PI Total time #CoIs, team
5
PI Total time #CoIs, team John Pritchard 107h (ELT 42m) 5-10 people who will reduce and analyse spectra and do NLTE atmospheric and radial velocity curve modelsing Not Further but Fainter: Eclipsing Binaries in the Magellanic Clouds Eclipsing binaries provide accurate Stellar masses, radii, luminosities and distances. EBs in the Magellanic Clouds allow the study of low metalicity EB systems as well as the distance and structure of these cosmologically important galaxies themselves. The ELT will open the way to make detailed spectroscopic studies of systems up to 3 magnitudes fainter than is currently possible. In this proposal we will take high resolution spectra of 30 MCEBs in the range V~16 -- V~18mag to give Radial Velocity curves and allow detailed atmospheric modeling thus increasing by factor of 3 the number of well studied such systems.
description
Not Further but Fainter: Eclipsing Binaries in the Magellanic Clouds - PowerPoint PPT Presentation
Transcript of PI Total time #CoIs, team
PI
Total time
#CoIs, team
John Pritchard
107h (ELT 42m)
5-10 people who will reduce and analyse spectra and do NLTE atmospheric and radial velocity curve modelsing
Not Further but Fainter:Eclipsing Binaries in the Magellanic Clouds
Eclipsing binaries provide accurate Stellar masses, radii, luminosities and distances. EBs in the Magellanic Clouds allow the study of low metalicity EB systems as well as the distance and structure of these cosmologically important galaxies themselves. The ELT will open the way to make detailed spectroscopic studies of systems up to 3 magnitudes fainter than is currently possible.In this proposal we will take high resolution spectra of 30 MCEBs in the range V~16 -- V~18mag to give Radial Velocity curves and allow detailed atmospheric modeling thus increasing by factor of 3 the number of well studied such systems.
Scientific Rationale
• Accurate stellar parameters at Low Metallicity:• Masses, Radii, Effective Temperatures,
Luminosities• Critical tests of stellar evolution, structure,
formation models
• Distance• LMC is the first rung of the cosmic distance scale
ladder, everything more distant than LMC is measured relative to the LMC
• Internal structure of the MCs
Immediate Objectives
• High resolution spectroscopy for Radial velocity curves and NLTE atmospheric modeling
• Increase sample of well studied systems from less than 10 to ~40.
• Study later spectral types than has so far been possible
• Detailed studies of long period systems with a Cepheid component
Run Target R.A. Dec. ToT Mag Notes
ABCD 40 MCEBs 1h,5h -60-75˚ 517h 16-19 S/N ~ 50
ABC 30 MCEBs 1h,5h -60-75˚ 107h 16-18 S/N ~ 50
ELT Justification: Exposure times are prohibitively long on (for example) UVES@VLT.
Data Reduction: No problems expected, “standard” techniques.
Run MP Mode AO T. FOV Pixel Notes
A 1 R=50k GLAO 5h 5’ 100 440nm B band/V~16
B 1 R=50k GLAO 21h 5’ 100 440nm B band/V~17
C 1 R=50k GLAO 81h 5’ 100 440nm B band/V~18
D 1 R=50k GLAO 410h 5’ 100 440nm B band/V~19
ESO-3.6m and the Milkyway
