter analogues: The planet search programme at the ESO CES and HAPRS. IV. The search for Jupiter analogues around solar-type stars, Zechmeister, Kürster, Endl, Lo Curto, Hartman, Nilsson, Henning, Hatzes, Cochran, 2012, A&A accepted (2) A search for planets around ac2ve stars. Mohler-Fischer, Henning, Launhardt, Müller, Guenther (work in progress) (3) The first RV-confirmed planet from HAT-South: HATS-1b: The first transiGng plamet discovered by the HATSOUTH survey, Penev, Bakos, Bayliss, Jordán, Mohler-Fischer, Zhou, Suc, Rabus, Hartman, Mancini, Béky, Zsurby, Buchhave, Henning, Nikolov, Csák, Brahm, Espinosa, Conroy, Noyes, Sasselov, Schmidt, Wright, Tinney, Addison, Lásár, Papp, Sári 2012, in prep. La Silla Observatory, ESO, Chile Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster ad (2): A search for planets around ac2ve stars. Mohler-Fischer, Henning, Launhardt, Müller, Guenther (work in progress) G9V star, v sin i = 20.8 km/s, 57 spectra taken with FEROS @ MPG/ESO 2.2m La Silla Variaon due to stellar ac2vity / surface features Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster ad (3): HATS-1b See yesterday’s talk by Gaspar Bakos RV confirma2on: CORALIE: filled circles àFEROS: open triangles CYCLOPS: filled triangles Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster Two talks you cannot miss: Nadia Kostogryz ``A spectral differenLal characterizaon of low-mass companions´´ This aernoon, but unfortunately cancelled: Florian Rodler ``The return of the mummy: evidence for starlight reflected from the massive hot Jupiter τ Boo b´´ Hot Planets and Cool Stars MPE Garching 13 November 2012 M. -
CCD Astrometry of the Host Star System HD 75289 with Exoplanet
Vol. 15 No. 1 January 1, 2019 Journal of Double Star Observations Page 184 CCD Astrometry of the Host Star System HD 75289 with Exoplanet Charize C. Balignasay1,2, Jocelynn F. Bolosan1,2, Vea Aubrey Bumatay1,2, Pink Mariz G. Felipe1,2, Jeffrey Friedman3, Shanti C. Mohanan1,2, Donald C. Napala1,2, Skecynyth H. Perlas1,2, Vanessa Rhea C. Sao1,2, Evan Sugayama1,2, Lea Stuart3, Sierra Ryden3, Yasmina Vafaie3, Mark Silliman2, Brandi Giese 1, Kakkala Mohanan1, Diana Castaneda4, ,James D. Armstrong5, and Russell Genet6 1. University of Hawaii, Leeward Community College, Oahu, Hawaii 2. Waipahu High School Early College, Oahu, Hawaii 3. Montessori School of Maui, Maui, Hawaii 4. University of Hawaii at Manoa, Oahu, Hawaii 5. University of Hawaii Institute for Astronomy, Maui, Hawaii 6. California Polytechnic State University, San Luis Obispo, California Abstract: Student teams from the Early College Program in Oahu and the Montessori School of the Maui Work and Service Program made remote CCD measurements of a southern neglected double stars system HD 75289 using the Las Cumbres Observatory (LCO) global telescope network. The differential magnitude between primary and secondary was 6.7 requir- ing the use of z’ and Y filters for observation. While the primary is an F9, the exoplanet host- ing secondary is reported to be an M2. Astrometric solutions of the pair indicate a separation of 21.33 arcsec and a position angle of 76.99 degrees. termine theoretical orbits in a shorter time interval. Introduction A group of nine Early College Program students Gravitationally bound stellar objects obey Kepler’s from Waipahu High school located on the island of Oa- Laws of Motion. -
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 ::::::::::::::::::::::::::::::::::::::: -
A Low-Mass Stellar Companion of the Planet Host Star HD 75289
A&A 425, 249–253 (2004) Astronomy DOI: 10.1051/0004-6361:20041009 & c ESO 2004 Astrophysics A low-mass stellar companion of the planet host star HD 75289 M. Mugrauer1, R. Neuhäuser1, T. Mazeh2,J.Alves3, and E. Guenther4 1 Astrophysikalisches Institut, Universität Jena, Schillergäßchen 2-3, 07745 Jena, Germany e-mail: [email protected] 2 Tel Aviv University, Tel Aviv 69978, Israel 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 4 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany Received 2 April 2004 / Accepted 3 June 2004 Abstract. We report on the detection of a new low-mass stellar companion of HD 75289, a G0V star that harbors one known radial-velocity planet (Udry et al. 2000, A&A, 356, 590). Comparing an image from 2MASS with an image we obtained with SofI at the ESO 3.58 m NTT three years later, we detected a co-moving companion located 21.465 ± 0.023 arcsec (621 ± 10 AU at 29 pc) east of HD 75289. A second SofI image taken 10 months later confirmed the common proper motion of HD 75289 B with its host star. The infrared spectrum and colors of the companion are consistent with an M 2 to M 5 main-sequence star at the distance of HD 75289. No further (sub)stellar companion down to H = 19 mag could be detected. With the SofI detection limit we can rule out additional stellar companions beyond 140 AU and substellar companions with masses m ≥ 0.050 M from 400 AU up to 2000 AU. -
2016 Publication Year 2021-04-23T14:32:39Z Acceptance in OA@INAF Age Consistency Between Exoplanet Hosts and Field Stars Title B
Publication Year 2016 Acceptance in OA@INAF 2021-04-23T14:32:39Z Title Age consistency between exoplanet hosts and field stars Authors Bonfanti, A.; Ortolani, S.; NASCIMBENI, VALERIO DOI 10.1051/0004-6361/201527297 Handle http://hdl.handle.net/20.500.12386/30887 Journal ASTRONOMY & ASTROPHYSICS Number 585 A&A 585, A5 (2016) Astronomy DOI: 10.1051/0004-6361/201527297 & c ESO 2015 Astrophysics Age consistency between exoplanet hosts and field stars A. Bonfanti1;2, S. Ortolani1;2, and V. Nascimbeni2 1 Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Received 2 September 2015 / Accepted 3 November 2015 ABSTRACT Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photo- metric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform deriva- tion of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of 0 log RHK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age. -
ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure. -
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. -
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). -
Chemical Abundance Study of Planetary Hosting Stars P
CHEMICAL ABUNDANCE STUDY OF PLANETARY HOSTING STARS P. Rittipruk and Y. W. Kang Department of Astronomy and Space Science Sejong University, Korea Planetary Hosting Stars Metallicity ∝ Probability of Hosting Planets Planetary Hosting Stars Planetary Hosting Stars 0.8 0.6 with planet 0.4 without planet 0.2 0.0 -0.2 -0.4 -0.6 Corr-Coef of [X/H] vs EP -0.8 -1.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) 1.2 c 0.8 0.4 0.0 -0.4 -0.8 Corr-Coef of [X/H] vs T with planet without planet -1.2 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) HD 20794 ‘s Planets Earth to Sun = 1 AU Mass = 0.70 Msun Radius = 0.92 Rsun Distance = 6.06 pc Age = 14±6 Gyr (Bernkopf+2012) = 5.76±0.66 (Gyr)(Pepe+ 2011) bcde M sin i 0.0085 0.0076 0.0105 0.0150 (MJ) (2.7) (2.4) (4.8) (4.7) a(AU) 0.1207 0.2036 0.3499 0.509 P(days) 18.315 40.114 90.309 147.2 HD 47536 ‘s Planets ■ Mass = 0.94 Msun Earth to Sun = 1AU ■ Radius = 23.47 Rsun ■ Distance = 121.36 pc ■ Age = 9.33 Gyr (Silva+2006) HD 47536b HD 47536c** M sin i (MJ) 4.96 6.98 a(AU) 1.61 3.72 P(days) 430 2500 Observation CHIRON Echelle Spectrometer Wavelength cover : 4200 – 8800 A Narrow Slit (R = 120,000) SMART-1.5m at CTIO, La Serena, Chile Observed Spectrum Echelle Spectrum of HD20794 obtained using CHIRON Spectrometers Reduced Spectrum Spectrum of HD20794 after reduction plotted with synthesis spectrum Algorithms Rotational Velocity (v sin i) Determination Reiners & Schmitt (2003) ⁄ sin 0.610 0.062 0.027 0.012 0.004