0Assigned ID: 334
----- Attempting Submission 1 (Fri Apr 08 00:41:17 GMT 2016) -----
HST Phase I Proposal 334 (cy24asse.apt) successfully submitted.
Receipt: # 334-1This Phase II was developed by reproducing and extending the Phase II for GO-14161 by Tom Ayres. That GO-14161 program
has successfully obtained E230H spectra at longer UV wavelengths of HD 140283, one of the targets in this proposal. The
Proposal Description incorporates the GO-14161 considerations for the observing plan, and includes highlights of the TAC
recommendations as well as the overall goals and analysis approach of this proposal. The only change from the proposal is
the minor adjustment in wavelength to the HD 140283 E230H spectral observations, granted prior approval from the PC. Sumitted by PC.1566924025----- Attempting Submission 1 (Tue Jul 12 23:19:54 GMT 2016) -----Tracing the Earliest Nucleosynthesis from Elements Just Past the Iron Peak in Extremely Metal-Poor DwarfsThe assembly sequence of our Galactic halo is encoded in spectra of its surviving low-metallicity turnoff stars. While the investigation of the heaviest elements (Z > 55) reveals they were produced in two independent time scales by rapid- and slow neutron capture (r- and s-process), the light trans-ironic elements with atomic number Z from 32 to 52 show striking abundance patterns that are open to a range of interpretation. Part of the mystery may be due to the need to determine their abundances in dwarfs from ultraviolet spectra, which are heavily contaminated by stronger lines whose identity is often unknown. We will provide clarification of their empirical behavior by adding high-resolution spectra near 2000A for two cool stars of low metallicity, 1/400 and 1/100 solar, and analyzing them together with similar spectra of other low-metallicity turnoff stars using all the latest tools. This includes incorporating newly-identified Fe I lines as they are found, comparing theoretical spectra for each star with high-resolution observations over all available optical and ultraviolet wavelengths, and comparing the results from two independent synthetic-spectrum approaches. This analysis should clarify current systematic errors in modeling and in line transition probabilities (gf-values). In so doing it will provide reliable abundances for a range of trans-Fe elements in extremely metal-poor stars, for quantitative comparison with a half-dozen viable models of their production. The results will shed light on the nature and time scales of production of these elusive elements, and their incorporation into stars that are relics of the earliest phase of our Galaxy.Our targets are two very metal-poor turnoff stars, HD 140283 and HD 19445. Both targets have been observed previously, safely, by STIS; and have sufficient STIS and IUE spectra to define accurate SEDs (for use with the STIS spectroscopic ETC). Each has a metallicity <1/100 solar. Our model parameters Teff, log g, [Fe/H] are 5700K, 3.6, -2.6 for HD 140283, and 6050, 4.5, -2.0 for HD 19445. HD 19445 is thus a true dwarf, while HD 140283 is a post-turnoff star. At the temperatures, luminosities, and ages of such halo turnoff stars, no flaring or other strong luminosity variation is expected, and indeed none has been observed in either star.
The TAC has emphasized that the UV observations are necessary to probe two processes, nu p and weak r, that are thought to be important for elements between Z of 32 and 52 [such as Mo, Ru at Z=42, 44], with Ge [Z=32] being a good discriminant for the processes involved, and As [Z=33] valuable due to its single stable isotope. As detailed in the proposal, to derive reliable light-element abundance ratios we will provide analyses, and address their systematics. Our analysis will include the hotter, weaker-lined star HD 84937, with Teff, log g, [Fe/H] = 6300K, 4.0, -2.25, and the stronger-lined star HD 94028, with 6050K, 4.3, -1.40, now that GO-14161 has obtained complete E230H coverage over 1880A - 3140A for both stars. It is critical to analyze all four stars together. Their modest but significant diversity in temperature and metallicity will help disentangle line blending and confirm trans-Fe gf values, as well as establish trends in trans-Fe ratios with metallicity and with other abundance excesses, notably those produced by the r-process, the rapid capture of neutrons believed to occur in Type II supernovae. The four stars may also represent different halo populations. HD 140283 has a near-solar [Mo/Fe] ratio and a very low [Ge/Fe] ratio, but is a rare low r-process star, like HD 122563 (the green star in Fig. 1 of the proposal). Both HD 84937 and HD 19445 have a near-solar [Ge/Fe] ratio and are moderately enhanced in heavy r-process elements, while HD 94028 has the highest [Mo/Fe] known among old stars with mild r-process enhancements. Intercomparing their light trans-Fe abundance ratios should reveal any potential dependence of their own production process(es) on r-process production and on overall metallicity, at levels corresponding to the Galaxy's oldest surviving individual stars and stars in globular clusters.
To detect the weak lines of trans-Fe elements, we will obtain E230H spectra at and below 2100A, using the standard slit width of 0.2" x 0.09" as was done for HD 84937 and HD 94028. For HD 19445, we adopt the standard c2013 grating setting, covering 1880A - 2145A. This will be the first E230H spectrum obtained for this star. For HD 140283, for which existing E230H spectra already cover 1950A - 3140A, we have received PC approval for the minor adjustment in wavelength caused by adopting the E230H i1963 setting, covering 1830A - 2095A. Using E230H values and stellar turnoff line widths in the Cayrel (1988) formulae (3) and (5), we find at S/N/resel = 60, a line 8% deep is a 4-sigma detection. The S/N level and weakness of the lines in this region, seen in Fig. 3 of our submitted proposal, led us to propose S/N=60 for HD 140283, and S/N=55 for HD 19445, both at 2000A. With IUE fluxes of 6.6E-13 at 2000A from LWR02380LL, and 3.0E-13 at 1850A from SWP02665, ETC runs #822431 and #822448 provide an exposure time of 56.8 ks for HD 140283, yielding S/N=60 at 2000A, >75 redward of 2050A, and 26.4 at 1850A. For HD 19445, with flux 5E-13 at 2000A (LWP17069LL) and 2.4E-13 at 1880A (SWP37935LL), ETC runs #794658 and #824119 for 58.7 ks yield S/N=55 at 2000A, >90 redward of 2080A, and 23 at 1880A.
In Phase II we have cast these exposures into visits of at most three orbits, as requested to ease the burden on scheduling. We target HD 19445 in one 2-orbit visit plus seven 3-orbit visits, for a total exposure time 59.8ks, and target HD 140283 in seven 3-orbit visits (54.7ks). Target acquisitions, modeled on those of GO-14161, initially are by the CCD, with the MIRROR and ND3 filter; exposure times are set to yield more than adequate counts. The peak-ups onto the slit are performed in dispersed light with the low-res optical grating, G430L, and the CCD; the minimal (0.2 s) exposure times yield roughly a million, or more, total counts; but avoid saturation of the spectral segment. The short 3-orbit sequences, each with a single grating setting, make throughput losses due to slight pointing drifts less likely, and allow breathing effects to be recognized more easily. As was done for the GO-14161 observations, we waive the proprietary period.Stellar PhysicsStellar Populations0falsetruefalsefalsefalsefalseSUPPORTEDSTARF3-F9HALOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates corrected to epoch 2016J2000J2000STARF3-F9HALOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates revised for epoch 2016 by T Ayres and adopted for GO-14161J2000J2000STIS/NUV-MAMASpectroscopicNoNoE230H2013STIS/NUV-MAMASpectroscopicNoNoE230H2013The scheduling data was generated by CASM 25.0.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit6749194601249289951.xml148781459100071.0(Tic-Visit
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