Tidied up formating. Checked page lengths.
Edits-757575623Assigned ID: 712
----- Attempting Submission 1 (Fri Mar 06 19:44:38 GMT 2020) -----
HST Phase I Proposal 712 successfully submitted.
Receipt: # 712-1
----- Attempting Submission 2 (Fri Mar 06 20:22:11 GMT 2020) -----
HST Phase I Proposal 712 successfully submitted.
Receipt: # 712-2
----- Attempting Submission 3 (Fri Mar 06 21:19:07 GMT 2020) -----First submission
2nd Sumbission - removed the constraint that Visit 2 occurs after Visit 1
3rd Submission - made Proposal Description text match removed constraint.-903138526----- Attempting Submission 1 (Mon Jun 29 15:19:58 GMT 2020) -----
HST Phase II Proposal 16256 successfully submitted.
Receipt: # 16256-1
----- Attempting Submission 2 (Wed Jul 01 13:03:30 GMT 2020) -----
HST Phase II Proposal 16256 successfully submitted.
Receipt: # 16256-2
----- Attempting Submission 3 (Thu Jul 02 13:37:13 GMT 2020) -----A Sensitive Test for Far Ultraviolet CO absorption in the Outflow of our Nearest Supernova Progenitor - AntaresThe massive red supergiant Antares (alpha Sco A: M1 Iab) is an excellent star to test theoretical models of mass loss because its distance, age, stellar parameters, mass-loss rate, and interstellar reddening are well established. The early-M supergiants pose a particular challenge for models of mass loss driven by radiation pressure on molecules and/or dust: The circumstellar molecular abundances and dust-to-gas mass ratios are lower than for later-M spectral-types, but they still manage to drive massive winds.
We request deep FUV and NUV observations to perform an extremely sensitive test for the most robust circumstellar molecule, CO, by observing its Fourth-Positive electronic bands against the FUV continuum of the M supergiant Antares. These observations will enable us measure any CO present in the outflow, and to place upper-limits on the effective radiation acceleration it can provide. The proposed observations will also provide an invaluable dataset for Antares, the oft neglected southern twin of Betelgeuse, and our nearest Type II supernova progenitor.This is a STIS spectroscopic program to observe the NUV and FUV spectrum of the M 1.5 Iab supergiant in the Antares (alpha Sco) system.
The M supergiant has a B3 V main-sequence orbital companion 2.67 arcsec West (PA=275 deg, Period >1250 years). The bright object constraint for non-variable objects within 5 arcsec of the target, namely the global count rate <200,00 cnt/s, requires that all the science observations be made with the 31x0.05 NDA aperture. This then requires the use of the ORIENT constraint to avoid placing the B star near the long aperture.
ORIENT: To place the long slit (31x0.05 arcsec) perpendicular to the stellar line of centers the +Y-axis should be 275-90=185 deg. The U3 axis is 45 deg from +Y, so the optimum ORIENT value is 185+45 = 230 deg, also in the opposite direction ORIENT=50 deg. We adopt a +/-45 deg ORIENT range on each direction giving bounds for each Visit as 5 to 95 deg AND 185-275 deg.
For the safety simulations in the STIS ETC we use the observed B star FUV and NUV spectrum (photospheric continuum) compiled from IUE Large Aperture spectra. For the faint M supergiant the science simulations use a slightly reddened, i.e. additional reddening of E(B-V)=0.1, HST STIS spectra of Betelgeuse (M2 Iab).
OBSERVATIONS:
ACQ: The ACQ is made with the STIS CCD with the F5ND5 aperture. [The M (V=0.91) star is ~400 times brighter than the B sar (V=5.91)]
Using the Castelli & Kurucz model M0I Teff=3650 K with E(B-V)=0.30 V=0.91 a S/N=145 is reached for Texp=0.1 sec. [STIS.ta.1447745]
We note that the position and proper motions are the best available (van Leeuwen 2007 Revised Hipparcos) which is tied to the ICRS frame.
PEAKUP: The PEAPKUP is made with G430M @5471 Ang in the 31x0.05 NDA aperture (which is also the science aperture).
Using the same model, a Texp=0.1 sec gives S/N=100 pre res. element. [STIS.sp.1447778]
SCIENCE: The earlier visits include the NUV where the M supergiant is bright enough to check the ACQ/PEAKUP sequence, and system throughout. No Visit schedule constraint is requested.
Subsequent Visits are a mix of FUV and NUV spectra, so that the FUV analysis can be initiated towards the beginning of the project. We use ACCUM to increase exposure times, and
put AUTO-WAVECAL at end of 2nd and subsequent orbits.
Science safety simulations assuming the B star is centered in the aperture, using observed IUE spectra:
E230H-2762 STIS sp.1447788 entire detector 159,196 cnt/s
E230H-2513 STIS.sp.1448283 ditto 191,248 cnt/s
E230H-2263 STIS.sp.1448287 ditto 174,589 cnt/s
E140H-1526 STIS.sp.1448300 ditto 170,242 cnt/s
All science observations use the 31x0.05 NDA aperture
Visit 1: 3 orbits E230H-2762 - Texp science ~6,200 sec [more in ACCUM, same for all below]
Visit 2: 3 orbits E140H-1598 - Texp science ~6,200 sec
Visit 3: 4 orbits E230H-2513 - Texp science ~8,500 sec
Visit 4: 3 orbits E140H-1598 - Texp science ~6,200 sec
Visit 5: 4 orbits E230H-2263 - Texp science ~6,200 sec
Visit 6: 3 orbits E140H-1598 - Texp science ~6,200 sec
Visit 7: 3 orbits E140H-1598 - Texp science ~6,200 secDr. Graham M. Harper has extensive experience with multi-wavelength observations and detailed radiative transfer modeling of the atmospheres of cool evolved stars. His focus is on the construction of semi-empirical models and the confrontation of theoretical models of mass loss. He has worked extensively in the FUV/UV with Hubble, IUE, GALEX, and FUSE (as Guest Observer), and also with radio interferometry, and wrote S-MULTI. The radio data shown in the proposal has recently been submitted to A&A by E. O'Gorman - colleague and former PhD student.
Prof. Keiichi Ohnaka is an expert on infrared interferometry, working extensively with the Very Large Telescope Interferometer. He recent work seeks to integrate dynamical modeling of spectro-interferometry. He performed the CO imaging study described in this proposal.
Prof. Edward F Guinan is a highly experience astronomer, extremely well known to the cool star astronomy community. He studies many classes of cool stars and their activity. He is also active in coordinating photometry of evolved cool stars, including that for this proposal.
Dr. Thomas Ayres, is a renoun cool star astronomer whose is a world leading expert on ultraviolet cool star spectroscopy (and data reduction techniques). he created the Hubble ASTRAL Library and he will assist in the data reduction for Antares.
The proposal team's research expertise and experience both complements and overlaps each other.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARCIRCUMSTELLAR MATTEREMISSION LINE STARM III-INOICRSANTARESJ2000J2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230M1978STIS/NUV-MAMASpectroscopicNoNoE230H2263STIS/NUV-MAMASpectroscopicNoNoE230H2513STIS/NUV-MAMASpectroscopicNoNoE230H2762/Users/grahamharper/Documents/Proposals/HST/CY28/PhaseII/OP-cache/16256-ACCUM_Jun29_ReSubmitted-v01.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.First Visit. Strong stellar signal - use this to verify ACQ and PEAK-UP, and photon throughputs work as intended(Tic-Visit
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