Confronting predictions of stellar evolution theory gregory feiden (uppsala) andrew mann (texas at austin) eric gaidos (hawaii) tabetha boyajian (yale)

Slides:



Advertisements
Similar presentations
Late gas accretion onto primordial mini-halos a model for pre-reionization dwarfs and extragalactic compact High-Velocity Clouds Massimo Ricotti (U of.
Advertisements

1 MSci Astrophysics 210PHY412 Stellar structure and evolution Dr. Stephen Smartt (Room S039) Department of Physics and Astronomy Online.
Small is Beautiful: Cataclysmic Variables from the SDSS John Southworth Boris Gänsicke Tom Marsh + many others.
Including Magnetic Effects in 1-D Stellar Models Greg Feiden & Brian Chaboyer (Dartmouth) Three color EUV image of the Sun. White lines show a model of.
Improving mass and age estimates of unresolved stellar clusters Margaret Hanson & Bogdan Popescu Department of Physics.
The Group of Bootis Stars Dr. Ernst Paunzen Institute for Astronomy University of Vienna.
The Distribution of DM in Galaxies Paolo Salucci (SISSA) TeVPa Paris,2010.
Exoplanet- Asteroseismology Synergies Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK EAHS2012, Oxford, 2012 March 15.
Eric Y. Hsiao University of Victoria.  less dust extinction  low redshift  standard candles in JHK bands  independent measure of Hubble constant 
SOLUTION 1: ECLIPSING BINARIES IN OPEN CLUSTERS The study of eclipsing binaries in open clusters allows strong constraints to be placed on theoretical.
Venice – Gregory RudnickMarch 2006 The Mean SED and Stellar Mass Density at z
Q. Daniel Wang and Cornelia Lang (U. of Massachusetts) Eric Gotthelf (Columbia U.) Chandra X-ray Survey of the Galactic Center: On the Nature of the X-ray.
Multiple, Coeval and Hubble-like bipolar outflows Romano L.M. Corradi Isaac Newton Group of Telescopes La Palma, Spain.
General Principles for References Use the most original source possible. Use the most up-to-date and reliable source available. Your paper is only as good.
PhyloSub Jiao et. al. BMC Bioinformatics 2014, 15:35.
Advanced Methods for Studying Astronomical Populations: Inferring Distributions and Evolution of Derived (not Measured!) Quantities Brandon C. Kelly (CfA,
Extrasolar Planets Z:\exo\presentations\EGS2001_exo.ppt, :54AM, 1 Tidal interactions of close-in extrasolar planets with their host stars.
References: Sozzetti, A., et al. 2007, ApJ, 664, 1190 Mandushev, G., et al. 2007, ApJ, 667, L195 Sozzetti, A., et al. 2007a, ApJ, in preparation Sozzetti,
A New Technique to Measure ΔY/ΔZ A. A. R. Valcarce (UFRN) Main collaborators: J. R. de Medeiros (UFRN)M. Catelan (PUC) XXXVII SAB meeting Águas de Lindóia,
I N T R O D U C T I O N The mechanism of galaxy formation involves the cooling and condensation of baryons inside the gravitational potential well provided.
Summary of Experiences from Observations of the Be  binary  Sco Anatoly Miroshnichenko University of North Carolina at Greensboro USA Properties of Be.
The study on Li abundances of solar-like stars Li Tanda Beijing Nomal University
Congratulations! n Everyone here chose and confronted a current original, empirical study and struggled to comprehend and communicate why and how it had.
Measuring Human Intelligence with Artificial Intelligence Adaptive Item Generation Sangyoon Yi Susan E. Embretson.
White Dwarf Binaries in Globular Clusters Fred Rasio (Northwestern)
CARMA Large Area Star-formation SurveY  Completing observations of 5 regions of square arcminutes with 7” angular resolution in the J=1-0 transitions.
What have we learned from Eclipsing Binaries in the Orion Nebula? Keivan Guadalupe Stassun Vanderbilt University.
1 Neptune Mass Exoplanets Jeff Valenti M Jupiter / 19 = M Neptune = 17 M Earth Geoff Marcy (Berkeley)Debra Fischer (Yale) Andrew Howard (Berkeley)John.
The Colonial Origins of Comparative Development: An Empirical Investigation A presentation in the context of institutions and coordination failure.
WEEK 1 You have 10 seconds to name…
Measurement of D-meson azimuthal anisotropy in Au+Au 200GeV collisions at RHIC Michael R. Lomnitz Kent State University Lawrence Berkeley National Laboratory.
A CDM view of the Local Group dSphs Jorge Peñarrubia In collaboration with Julio F. Navarro & Alan McConnachie Jorge Peñarrubia In collaboration with Julio.
 Density and temperature conspire to have higher ionization species peak at higher radii (below); this qualitative behavior is seen for all feedback models.
CHARA Collaboration Year-Five Science Review Dynamite Diameters Tabetha Boyajian GSU/CHARA Presented by Hal McAlister.
WIDE BINARY SCIENCE USING PAN-STARRS1 NIALL DEACON (MPIA) MICHAEL LIU, EUGENE MAGNIER, WILL BEST, KIMBERLY ALLER, MICHAEL KOTSON (HAWAII), BRENDAN BOWLER.
A Pulsar Wind Nebula Origin for Luminous TeV Source HESS J Joseph Gelfand (NYUAD / CCPP) Eric Gotthelf, Jules Halpern (Columbia University), Dean.
Dynamite Diameters Observations of main sequence stars with long baseline optical/infrared interferometry Tabetha Boyajian (Georgia State University /
BBN abundance observations Karl Young and Taryn Heilman Astronomy 5022 December 4, 2014.
The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2 Christopher J. Conselice (University of Nottingham) with Asa Bluck, Ruth Gruethbacher,
Figure 6 from HST/WFC3 Near-infrared Spectroscopy of Quenched Galaxies at z ~ 1.5 from the WISP Survey: Stellar Population Properties (Image 1 of 8) A.
Figure 15 from Star Formation in the Central 400 pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects (Image 1 of 2) F. Yusef-Zadeh.
Week-2-Individual-Reliability-and-Validity- Paper Check this A+ tutorial guideline at 382/BSHS-382-Week-2-Individual-Reliability-
Figure 7 from The Evolution of Dwarf Galaxy Satellites with Different Dark Matter Density Profiles in the ErisMod Simulations. I. The Early Infalls Mihai.
The Complete Calibration of the Color-Redshift Relation (C3R2) Survey
Figure 5 from The ACS LCID Project. II
On the origin of Microturbulence in hot stars
Gregory D. Fleishman et al ApJ doi: / X/802/2/122 Information:
Figure 3 from The ACS Nearby Galaxy Survey Treasury. VIII
Figure 4 from Spectroscopic Properties of Star-forming Host Galaxies and Type Ia Supernova Hubble Residuals in a nearly Unbiased Sample Chris B. D'Andrea.
Figure 1 from Spectroscopic Properties of Star-forming Host Galaxies and Type Ia Supernova Hubble Residuals in a nearly Unbiased Sample Chris B. D'Andrea.
Figure 3 from On the Incorporation of Metallicity Data into Measurements of Star Formation History from Resolved Stellar Populations Andrew E. Dolphin.
Figure 2 from Large-scale Kinematics, Astrochemistry, and Magnetic Field Studies of Massive Star-forming Regions through HC3N, HNC, and C2H Mappings (Image.
Figure 2 from Thermodynamics of the Solar Corona and Evolution of the Solar Magnetic Field as Inferred from the Total Solar Eclipse Observations of 2010.
Figure 6 from Detailed Compositional Analysis of the Heavily Polluted DBZ White Dwarf SDSS J : A Window on Planet Formation? (Image 1.
EDD 563 Competitive Success/snaptutorial.com
EDD 563 Innovative Education- -snaptutorial.com
EDD 563 Education for Service-- snaptutorial.com.
EDD 563 Teaching Effectively-- snaptutorial.com
IMF inferred based on field stars (red) and based on a variety of clusters (blue, green, and black) (Kroupa 2002)
What (exo)-planetary science can be done with microlensing?
Speaker:Yi Xie Lunch Talk
B1 long answer questions
Specific Star Formation Rates to z=1.5
Galactic Astronomy 銀河物理学特論 I Lecture 3-4: Chemical evolution of galaxies Seminar: Erb et al. 2006, ApJ, 644, 813 Lecture: 2012/01/23.
A Search for Quiet Massive X-Ray Binaries
Note topic for chapter 17 what is the source of the sun’s energy
Q. Daniel Wang and Cornelia Lang (U. of Massachusetts)
Galactic Astronomy 銀河物理学特論 I Lecture 3-3: Stellar mass function of galaxies Seminar: Perez-Gonzalez et al. 2008, ApJ, 675, 234 Lecture: 2012/01/16.
BETONLINEBETONLINE A·+A·+
Lease and Real Estate Service in Austin, Texas.
Presentation transcript:

confronting predictions of stellar evolution theory gregory feiden (uppsala) andrew mann (texas at austin) eric gaidos (hawaii) tabetha boyajian (yale) the case of single field

knowing your dwarf 05 Jan 2015AAS 225 Feiden & Chaboyer (2012, ApJ, 757, 42)Boyajian et al. (2012, ApJ, 757, 112)

parameter inference 05 Jan 2015AAS 225 Gl 411

model reliability 05 Jan 2015AAS 225

origins 05 Jan 2015AAS 225

origins 05 Jan 2015AAS 225

empirically determining dwarf properties and model comparisons 05 Jan 2015AAS 225 see talk by andrew mann full paper on the arXiv this week