0Assigned ID: 792
----- Attempting Submission 1 (Fri Apr 07 19:31:56 GMT 2017) -----
HST Phase I Proposal 792 (HSTcycle25.apt) successfully submitted.
Receipt: # 792-1
----- Attempting Submission 2 (Fri Apr 07 23:52:09 GMT 2017) -----As described in the respective object Visits. We have been approved to change the total number
of orbits for HD-28406 and HD-28608 from 4 to 3 each. In contrast, we have increased the
total number of orbits for HR-1201 and -48-TAU from 1 each to 2 each.
The BOT gave warnings for all of our targets, but this is because the BOT assumes that all stars are
O5V. We know that all of our targets are approximately F2V to F8V stars, and under these conditions
they do not reach any brightness limits.
RESUBMISSION: In our original submission additional acquisition steps on each subsequent orbit on
a target were used but not necessary. We have removed the unecessary acquisition steps and have
added that time to our target exposures.
RESUBMISSION2: Visit 07's target was deemed too bright for the limits of our COS observational setup. We have requested and were
granted permission to change that target's observations from COS to STIS with an appropriate setup for its brightness. We have also
modified our exposure times for Visit 08's target, which before had issues with its Buffer Time setting.
SUBMISSION.DEC10 - All orbits have been updated according to the new target aquisition times. Additionally, the STIS aquisition and
observations setup for VISIT 07 have been updated according to discussions with Joleen Carlberg. The Buffer Times for Visit 08 were
also double checked and were fine.442948945----- Attempting Submission 1 (Thu Jul 20 19:57:52 GMT 2017) -----
----- Attempting Submission 2 (Mon Dec 04 16:14:09 GMT 2017) -----
----- Attempting Submission 3 (Tue Nov 27 15:51:37 GMT 2018) -----
----- Attempting Submission 4 (Tue Dec 11 00:46:43 GMT 2018) -----Boron in Hyades F Dwarfs - Tracing Deep Into the Li-Be GapDramatic deficiencies of Li in the mid-F stars of the Hyades cluster were discovered by Boesgaard and Tripicco in 1986. Using high-resolution, high signal-to-noise spectra from the Keck 10-m telescope, Boesgaard and King discovered the corresponding deficiencies in Be in the same narrow temperature region in the Hyades. We propose an investigation into the B abundance in the Hyades F stars to ascertain if there is also a B gap. Boron can only be observed with HST; we plan to use the resonance line of B I at 2497 Angstroms. Each of these three elements is destroyed inside stars, but at different depths. Li, Be, and B survive to progressively greater depths, and their surface abundances act as a report on the depth and thoroughness of physical processes occurring in the star. The Li-Be gaps strongly contradict standard theory. Previous work favors rotational mixing that results from angular momentum loss as the dominant mechanism over diffusion, mass loss, and other types of rotational mixing. However, combinations of these mechanisms or other possibilities could still be at work. These observations will help determine the nature of the mixing mechanism(s) and the connection to stellar rotation. The abundance of *all three* light elements in a cluster of known age and metallicity can provide the information needed to discern internal stellar processes. The Li and Be deficiencies occur in field and cluster stars in this mass range (1.1 - 1.25 solar masses), but the mechanisms can best be studied in a cluster of stars of common origin and known characteristics. The Hyades cluster at 650 Myr is close enough to contain stars bright enough for this investigation.We propose to observe eight judiciously selected Hyades dwarfs to search, primarily, for evidence of a B gap like the previously discovered Li gap and the more recently discovered Be gap. All of our stars have met the stringent selection criteria of having small Teff (<75 K) as determined from all ten colors constructed from UBVRI photometry (Johnson et al. 1962 and Mendoza 1967) and no evidence for binarity listed in Perryman et al. (1998). Stars are selected on the basis of their A(Li) (from C17) and presented in Table 1.
These data will be combined with the B data of the two severely Li- and Be- depleted stars in the Li-Be gap (vB 13 and vB 37), whose A(B) were argued to be robust (Scientific Justification). Conversely, the A(B) of vB 14, 62, and 65 were argued to be suspect. The Hyades archive also contains B data for vB 121, vB 77, and for a few giants that are irrelevant.
Figure 4 shows syntheses of the B I resonance line (2497 A at R ~ 20,000) for each star type we propose to observe. These syntheses explicitly contain noise at the levels discussed below, which helps to explicitly illustrate the need for the requested SNR. The A(B) shown vary by a factor of two from curve to curve. The A(B) are 1.98 (green), 2.28 (red), 2.58 (black) and 2.88 (blue) dex. The dispersion is ~0.033 A per pixel; we have binned all panel b) by three and all others by two. The rotation in these syntheses correspond to the stars we propose to observe. The SNR indicated below take into account that for the first orbit, approximately 16.5 minutes are taken by overhead for guide star acquisition, target acquisition, peak-up, and other overheads. We also plan to follow recommended procedures (e.g. multiple exposures and multiple center wavelengths) to help achieve the highest SNR values.
Four stars with high A(Li) will be used to determine the critically important undepleted A(B). Two stars (vB 6 and vB 20) are hotter than the Li gap and two stars (vB 19 and vB 48) are cooler than the Li gap and are on the Li plateau. All stars have A(Li) > 2.96. The two hotter stars are the most likely to be undepleted in Li or nearly so, with A(Li)~3.3-3.4. Although these stars are rotating fairly rapidly, their A(B) can be determined reliably with just 2 orbits, each (panel a; SNR~160 per pixel). No better stars are available hotter than the Li gap, as other stars rotate even more rapidly. The two cooler stars are fainter, and thus require 4 orbits each (panel e, SNR~97 per pixel) in spite of their lower v sin i, which helps deblend the B lines. These two stars have the highest A(Li) on the Li plateau (of the stars with low Teff ) and no evidence for binarity), but even so, their A(Li)~3.0 seems slightly depleted relative to the two hot stars. It is also a possibility that we might detect a very slight difference in B (of order 0.1 dex) in the average of these two stars compared to the two hotter stars, which would provide invaluable constraints on rotational mixing.
Just two stars do not, alone, provide a robust detection of a B gap. Thus, A(B) in more Li-Be gap stars (besides vB 13 and vB 37) are needed. We propose to observe vB 51 and vB 90, which have an upper limit and detection in A(Li), respectively. 4 orbits for each star will yield SNR ~ 85 per pixel, which will reasonably detect depleted A(B) (panels b, d). Robust detection of a B gap and its magnitude can help differentiate the relative contributions of diffusion, mass loss, and different types of rotational mixing. Finally, we propose to observe two stars, vB 78 and vB 86, with intermediate A(Li) ~ 2.3. These are important for delineating the B-Li correlation, if any. Such a correlation offers even more robust constraints for stellar models. 3 orbits for each star will yield SNR ~ 70 per pixel, which is sufficient for an accurate abundance (panel c).Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARF3-F9NOVB78J2000J2000STARF3-F9NOVB86J2000J2000STARF3-F9NOVB51J2000J2000STARF0-F2NOVB6J2000J2000STARF3-F9NOVB20J2000J2000STARF3-F9NOVB19J2000J2000STARF3-F9NOVB48J2000J2000STARF3-F9NOVB90J2000J2000COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390COS/NUVSpectroscopicNoNoG225M2390The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode./Users/jeff/Documents/OP-cache/phaseIIDecember10-v01.xml(Tic-Visit
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