Fundamental stellar parameters & the fine structure of the Low Main Sequence
|
|
- Dulcie Sims
- 6 years ago
- Views:
Transcription
1 Fundamental stellar parameters & the fine structure of the Low Main Sequence Luca Casagrande MPA: I. Ramírez, M. Asplund CAUP: J. Meléndez ANU: M. Bessell Casagrande et al. (2010, A&A - in press; arxiv: )
2 Effective Temperatures Fundamental stellar Bolometric Luminosities parameters Angular diameters & the fine structure of the Low Main Sequence Luca Casagrande MPA: I. Ramírez, M. Asplund CAUP: J. Meléndez ANU: M. Bessell Casagrande et al. (2010, A&A - in press; arxiv: )
3 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) Gustafsson et al. (2008) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009)
4 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) Gustafsson et al. (2008) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009)
5 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration Asplund (2005) τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009) Gustafsson et al. (2008) Ramírez et al. (2009)
6 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration Asplund (2005) τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009) Gustafsson et al. (2008) Ramírez et al. (2009)
7 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration Asplund (2005) τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009) Gustafsson et al. (2008) Ramírez et al. (2009)
8 Effective Temperature Direct: interferometry (Hanbury Brown et al. 1974, van Belle & von Braun 2009) precise & accurate - nearby stars (limited range) - uniform disk Kervella et al. (2008) UD Allende Prieto et al. (2002) Bigot et al. (2006) Koesterke et al. (2008) LD Semi-Direct: InfraRed Flux Method Allende Prieto et al. (2002) precise ~ model-independent any star (photometry) - reddening - accuracy: absolute calibration Asplund (2005) τ = 2 3 Indirect: ionization/excitation, Balmer lines, line-depth ratio precise any stars (spectra) - model dependent (NLTE, inhomogeneity, e.g. Asplund 2005, Ludwig et al. 2009) Gustafsson et al. (2008) Ramírez et al. (2009)
9 InfraRed Flux Method Blackwell et al. (1977,1978,1979) Casagrande et al. (2006, 2010)
10 InfraRed Flux Method Blackwell et al. (1977,1978,1979) Casagrande et al. (2006, 2010)
11 InfraRed Flux Method log g Teff [Fe/H] Castelli & Kurucz(2004)
12 InfraRed Flux Method log g Teff absolutely calibrated [Fe/H] Castelli & Kurucz(2004) flux scale: overall absolute calibration shape: spectral library
13 IRFM: Pros & Cons
14 IRFM: Pros & Cons
15 IRFM: Pros & Cons
16 IRFM: Pros & Cons ~2/3% ~0.01 mag ~ 4% = 80 K
17 IRFM: Pros & Cons ~2/3% ~0.01 mag ~ 4% = 80 K But recently, towards 1% accuracy : Bohlin (2007) Apellaniz (2007) Bohlin & Cohen (2008) Rieke et al. (2008)
18 Comparing different versions Alonso et al. (1996)
19 Comparing different versions Alonso et al. (1996) Ramírez & Meléndez (2005) same input data used
20 Comparing different versions Alonso et al. (1996) Ramírez & Meléndez (2005) same input data used González Hernández & Bonifacio (2009)
21 Comparing different versions Alonso et al. (1996) Ramírez & Meléndez (2005) IRFM can accommodate any T eff scale We understand the differences Which one do we choose? same input data used González Hernández & Bonifacio (2009)
22 photometry Resolving Solar Analogs different versions Teff
23 photometry Resolving Solar Analogs different versions Teff
24 Solar Analogs Twins photometry Teff
25 Solar Analogs Twins photometry Teff Meléndez et al. (2009) Ramírez et al. (2009) R~65000, S/N >450 EW same instrument NLTE, granulation high-quality no a priori model-independent high-accuracy
26 Solar Analogs Twins photometry Teff ~15-20 K Meléndez et al. (2009) Ramírez et al. (2009) R~65000, S/N >450 EW same instrument NLTE, granulation high-quality no a priori model-independent high-accuracy
27 Angular diameters F Bol = ( ) 2 θ T eff 2 θ = 0.6 ± 1.7% T eff = 18 ± 50K
28 HST Spectro-photometry STIS NICMOS HD209458, [Fe/H] = 0.03 BD , [Fe/H] = -1.74
29 HST Spectro-photometry STIS NICMOS HD209458, [Fe/H] = 0.03 ~20-40 K BD , [Fe/H] = -1.74
30 More Spectro-photometry M. Bessell (private comm.) HD BD Flambda Flambda Blue: 5875 old Red : 6125 IRFM : 6135 K Blue: 6250 old Red : 6500 IRFM : 6420 K Wavelength Angstroms Wavelength Angstroms
31 Solar like stars: CMD B-V = ± ± B-V = ± (Pasquini et al. 2008) Vandenberg, Casagrande & Stetson, in prep.
32 Solar like stars: field Geneva-Copenhagen Survey Nordström et al. (2004); Holmberg et al. (2007, 2009) Revisiting the Geneva-Copenhagen Survey : Casagrande, Schönrich, Asplund, Ramírez, Meléndez, Bensby (2010)
33 Improved Teff GCS
34 Improved Teff Improved [Fe/H] GCS
35 Metallicity distribution function Peaks ~ solar but see Meléndez et al. (2009), Ramírez et al. (2009) for the peculiar solar chemical composition
36 Something new under the Sun
37 IRFM goes cool Casagrande, Flynn & Bessell (2008)
38 IRFM goes cool Yes we can! Casagrande, Flynn & Bessell (2008)
39 M dwarfs angular diameters Casagrande, Flynn & Bessell (2008)
40 M dwarfs angular diameters Test on CM Draconis (Morales et al. 2009) Barnard s star Casagrande, Flynn & Bessell (2008)
41 Fine Structure 222 GKM dwarfs σ parallaxes better 15% Hipparcos to remove variables/binaries Casagrande, Flynn & Bessell (2008)
42 Fine Structure 222 GKM dwarfs σ parallaxes better 15% Hipparcos to remove variables/binaries Casagrande, Flynn & Bessell (2008)
43 Fine Structure Baraffe et al. (1998) Solar 5 Gyr [M/H]=-0.0 [M/H]= GKM dwarfs σ parallaxes better 15% Hipparcos to remove variables/binaries Casagrande, Flynn & Bessell (2008)
44 M dwarfs radii good agreement: e.g. Delfosse et al. 2000; López-Morales 2007; Demory et al Casagrande, Flynn & Bessell (2008)
45 [Fe/H] M dwarfs radii GJ205; GJ436; GJ191; Casagrande et al. (2008) Baines et al. (2008); Kervella & Fouqué (2008); Ségransan et al. (2003); Berger et al. (2006); Demory et al. (2009) Gillon et al. (2007); Torres (2007)
46 [Fe/H] M dwarfs radii GJ205; GJ436; GJ191; Casagrande et al. (2008) Baines et al. (2008); Kervella & Fouqué (2008); Ségransan et al. (2003); Berger et al. (2006); Demory et al. (2009) Gillon et al. (2007); Torres (2007)
47 [Fe/H] M dwarfs radii GJ205; GJ436; GJ191; Casagrande et al. (2008) Baines et al. (2008); Kervella & Fouqué (2008); Ségransan et al. (2003); Berger et al. (2006); Demory et al. (2009) Gillon et al. (2007); Torres (2007)
48 3 characters in search of an author inflated radii in M dwarfs not only in eclipsing binaries, also single field stars Mixing Length (e.g. Chabrier et al. 2007) Magnetic activity (e.g. Mullan & MacDonald 2001; López-Morales & Ribas 2005) Opacity (e.g. Berger et al. 2006)
49 The Epilogue Teff : FGK dwarfs understand the differences among scales settle the issue solar twins HST spectro-photometry angular diameters } ~ 20 K chemical evolution Solar Neighbourhood Teff : M dwarfs Teff scale robust down to 3000 K discontinuity in obs. plane! inflated radii?!?
Classical observations of stellar properties
Classical observations of stellar properties Luca Casagrande M. Bessell - J. Meléndez - I. Ramírez / M. Asplund R. Schönrich / V. Silva Aguirre Spectroscopy F(l) : lots of info, but also model dependent
More informationDiameters and Temperatures of Main Sequence Stars
Diameters and Temperatures of Main Sequence Stars Tabetha Boyajian (GSU / Hubble Fellow) and a whole lot of y all Interest and motivation Fundamental properties of stars Radius: f (θ, π) Temperature: f
More informationFundamental stellar parameters
Fundamental stellar parameters flux received at Earth f º = direct determination of Teff R = radius of the spherical star, D = distance to the star. Luminosity : L = 4π R 2 F º dº T eff 4 = 4π R 2 F =
More informationInterferometric Constraints on Fundamental Stellar Parameters
Interferometric Constraints on Fundamental Stellar Parameters Pierre Kervella LESIA, Paris Observatory photo: S. Guisard Heat Heat Transport Heat Transport Photosphere Radiation Heat Transport Photosphere
More informationClassical Methods for Determining Stellar Masses, Temperatures, and Radii
Classical Methods for Determining Stellar Masses, Temperatures, and Radii Willie Torres Harvard-Smithsonian Center for Astrophysics 2010 Sagan Exoplanet Summer Workshop 1 Outline Basic properties of stars
More informationInterferometric Observations of Supergiants: Direct Measures of the Very Largest Stars
Interferometric Observations of Supergiants: Direct Measures of the Very Largest Stars Gerard T. van Belle PRIMA Instrument Scientist Observatory April 7, 2008 Interferometric Observations of Supergiants:
More information12. Physical Parameters from Stellar Spectra. Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances
12. Physical Parameters from Stellar Spectra Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances 1 Fundamental Properties of Stars Temperature (T) Radius (R) Chemical
More informationMeasurement of the stellar irradiance
Measurement of the stellar irradiance Definitions Specific Intensity : (monochromatic) per unit area normal to the direction of radiation per unit solid angle per unit wavelength unit (or frequency) per
More informationPoS(NIC XI)301. Andreas Korn. IFA, Uppsala University. Heidelberg,
Andreas Korn IFA, Uppsala University Heidelberg, 2010-07-17 Who is this guy? Born in 1972, raised in Marburg, Germany MSc in Astrophysics (1996, U of London) Diploma in Physics (1998, U of Heidelberg)
More informationarxiv:astro-ph/ v1 6 Nov 2005
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 18 April 2018 (MN LATEX style file v1.4) The colours of the Sun Johan Holmberg 1, Chris Flynn 1 and Laura Portinari 1 1 Tuorla Observatory, Väisäläntie
More informationThe effective temperature scale of giant stars (F0 K5)
ASTRONOMY & ASTROPHYSICS OCTOBER II 1999, PAGE 335 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 139, 335 358 (1999) The effective temperature scale of giant stars (F0 K5) I. The effective temperature
More informationStellar Formation and Evolution
Stellar Formation and Evolution Wen Ping Chen http://www.astro.ncu.edu.tw/~wchen/courses/stars/default.htm What is a star? How hot is the surface of the Sun? How is this known? The Sun is gaseous, so how
More informationDelicious Diameters of Dwarfs (in particular, the juicy red ones)
Delicious Diameters of Dwarfs (in particular, the juicy red ones) Tabetha Boyajian GSU / Hubble Fellow In collaboration with a whole bunch of y all Radical Radii of Red Stars Tabetha Boyajian GSU / Hubble
More informationarxiv: v1 [astro-ph.sr] 5 Jun 2018
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 7 June 2018 (MN LATEX style file v2.2) On the use of Gaia magnitudes and new tables of bolometric corrections arxiv:1806.01953v1 [astro-ph.sr] 5 Jun
More informationTests of stellar physics with high-precision data from eclipsing binary stars
Tests of stellar physics with high-precision data from eclipsing binary stars Ignasi Ribas Institut de Ciències de l Espai (CSIC-IEEC, Barcelona) Barcelona, April 2013 Eclipsing binary systems Eclipsing
More informationChapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
More informationOxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!
Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at
More informationarxiv:astro-ph/ v1 3 Jan 2006
Astronomy & Astrophysics manuscript no. masana February 5, 28 (DOI: will be inserted by hand later) Effective temperature scale and bolometric corrections from 2MASS photometry arxiv:astro-ph/6149v1 3
More informationTHE EFFECTIVE TEMPERATURE SCALE OF FGK STARS. II. T eff : COLOR : [Fe/H] CALIBRATIONS
The Astrophysical Journal, 626:465 485, 2005 June 10 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. A THE EFFECTIVE TEMPERATURE SCALE OF FGK STARS. II. T eff : COLOR
More informationCharacterization of Exoplanet-Host Stars Vardan Adibekyan Instituto de Astrofísica e Ciências do Espaço
Characterization of Exoplanet-Host Stars Vardan Adibekyan Instituto de Astrofísica e Ciências do Espaço vardan.adibekyan@astro.up.pt Why not Sergio? It was a real war with casualties... Before going to
More informationCHARA 2016: Adaptive Optics and Perspectives on Visible Interferometry
PAVO Science Update Tim White (Aarhus), Daniel Huber (Sydney), Iva Karovicova (Heidelberg), Ethan Ryan (Sydney), Amalie Stockholm (Aarhus), Benjamin Pope (Oxford), Peter Tuthill (Sydney), Mike Ireland
More informationLAST RESULTS ON THE CHARACTERIZATION OF EXOPLANETS AND THEIR STELLAR HOSTS with VEGA/CHARA Ligi et al. 2016, A&A, 586, A94
LAST RESULTS ON THE CHARACTERIZATION OF EXOPLANETS AND THEIR STELLAR HOSTS with VEGA/CHARA Ligi et al. 2016, A&A, 586, A94 ROXANNE LIGI CNES POST-DOCTORAL FELLOW LABORATOIRE D ASTROPHYSIQUE DE MARSEILLE
More informationStellar Evolution & issues related to the post Turn-Off evolution
Stellar Evolution & issues related to the post Turn-Off evolution Santi Cassisi INAF - Astronomical Observatory of Teramo, Italy The point of view of Population Synthesis users What do they want? Magnitudes
More informationStars: basic observations
Stars: basic observations Basic properties of stars we would like to know in order to compare theory against observations: Stellar mass M Stellar radius R Surface temperature - effective temperature T
More informationChemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia J. Andersen 1,2, B. Nordström 1,2 1 Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Denmark 2 Stellar Astrophysics
More informationSolar analogues and solar twins in the HARPS archive
Advance Access publication 2014 February 5 doi:10.1093/mnras/stu026 Solar analogues and solar twins in the HARPS archive Juliet Datson, 1 Chris Flynn 2,3,4 and Laura Portinari 1 1 Tuorla Observatory, Department
More informationFundamental (Sub)stellar Parameters: Masses and Radii. PHY 688, Lecture 10
Fundamental (Sub)stellar Parameters: Masses and Radii PHY 688, Lecture 10 Outline Review of previous lecture brown dwarf effective temperatures finding cool brown dwarfs current problem: what are the coolest
More informationASTRONOMY AND ASTROPHYSICS. Synthetic photometry from ATLAS9 models in the UBV Johnson system. Fiorella Castelli
Astron. Astrophys. 346, 564 585 (1999) ASTRONOMY AND ASTROPHYSICS Synthetic photometry from ATLAS9 models in the UBV Johnson system Fiorella Castelli CNR-Gruppo Nazionale Astronomia and Osservatorio Astronomico,
More informationThe HST Set of Absolute Standards for the 0.12 µm to 2.5 µm Spectral Range
Instrument Science Report CAL/SCS-010 The HST Set of Absolute Standards for the 0.12 µm to 2.5 µm Spectral Range L. Colina, R. Bohlin, D. Calzetti, C. Skinner, S. Casertano October 3, 1996 ABSTRACT A proposal
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationInterferometric orbits of new Hipparcos binaries
Interferometric orbits of new Hipparcos binaries I.I. Balega 1, Y.Y. Balega 2, K.-H. Hofmann 3, E.V. Malogolovets 4, D. Schertl 5, Z.U. Shkhagosheva 6 and G. Weigelt 7 1 Special Astrophysical Observatory,
More informationarxiv: v1 [astro-ph.sr] 17 May 2010
Astronomy & Astrophysics manuscript no. li 17may2010 c ESO 2018 November 8, 2018 Observational evidence for a broken Li Spite plateau and mass-dependent Li depletion J. Meléndez 1, L. Casagrande 2, I.
More informationAsterseismology and Gaia
Asterseismology and Gaia Asteroseismology can deliver accurate stellar radii and masses Huber et al 2017 compare results on distances from Gaia and asteroseismology for 2200 Kepler stars Asteroseismology
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
More informationCNO abundances in the Sun and Solar Twins
CNO abundances in the Sun and Solar Twins Jorge Meléndez Departamento de Astronomia, IAG, Universidade de São Paulo Sunset in Paracas, Peru (c) www.flickr.com/photos/rodrigocampos/ Why are C, N, O (and
More informationExploring the giant planet - brown dwarf connection with astrometry. Johannes Sahlmann ESA Research Fellow at ESAC
Exploring the giant planet - brown dwarf connection with astrometry ESA Research Fellow at ESAC Who s Who, Paris - 2 July 215 IS MASS A GOOD DEMOGRAPHIC INDICATOR? 2MASSWJ127334 393254 first image of a
More informationGalactic Projects at ESO Disk and halo. Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark
Galactic Projects at ESO Disk and halo Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark B. Nordstrom Prague 15 April 2014 1980: Milky Way Structure was Known - the formation and evolution
More informationTHE PHYSICAL CHARACTERIZATION OF THE STARS. 1 Introduction
THE PHYSICAL CHARACTERIZATION OF THE STARS CARME JORDI, EDUARD MASANA Departamento de Astronomía y Meteorología, Universidad de Barcelona, Martí i Franqués 1, E-08028 Barcelona, SPAIN Institut de Ciències
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Update date: December 13, 2010 Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle,
More informationThe Color-Magnitude Diagram for local stars from Hipparcos. Red Giant Branch (RGB) Red clump. Absolute Magnitude Main Sequence. White dwarfs.
The Color-Magnitude Diagram for local stars from Hipparcos Absolute Magnitude Main Sequence Red clump Red Giant Branch (RGB) White dwarfs Kovalevsky 1998 Color Lebreton 2001 The Hipparcos H-R Diagram of
More informationHertzprung-Russel and colormagnitude. ASTR320 Wednesday January 31, 2018
Hertzprung-Russel and colormagnitude diagrams ASTR320 Wednesday January 31, 2018 H-R diagram vs. Color- Magnitude Diagram (CMD) H-R diagram: Plot of Luminosity vs. Temperature CMD: Plot of magnitude vs.
More informationStellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
More informationA complete CHARActerization of the HD and the HD systems
A complete CHARActerization of the HD189733 and the HD209458 systems Tabetha Boyajian Kaspar von Braun, Gregory A. Feiden, Daniel Huber, Sarbani Basu, Pierre Demarque, Debra A. Fischer, Gail Schaefer,
More informationANGULAR DIAMETERS OF THE G SUBDWARF CASSIOPEIAE A AND THE K DWARFS DRACONIS AND HR 511 FROM INTERFEROMETRIC MEASUREMENTS WITH THE CHARA ARRAY
The Astrophysical Journal, 683:424Y432, 2008 August 10 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. A ANGULAR DIAMETERS OF THE G SUBDWARF CASSIOPEIAE A AND THE K DWARFS
More informationRecent results from VEGA Perspective of a 6T visible combiner
Recent results from VEGA Perspective of a 6T visible combiner Denis Mourard O. Creevey, N.Nardetto, K. Perraut And the VEGA group 2014 Statistics 17 proposals (13 from Nice, 3 from Grenoble, 1 from Paris)
More informationThe Stellar Populations of Galaxies H. W. Rix IMPRS Galaxies Course March 11, 2011
The Stellar Populations of Galaxies H. W. Rix IMPRS Galaxies Course March 11, 2011 Goal: Determine n * (M *,t age,[fe/h],r) for a population of galaxies How many stars of what mass and metallicity formed
More informationUpdates on Characterization of Stars (with and without Planets)
Updates on Characterization of Stars (with and without Planets) Kaspar von Braun (Lowell Observatory) with T. Boyajian, A. Mann, G. van Belle, S. Kane, D. Ciardi, G. Schaefer, J. Jones, C. Farrington,
More informationarxiv:astro-ph/ v1 25 Aug 2006
Astronomy & Astrophysics manuscript no. 5647 September 28, 2018 (DOI: will be inserted by hand later) Fundamental Parameters and Abundances of Metal-Poor Stars: The SDSS Standard BD +17 4708 I. Ramírez,
More informationTechniques for measuring astronomical distances generally come in two variates, absolute and relative.
Chapter 6 Distances 6.1 Preliminaries Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Absolute distance measurements involve objects possibly unique
More informationGalac%c Unprecedented Precision (0.01 dex)
Li Be B Si O Fe Dy Ce Ru Y Pb C a Ti L V b Y Eu Al N Pr d Sr Mo Ba P Ca K Cr S N Sm Gd U Ag Pd Mg Ni Galac%c Archaeology @ Unprecedented Precision (0.01 dex) @DrJorgeMelendez Dep. Astronomia, Univ. São
More informationThe effective temperature scale of giant stars (F0 K5)
ASTRONOMY & ASTROPHYSICS DECEMBER II 1999, PAGE 261 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 140, 261 277 (1999) The effective temperature scale of giant stars (F0 K5) II. Empirical calibration
More information! p. 1. Observations. 1.1 Parameters
1 Observations 11 Parameters - Distance d : measured by triangulation (parallax method), or the amount that the star has dimmed (if it s the same type of star as the Sun ) - Brightness or flux f : energy
More informationarxiv:astro-ph/ v1 7 Sep 2005
Astronomy & Astrophysics manuscript no. 3187 February 5, 2008 (DOI: will be inserted by hand later) The limb darkening of αcen B Matching 3D hydrodynamical models with interferometric measurements L. Bigot
More informationScience Opportunities in Stellar Physics. Douglas R. Gies CHARA, Georgia State Univ., and the Stellar Physics Working Group
Science Opportunities in Stellar Physics Douglas R. Gies CHARA, Georgia State Univ., gies@chara.gsu.edu and the Stellar Physics Working Group General Themes! Fundamental properties! Interior structure
More informationBuilding the cosmic distance scale: from Hipparcos to Gaia
The Fundamental Distance Scale: state of the art and the Gaia perspectives 3-6 May 2011 Building the cosmic distance scale: from Hipparcos to Gaia Catherine TURON and Xavier LURI 1 ESA / ESO-H. Heyer Fundamental
More informationFundamental parameters and abundances of metal-poor stars: the SDSS standard BD
A&A 459, 613 625 (2006) DOI: 10.1051/0004-6361:20065647 c ESO 2006 Astronomy & Astrophysics Fundamental parameters and abundances of metal-poor stars: the SDSS standard BD +17 4708 I. Ramírez, C. Allende
More informationarxiv: v2 [astro-ph.sr] 11 Sep 2014
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 15 September 2014 (MN LATEX style file v2.2) Synthetic Stellar Photometry I. General considerations and new transformations for broad-band systems.
More informationDETERMINING STELLAR PARAMETERS FROM SPECTROSCOPIC OBSERVATIONS. Philip Muirhead Department of Astronomy Boston University
DETERMINING STELLAR PARAMETERS FROM SPECTROSCOPIC OBSERVATIONS Philip Muirhead Department of Astronomy Boston University FOR THE FUNDAMENTALS My personal recommendation for the fundamentals of acquiring
More informationPractice Problem!! Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.
Practice Problem Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.05 cm -3 (a) estimate the minimum mass that could collapse, (b) what is the
More informationFundamental Stellar Astrophysics Revealed at Very High Angular Resolution
Fundamental Stellar Astrophysics Revealed at Very High Angular Resolution Contact: Jason Aufdenberg (386) 226-7123 Embry-Riddle Aeronautical University, Physical Sciences Department aufded93@erau.edu Co-authors:
More informationNew Dimensions of Stellar Atmosphere Modelling
New Dimensions of Stellar Atmosphere Modelling Derek Homeier 1,2 France Allard 1,3 Bernd Freytag 1 1 CRAL/École Normale Supérieure de Lyon 2 Förderkreis Planetarium Göttingen e.v. 3 Institut d Astrophysique
More informationFIA0221: Taller de Astronomía II. Lecture 14 Spectral Classification of Stars
FIA0221: Taller de Astronomía II Lecture 14 Spectral Classification of Stars Spectral types along the stellar CMD. Oh, Be A Fine Girl Kiss Me! Classification of Stellar spectra: The MK system: strong He+
More informationOn the relation between stars and their planets
On the relation between stars and their planets Nuno C. Santos Centro de Astrofísica, Universidade do Porto Instituto de Astrofísica e Ciências do Espaço Why we stellar parameters are important in exoplanets
More informationLecture 12: Distances to stars. Astronomy 111
Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions
More informationObserved Properties of Stars - 2 ASTR 2110 Sarazin
Observed Properties of Stars - 2 ASTR 2110 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Stellar Colors Stellar Colors Stellar Colors Stars
More informationThe cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
More information5. The Baade-Wesselink Method
Rolf Kudritzki SS 2017 5. The Baade-Wesselink Method Baade-Wesselink Method (BWM): distance determination method for stellar objects, for which the photosphere can be approximated as a spherically moving
More informationParallax: Measuring the distance to Stars
Measuring the Stars Parallax: Measuring the distance to Stars Use Earth s orbit as baseline Parallactic angle = 1/2 angular shift Distance from the Sun required for a star to have a parallactic angle of
More informationStars and Stellar Astrophysics. Kim Venn U. Victoria
Stars and Stellar Astrophysics with ngcfht Kim Venn U. Victoria Stellar SWG: Katia Cunha (NOAO), Rolf-Peter Kudritzki (IfA), Else Starkenburg (U. Victoria) Patrick Dufour (U.Montreal) Zhanwen Han (Yunnan
More informationSTELLAR STRUCTURE AND EVOLUTION: Deductions from Hipparcos
Annu. Rev. Astron. Astrophys. 2001. 38:35 77 Copyright c 2000 by Annual Reviews. All rights reserved STELLAR STRUCTURE AND EVOLUTION: Deductions from Hipparcos Yveline Lebreton Observatoire de Paris, DASGAL-UMR
More informationAsteroseismology for Galactic Archaeology: bridging two fields
Asteroseismology for Galactic Archaeology: bridging two fields Luca Casagrande Victor Silva Aguirre Dennis Stello, Aldo Serenelli Daniel Huber, Katie Schlesinger, Ralph Schönrich, Sofia Feltzing Asteroseismology
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationarxiv:astro-ph/ v1 18 Apr 2000
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 07(08.01.1, 08.01.3, 08.06.3, 08.09.2 G271-162, 09.03.2) ASTRONOMY AND ASTROPHYSICS The lithium isotope ratio in the metal-poor
More information6. Detached eclipsing binaries
Rolf Kudritzki SS 2015 6. Detached eclipsing binaries 50% of all stars live in binary systems and some of them are eclipsing 1 Rolf Kudritzki SS 2015 classification of binary systems by geometry of equipotential
More informationGalactic, stellar (and planetary) archaeology with Gaia: The galactic white dwarf population
Galactic, stellar (and planetary) archaeology with Gaia: The galactic white dwarf population Boris Gänsicke & Roberto Raddi Richard Ashley Jay Farihi Nicola Gentile Fusillo Mark Hollands Paula Izquierdo
More informationSkyMapper and EMP stars
SkyMapper and EMP stars Mike Bessell on behalf of the EMP team Research School of Astronomy & Astrophysics Slide 2 The discovery of the ancient star with no Fe lines. SkyMapper 2.3m WiFeS Magellan MIKE
More informationTECHNICAL REPORT. Doc #: Date: Rev: JWST-STScI , SM-12 August 31, Authors: Karl Gordon, Ralph Bohlin. Phone:
When there is a discrepancy between the information in this technical report and information in JDox, assume JDox is correct. TECHNICAL REPORT Title: Title: JWST Absolute Flux Calibration II: Expanded
More informationAnomalous Spectral Types and Intrinsic Colors of Young Stars
Young Stars & Planets Near the Sun Proceedings IAU Symposium No. 314, 2015 J. H. Kastner, B. Stelzer, & S. A. Metchev, eds. c International Astronomical Union 2016 doi:10.1017/s1743921315006079 Anomalous
More informationThe science potential of atmospheric Cherenkov arrays used as intensity interferometers
The science potential of atmospheric Cherenkov arrays used as intensity interferometers Michael Daniel for Willem-Jan de Wit w.j.m.dewit@leeds.ac.uk Atmospheric Cherenkov Telescope Arrays Multiple telescopes
More informationLines of Hydrogen. Most prominent lines in many astronomical objects: Balmer lines of hydrogen
The Family of Stars Lines of Hydrogen Most prominent lines in many astronomical objects: Balmer lines of hydrogen The Balmer Thermometer Balmer line strength is sensitive to temperature: Most hydrogen
More informationarxiv: v1 [astro-ph.sr] 22 Sep 2011
Fundamental Parameters of the Exoplanet Host K Giant Star ι Draconis from the CHARA Array Ellyn K. Baines arxiv:1109.4950v1 [astro-ph.sr] 22 Sep 2011 Remote Sensing Division, Naval Research Laboratory,
More informationLecture Three: Stellar Populations. Stellar Properties: Stellar Populations = Stars in Galaxies. What defines luminous properties of galaxies
Lecture Three: ~2% of galaxy mass in stellar light Stellar Populations What defines luminous properties of galaxies face-on edge-on https://www.astro.rug.nl/~etolstoy/pog16/ 18 th April 2016 Sparke & Gallagher,
More informationarxiv: v1 [astro-ph.sr] 29 Jul 2010
Astronomy & Astrophysics manuscript no. uvby twins2010jul25 c ESO 2013 October 10, 2013 uvby-β photometry of solar twins The solar colors, model atmospheres, and the T eff and metallicity scales J. Meléndez
More informationarxiv: v1 [astro-ph] 19 Jun 2007
Measuring the Balmer jump and the effective gravity in FGK stars Michael S. Bessell arxiv:0706.2739v1 [astro-ph] 19 Jun 2007 RSAA, The Australian National University, Mt Stromlo, Cotter Rd, Weston, ACT
More informationarxiv:astro-ph/ v1 22 Jun 1999
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 05(02.01.1, 11.01.2, 11.14.1, 11.17.3, 11.19.1) ASTRONOMY AND ASTROPHYSICS Barnes Evans relations for late type giants and
More informationThe Composition and Evolutionary Status of Proxima Centauri
American Journal of Astronomy and Astrophysics 2017; 5(1): 1-5 http://www.sciencepublishinggroup.com/j/ajaa doi: 10.11648/j.ajaa.20170501.11 ISSN: 2376-4678 (Print); ISSN: 2376-4686 (Online) Letter The
More informationTHE AGE OF THE KIC SYSTEM. James MacDonald and D. J. Mullan Department of Physics and Astronomy, DE 19716, USA
THE AGE OF THE KIC 7177553 SYSTEM James MacDonald and D. J. Mullan Department of Physics and Astronomy, DE 19716, USA ABSTRACT KIC 7177553 is a quadruple system containing two binaries of orbital periods
More informationarxiv: v1 [astro-ph.sr] 6 Sep 2012
Astron. Nachr. / AN 334, No. 1, 1 7 (2013) / DOI This.is/not.aDOI Fundamental properties of lower main-sequence stars Guillermo Torres Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge
More informationarxiv:astro-ph/ v2 2 Mar 2005
Astronomy & Astrophysics manuscript no. Ha281 February 2, 2008 (DOI: will be inserted by hand later) A planet-sized transiting star around OGLE-TR-122 Accurate mass and radius near the Hydrogen-burning
More informationLecture Outlines. Chapter 17. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 17 Astronomy Today 8th Edition Chaisson/McMillan Chapter 17 Measuring the Stars Units of Chapter 17 17.1 The Solar Neighborhood 17.2 Luminosity and Apparent Brightness 17.3 Stellar
More informationObserved Properties of Stars - 2 ASTR 2120 Sarazin
Observed Properties of Stars - 2 ASTR 2120 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Hipparchus 1) Classified stars by brightness,
More informationDetermination of effective temperatures for an extended sample of dwarfs and subdwarfs (F0-K5)
ASTRONOMY & ASTROPHYSICS JUNE I 1996, PAGE 227 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 117, 227-254 (1996) Determination of effective temperatures for an extended sample of dwarfs and subdwarfs
More informationarxiv: v1 [astro-ph.ga] 20 Jun 2013
IAUS298 Setting the scene for Gaia and LAMOST Proceedings IAU Symposium No. 298, 2014 S. Feltzing, G. Zhao, N.A. Walton & P.A. Whitelock, eds. c 2014 International Astronomical Union DOI: 00.0000/X000000000000000X
More informationKinematics of solar neighborhood stars and its dependence on age and metallicity
RAA 2015 Vol. 15 No. 3, 393 406 doi: 10.1088/1674 4527/15/3/008 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Kinematics of solar neighborhood stars
More informationarxiv:astro-ph/ v2 23 Apr 1999
A Study of the B V Colour Temperature Relation Maki Sekiguchi 1 and Masataka Fukugita 2,1 1 Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan 2 Institute for Advanced Study,
More informationUniverse. Tenth Edition. The Nature of the Stars. Parallax. CHAPTER 17 The Nature of Stars
Universe Tenth Edition The Nature of the Stars Roger A. Freedman, Robert M. Geller, William J. Kaufmann III CHAPTER 17 The Nature of Stars W. H. Freeman and Company Parallax Careful measurements of the
More informationThe helium abundance and ΔY/ΔZ in lower main-sequence stars
Mon. Not. R. Astron. Soc. 382, 1516 1540 (2007) doi:10.1111/j.1365-2966.2007.12512.x The helium abundance and ΔY/ΔZ in lower main-sequence stars Luca Casagrande, 1 Chris Flynn, 1 Laura Portinari, 1 Leo
More informationLimb darkening laws for two exoplanet host stars derived from 3D stellar model atmospheres
Astronomy & Astrophysics manuscript no. LDC paper c ESO 2012 January 29, 2012 Limb darkening laws for two exoplanet host stars derived from 3D stellar model atmospheres Comparison with 1D models and HST
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationLessons learnt from the Solar neighbourhood and the Kepler field
Astronomische Nachrichten, 9 December 2015 Lessons learnt from the Solar neighbourhood and the Kepler field Luca Casagrande 1,, Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The
More information