The Weight-Watcher Program for Subdwarfs
We propose to use HST/FGS1r to measure five subdwarf spectroscopic binaries to determine masses for the components. Their metallicities, [Fe/H], range from -0.5 to -2.5, and their projected minimum separations range from 9 to 24 mas. These binaries are resolvable with HST/FGS1r but not any ground-based technique.
Currently, there are only two subdwarf systems having any mass measurements. The proposed work will boost the total number of subdwarf systems with masses from two to seven, and allow us to construct the first mass-luminosity relation for low-metallicity stars.
We will use FGS1r to observe the targets in TRANSFER mode in an attempt to resolve the spectroscopic binaries. The observations will be made at a time that corresponds to maxium elongation (or projected separation). This measurement will be used to establish the angular extent of each binary's semi-major axis. which will yield the orbital inclination, and when combined with the spectroscopic data, the mass of each star.
COOL STARS
12
false
0.0
false
false
false
false
false
false
SUPPORTED
STAR
POPULATION II
B-V=1.56
J2000
03 39 35.1000
+18 18 43.00
J2000
STAR
POPULATION II
B-V=0.70
J2000
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+04 10 35.00
J2000
STAR
POPULATION II
B-V=0.67
J2000
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+18 41 40.00
J2000
STAR
POPULATION II
B-V=0.44
J2000
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+25 42 8.00
J2000
STAR
POPULATION II
B-V=0.93
J2000
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+27 55 18.00
J2000
FGS
TRANS
No
F583W
FGS
TRANS
No
F583W
FGS
TRANS
No
F583W
FGS
TRANS
No
F583W
FGS
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No
F583W
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