Target Selection for the SUNS and DEBRIS Surveys for Debris Discs In

Total Page:16

File Type:pdf, Size:1020Kb

Target Selection for the SUNS and DEBRIS Surveys for Debris Discs In Mon. Not. R. Astron. Soc. 000, 1–?? (2009) Printed 19 November 2009 (MN LATEX style file v2.2) Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood N. M. Phillips1, J. S. Greaves2, W. R. F. Dent3, B. C. Matthews4 W. S. Holland3, M. C. Wyatt5, B. Sibthorpe3 1Institute for Astronomy (IfA), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 2School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS 3UK Astronomy Technology Centre (UKATC), Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ 4Herzberg Institute of Astrophysics (HIA), National Research Council of Canada, Victoria, BC, Canada 5Institute of Astronomy (IoA), University of Cambridge, Madingley Road, Cambridge, CB3 0HA Accepted 2009 September 2. Received 2009 July 27; in original form 2009 March 31 ABSTRACT Debris discs – analogous to the Asteroid and Kuiper-Edgeworth belts in the Solar system – have so far mostly been identified and studied in thermal emission shortward of 100 µm. The Herschel space observatory and the SCUBA-2 camera on the James Clerk Maxwell Telescope will allow efficient photometric surveying at 70 to 850 µm, which allow for the detection of cooler discs not yet discovered, and the measurement of disc masses and temperatures when combined with shorter wavelength photometry. The SCUBA-2 Unbiased Nearby Stars (SUNS) survey and the DEBRIS Herschel Open Time Key Project are complimentary legacy surveys observing samples of ∼500 nearby stellar systems. To maximise the legacy value of these surveys, great care has gone into the target selection process. This paper describes the target selection process and presents the target lists of these two surveys. Key words: solar neighbourhood – stars: statistics – circumstellar matter – surveys – stars: distances 1 INTRODUCTION tained simultaneously, and deep images at 450 µm will be proposed to follow-up 850 µm detections. The solar neighbourhood is an ideal testing ground for the study of debris discs and planetary systems. Proximity max- The Disc Emission via a Bias-free Reconnaissance in imises dust mass sensitivity and can allow systems to be spa- the Infrared/Sub-millimetre (DEBRIS) Herschel Open Time tially resolved. Systems near the Sun span a wide range of Key Program will image 446 systems (356 in common with arXiv:0911.3426v1 [astro-ph.SR] 18 Nov 2009 stellar parameters e.g., mass, age, metallicity, multiplicity. SUNS) at 110 and 170 µm using the PACS (Photodetec- Whilst determining these parameters may not be easy, the tor Array Camera and Spectrometer; Poglitsch et al. 2008) diversity included in volume limited samples makes them instrument, with follow-up of around 100 systems at 250, ideal for legacy surveys where one may wish to investigate 350 and 500 µm using the SPIRE (Spectral and Photo- trends as a function of many system parameters. metric Imaging Receiver; Griffin et al. 2008) instrument. This paper presents five all-sky volume limited samples This survey is primarily driven by the 110 µm band, which of nearby stellar systems with main-sequence primaries of has the highest dust mass sensitivity for cold discs such spectral type A,F,G,K,M. These form the basis of the target as the Kuiper-Edgeworth belt of our Solar System. The lists of two complimentary surveys for debris discs using the intended flux RMS at 110 µm is 1.2mJy/beam, which is SCUBA-2 (Submillimetre Common User Bolometer Array twice the predicted extragalactic confusion limit. 170 µm 2; Holland et al. 2003; Audley et al. 2004) camera on the images are taken simultaneously with a predicted RMS of James Clerk Maxwell Telescope (JCMT), and the Herschel 1.7mJy/beam, equal to the predicted extragalactic confu- space observatory (Pilbratt 2008). sion limit in this band. The SCUBA-2 Unbiased Nearby Stars survey (SUNS; The primary goals of these surveys are statistical: In Matthews et al. 2007) is a large flux-limited survey of 500 general how do debris disc properties vary with stellar mass, systems at 850 µm. The target flux RMS is 0.7mJy/beam, age, metallicity, system morphology (multiplicity, compo- equal to the extragalactic confusion limit of the JCMT at nent masses, separations), presence of planets etc. To be able 850 µm. Shallow 450 µm images of varying depth will be ob- to answer so many questions, and to minimise the risk of un- c 2009 RAS 2 N. M. Phillips et al. foreseen selection effects, large samples and simple, clearly -2 A defined target selection criteria are required. Volume limited 0 F G samples satisfy these requirements, and as well as maximis- K 2 M ing the proximity of the targets, the stars nearest the Sun isochrones are very widely studied. For example, nearby stars are the 4 main targets of radial velocity, astrometry and direct imag- 6 ing planet searches. The majority of SUNS and DEBRIS tar- V 8 gets also have photometry at 24 and 70 µm from the MIPS M (Multiband Imaging Photometer and Spectrometer) instru- 10 ment on the Spitzer space telescope, which ceased operation 12 at the end of March 2009. This large spectral coverage, from 24 to 850 µm for over 300 systems will be an incredible re- 14 source for detailed spectral energy distribution modelling of 16 systems with debris discs. 18 Given that we are considering the closest systems to 0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 2.2 the Sun, substantial effort was required to compile the sam- B - V ples presented here. Late M-type stars within 10 pc are still Figure 1. Johnson B,V absolute colour-magnitude diagram for being discovered (e.g. Henry et al. 2006), and complete ho- system primaries. Overlaid are [Fe/H] = 0.0, [α/Fe] = 0.0 mogeneous datasets covering the spectral type and distance isochrones from the Dartmouth Stellar Evolution Database (Dot- ranges we consider do not exist. We have tried to make our ter et al. 2008) with ages of 0.25, 0.5, 1, 2, 4, 8 Gyr (with turn-offs sample selection using the most complete and accurate data going from left to right). The photometry is mostly converted available at the time of the DEBRIS proposal submission in from Tycho photometry (Tycho-2 or TDSC) using transforma- October 2007. tions for unreddened main-sequence stars. For most M-type tar- gets Johnson B,V photometry from various sources was used (see text). Note that primaries in some close binaries are not individ- ually resolved in this photometry. 2 SELECTION CRITERIA Our systems all have primaries (defined here as the compo- in age and composition. The fact that several interesting ob- nent with the brightest visible magnitude) which we believe jects (e.g. with known IR excess, or planets) are considered are main-sequence (i.e. hydrogen burning) stars. The sample here as secondaries does not affect the statistical usefulness is split into 5 volume limited subsamples based on spectral of the sample, although it has the disadvantage that such type: A, F, G, K, M. In the rest of this paper we use the objects may not be observed by these surveys (see below). term “X-type system” to mean “system with X-type pri- The number of systems in each subsample was deter- mary”. Using separate subsamples is necessary due to the mined by the selection criteria for SUNS, which required steep nature of the stellar mass function, which for example 100 systems in each subsample in the declination range means that a single volume limited sample would contain −40◦ <δ < +80◦. Hence the all-sky samples presented over 100 times as many M-type systems as A-type systems. here contain roughly 123 (100×2/(sin 80◦ +sin 40◦)) systems The choice of using spectral types to split the sample, rather each. The SUNS sample sizes were chosen to allow detection than stellar mass, is purely practical as, with the exception rates for various subsets e.g. planet hosts to be distinguished of certain binary systems, stellar masses cannot be directly (see Matthews et al. 2007). determined observationally. Using spectral types does how- The DEBRIS target list comprises the nearest systems ever have the effect that the subsamples cover quite different presented here (all-sky), subject to a cut in the predicted ranges in logarithmic mass space. 110 µm cirrus confusion level towards each system. The con- The early type, upper mass, limit of A0 is chosen as fusion prediction was taken from the Herschel Confusion stars of earlier type are too rare in the solar neighbourhood Noise Estimator (HCNE), which is part of the Herschel to build a suitably large sample. A conservative late type Observation Planning Tool (HSPOT). Systems with total limit of M7.0 was chosen to avoid the inclusion of any brown predicted confusion for point-source detections greater than dwarfs, and also to improve the completeness of the M-type 1.2mJy/beam, corresponding to twice the predicted extra- sample. M-type stars span the largest log M range of any of galactic confusion limit, were rejected. To maximise the our spectral classes, so making a cut at M7.0 will not restrict number of systems observed, DEBRIS will not image sec- the statistical usefulness of the sample. ondary components in systems where they will not fit in the We do not discriminate against multiple star systems, PACS point-source field of view (FoV) (150′′ × 50′′ with un- and they are included naturally within the volume limits. We constrained orientation) with the primary. This will affect consider common proper motion stars (with compatible par- between 20 and 49 systems depending on the actual field allax where available) as members of the same system, with orientations.
Recommended publications
  • Université De Montréal Relevé Polarimétrique D'étoiles Candidates
    Université de Montréal Relevé polarimétrique d’étoiles candidates pour des disques de débris par Amélie Simon Département de physique Faculté des arts et des sciences Mémoire présenté à la Faculté des études supérieures en vue de l’obtention du grade de Maître ès sciences (M.Sc.) en physique Août, 2010 c Amélie Simon, 2010 Université de Montréal Faculté des études supérieures Ce mémoire intitulé: Relevé polarimétrique d’étoiles candidates pour des disques de débris présenté par: Amélie Simon a été évalué par un jury composé des personnes suivantes: Serge Demers, président-rapporteur Pierre Bastien, directeur de recherche Gilles Fontaine, membre du jury Mémoire accepté le: Sommaire Le relevé DEBRIS est effectué par le télescope spatial Herschel. Il permet d’échantillonner les disques de débris autour d’étoiles de l’environnement solaire. Dans la première partie de ce mémoire, un relevé polarimétrique de 108 étoiles des candidates de DEBRIS est présenté. Utilisant le polarimètre de l’Observatoire du Mont-Mégantic, des observations ont été effec- tuées afin de détecter la polarisation due à la présence de disques de débris. En raison d’un faible taux de détection d’étoiles polarisées, une analyse statistique a été réalisée dans le but de comparer la polarisation d’étoiles possédant un excès dans l’infrarouge et la polarisation de celles n’en possédant pas. Utilisant la théorie de diffusion de Mie, un modèle a été construit afin de prédire la polarisation due à un disque de débris. Les résultats du modèle sont cohérents avec les observations. La deuxième partie de ce mémoire présente des tests optiques du polarimètre POL-2, construit à l’Université de Montréal.
    [Show full text]
  • CARMENES Input Catalogue of M Dwarfs IV. New Rotation Periods from Photometric Time Series
    Astronomy & Astrophysics manuscript no. pk30 c ESO 2018 October 9, 2018 CARMENES input catalogue of M dwarfs IV. New rotation periods from photometric time series E. D´ıezAlonso1;2;3, J. A. Caballero4, D. Montes1, F. J. de Cos Juez2, S. Dreizler5, F. Dubois6, S. V. Jeffers5, S. Lalitha5, R. Naves7, A. Reiners5, I. Ribas8;9, S. Vanaverbeke10;6, P. J. Amado11, V. J. S. B´ejar12;13, M. Cort´es-Contreras4, E. Herrero8;9, D. Hidalgo12;13;1, M. K¨urster14, L. Logie6, A. Quirrenbach15, S. Rau6, W. Seifert15, P. Sch¨ofer5, and L. Tal-Or5;16 1 Departamento de Astrof´ısicay Ciencias de la Atm´osfera, Facultad de Ciencias F´ısicas,Universidad Complutense de Madrid, E-280140 Madrid, Spain; e-mail: [email protected] 2 Departamento de Explotaci´ony Prospecci´onde Minas, Escuela de Minas, Energ´ıay Materiales, Universidad de Oviedo, E-33003 Oviedo, Asturias, Spain 3 Observatorio Astron´omicoCarda, Villaviciosa, Asturias, Spain (MPC Z76) 4 Centro de Astrobiolog´ıa(CSIC-INTA), Campus ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Ca~nada,Madrid, Spain 5 Institut f¨ur Astrophysik, Georg-August-Universit¨at G¨ottingen, Friedrich-Hund-Platz 1, D-37077 G¨ottingen, Germany 6 AstroLAB IRIS, Provinciaal Domein \De Palingbeek", Verbrandemolenstraat 5, B-8902 Zillebeke, Ieper, Belgium 7 Observatorio Astron´omicoNaves, Cabrils, Barcelona, Spain (MPC 213) 8 Institut de Ci`enciesde l'Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, E-08193 Bellaterra, Barcelona, Spain 9 Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain 10
    [Show full text]
  • Spektralanalyse Ausgewählter Carmenes Daten
    Master’s Thesis Spektralanalyse ausgewählter Carmenes Daten Spectroscopic analysis of Carmenes sample prepared by Andre Lamert from Merkers at the Institut für Astrophysik, Göttingen Thesis period: 1st April 2014 until 10th September 2014 First referee: Dr. Sandra Jeffers Second referee: Prof. Dr. Ansgar Reiners Abstract In the last years the number of detected exoplanets increased rapidly. Upcoming projects like CARMENES, which is planned to find terrestrial planets in the hab- itable zone of M-dwarfs, will close the gap of Earth-mass planets in the exoplanet distribution. This thesis investigates the spectral type, radial velocity and magnetic activity of candidate M-dwarfs for the CARMENES project input catalog CARMENCITA.It focuses on the determination of spectral M-type stars. Based on calibration func- tions of the code THE HAMMER, different atomic and molecular lines and bands are used to calculate spectral indices. With the aim of increasing the determination accuracy, I have written an algorithm which uses only few, but very sensitive indices. These are particular dominant for M-type stars. Additionally, the Hα line is used to determine the magnetic activity. To determine the spectral type, the radial velocity and an activity indicator I use 900 high-resolution spectra taken from 364 different stars of the input catalog. 348 of these spectra were provided as raw data from the CAFE spectrograph. I use the IDL-Package REDUCE for reduction and add a new flux extraction procedure and a modified order definition procedure to increase the extracted wavelength range and the quality of the extracted flux values. The writ- ten fast working spectral typing algorithm calculates quite accurate spectral types for high-resolution spectra, since the results of this typing confirm former results collected in CARMENCITA using low-resolution spectroscopy.
    [Show full text]
  • Li Abundances in F Stars: Planets, Rotation, and Galactic Evolution,
    A&A 576, A69 (2015) Astronomy DOI: 10.1051/0004-6361/201425433 & c ESO 2015 Astrophysics Li abundances in F stars: planets, rotation, and Galactic evolution, E. Delgado Mena1,2, S. Bertrán de Lis3,4, V. Zh. Adibekyan1,2,S.G.Sousa1,2,P.Figueira1,2, A. Mortier6, J. I. González Hernández3,4,M.Tsantaki1,2,3, G. Israelian3,4, and N. C. Santos1,2,5 1 Centro de Astrofisica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 3 Instituto de Astrofísica de Canarias, C/via Lactea, s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 5 Departamento de Física e Astronomía, Faculdade de Ciências, Universidade do Porto, Portugal 6 SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK Received 28 November 2014 / Accepted 14 December 2014 ABSTRACT Aims. We aim, on the one hand, to study the possible differences of Li abundances between planet hosts and stars without detected planets at effective temperatures hotter than the Sun, and on the other hand, to explore the Li dip and the evolution of Li at high metallicities. Methods. We present lithium abundances for 353 main sequence stars with and without planets in the Teff range 5900–7200 K. We observed 265 stars of our sample with HARPS spectrograph during different planets search programs. We observed the remaining targets with a variety of high-resolution spectrographs.
    [Show full text]
  • Download This Article in PDF Format
    A&A 583, A85 (2015) Astronomy DOI: 10.1051/0004-6361/201526795 & c ESO 2015 Astrophysics Reaching the boundary between stellar kinematic groups and very wide binaries III. Sixteen new stars and eight new wide systems in the β Pictoris moving group F. J. Alonso-Floriano1, J. A. Caballero2, M. Cortés-Contreras1,E.Solano2,3, and D. Montes1 1 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain 3 Spanish Virtual Observatory, ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain Received 19 June 2015 / Accepted 8 August 2015 ABSTRACT Aims. We look for common proper motion companions to stars of the nearby young β Pictoris moving group. Methods. First, we compiled a list of 185 β Pictoris members and candidate members from 35 representative works. Next, we used the Aladin and STILTS virtual observatory tools and the PPMXL proper motion and Washington Double Star catalogues to look for companion candidates. The resulting potential companions were subjects of a dedicated astro-photometric follow-up using public data from all-sky surveys. After discarding 67 sources by proper motion and 31 by colour-magnitude diagrams, we obtained a final list of 36 common proper motion systems. The binding energy of two of them is perhaps too small to be considered physically bound. Results. Of the 36 pairs and multiple systems, eight are new, 16 have only one stellar component previously classified as a β Pictoris member, and three have secondaries at or below the hydrogen-burning limit.
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • HOW to CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, and RADIUS Andrew W
    The Astrophysical Journal, 804:64 (38pp), 2015 May 1 doi:10.1088/0004-637X/804/1/64 © 2015. The American Astronomical Society. All rights reserved. HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS Andrew W. Mann1,2,8,9, Gregory A. Feiden3, Eric Gaidos4,5,10, Tabetha Boyajian6, and Kaspar von Braun7 1 University of Texas at Austin, USA; [email protected] 2 Institute for Astrophysical Research, Boston University, USA 3 Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20, Uppsala, Sweden 4 Department of Geology and Geophysics, University of Hawaii at Manoa, Honolulu, HI 96822, USA 5 Max Planck Institut für Astronomie, Heidelberg, Germany 6 Department of Astronomy, Yale University, New Haven, CT 06511, USA 7 Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ, USA Received 2015 January 6; accepted 2015 February 26; published 2015 May 4 ABSTRACT Precise and accurate parameters for late-type (late K and M) dwarf stars are important for characterization of any orbiting planets, but such determinations have been hampered by these stars’ complex spectra and dissimilarity to the Sun. We exploit an empirically calibrated method to estimate spectroscopic effective temperature (Teff) and the Stefan–Boltzmann law to determine radii of 183 nearby K7–M7 single stars with a precision of 2%–5%. Our improved stellar parameters enable us to develop model-independent relations between Teff or absolute magnitude and radius, as well as between color and Teff. The derived Teff–radius relation depends strongly on [Fe/H],as predicted by theory.
    [Show full text]
  • Arxiv:0705.4290V2 [Astro-Ph] 23 Aug 2007
    DRAFT VERSION NOVEMBER 11, 2018 Preprint typeset using LATEX style emulateapj v. 08/13/06 THE GEMINI DEEP PLANET SURVEY – GDPS∗ DAVID LAFRENIÈREA,RENÉ DOYONA , CHRISTIAN MAROISB ,DANIEL NADEAUA, BEN R. OPPENHEIMERC,PATRICK F. ROCHED , FRANÇOIS RIGAUTE, JAMES R. GRAHAMF ,RAY JAYAWARDHANAG,DOUG JOHNSTONEH,PAUL G. KALASF ,BRUCE MACINTOSHB, RENÉ RACINEA Draft version November 11, 2018 ABSTRACT We present the results of the Gemini Deep Planet Survey, a near-infrared adaptive optics search for giant planets and brown dwarfs around nearby young stars. The observations were obtained with the Altair adaptive optics system at the Gemini North telescope and angular differential imaging was used to suppress the speckle noise of the central star. Detection limits for the 85 stars observed are presented, along with a list of all faint point sources detected around them. Typically, the observations are sensitive to angular separations beyond 0.5′′ with 5σ contrast sensitivities in magnitude difference at 1.6 µm of 9.5 at 0.5′′, 12.9 at 1′′, 15.0 at 2′′, and 16.5 at 5′′. For the typical target of the survey, a 100 Myr old K0 star located 22 pc from the Sun, the observations are sensitive enough to detect planets more massive than 2 MJup with a projected separation in the range 40–200 AU. Depending on the age, spectral type, and distance of the target stars, the detection limit can be as low as 1 MJup. Second epoch observations of 48 stars with candidates (out of 54) have confirmed that all candidates are∼ unrelated background stars. A detailed statistical analysis of the survey results, yielding upper limits on the fractions of stars with giant planet or low mass brown dwarf companions, is presented.
    [Show full text]
  • INAUGURAL–DISSERTATION Zur Erlangung Der Doktorwürde Der
    INAUGURAL{DISSERTATION zur Erlangung der Doktorwurde¨ der Naturwissentschaftlich{Mathematischen Gesamtfakult¨at der Ruprecht{Karls{Universit¨at Heidelberg vorgelegt von Dipl.{Phys. Agn`es D.F. Metanomski aus Paris Tag der mundl.¨ Prufung:¨ 22. April 1998 Optical study of F, G and K stars in the ROSAT All-Sky Survey Gutachter: Herr Prof. Dr. Joachim Krautter Herr Prof. Dr. Reiner Wehrse Zusammenfassung Ich untersuche eine Stichprobe von 107 Sudhimmels-Sternen¨ von Spektraltyp A bis K. Diese Sterne sind als die optischen Gegenstuc¨ ke zu R¨ontgen-Quellen, die der ROSAT Satellit w¨ahrend seines All-Sky Survey (RASS) entdeckte, iden- tifiziert wurden. Die Untersuchung wird mit Hilfe optischen Beobachtungen, sowohl photometrischer als auch spektroskopischer, durchgefuhrt.¨ Verschiedene Parameter werden fur¨ die untersuchten Objekte bestimmt, wie z.B. Spektraltyp und Leuchtkraftklasse, absolute Helligkeit, Entfernung, Radialgeschwindigkeit, projezierte Rotationsgeschwindigkeit, Effektivtemperatur, Lithium H¨aufigkeit. Ich vergleiche die R¨ontgen-Parameter meiner Stichproben-Sterne mit denen aus einer ahnlic¨ hen Stichprobe von Sternen, die vom Einstein Observatory w¨ahrend dessen Medium Sensitivity Survey (EMSS) entdeckt wurden. Ich suche auch nach Korrelationen zwischen verschiedenen Parametern, die fur¨ meine Stichproben- Sterne bestimmt wurden und vergleiche die Ergebnisse mit denen, die fur¨ die EMSS Stichprobe erhalten wurden, sowie mit den Ergebnissne anderer, fruherer¨ Studien. Abstract I analyze a sample of 107 southern stars of spectral types A to K, which were identified as the optical counterparts of X-ray sources detected by ROSAT during its All-Sky Survey. The study is conducted using optical observations, photometric as well as spectroscopic (high-resolution). Various parameters are determined for the sample objects, mainly spectral types and luminosity classes, absolute magnitudes, distances, radial velocities, projected rotational velocities, effective temperatures, Lithium abundances.
    [Show full text]
  • Ioptron CEM40 Center-Balanced Equatorial Mount
    iOptron®CEM40 Center-Balanced Equatorial Mount Instruction Manual Product CEM40 (#7400A series) and CEM40EC (#7400ECA series, as shown) Please read the included CEM40 Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper operation will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while using a telescope. 2 Table of Contents Table of Contents ........................................................................................................................................ 3 1. CEM40 Introduction ............................................................................................................................... 5 2. CEM40 Overview ................................................................................................................................... 6 2.1. Parts List .........................................................................................................................................
    [Show full text]
  • To Trappist-1 RAIR Golaith Ship
    Mission Profile Navigator 10:07 AM - 12/2/2018 page 1 of 10 Interstellar Mission Profile for SGC Navigator - Report - Printable ver 4.3 Start: omicron 2 40 Eri (Star Trek Vulcan home star) (HD Dest: Trappist-1 2Mass J23062928-0502285 in Aquarii [X -9.150] [Y - 26965) (Keid) (HIP 19849) in Eridani [X 14.437] [Y - 38.296] [Z -3.452] 7.102] [Z -2.167] Rendezvous Earth date arrival: Tuesday, December 8, 2420 Ship Type: RAIR Golaith Ship date arrival: Tuesday, January 8, 2419 Type 2: Rendezvous with a coasting leg ( Top speed is reached before mid-point ) Start Position: Start Date: 2-December-2018 Star System omicron 2 40 Eri (Star Trek Vulcan home star) (HD 26965) (Keid) Earth Polar Primary Star: (HIP 19849) RA hours: inactive Type: K0 V Planets: 1e RA min: inactive Binary: B, C, b RA sec: inactive Type: M4.5V, DA2.9 dec. degrees inactive Rank from Earth: 69 Abs Mag.: 5.915956445 dec. minutes inactive dec. seconds inactive Galactic SGC Stats Distance l/y Sector X Y Z Earth to Start Position: 16.2346953 Kappa 14.43696547 -7.10221947 -2.16744969 Destination Arrival Date (Earth time): 8-December-2420 Star System Earth Polar Trappist-1 2Mass J23062928-0502285 Primary Star: RA hours: inactive Type: M8V Planets 4, 3e RA min: inactive Binary: B C RA sec: inactive Type: 0 dec. degrees inactive Rank from Earth 679 Abs Mag.: 18.4 dec. minutes inactive Course Headings SGC decimal dec. seconds inactive RA: (0 <360) 232.905748 dec: (0-180) 91.8817176 Galactic SGC Sector X Y Z Destination: Apparent position | Start of Mission Omega -9.09279603 -38.2336637 -3.46695345 Destination: Real position | Start of Mission Omega -9.09548281 -38.2366036 -3.46626331 Destination: Real position | End of Mission Omega -9.14988933 -38.2961361 -3.45228825 Shifts in distances of Destination Distance l/y X Y Z Change in Apparent vs.
    [Show full text]
  • The HARPS Search for Earth-Like Planets in the Habitable Zone I
    A&A 534, A58 (2011) Astronomy DOI: 10.1051/0004-6361/201117055 & c ESO 2011 Astrophysics The HARPS search for Earth-like planets in the habitable zone I. Very low-mass planets around HD 20794, HD 85512, and HD 192310, F. Pepe1,C.Lovis1, D. Ségransan1,W.Benz2, F. Bouchy3,4, X. Dumusque1, M. Mayor1,D.Queloz1, N. C. Santos5,6,andS.Udry1 1 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Versoix, Switzerland e-mail: [email protected] 2 Physikalisches Institut Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 3 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France 4 Observatoire de Haute-Provence/CNRS, 04870 St. Michel l’Observatoire, France 5 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal Received 8 April 2011 / Accepted 15 August 2011 ABSTRACT Context. In 2009 we started an intense radial-velocity monitoring of a few nearby, slowly-rotating and quiet solar-type stars within the dedicated HARPS-Upgrade GTO program. Aims. The goal of this campaign is to gather very-precise radial-velocity data with high cadence and continuity to detect tiny signatures of very-low-mass stars that are potentially present in the habitable zone of their parent stars. Methods. Ten stars were selected among the most stable stars of the original HARPS high-precision program that are uniformly spread in hour angle, such that three to four of them are observable at any time of the year.
    [Show full text]