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