0
Assigned ID: 37
----- Attempting Submission 1 (Wed Mar 29 16:33:48 GMT 2017) -----
HST Phase I Proposal 37 (cy25fei.apt) successfully submitted.
Receipt: # 37-1
0
----- Attempting Submission 1 (Fri Jul 14 14:16:25 GMT 2017) -----
Astrophysics Meets Atomic Physics: Fe I Line Identifications and Templates for Old Stellar Populations from Warm and Hot Stellar UV Spectra
Imaging surveys from the ultraviolet to the infrared are recording ever more distant astronomical sources. Needed to interpret them are high-resolution ultraviolet spectral templates at all metallicities for both old and intermediate-age stars, and the atomic physics data essential to model their spectra. To this end we are proposing new UV spectra of four warm and hot stars spanning a wide range of metallicity. These will provide observational templates of old and young metal-poor turnoff stars, and the "laboratory source" for the identification of thousands of lines of neutral iron that appear in stellar spectra but are not identified in laboratory spectra. By matching existing and new stellar spectra to calculations of energy levels, line wavelengths, and gf-values, Peterson & Kurucz (2015) and Peterson, Kurucz, & Ayres (2017) identified 124 Fe I levels with energies up to 8.4eV. These provided ~3000 detectable Fe I lines from 1600A to 5.4mu, and yielded empirical gf-values for 640 of these. Here we propose high-resolution UV spectra reaching 1780A for the first time at the turnoff, to detect and identify the strongest Fe I lines at 1800 - 1850A. This should add ~250 new Fe I levels. These spectra, plus one at lower resolution reaching 1620A, will also provide empirical UV templates for turnoff stars at high redshifts as well as low. This is essential to deriving age and metallicity independently for globular clusters and old galaxies out to z~3. It will also improve abundances of trace elements in metal-poor stars, constraining nucleosynthesis at early epochs and aiding the reconstruction of the populations of the Milky Way halo and of nearby globular clusters.
The observing program is straightforward. All of the targets have been observed previously, safely, by STIS, and all have sufficient STIS and IUE spectra to accurately characterize SEDs for use with the STIS spectroscopic ETC, despite having heavy-element abundances that range from 1/200 solar to twice solar. None of these stars are known to flare. None are known to be variable, including HD 128167, neither from its archival E230H spectra (GO 7433, PI Heap) nor from the photometric determination of its temperature (Paunzen et al. 2014, A&A, 567, A67). The use of narrow slits, and previous STIS and IUE NUV spectra, preclude possible interference from nearby stars. Target acquisitions initially are by the CCD, with the MIRROR and ND3 filter; exposure times are set to yield more than adequate counts. The narrow-slit peak-ups are performed in dispersed light with the low-res optical grating, G430L, and the CCD. The minimal (0.1 s) peak-up exposure time yields more than sufficient total counts while avoiding saturation of the spectral stripe. For the two brightest stars, the exposures at each E230H grating setting are broken into two segments, for safety and calibration purposes.
For all E230H spectra, our program uses standard E230H primary grating settings, completing NUV E230H spectral coverage to 1780A for one very weak-lined turnoff star, and to various NUV limits for three hotter stars spanning a wide range of line strengths, as this is vital for Fe I identifications. The longest E230H exposures are required to discern the thousand unidentified Fe I lines needed for the anticipated identification of ~250 new Fe I levels, and to weed out Fe II contaminants. For the brightest star HD 128167, the only mildly metal-poor, mildly-rotating early-F star with a STIS-accessible spectrum below 1880A, our program completes its archival E230H coverage only to 2130A with a standard c2263 spectrum, but adds a standard c1978 E230M spectrum blueward. The resulting coverage from 1730A to 3140A will provide the first empirical high-resolution NUV spectroscopic template for a hotter, mildly metal-poor star over this entire range, and will critically test whether our spectral modeling can reproduce its flux distribution. Both are required to discern diagnostics that can distinguish such younger, mildly metal-poor populations from older, more metal-poor systems at great distances, notably at high redshift with HST and JWST.
Because spectral resolution is critical to disentangle the formidable NUV line blends, the 0.2" x 0.09" slit will be used for all E230H spectra, and the 0.2" x 0.06" slit for the E230M spectrum. Our spectroscopic observations, and all but one of the NUV ETC spectroscopic runs, are adopted directly from Table 1 of the proposal's Description of Observations. IUE large-aperture LWR/P spectra of each target were used for the ETC normalizations of all E230H spectra. For the c1978 E230M ETC of HD 128167, whose SWP IUE spectra suffer many bad pixels, the ACQ/PEAK normalization was adopted instead. This yields an input ETC spectrum that agrees well with its LWR/P IUE spectra redward of 2100A, where ~3/4 the total GCR originates.
Stellar Populations
Stellar Physics
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false
false
true
false
false
false
false
SUPPORTED
STAR
A0-A3 V-IV
Teff = 9525, log g = 4.0, [Fe/H] = +0.35; metallic-lined A star
J2000
J2000
STAR
F3-F9
Teff = 6300, log g = 4.0, [Fe/H] = -2.25; very metal-poor turnoff star
J2000
J2000
STAR
A0-A3 V-IV
Teff = 8000, log g = 3.2, [Fe/H] = -1.60; metal-poor blue horizontal branch star
J2000
J2000
STAR
F3-F9
Teff = 6850, log g = 4.3, [Fe/H] = -0.40; mildly metal-poor blue straggler
J2000
J2000
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2013
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
3012
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
1763
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
1763
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2013
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2263
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2513
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
3012
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2762
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2263
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:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 332128
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15179
:visit-id "D0"
:obset-id "D0"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15179
:visit-id "D0"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2892
:al-overhead-at-end 0
:internal-dur-at-end 113
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3165
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 15179
:visit-id "D0"
:orbit-number 2
:pcs-time 302
:si-vis-utilization 3003
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3165
:pcs-gap 0
)
true
2
2
Castelli-Kurucz Models F2V 7000 4.0; Renormalized to vegamag = 4.47 in filter Johnson/V
Time to Saturation (for a single exposure) = 0.70 seconds; 39,899 e- in 0.1s
(Note: assumed spectral type differs from SIMBAD F4V owing to metal deficiency of star.)
Castelli-Kurucz Models F2V 7000 4.0; Renormalized to vegamag = 4.47 in filter Johnson/V
Time to Saturation (for a single exposure) = 0.59 seconds; 9,271,631 e- in 0.1s
(Note: assumed spectral type differs from SIMBAD F4V owing to metal deficiency of star.)
GCR=111K; not a variable source
GCR=119K; not a variable source