DOCSLIB.ORG

Observed Stellar Spectra As Templates for Gaia

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Observed Stellar Spectra As Templates for Gaia Universit`adegli Studi di Padova DIPARTIMENTO DI ASTRONOMIA Dottorato di Ricerca in Astronomia XXIII ciclo Observed Stellar Spectra As Templates For Gaia Coordinatore: Prof. Giampaolo Piotto Supervisori: Prof. Antonella Vallenari Prof. Ulisse Munari Dottoranda: Tenay Saguner 2 31 Gennaio 2011 To My Family & To Prof. I. Ethem Derman Contents Index i Figures List x Tables List x 1 Introduction 1 2 The Gaia Mission 3 2.1 OverviewOfTheGaiaMission . 5 2.1.1 MeasurementPrinciples . 5 2.1.2 ObservationPrinciple . 7 2.1.3 Instruments And Performances . 7 2.1.4 TheAccuracyOfGaiaMeasurements . 10 2.2 The Classification of Gaia objects . ..... 15 2.3 TheFinalCatalogue ............................... 16 2.4 TheImportanceoftrainingdata . 16 3 The Red Clump Stars 19 3.1 The Structure And The Evolution Of the Red Clump . 19 3.2 RedClumpStarsInTheLiterature. 21 4 Target Selection and The Input Catalog 23 4.1 TargetSelectionCriteria. 23 i ii 5 Observations And Data Reduction 27 5.1 The B&C Spectrograph At The 1.22 meter TelescopeInAsiago ............................... 27 5.2 Softwares To Use The 1.22 meter Telescope . ..... 29 5.3 DataAcquisitionAtTheTelescope . 29 5.4 Selecting The Wavelength Interval To Observe . ....... 31 5.5 DataReduction.................................. 35 5.5.1 WavelengthCalibration . 38 5.5.2 ContinuumNormalization . 38 5.5.3 HeliocentricCorrection . 41 6 Measuring Radial Velocities 45 6.1 Cross-CorrelationTechnique. 45 6.2 Accuracy Tests With IAU Radial Velocity Standards . ........ 48 6.3 ExtendedTestsOnRadialVelocities . ..... 52 7 Atmospheric Parameter Determonation 55 7.1 χ2 Technique ................................... 55 7.1.1 TheSyntheticspectralLibrary . 56 7.1.2 The χ2 Methods ............................. 58 7.2 Accuracy Tests With Red Clump Stars In the Literature . ........ 59 7.3 Comparison With Photometric Temperatures . ...... 65 8 Repeated Observations Of Target Stars 71 8.1 The Final Data Quality Control From Repeated Observations........ 71 8.2 RadialVelocities ................................ 72 8.3 AtmosphericParameters. 74 9 Constructing The Output Catalog 75 9.1 Determination Of Spectro-photometric Distances . ......... 75 9.1.1 LuminosityClassII ........................... 79 9.2 Determination Of The Galactocentric Galactic Coordinates ......... 80 iii 9.3 Determination Of The Galactic Velocities . ....... 80 9.3.1 The Uncertainties In The Velocity Components . ..... 83 9.4 The Output Catalog Of 305 Red Clump Stars . 84 10 The Catalog Stars As Solar Vicinity Tracers 101 10.1 Atmospheric Parameters Of Red Clump Stars As A Function Of Spectral TypeandMetallicity...............................102 10.2TheMilkyWay..................................103 10.2.1 Milky Way Kinematics Traced By Red Clump Giants . 104 10.2.2 MovingGroups..............................106 10.2.3 StarKinematics .............................109 10.2.4 ToomreDiagram . .111 10.2.5 LocalStandardOfRest . .112 10.2.6 Milky Way Structure Traced By Red Clump Giants . 115 10.3 Age-MetallicityRelation . 115 Bibliography 121 iv List of Figures 2.1 An artistic expression of Gaia satellite. ......... 7 2.2 TheGaiascanninglaw.............................. 8 2.3 The sky coverage of Gaia after 5 years mission time . ....... 8 2.4 TheFocalPlaneOfGaia ............................ 9 2.5 Gaia’sspinaxisandfielsofviews . 10 2.6 Example of spectra of A, G, M supergiants in the Gaia range ........ 12 2.7 Correlation between the 8620 A˚ DIBandthereddening . 13 3.1 Hertzsprung-Russell Diagram of 41704 single stars from Hipparcos Catalog 20 4.1 Aitoff projection in Equatorial coordinates of our target stars. The thick linerepresentstheGalacticequator. 24 4.2 Aitoff projection in Galactic coordinates of our target stars. ......... 24 4.3 Distribution in V and K magnitudes and spectral type of our target stars and the other surveys of Red Clump stars in the literature: Takeda et al. (2008), Hekker & Melendez (2007), Mishenina et al. (2006). ........ 25 4.4 The comparison of the properties for Red Clump stars in Valentini & Munari (2010) spectroscopic survey and in this study. ...... 26 5.1 Schematic Description For The Instruments . ....... 27 5.2 Wavelength range of survey stars . 32 5.3 Trial wavelength range for performance tests. ......... 32 5.4 Comparison of atmospheric parameters from first wavelength range . 36 5.5 Comparison of atmospheric parameters from second wavelength range . 36 5.6 Re-identifiedFe-ArCalibrationLamp . 39 v vi 5.7 Re-identified Fe-Ar Calibration Lamp Continued . ...... 40 6.1 Gaussian fit to the maximum of the correlation peak . ....... 47 6.2 Object and the template spectra for cross-correlation at FXCOR ...... 47 6.3 Radial velocity determination tests on IAU RV standards .......... 49 6.4 Comparison of radial velocities for IAU RV standards . ......... 50 6.5 Comparison of radial velocities with Pulkovo compilation of radial velocities 52 7.1 The χ2 interface that we used for atmospheric parameter calculation . 56 7.2 The χ2 interface that we used for atmospheric parameter calculation . 57 7.3 The χ2 interface that we used for atmospheric parameter calculation . 57 7.4 Differences between atmospheric parameters derived from χ2 and those from literature. Empty squares are the data from Takeda et al. (2008),filled triangles Hekker & Melendez (1997) and the crosses from Soubiran (2005). 64 7.5 Temperatures from V K ...................... 67 tycho − 2Mass 7.6 Temperatures from B V ....................... 67 Tycho − Tycho 7.7 Temperatures from (J K)........................... 68 − 7.8 TemperaturesfromMcWilliam . 69 8.1 Used night sky lines for data quality control from FWHM of the lines. 72 8.2 Comparison of the differences in atmospheric parameters with FWHM cut . 73 8.3 Distribution of the differences in radial velocities for repeated observations of60RedClumpstars............................... 73 8.4 Distribution of the differences in atmospheric parameters for repeated ob- servationsof60RedClumpstars.. 74 8.5 The differences in effective temperature, gravity and metallicity against same values from first epoch observations for repeated observations. 74 9.1 The distribution of uncertainty of distances σπ/π from Hipparcos New Re- duction (2007) for target stars. 75 9.2 The intrinsic absolute magnitude in Johnson V band calibration by Keenan & Barnbaum (1999) as a function of spectral type for class IIIb giants. 76 9.3 Thecomparisonofdistances. 78 vii 9.4 The comparison of distances derived with absolute V band magnitude cal- ibration by Keenan & Barnbaum and with absolute K band magnitude calibrationbyAlves. ............................... 78 9.5 Relation between surface gravity and orbital energy . .......... 79 9.6 The derived Galactic positions (X,Y,Z) for target stars as seen from the vantage point of North Galactic Pole (α = 12h49s,δ = 27◦.4). The red circle represents 0.2kpc field and the green circle represents 0.4kpc field. 81 9.7 The definition of Galactic velocities (U,V,W ).................. 81 9.8 The derived Galactic velocities (U,V,W ) for target stars. 83 9.9 The distribution of the uncertainties of the (U,V,W ) velocity components. 84 10.1 Positional properties of observed Red Clump stars . ..........101 10.2 Teff , logg, [M/H] and U,V,W space velocities as a function of spectral type. 102 10.3 Teff - log g plane plotted as a function of spectral type. 103 10.4 Teff - log g plane plotted as a function of the metallicity. 103 10.5 The (U,V,W ) space velocity distribution of the 245 Red Clump stars. 105 10.6 The (U,V,W ) space velocities as a function of metallicity [M/H]. 106 10.7 The (U,V,W ) space velocities as a function of metallicity [M/H]. 106 10.8 The (U,V,W ) space velocities as a function of gravity (log g). ........107 10.9 The (U,V,W ) space velocities as a function of spectral type.. 107 10.10The relative U velocity and average star counts to define streams, taken fromSkuljanetal.1999..............................108 10.11The relative U velocity and average star counts for defining streams traced by245RedClumpstars .............................109 10.12Density field in the Vrot-[Fe/H] plane from Antoja et al. 2008 . 109 10.13The U-V space velocities for different metallicities . ............111 10.14Toomre diagram of 245 observed Red Clump stars. The dotted lines show a constant space velocity with respect to LST in steps of 50 kms−1 . 112 10.15The distribution of the Galactic space velocities calculated for 245 observed RedClumpstars..................................114 10.16The distribution of the Galactic space velocities calculated for high proba- bilitythindiscstars. ............................... 115 viii 10.17The distance versus Galactic scale height as a function of metallicity for observedRedClumpgiants.. .116 10.18Comparison of the Galactic (X,Y,X) coordinates with Valentini & Munari (2010)........................................117 10.19Age-Metallicity relation of target stars. ...........118 10.20(B V ) colours by Tycho-2 and by Girardi’s Param are compared (left − panel). logg values derived by χ2 fitting and derived from Girardi’s Param Evolutionary tracks are compared (right panel). .......119 10.21The Radii-Mass and Radii-logg plot for target stars. ..........120 List of Tables 2.1 Expected numbers of specific objects observed by Gaia . ......... 5 2.2 Main differences between Gaia and Hipparcos missions . ......... 6 2.3 StandarderrorsonGaiaparallaxes . ..... 10 2.4 Standard errors on Gaia spectrophotometry . ....... 11 2.5 Standard Errors on Gaia Radial Velocities . ....... 14 2.6 Expected precision
Load more

Recommended publications
  • Radial Velocity Variations in Red Giant Stars: Pulsations, Spots and Planets
    RADIAL VELOCITY VARIATIONS IN RED GIANT STARS: PULSATIONS, SPOTS AND PLANETS RADIAL VELOCITY VARIATIONS IN RED GIANT STARS: PULSATIONS, SPOTS AND PLANETS Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van de Rector Magnificus prof. mr. P. F. van der Heijden, volgens besluit van het College voor Promoties te verdedigen op 18 september 2007 klokke 13:45 uur door Saskia Hekker geboren te Heeze in 1978 Promotiecommissie Promotor: Prof. dr. A. Quirrenbach Sterrewacht Leiden Landessternwarte Heidelberg Promotor: Prof. dr. C. Aerts Katholieke Universiteit Leuven Radboud Universiteit Nijmegen Co-promotor: Dr. I. A. G. Snellen Sterrewacht Leiden Overige leden: Prof. dr. E. F. van Dishoeck Sterrewacht Leiden Prof. dr. K. H. Kuijken Sterrewacht Leiden Prof. dr. P. T. de Zeeuw Sterrewacht Leiden Dr. M. Hogerheijde Sterrewacht Leiden Dr. J. Lub Sterrewacht Leiden Dit proefschrift is tot stand gekomen met steun van No pain, no gain Contents 1 Introduction 1 1.1 Redgiantstars................................... 2 1.2 Observations ................................... 4 1.2.1 Iodinecell................................. 4 1.2.2 SimultaneousThAr............................ 4 1.3 Oscillations .................................... 5 1.3.1 Excitationmechanism .......................... 9 1.3.2 Asymptoticrelation. 10 1.3.3 Scalingrelations ............................. 10 1.4 Starspots...................................... 11 1.5 Sub-stellarcompanions . ... 12 1.6 Why can oscillations, spots and companions be observed as
    [Show full text]
  • Precise Radial Velocities of Giant Stars. III. Spectroscopic Stellar Parameters
    Astronomy & Astrophysics manuscript no. finalversionlcor6nov1 c ESO 2018 October 28, 2018 Precise radial velocities of giant stars. III.⋆ Spectroscopic stellar parameters S. Hekker1 and J. Mel´endez2 1 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands 2 Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia Received ¡date¿; accepted ¡date¿ ABSTRACT Context. A radial velocity survey of about 380 G and K giant stars is ongoing at Lick observatory. For each star we have a high signal to noise ratio template spectrum, which we use to determine spectroscopic stellar parameters. Aims. The aim of this paper is to present spectroscopic stellar parameters, i.e. effective temperature, surface gravity, metallicity and rotational velocity for our sample of G and K giant stars. Methods. Effective temperatures, surface gravities and metallicities are determined from the equivalent width of iron lines, by imposing exci- tation and ionisation equilibrium through stellar atmosphere models. Rotational velocities are determined from the full width at half maximum (FWHM) of moderate spectral lines. A calibration between the FWHM and total broadening (rotational velocity and macro turbulence) is ob- tained from stars in common between our sample and the sample from Gray (1989). Macro turbulence is determined from the macro turbulence vs. spectral type relations from Gray (2005). Results. The metallicity we derive is essentially equal to the literature values, while the effective temperature and surface gravity are slightly higher by 56 K and 0.15 dex, respectively. A method comparison is performed with 72 giants in common with Luck and Heiter (2007), which shows that both methods give similar results.
    [Show full text]
  • Exploring Milky Way Halo Substructures with Large-Area Sky Surveys
    EXPLORING MILKY WAY HALO SUBSTRUCTURES WITH LARGE-AREA SKY SURVEYS A Dissertation by TING LI Submitted to the Office of Graduate and Professional Studies of Texas A&M University in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY Chair of Committee, Darren L. DePoy Co-Chair of Committee, Jennifer L. Marshall Committee Members, Nicholas B. Suntzeff Casey J. Papovich Sherry J. Yennello Head of Department, George R. Welch August 2016 Major Subject: Physics Copyright 2016 Ting Li ABSTRACT Over the last two decades, our understanding of the Milky Way has been improved thanks to large data sets arising from large-area digital sky surveys. The stellar halo is now known to be inhabited by a variety of spatial and kinematic stellar substructures, including stellar streams and stellar clouds, all of which are predicted by hierarchical Lambda Cold Dark Matter models of galaxy formation. In this dissertation, we first present the analysis of spectroscopic observations of individual stars from the two candidate structures discovered using an M-giant catalog from the Two Micron All-Sky Survey. The follow-up observations show that one of the candidates is a genuine structure which might be associated with the Galactic Anticenter Stellar Structure, while the other one is a false detection due to the systematic photometric errors in the survey or dust extinction in low Galactic latitudes. We then presented the discovery of an excess of main sequence turn-off stars in the direction of the constellations of Eridanus and Phoenix from the first-year data of the Dark Energy Survey (DES) { a five-year, 5,000 deg2 optical imaging survey in the Southern Hemisphere.
    [Show full text]
  • Club Astronomie Des Moulins
    Club Astronomie des Moulins Le Lézard Lacerta, Lacertae, Lac Le Lézard est une petite constellation placée sur les cartes par Jean Hévélius au XVIIe siècle, dans une région entre et Andromède, Cassiopée et le Cygne. Histoire La Lézard fut créée par Johannes Hevelius en 1687 dans une région du ciel pauvre en étoiles brillantes. Son nom provient probablement de la forme en zig-zag décrite par ses étoiles les plus lumineuses. Avant Hevelius, l'astronome Augustin Royer créa, au même endroit, la constellation du Sceptre (la Main de Justice) pour rendre hommage au Roi de France Louis XIV. Cette appellation courtisane ne prit pas racine. Une légende grecque liée à Déméter, où cette dernière recherche sa fille Perséphone. Le roi Céléos lui offre alors l'hospitalité. Mais alors qu'elle est en train de manger, le fils du roi lui fait une remarque insultante, et Démeter le change en lézard. - 1 - Club Astronomie des Moulins LES ÉTOILES Bêta Lac Alpha Lac Étoile dans le Lézard de type spectral : G9III Étoile dans le Lézard de type spectral : A1V Ascention droite : 22h23'33,63" Ascention droite : 22h31'17,51" Déclinaison : +52°13'44,6" Déclinaison : +50°16'57,0" Magnitude : 4,420 Magnitude : 3,760 Distance : 169,88 al Distance : 102,37 al 5 Lac 11 Lac Étoile dans le Lézard de type spectral : M0II Étoile dans le Lézard de type spectral : K3III Ascention droite : 22h29'31,83" Ascention droite : 22h40'30,87" Déclinaison : +47"42'24,8" Déclinaison : +44°16'34,8" Magnitude : 4,340 Magnitude : 4,500 Distance ; 1164,9 al Distance : 301,72 al 6 Lac HD 211073
    [Show full text]
  • FORM No. STK — 7 NOTICE of STRIKING OFF and DISSOLUTION Government of India Ministry of Corporate Affairs Office of Registrar
    FORM No. STK — 7 NOTICE OF STRIKING OFF AND DISSOLUTION [Pursuant to sub-section (5) of section 248 of the Companies Act, 2013 and rule 9 of the Companies (Removal of Names of Companies from the Register of Companies) Rules, 2016] Government of India Ministry of Corporate Affairs Office of Registrar of Companies, NCT of Delhi & Haryana IFCI Tower, 4th Floor, 61, Nehru Place, New Delhi —110019. Email: [email protected] Phone: 011-26235703/Fax: 26235702 Notice No- ROC-DEL/248(5)/STK-7/2879 Date: 30.06.2017 Reference: In the matter of Companies Act, 2013 and 22864 Companies as per list attached as Annexure "A". This is with respect to this Office Notice ROC-DEL/248(1) even dated and notice in form STK-5 No. ROC-DEL/248/STK-5/721 issued on dated 27.04.2017. Notice is hereby published that pursuant to sub-section (5) of Section 248 of the Companies Act, 2013 the name of 22864 Companies as per list attached as Annexure "A" have this day i.e . 07th day of June, 2017 been struck off the register of the companies and the said companies are dissolved. Registrar of Companies, NCT of Delhi & Haryana ANNEXURE -A Sr No CIN Company name 1 U55100DL2012PTC237037 10 ESCAPES PRIVATE LIMITED 2 U45200DL2012PTC233848 1TOALL PROMOTERS & DEVELOPERS PRIVATE LIMITED 3 U74900DL2012PTC231508 24 FRAMES CINE PRIVATE LIMITED 4 U70109DL2011PTC228855 241 ACRE'S BUILDERSAND DEVELOPERS PRIVATE LIMITED 5 U74900DL2012PTC237892 24X7 CONCIERGE SERVICES PRIVATE LIMITED 6 U72200HR2011PTC044293 2I INFOSYSTEMS PRIVATE LIMITED 7 U93000HR2011PTC044186 30 DEGREES NORTH SERVICES
    [Show full text]
  • Collocato In
    Collocato in: http://digilander.libero.it/occultazioni/ I/149A Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) ================================================================================ Fifth Fundamental Catalogue (FK5) Part I Fricke W., Schwan H., Lederle T. (in collaboration with Bastian U., Bien R., Burkhardt G., du Mont B., Hering R., Jaehrling R., Jahreiss H., Roeser S., Schwerdtfeger H.M., Walter H.G.) <Veroeff. Astron. Rechen-Institut Heidelb. No. 32 (1988)> =1988VeARI..32....1F ================================================================================ ADC_Keywords: Proper motions ; Positional data Abstract: The Basic Fifth Fundamental Catalogue (FK5) Part I provides improved mean positions and proper motions for the 1535 classical fundamental stars that had been included in the FK3 and FK4 catalogs. The machine version of the catalog contains the positions and proper motions of the Basic FK5 stars for the epochs and equinoxes J2000.0 and B1950.0, the mean epochs of individual observed right ascensions and declinations used to determine the final positions, the mean errors of the final positions and proper motions for the reported epochs, and ancillary data such as magnitudes, spectral types, parallaxes, radial velocities, and cross identifications to other catalog designations. Introduction: The Basic FK5 is the successor to the FK4 (Fricke & Kopff 1963) and contains the 1535 classical fundamental stars used to define the latter system. It represents a revision of the FK4 and results from the determination of systematic and individual corrections to the mean positions and proper motions of the FK4, the elimination of the error in the FK4 equinox, and the introduction of the IAU (1976) system of astronomical constants. About 300 catalogs providing star positions obtained from throughout the world are included in the FK5.
    [Show full text]
  • Uva-DARE (Digital Academic Repository)
    UvA-DARE (Digital Academic Repository) Giants with infrared excess Plets, H.; Waelkens, C.; Oudmaijer, R.D.; Waters, L.B.F.M. Publication date 1997 Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Plets, H., Waelkens, C., Oudmaijer, R. D., & Waters, L. B. F. M. (1997). Giants with infrared excess. Astronomy & Astrophysics, 323, 513-523. 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:30 Sep 2021 Astron. Astrophys. 323, 513–523 (1997) ASTRONOMY AND ASTROPHYSICS Giants with infrared excess H. Plets1, C. Waelkens1, R.D. Oudmaijer2, and L.B.F.M. Waters3 1 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium ([email protected]; [email protected]) 2 Imperial College of Science, Technology and Medicine, Blackett Laboratory, Prince Consort Road, London, SW7 2BZ, UK ([email protected]) 3 Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands ([email protected]) Received 30 July 1996 / Accepted 6 January 1997 Abstract.
    [Show full text]
  • Ca Ii H and K Emission from Late-Type Stars
    CA II H AND K EMISSION FROM LATE-TYPE STARS PROEFSCHRIFT TER VERKRIJGING VAN DE GRAAS VAN DOCTOR IN DE WISKUNDE EN NATUURWETENSCHAPPEN AAN DE RIJKSUNIVERSITEIT TE UTRECHT, OP GEZAG VAN DE RECTOR MAGNIFICUS PROF. DR. M.A. SOUMAN, VOLGENS BESLUIT VAN HET COLLEGE VAN DECANEN IN HET OPENBAAR TE VE^EDIGBN OP MAANDAG 5 JULI 1982 DES NAMIDDAGS TE 4.IS UUR DOOR FRANS MIDDELKOOP GEBOREN OP 30 JANUARI 1953 TE ROTTERDAM •\ PROMOTOR: PROF.DR.C.ZWAAN opgedragen aan: Ans de Jong (mijn vrouw), Adrianus Middelkoop {mijn vader), Alie Twigt (mijn moeder). De hemelen vertellen Gods eer en het uitspansel verkondigt het werk zijner handen Psalm V9:2 Dankbetuiging Graag wil Ik alle personen en Instellingen die bijgedragen hebben tot de totstandkoming van dit proefschrift van harte bedanken. In de eerste plaats dank Ik mijn promotor, Prof.Dr. Kees Zwaan. Zijn steun en begeleiding zijn, vooral in het eerste jaar van dit onderzoek, van groot belang geweest. Zijn enthousiasme en toewijding hebben mij altijd zeer gestimuleerd. Ook ben ik veel dank verschuldigd aan mijn vriend en collega Barto Oranje. De vele gesprekken die ik met hem heb gevoerd hebben duidelijk invloed op dit proefschrift gehad. Dr. Rene' van Helden heeft mij, op bijzonder prettige en leerzame wijze, de eerste beginselen van de sterrekunde bijgebracht en mij in contact gebracht met mijn promotor. Dr. Tony Hearn stond altijd voor mij klaar als de Interne referee van mijn publikaties. I am also indebted to Dr. Arthur Vaughan who has instructed me on how to use his excellent Ca II H and K photometer.
    [Show full text]
  • An Evolutionary System of Mineralogy, Part I
    1 REVISION #1—submitted to American Mineralogist—07 November 2019 2 3 An evolutionary system of mineralogy, part I: 4 stellar mineralogy (>13 to 4.6 Ga) 5 1,* 1 6 ROBERT M. HAZEN AND SHAUNNA M. MORRISON 1 7 Geophysical Laboratory, Carnegie Institution for Science, 8 5251 Broad Branch Road NW, Washington, DC 20015, U. S. A. 9 10 “The science of Mineralogy has made rapid progress in the past six years; chemistry has 11 opened to us a better knowledge of the nature and relations of compounds; and philosophy 12 has thrown new light on the principles of classification. To change is always seeming 13 fickleness. But not to change with the advance of science, is worse; it is persistence in error.” 14 James Dwight Dana, System of Mineralogy, Third Edition, 1850, p. 5 15 16 ABSTRACT 17 Minerals preserve records of the physical, chemical, and biological histories of their origins 18 and subsequent alteration, and thus provide a vivid narrative of the evolution of Earth and other 19 worlds through billions of years of cosmic history. Mineral properties, including trace and minor 20 elements, ratios of isotopes, solid and fluid inclusions, external morphologies, and other 21 idiosyncratic attributes, represent information that points to specific modes of formation and 22 subsequent environmental histories—information essential to understanding the co-evolving 23 geosphere and biosphere. This perspective suggests an opportunity to amplify the existing 24 system of mineral classification, by which minerals are defined solely on idealized end-member 25 chemical compositions and crystal structures. Here we present the first in a series of 26 contributions to explore a complementary evolutionary system of mineralogy—a classification 27 scheme that links mineral species to their paragenetic modes.
    [Show full text]
  • EXPLORING HALO SUBSTRUCTURE with GIANT STARS. XV. DISCOVERY of a CONNECTION BETWEEN the MONOCEROS RING and the TRIANGULUM-ANDROMEDA OVERDENSITY?*†‡ Ting S
    Draft version November 13, 2018 Preprint typeset using LATEX style emulateapj v. 01/23/15 EXPLORING HALO SUBSTRUCTURE WITH GIANT STARS. XV. DISCOVERY OF A CONNECTION BETWEEN THE MONOCEROS RING AND THE TRIANGULUM-ANDROMEDA OVERDENSITY?*yz Ting S. Li1,2,3, Allyson A. Sheffield4, Kathryn V. Johnston5, Jennifer L. Marshall2,3, Steven R. Majewski6, Adrian M. Price-Whelan7, Guillermo J. Damke6,8, Rachael L. Beaton9, Edouard J. Bernard10, Whitney Richardson6, Sanjib Sharma11, Branimir Sesar12 Draft version November 13, 2018 ABSTRACT Thanks to modern sky surveys, over twenty stellar streams and overdensity structures have been discovered in the halo of the Milky Way. In this paper, we present an analysis of spectroscopic observations of individual stars from one such structure, \A13", first identified as an overdensity using the M giant catalog from the Two Micron All-Sky Survey. Our spectroscopic observations show −1 that stars identified with A13 have a velocity dispersion of . 40 km s , implying that it is a genuine coherent structure rather than a chance super-position of random halo stars. From its position on the sky, distance (∼15 kpc heliocentric), and kinematical properties, A13 is likely to be an extension of another low Galactic latitude substructure { the Galactic Anticenter Stellar Structure (also known as the Monoceros Ring) { towards smaller Galactic longitude and farther distance. Furthermore, the kinematics of A13 also connect it with another structure in the southern Galactic hemisphere { the Triangulum-Andromeda overdensity. We discuss these three connected structures within the context of a previously proposed scenario that one or all of these features originate from the disk of the Milky Way.
    [Show full text]
  • The Hitch-Hiker's Guide to Photoelectric Photometry (PEP)
    The Hitch-hiker's Guide to Photoelectric Photometry (PEP) Version 1.0 Tom Calderwood Our vision: High quality photometry of bright, astrophysically interesting stars. The AAVSO photoelectric section was founded in the late 1970s. We use old-school technology, but we can get superior results on bright stars. Compared to CCD or DSLR systems, our equipment is fundamentally simpler to calibrate and operate, and data reduction is straightforward. What we lack in sensitivity, we make up for in quality. With properly chosen targets and careful technique, we remain a viable research group. Talk to us— we're friendly people, and there is no substitute1 for conversations with experienced observers. Our web page is at https://www.aavso.org/content/aavso-photoelectric-photometry-pep-program. This document is a work-in-progress, representing my best understanding of PEP as practiced at AAVSO. It lacks the polish of other AAVSO manuals, but I think you will find it entertaining reading. The content lies somewhere in between a cookbook and a reference book. I will try to provide a wide, but not too deep overview of the equipment and practice of photometry with single-channel photometers. I will fudge on the details, occasionally, in the service of clarity. Readers should also check out the Optec photometer manuals on-line. See Appendix C, where you will also find pointers to more advanced works on photometry, which will hopefully be less intimidating after digesting this guide. 1 Including this guide! Tool of the Trade Optec SSP3 Photometer © Optec Corporation Revision history 17 January 2017 First general release Acknowledgements I would like to thank Richard Berry, Mike Beeler, Terry Moon, and Jim Kay for helpful reviews of this document.
    [Show full text]