GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat Algorithms for CU8 (1/10)

Slides:

Advertisements

Similar presentations

THESIS – the Terrestrial and Habitable-zone Exoplanet Spectroscopy Infrared Spacecraft a concept for a joint NASA/ESA exoplanet characterization mission.

Advertisements

PROGRAMMING LANGUAGE (JAVA) UNIT 42 BY ROBERT BUTTERFIELD TELEPHONE Data Structures and Algorithms.

THE LIFE CYCLE OF STARS Chapter 15 – 2 Part 2. A Tool for Studying Stars A Danish astronomer, Ejnar Hertzsprung, and American astronomer, Henry Russel,

Star Properties!!.

Agenda Review magnitude scale and HR diagrams

Spectral Classification: The First Step in Quantitative Spectral Analysis Richard Gray Appalachian State University.

Reaching the 1% accuracy level on stellar mass and radius determinations from asteroseismology Valerie Van Grootel (University of Liege) S. Charpinet (IRAP.

Probing the evolution of stellar systems Andreas Zezas Harvard-Smithsonian Center for Astrophysics.

Spectra of different kinds of celestial objects Makemake.

ECLIPSING BINARIES IN OPEN CLUSTERS John Southworth Dr Pierre Maxted Dr Barry Smalley Astrophysics Group Keele University.

The HR Diagram Astronomy 315 Professor Lee Carkner Lecture 8.

Science Team Management Claire Max Sept 14, 2006 NGAO Team Meeting.

Stars science questions Origin of the Elements Mass Loss, Enrichment High Mass Stars Binary Stars.

GHOST, Brussels, Feb.14th The GHOST in CU8 Coralie Neiner Paris-Meudon Observatory GHOST website:

1 Explain how knowledge of Stefan-Boltzmann law leads to understanding of temperatures and radii of stars. Summarize the circumstances under which objects.

White Dwarfs. References D. Koester, A&A Review (2002) “White Dwarfs: Recent Developments” Hansen & Liebert, Ann Rev A&A (2003) “Cool White Dwarfs” Wesemael.

Dusty old star offers window to our future --- GD 362 Department of Physics National Tsing Hua University G.T. Chen 2005/10/20.

Compilation of stellar fundamental parameters from literature : high quality observations + primary methods Calibration stars for astrophysical parametrization.

Properties of Main Sequence Stars Masses Luminosities Lifetimes Distribution.

The Life Cycles of Stars and our Sun. Gravity R 1/2 R a=0 a= GM’/(1/2 R) 2 ~ R a= GM/R 2.

Properties of Stars. Distance Luminosity (intrinsic brightness) Temperature (at the surface) Radius Mass.

The Life Cycle of a Star Presenters:. The Life Cycle of a Low-Mass Star Stellar Nebula Giant White Dwarf.

Astrophysical Parameters: Classification and Stellar Evolution A. Vallenari, R. Sordo, A. Lanzafame, A. Sozzetti, V. Andretta, G. Scandariato, I. Busà,

Layers of the Solar Atmosphere Corona Chromosphere Photosphere Details of solar activity can be seen more easily in the hotter outer layers, which are.

Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.

Spectroscopy in Stellar Astrophysics Alberto Rebassa Mansergas.

Quiz – stellar spectra.

Die Vermessung der Milchstraße: Hipparcos, Gaia, SIM Vorlesung von Ulrich Bastian ARI, Heidelberg Sommersemester 2004.

The study of evolutionary changes in intermediate mass magnetic CP stars across the HR diagram Evgeny Semenko Special Astrophysical Observatory of the.

Chapter 13: Taking the Measure of Stars Stars come in a wide range of temperatures, sizes, masses and colors. The constellation of Orion is a good example.

Zoran Simić and Milan S. Dimitrijević Astronomical Observatory, Volgina 7, Belgrade, Serbia

Stellar Classification. How we know We learn about stars by looking at them through spectroscopes. All stars produce a spectra that tells us about their.

Ground based observations for Gaia 2001 : need to have reference stars to calibrate AP algorithms for Gaia i.e. stars with well-known APs that will observed.

Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 17 The Nature of Stars CHAPTER 17 The Nature of Stars.

Upcoming Events Project Medley Sign-Up Next Week. Pick a project before then!

The White Dwarf in SS Cygni: FUSE + HST Spectral Analysis Edward M. Sion, Patrick Godon, Janine Myszka Edward M. Sion, Patrick Godon, Janine Myszka Department.

Properties of Stars.

Sait Teramo – May 6 th, 2008 Antonella Vallenari Spectral Libraries for Gaia Synthetic Spectral Libraries for Gaia A.Vallenari INAF, Osservatorio Astronomico.

Physical properties. Review Question What are the three ways we have of determining a stars temperature?

Ground Based Observations for the ESP V-1 1.Existing data and catalogues 2.Planned observations 3.Needed observations 4.Telescopes 5.Questions Sources:

Charge Exchange in Cygnus Loop R. S. Cumbee et al Satoru Katsuda et al Zhang Ningxiao.

Stellar Characteristics. Temperature Temp. is measured in Kelvins Blue stars are hot, above 30,000 K Yellow stars are warm Red stars are cool, below 3,000.

The Origins of Hot Subdwarf Stars as Illuminated by Composite- Spectrum Binaries Michele A. Stark (Penn State University) Advisor: Richard A. Wade Thursday.

CU5-DU13: Ground-based support observations for Gaia absolute photometric calibration BOLOGNA: C. Cacciari, G. Altavilla, M. Bellazzini, A. Bragaglia,

Stellar parameters estimation using Gaussian processes regression Bu Yude (Shandong University at Weihai)

20/04/02 - F.A.DMS/PS organisation 1 Proposal for tasks and schedule -Coordination is needed -Tasks -Tools -Topics -Which areas are not covered -Manpower.

Classical Novae on a Helium White Dwarf Irit Idan (Technion) Lars Bildsten ((KITP, UCSB) Ken Shen (UCSB)

Il ruolo della spettroscopia a grande campo per Gaia B. Bucciarelli - INAF/Osservatorio Astronomico di Torino S. Randich - INAF /Osservatorio Astrofisico.

GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat Choice of hot and emission stars for GBO(1/7) Objectives: Preparation phase: to develop and to test.

The Hertszprung-Russell diagram plots the luminosities (absolute magnitudes) of stars as a function of their spectral type, and reveals that stars with.

Fluorine in RCB and EHe Stars. ► RCB stars comprise a sequence of H-deficient supergiants with effective temperatures from about 3500 K, as represented.

SEGUE Target Selection on-going SEGUE observations.

Spectral Analysis Pipeline for LAMOST Project A-Li Luo LAMOST Science Division NAOC, CAS.

Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.

Fiona Ward Emily Linden. “Explain the usefulness of classifying stars according to their colors, surface temperatures, and spectral characteristics.”

Unit 2 - Cosmology Part 1: Stars Part 2: Galaxies Part 3: Origin and Evolution of the Universe.

Spectroscopy and the evolution of hot subdwarf stars

The Hubble Legacy Archive (HLA) Slitless Spectroscopy Project

Magnetic activity of F stars

To look at the theories of how the Universe began

Classification of GAIA data

How light from the stars can tell us (almost) everything about them!

A Pulsational Mechanism for Producing Keplerian Disks around Rapidly Rotating Stars Steven R. Cranmer Harvard-Smithsonian CfA.

THE LIFE CYCLE OF STARS Chapter 15 – 2 Part 2.

Origin of the Universe Bell work: Pick up handouts

Stellar spectroscopy with XTGRID

Constraints on Star Forming Galaxies at z>6.5

Distance of the Hyades A250 Lab #1. Distance of the Hyades A250 Lab #1.

1 HiCannon: Data-driven spectroscopy of cool stars at high spectral resolution Aida Behmard1, Erik Petigura2,3, Andrew Howard2 1Division of Geological.

THE LIFE CYCLE OF STARS Chapter 15 – 2 Part 2.

Presentation transcript:

GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat Algorithms for CU8 (1/10)

Algorithms for CU8 (2/10) Use photometry of unresolved ‘slow’ sources to determine the broad class of the object (single star, binary, QSO, …) GWP-S-821Discrete Source Classifier (DSC) Manager: C.Bailer-Jones GWP-S-822Generalized Stellar Parametrizer – Photometry (GSP-Phot) Manager: C.Bailer-Jones Estimate APs for the full range of type of single stars based on photometry (and parallaxes in late-mission) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat x x

Algorithms for CU8 (3/10) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat GWP-S-823Generalized Stellar Parametrizer – Spectroscopy (GSP-Spec) Manager: A.Recio-Blanco Estimate APs for the full range of type of single stars based on RVS and GSP-Phot GHOST contribution: provide spectral criteria for hot stars and emission line stars (?) x

Algorithms for CU8 (4/10) Manager: Y.Frémat The Extended Stellar Parametrizer (GWP-S ) will propose and test alternatives for the treatment of a restricted subset of "extreme" stars:  to provide a better estimate of the astrophysical parameters;  to provide additional parameters suitable to the specific type of object;  to explain, when needed, the origin of astrophysical parameters discrepancies. GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat x GWP-S-835Extended Stellar Parametrizer (ESP) GWP-S-835Extended Stellar Parametrizer (ESP)

Algorithms for CU8 (5/10) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat Hot Stars Cool Stars Emission Line Stars Anomalous Abundance Stars Teff > ~ K Teff < ~ K > ~ 2500 K C.Neiner C.Martayan A.C.Lanzafame V.Straizys D.Barrado Teff < ~ 2500 K Ultra Cool Dwarfs /Stars GWP-S-835Extended Stellar Parametrizer (ESP)

Hot Stars Cool Stars Emission Line Stars Anomalous Abundance Stars Teff > ~ K Teff < ~ K > ~ 2500 K C.Neiner C.Martayan A.C.Lanzafame V.Straizys D.Barrado Teff < ~ 2500 K Ultra Cool Dwarfs /Stars GHOST Algorithms for CU8 (6/10) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat GWP-S-835Extended Stellar Parametrizer (ESP)

Algorithms for CU8 (7/10) x GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat GWP-S-835Extended Stellar Parametrizer (ESP)

Algorithms for CU8 (8/10) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat GWP-S-835Extended Stellar Parametrizer (ESP)

GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat Algorithms for CU8 (9/10) GWP-S-835Extended Stellar Parametrizer (ESP) Development plan First algorithm delivery: mid-April 2007 (end of cycle 2) !! Objective:  Provide a prototype of the java interface software that will select the right procedure or scenario for a given « extreme-» star  with « place-holders » for the procedures. For cycle 3 the « place-holders » will have to be filled. !!!

Algorithms for CU8 (10/10) GWP-S-835Extended Stellar Parametrizer (ESP) GHOST #2: Marseille: Nov 13-14, 2006 – Yves Frémat To Dos … Emission Line Stars: can we do something for cycle 3 ?