The search for eclipsing binaries and rotation rates for Pre Main Sequence (PMS) Stars
Kurt SotoAdvisor : Keivan Stassun
Masses of Pre-Main-Sequence Stars• Life of a star determined by its mass• Theoretical models used to infer masses of stars have not
been well tested for sub-solar masses• Need eclipsing binary stars!• Only 1 sub-solar mass PMS eclipsing binary
Angular Momentum• Stars deplete most of their angular momentum
by the time they reach the main sequence• The details of this are still poorly understood • Need rotation rates of stars at various stages of
early evolution
Obtaining the Data(WIYN 0.9m!)
• Mosaic capable of imaging 1 degree by 1 degree• 1.8 degree by 1.8 degree region• Two exposure lengths: 2 sec, 240 sec• Cycle every 45 minutes (detect eclipses)• 9 night observing run• Collaborator extends observing length to 20 days (long
rotation periods and diurnal gaps)• 660 frames = 70 Gb of raw data => light curves for
100,000 stars
Crosstalk
Zero Correction
Dome Flats
Sky Flats
Area Correction
Astrometry
What’s Next
• Use DAOFIND to locate stars from frame to frame
• Adjust images for sky opacity• Prepare light curves• Look for signature eclipsing binary light
curves• Calculate rotation rates and masses
