Radii and Effective Temperatures for G, K and M
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On the Metallicity of Open Clusters II. Spectroscopy
Astronomy & Astrophysics manuscript no. OCMetPaper2 c ESO 2013 November 12, 2013 On the metallicity of open clusters II. Spectroscopy U. Heiter1, C. Soubiran2, M. Netopil3, and E. Paunzen4 1 Institutionen för fysik och astronomi, Uppsala universitet, Box 516, 751 20 Uppsala, Sweden e-mail: [email protected] 2 Université Bordeaux 1, CNRS, Laboratoire d’Astrophysique de Bordeaux UMR 5804, BP 89, 33270 Floirac, France 3 Institut für Astrophysik der Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria 4 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlárskᡠ267/2, 611 37 Brno, Czech Republic Received 29 August 2013 / Accepted 20 October 2013 ABSTRACT Context. Open clusters are an important tool for studying the chemical evolution of the Galactic disk. Metallicity estimates are available for about ten percent of the currently known open clusters. These metallicities are based on widely differing methods, however, which introduces unknown systematic effects. Aims. In a series of three papers, we investigate the current status of published metallicities for open clusters that were derived from a variety of photometric and spectroscopic methods. The current article focuses on spectroscopic methods. The aim is to compile a comprehensive set of clusters with the most reliable metallicities from high-resolution spectroscopic studies. This set of metallicities will be the basis for a calibration of metallicities from different methods. Methods. The literature was searched for [Fe/H] estimates of individual member stars of open clusters based on the analysis of high-resolution spectra. For comparison, we also compiled [Fe/H] estimates based on spectra with low and intermediate resolution. -
Chromospheric Ca II Emission in Nearby F, G, K, and M Stars1
Chromospheric Ca II emission in Nearby F, G, K, and M stars1 J. T. Wright2, G. W. Marcy2, R. Paul Butler3, S. S. Vogt4 ABSTRACT We present chromospheric Ca II H & K activity measurements, rotation pe- riods and ages for »1200 F-, G-, K-, and M- type main-sequence stars from »18,000 archival spectra taken at Keck and Lick Observatories as a part of the California and Carnegie Planet Search Project. We have calibrated our chromo- spheric S values against the Mount Wilson chromospheric activity data. From 0 these measurements we have calculated median activity levels and derived RHK, stellar ages, and rotation periods from general parameterizations for 1228 stars, »1000 of which have no previously published S values. We also present precise time series of activity measurements for these stars. Subject headings: stars: activity, rotation, chromospheres 1. Introduction The California & Carnegie Planet Search Program has included observations of »2000 late-type main-sequence stars at high spectral resolution as the core of its ongoing survey of bright, nearby stars to ¯nd extrasolar planets through precision radial velocity measurements (e.g., Cumming, Marcy, & Butler 1999; Butler et al. 2003). One source of error in the measured velocities is that due to \photospheric jitter": flows and inhomogeneities on the 1Based on observations obtained at Lick Observatory, which is operated by the University of California, and on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology. The Keck Observatory was made possible by the generous ¯nancial support of the W.M. -
Infrared Photometry and Evolution of Mass-Losing AGB Stars
A&A 445, 1069–1080 (2006) Astronomy DOI: 10.1051/0004-6361:20053208 & c ESO 2006 Astrophysics Infrared photometry and evolution of mass-losing AGB stars I. Carbon stars revisited R. Guandalini1, M. Busso1, S. Ciprini2,1, G. Silvestro3,andP.Persi4 1 Dipartimento di Fisica, Università di Perugia, via A. Pascoli, 06123 Perugia, Italy e-mail: [email protected] 2 Tuorla Astronomical Observatory, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland e-mail: [email protected] 3 Dipartimento di Fisica Generale, Università di Torino, via P. Giuria 1, 10125 Torino, Italy e-mail: [email protected] 4 Istituto di Astrofisica Spaziale e Fisica Cosmica, 00100 Roma, Italy e-mail: [email protected] Received 7 April 2005 / Accepted 12 September 2005 ABSTRACT As part of a reanalysis of galactic Asymptotic Giant Branch (AGB) stars at infrared (IR) wavelengths, we discuss a sample (357) of carbon stars for which mass loss rates, near-IR photometry and distance estimates exist. For 252 sources we collected mid-IR fluxes from the MSX (6C) and the ISO-SWS catalogues. Most stars have spectral energy distributions up to 21 µm, and some (1/3) up to 45 µm. This wide wavelength coverage allows us to obtain reliable bolometric magnitudes. The properties of our sample are discussed with emphasis on ∼70 stars with astrometric distances. We show that mid-IR fluxes are crucial to estimate the magnitude of stars with dusty envelopes. We construct HR diagrams and show that the luminosities agree fairly well with model predictions based on the Schwarzschild’s criterion, contrary to what is widely argued in the literature. -
Discovery of a Large Population of Nitrogen-Enhanced Stars in the Magellanic Clouds
Draft version October 2, 2020 Typeset using LATEX twocolumn style in AASTeX62 Discovery of a large population of Nitrogen-Enhanced stars in the Magellanic Clouds Jose´ G. Fernandez-Trincado´ ,1 Timothy C. Beers,2 Dante Minniti,3, 4 Leticia Carigi,5 Beatriz Barbuy,6 Vinicius M. Placco,2, 7 Christian Moni Bidin,8 Sandro Villanova,9 Alexandre Roman-Lopes,10 and Christian Nitschelm11 1Instituto de Astronom´ıay Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiap´o,Chile 2Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA 3Depto. de Cs. F´ısicas, Facultad de Ciencias Exactas, Universidad Andr´esBello, Av. Fern´andezConcha 700, Las Condes, Santiago, Chile 4Vatican Observatory, V00120 Vatican City State, Italy 5Instituto de Astronom´ıa, Universidad Nacional Aut´onomade M´exico, A.P. 70-264, 04510, Ciudad de M´exico, Mexico 6Universidade de S~aoPaulo, IAG, Rua do Mat~ao1226, Cidade Universit´aria,S~aoPaulo 05508-900, Brazil 7NSF's Optical-Infrared Astronomy Research Laboratory, Tucson, AZ 85719, USA 8Instituto de Astronom´ıa,Universidad Cat´olica del Norte, Av. Angamos 0610, Antofagasta, Chile 9Departamento de Astronom´ıa,Casilla 160-C, Universidad de Concepci´on,Concepci´on,Chile 10Departamento de Astronom´ıa,Universidad de La Serena - Av. Juan Cisternas, 1200 North, La Serena, Chile 11Centro de Astronom´ıa(CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta 1270300, Chile ABSTRACT We report the APOGEE-2S+ discovery of a unique collection of nitrogen-enhanced mildly metal- poor giant stars, peaking at [Fe/H]∼ −0:89 with no carbon enrichment, toward the Small and Large Magellanic Clouds (MCs), with abundances of light- (C, N), odd-Z (Al, K) and α−elements (O, Mg, Si) that are typically found in Galactic globular clusters (GCs). -
COMMISSIONS 27 and 42 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 4101{4200 1994 October { 1995 May EDITORS: L. SZ
COMMISSIONS AND OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Nos Octob er May EDITORS L SZABADOS and K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI KONKOLY OBSERVATORY H BUDAPEST PO Box HUNGARY IBVSogyallakonkolyhu URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN 2 CONTENTS 1994 No page E F GUINAN J J MARSHALL F P MALONEY A New Apsidal Motion Determination For DI Herculis ::::::::::::::::::::::::::::::::::::: D TERRELL D H KAISER D B WILLIAMS A Photometric Campaign on OW Geminorum :::::::::::::::::::::::::::::::::::::::::::: B GUROL Photo electric Photometry of OO Aql :::::::::::::::::::::::: LIU QUINGYAO GU SHENGHONG YANG YULAN WANG BI New Photo electric Light Curves of BL Eridani :::::::::::::::::::::::::::::::::: S Yu MELNIKOV V S SHEVCHENKO K N GRANKIN Eclipsing Binary V CygS Former InsaType Variable :::::::::::::::::::: J A BELMONTE E MICHEL M ALVAREZ S Y JIANG Is Praesep e KW Actually a Delta Scuti Star ::::::::::::::::::::::::::::: V L TOTH Ch M WALMSLEY Water Masers in L :::::::::::::: R L HAWKINS K F DOWNEY Times of Minimum Light for Four Eclipsing of Four Binary Systems :::::::::::::::::::::::::::::::::::::::::: B GUROL S SELAN Photo electric Photometry of the ShortPeriod Eclipsing Binary HW Virginis :::::::::::::::::::::::::::::::::::::::::::::: M P SCHEIBLE E F GUINAN The Sp otted Young Sun HD EK Dra ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::: M BOS Photo electric Observations of AB Doradus ::::::::::::::::::::: YULIAN GUO A New VR Cyclic Change of H in Tau :::::::::::::: -
Arxiv:1705.01114V2 [Astro-Ph.SR] 15 Sep 2017 Aucitfor Manuscript E4 Srla O Aaae Rgnmercspeia Ooe N Colores Y Mag
Manuscript for Revista Mexicana de Astronom´ıa y Astrof´ısica (2017) ABSOLUTE Nuv MAGNITUDES OF GAIA DR1 ASTROMETRIC STARS AND A SEARCH FOR HOT COMPANIONS IN NEARBY SYSTEMS Valeri V. Makarov US Naval Observatory, 3450 Massachusetts Ave NW, Washington DC 20392-5420, USA Received: May 2 2017; Accepted: June 23 2017 RESUMEN Se combinan paralajes del Gaia DR1 (TGAS) con magnitudes visuales Nuv del GALEX para obtener magnitudes absolutas Mnuv as´ıcomo un diagrama HR ultravioleta para una muestra de estrellas astrom´etricas. Se deriva un ajuste para la envolvente inferior de la secuencia principal para las 1403 estrellas con distancias < 40 pc, que no tendr´ıan enrojecimiento. Se seleccionan 50 estrellas cercanas con un exceso Nuv considerable. Estas estrellas son principalmente de tipo K tard´ıo y M temprano, frecuentemente asociadas con fuentes de rayos X, y con otras manifestaciones de actividad magn´etica. La muestra puede incluir sistemas con enanas blancas ocultas, estrellas m´as j´ovenes que las Pl´eyades o binarias interactuantes de tipo BY Dra. Se presenta otra muestra de 40 estrellas con paralajes trigonom´etricas precisas y colores Nuv-G m´as azules que 2 mag. Esta´ incluye varias novas, enanas blancas y binarias con subenanas calientes como compa˜neras. ABSTRACT Accurate parallaxes from Gaia DR1 (TGAS) are combined with GALEX vi- sual Nuv magnitudes to produce absolute Mnuv magnitudes and an ultraviolet HR diagram for a large sample of astrometric stars. A functional fit is derived of the lower envelope main sequence of the nearest 1403 stars (distance < 40 pc), which should be reddening-free. -
1.1 RR Lyrae Stars
Universita` degli studi di Roma “Tor Vergata” Facolta` di Scienze Matematiche, Fisiche e Naturali Dottorato di Ricerca in Astronomia XIX ciclo (2003-2006) SELF-CONSISTENT DISTANCE SCALES FOR POPULATION II VARIABLES Marcella Di Criscienzo Coordinator: Supervisors: PROF. R. BUONANNO PROF. R. BUONANNO PROF.SSA F. CAPUTO DOTT.SSA M. MARCONI Vedere il mondo in un granello di sabbia e il cielo in un fiore di campo tenere l’infinito nel palmo della tua mano e l'eternita´ in un ora. (William Blake) ii Dedico questa tesi a: Mamma e Papa´ Sarocchia Giuliana Marcella & Vincenzo Massimo Filippina Caputo Massimo Capaccioli Roberto Buonanno che mi aiutarono a trovare la strada, e a Tommaso che su questa strada ha viaggiato con me per quasi tutto il tempo Contents The scientific project xv 1 Population II variables 1 1.1 RR Lyrae stars 3 1.1.1 Observational properties 4 1.1.2 Evolutionary properties 6 1.1.3 RR Lyrae as standard candles 8 1.1.4 RR Lyrae in Globular Clusters 9 1.2 Population II Cepheids 13 1.2.1 Present status of knowledge 13 2 Some remarks on the pulsation theory and the computational methods 15 2.1 The pulsation cycle: observations 15 2.2 Pulsation mechanisms 17 2.3 Theoretical approches to stellar pulsation 19 2.4 Computational methods 23 3 Updated pulsation models of RR Lyrae and BL Herculis stars 25 3.1 RR Lyrae (Di Criscienzo et al. 2004, ApJ, 612; Marconi et al., 2006, MNRAS, 371) 25 3.1.1 The instability strip 30 3.1.2 Pulsational amplitudes 31 3.1.3 Some important relations for RR Lyrae studies 36 3.1.4 New results in the SDSS filters 39 3.2 BL Herculis stars (Marconi & Di Criscienzo, 2006, A&A, in press) 43 iv REFERENCES 3.2.1 Light curves and pulsation amplitudes 46 3.2.2 The instability strip 48 4 Comparison with observed RR Lyrae stars and Population II Cepheids 51 4.1 RR Lyrae 52 4.1.1 Comparison of models in Johnson-Cousin filters with current ob- servations (Di Criscienzo et al. -
Sacrilege in Dinétah: Native Encounters with Glen Canyon Dam Sonia Dickey
University of New Mexico UNM Digital Repository History ETDs Electronic Theses and Dissertations 8-19-2011 Sacrilege in Dinétah: Native Encounters with Glen Canyon Dam Sonia Dickey Follow this and additional works at: https://digitalrepository.unm.edu/hist_etds Part of the History Commons Recommended Citation Dickey, Sonia. "Sacrilege in Dinétah: Native Encounters with Glen Canyon Dam." (2011). https://digitalrepository.unm.edu/ hist_etds/21 This Dissertation is brought to you for free and open access by the Electronic Theses and Dissertations at UNM Digital Repository. It has been accepted for inclusion in History ETDs by an authorized administrator of UNM Digital Repository. For more information, please contact [email protected]. i SACRILEGE IN DINÉTAH: NATIVE ENCOUNTERS WITH GLEN CANYON DAM BY SONIA L. DICKEY B.A., History, Georgia Southern University, 1998 M.A., History, Georgia Southern University, 2001 DISSERTATION Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy History The University of New Mexico Albuquerque, New Mexico May 2011 ii Acknowledgments Like any large project, this dissertation benefitted from research grants and scholarships. I would like to thank the History Department at the University of New Mexico, the Charles Redd Center for Western Studies at Brigham Young University, and the New Mexico branch of the Daughters of the American Revolution for providing much needed monies that enabled me to research at institutions all over the Intermountain West. I am extremely grateful for the funding opportunities Dr. Tobias Duran and the Center for Regional Studies have given me during my tenure at the University of New Mexico. -
Observer's Guide to Galaxies
Observer’s Guide to Galaxies By Rob Horvat (WSAAG) Mar 2020 This document has evolved from a supplement to Night-Sky Objects for Southern Observers (Night-Sky Objects for short), which became available on the web in 2009. The document has now been split into two, this one being called the Observer’s Guide to Galaxies. The maps have been designed for those interested in locating galaxies by star-hopping around the constellations. However, like Night-Sky Objects, the resource can be used to simply identify interesting galaxies to GOTO. As with Night-Sky Objects, the maps have been designed and oriented for southern observers with the limit of observation being Declination +55 degrees. Facing north, the constellations are inverted so that they are the “right way up”. Facing south, constellations have the usual map orientation. Pages are A4 in size and can be read as a pdf on a computer or tablet. Note on copyright. This document may be freely reproduced without alteration for educational or personal use. Contributed images by WSAAG members remain the property of their authors. Types of Galaxies Spiral (S) galaxies consist of a rotating disk of stars, dust and gas that surround a central bulge or concentration of stars. Bulges often house a central supermassive black hole. Most spiral galaxies have two arms that are sites of ongoing star formation. Arms are brighter than the rest of the disk because of young hot OB class stars. Approx. 2/3 of spiral galaxies have a central bar (SB galaxies). Lenticular (S0) galaxies have a rather formless disk (no obvious spiral arms) with a prominent bulge. -
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