** Copied visit 08 into visit 58 for rescheduling due to MAMA suspension 9/14/10 **
----- Attempting Submission 1 (Wed Jul 02 20:47:55 GMT 2008) -----
----- Attempting Submission 2 (Mon Sep 20 14:38:25 GMT 2010) -----
everything has been checked over
Assigned ID: 454
----- Attempting Submission 1 (Fri Mar 07 18:25:06 GMT 2008) -----
Cosmo-chronometry and Elemental Abundance Distribution of the Ancient Star HE1523-0901
We propose to obtain near-UV HST/STIS spectroscopy of the extremely metal-poor, highly r-process-enhanced halo star HE 1523-0901, in order to produce the most complete abundance distribution of the heaviest stable elements, including platinum, osmium, and lead. These HST abundance data will then be used to estimate the initial abundances of the long-lived radioactive elements thorium and uranium, and by comparison with their observed abundances, enable an accurate age determination of this ancient star. The use of radioactive chronometers in stars provides an independent lower limit on the age of the Galaxy, which can be compared with alternative limits set by globular clusters and by analysis from WMAP. Our proposed observations of HE1523-0901 will also provide significant new information about the early chemical history of the Galaxy, specifically, the nature of the first generations of stars and the types of nucleosynthetic processes that occurred at the onset of Galactic chemical evolution.
We propose to obtain 26 orbits of HE 1523-0901. The inital exposure times we employed adopted expected total overheads of 24 min for the first orbit (including guide star acquisition, target acquisition, peakup target acquisition, overheads -- 6 minutes each), and 11 min for all subsequent orbits (reacquisition time (5 min), overheads (6 min)), and a visibility time of 54 min per orbit. This is now slightly changed, but the total exposure time has not changed a lot. Each visit now contains 3 orbits to ensure that accurate pointing is maintained throughout the visit. All visits are straight forward since they are all the same and there is only one target. We have 9 visits in total, where the last visit contains only 2 orbits.
Our target S/N is set to 51/1 at 2900A, 45 at 2650A, and 26 at 2450A. The expected S/N ratios have been calculated by comparison with previous HST observations of the metal-poor star CS 22892-052, a star with similar physical parameters to HE 1523-0901. The physical parameters adopted for HE 1523-0901 are Teff/logg/[Fe/H] = 4630/1.0/-3.0, while those for CS 22892-052 are 4760/1.3/-3.1.
We use the STIS ETC as well as adopting previously measured HST fluxes for CS 228982-052 of 3.8x10^-15 (2900 A) and 5.5x10^-15 (3060A) in the following calculations. We increase the expected flux for
HE 1523-0901 (V = 11.1) by the V magnitude differences with respect to CS 22892-052 (V = 13.2), and use the STIS ETC to obtain the following estimates of S/N.
We are requesting full resolution in the original data because we hope to detect many weak, blended lines which will require the highest resolution possible. The star has a surprising rich optical spectrum, so we do not wish to miss the opportunity of detecting weak lines from unanticipated species by observing at less than the full resolution of the STIS Echelle. The wavelengths chosen for expected S/N correspond to local peaks in the continuum in various intervals, and the S/N estimates quoted are per resolution element.
Peak up problems
COOL STARS
12
false
0.0
0.0
false
false
false
false
false
false
SUPPORTED
STAR
HALO
K III-I
POPULATION II
Coordinates are from GSC2.2
B=12.2+-0.05
S231023250
2MASSJ15260106-0911388
J2000
15 26 1.2000
-09 11 38.00
J2000
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
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