Assigned ID: 992
----- Attempting Submission 1 (Sat Feb 25 00:25:46 GMT 2012) -----
Everything looks good as far as I can tell. We observed both of these stars successfully in Cycle 18 using
the same STIS setup (except for a different central wavelength setting), and I have used the same input
parameters for the coordinates, proper motions, parallaxes, etc. here. The new target confirmation
charts look good. Please advise me if you see any reasons this submission may be deficient. Thanks
for your help! -Ian
Submission failed due to an error:
sun.awt.X11.XException: Cannot write XdndAware property
Submission failed due to an error:
sun.awt.X11.XException: Cannot write XdndAware property
Submission failed due to an error:
sun.awt.X11.XException: Cannot write XdndAware property
Submission failed due to an error:
sun.awt.X11.XException: Cannot write XdndAware property
----- Attempting Submission 2 (Thu Jun 21 20:18:14 GMT 2012) -----
The Most Complete Template for r-process Nucleosynthesis beyond the Solar System
We propose to observe two metal-poor stars that present a unique opportunity to expand the chemical inventory to unprecedented levels in an environment beyond the solar system. The proposed observations will allow us to detect several key elements, including arsenic (As, Z=33) and selenium (Se, Z=34), that cannot be detected from the ground. These elements are key to understanding the nature of the r-process in the first generations of stars that drive chemical evolution of the Galaxy, yet their abundance in the one star where they have been detected is not fully explained by current models. We will use STIS to obtain high-resolution UV spectra from 1900 to 2380 Angstroms in two metal-poor stars enriched with modest but differing amounts of r-process material, HD 108317 and HD 128279. We will perform an abundance analysis and derive abundances or meaningful upper limits for the heavy elements Cu, Zn, Ge, As, Se, Zr, Mo, Cd, Te, Yb, Os, Ir, Pt, and Pb. This work is supported by recent laboratory experiments and theoretical studies that continue to provide data of wider interest to the atomic, nuclear, and astrophysics communities.
We will use STIS to observe a 2 metal-poor stars that have been enriched by small amounts of r-process material to study elements rarely detected in late-type stellar atmospheres. The goal of these observations is to acquire as many photons as possible from 1900 to 2300A at R~30,000 for each star. There are no time constraints on the observations.
COOL STARS
12
false
0.0
0.0
false
false
false
false
SUPPORTED
STAR
G III-I
POPULATION II
This object was generated by the targetselector and retrieved from the SIMBAD database.
GSC00288-00288
J2000
J2000
(B-V)=0.60+/-0.05, E(B-V)=0.02+/-0.02, TYPE=G5III
STAR
G III-I
POPULATION II
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(B-V)=0.60+/-0.05, E(B-V)=0.10+/-0.05, TYPE=G5III
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
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