Probing the Distance and Structure of the LMC Using Eclipsing Binaries: STIS Spectrophotometry

Details Probing the Distance and Structure of the LMC Using Eclipsing Binaries: STIS Spectrophotometry Probing the Distance and Structure of the LMC Using Eclipsing Binaries: STIS Spectrophotometry

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9509g&link_type=abstract

HST Proposal ID #9509

Computer Science

Hst Proposal Id #9509

Scientific paper

The distance to the LMC is crucial to calibrating the Cosmic Distance Scale but remains controversial and uncertain despite the efforts of many investigators. We have shown that the analysis of eclipsing binary {EB} systems has the potential to resolve this controversy. We have determined accurate distances to three eclipsing binaries in the LMC. Two EBs in the LMC bar, HV 2274 and EROS 1044, yield a consistent distance of 46.0+/-1.2 kpc for the bar itself. A third system, HV 982, is located at a greater distance {50.2+/-1.2 kpc}, which is similar to that of the nearby SN 1987A {51.4+/-1.2 kpc}. These results may suggest a significant depth to the LMC populations but a larger stellar sample is needed to verify this. The distances of the program stars were derived from ground-based light curves, HST or CTIO radial velocity data, and HST UV/optical spectrophotometry. We propose HST/STIS low-resolution spectra of seven LMC EBs for which we already have radial velocity and light curves. This will permit us to complete the analysis and derive accurate {to 3%} individual distances. HST/STIS spectroscopy {covering 115-800nm} is a key dataset because it provides Teff, Fe/H, and A_lambda. The ensemble of targets, in addition to nailing down the distance to the LMC, will provide fundamental stellar properties and a detailed probe of the structure and spatial extent of this important galaxy, in particular its line-of-sight depth.

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