Goal: identify candidate E-M counterparts to observe with ground-based telescopes.
Approach: select candidates, jointly, on the basis of position (RA,Dec), distance (parallax), frequency (optical variability), inclination (eclipsing).
Specific needs:
Select list of targets on the basis of Galactic (l,b) or Celestial coordinates (RA,Dec).
a. All SNR>XX objects above b>30 deg, or
b. Within XX deg of (RA,Dec) coordinate
Given an input prior on Chirp Mass, output distance posterior.
a. A simple prior on chirp mass should capture most WD+WD binaries. Chirp mass for He+He ~ 0.2, He+CO ~ 0.35, CO+CO ~ 0.5.
Use inclination as an optional constraint on eclipsing systems. Reject face-on systems (no optical variability).
Export candidates in human-readable format (columns of ASCII numbers).
Goal: identify candidate E-M counterparts to observe with ground-based telescopes.
Approach: select candidates, jointly, on the basis of position (RA,Dec), distance (parallax), frequency (optical variability), inclination (eclipsing).
Specific needs:
Select list of targets on the basis of Galactic (l,b) or Celestial coordinates (RA,Dec). a. All SNR>XX objects above b>30 deg, or b. Within XX deg of (RA,Dec) coordinate
Given an input prior on Chirp Mass, output distance posterior. a. A simple prior on chirp mass should capture most WD+WD binaries. Chirp mass for He+He ~ 0.2, He+CO ~ 0.35, CO+CO ~ 0.5.
Use inclination as an optional constraint on eclipsing systems. Reject face-on systems (no optical variability).
Export candidates in human-readable format (columns of ASCII numbers).