PHAT. XIX. The Ancient Star Formation History of the M31 Disk

• Main Authors: Williams, Benjamin F., Dolphin, Andrew E., Dalcanton, Julianne J., Weisz, Daniel R., Bell, Eric F., Lewis, Alexia R., Rosenfield, Philip, Choi, Yumi, Skillman, Evan, Monachesi, Antonela
• Other Authors: Univ Arizona, Steward Observ
• Language: en
• Published: IOP PUBLISHING LTD 2017
• Subjects: galaxies: evolution; galaxies: individual (M31); galaxies: stellar content
• Online Access: http://hdl.handle.net/10150/625807; http://arizona.openrepository.com/arizona/handle/10150/625807

We map the star formation history across M31 by fitting stellar evolution models to color-magnitude diagrams of each 83 '' x 83 '' (0.3 x 1.4 kpc, deprojected) region of the Panchromatic Hubble Andromeda Treasury (PHAT) survey outside of the innermost 6' x 12' portion. We find that most of the star formation occurred prior to similar to 8 Gyr ago, followed by a relatively quiescent period until similar to 4 Gyr ago, a subsequent star formation episode about 2 Gyr ago, and a return to relative quiescence. There appears to be little, if any, structure visible for populations with ages older than 2 Gyr, suggesting significant mixing since that epoch. Finally, assuming a Kroupa initial mass function from 0.1 to 100 M-circle dot, we find that the total amount of star formation over the past 14 Gyr in the area over which we have fit models is 5 x 10(10) M-circle dot. Fitting the radial distribution of this star formation and assuming azimuthal symmetry, (1.5 +/- 0.2). x 10(11) M-circle dot of stars has formed in the M31 disk as a whole, (9 +/- 2) x 10(10). M-circle dot of which has likely survived to the present after accounting for evolutionary effects. This mass is about one-fifth of the total dynamical mass of M31.