First Detection of the White-Dwarf Cooling Sequence of the Galactic Bulge

TL;DR

This study uses Hubble Space Telescope data to identify the first white dwarf cooling sequence in the Galactic bulge, revealing a significant population of low-mass white dwarfs and binaries.

Contribution

It presents the first detection of a white dwarf cooling sequence in the Galactic bulge using proper motion separation, highlighting a substantial population of low-mass white dwarfs.

Findings

First identification of white dwarf cooling sequence in the bulge

30% of white dwarfs are redder than standard cooling tracks

Detection of binary systems and cataclysmic variables in the bulge

Abstract

We present Hubble Space Telescope data of the low-reddening Sagittarius window in the Galactic bulge. The Sagittarius Window Eclipsing Extrasolar Planet Search field (3'x3'), together with three more Advanced Camera for Surveys and eight Wide Field Camera 3 fields, were observed in the F606W and F814W filters, approximately every two weeks for two years, with the principal aim of detecting a hidden population of isolated black holes and neutron stars through astrometric microlensing. Proper motions were measured with an accuracy of ~0.1 mas/yr (~4 km/s) at F606W~25.5 mag, and better than ~0.5 mas/yr (20 km/s) at F606W~28 mag, in both axes. Proper-motion measurements allowed us to separate disk and bulge stars and obtain a clean bulge color-magnitude diagram. We then identified for the first time a white dwarf (WD) cooling sequence in the Galactic bulge, together with a dozen candidate extreme horizontal branch stars. The comparison between theory and observations shows that a substantial fraction of the WDs (30%) are systematically redder than the cooling tracks for CO-core H-rich and He-rich envelope WDs. This evidence would suggest the presence of a significant number of low-mass WDs and WD - main sequence binaries in the bulge. This hypothesis is further supported by the finding of two dwarf novae in outburst, two short-period (P < 1 d) ellipsoidal variables, and a few candidate cataclysmic variables in the same field.