chnaged "AVAILABLE" to "SUPPORTED"26013512----- Attempting Submission 1 (Sat Sep 19 18:16:41 GMT 2015) -----
HST Phase II Proposal 14350 (GO-14350-AlpCMi.apt) successfully submitted.
Receipt: # 14350-1
----- Attempting Submission 2 (Sat Sep 19 18:22:02 GMT 2015) -----The target has previously been observed succesfully by STIS: there are no BOT issues.
The target is a very bright star with well-known coordinates, so the Target Confirmation
Tool is not needed.Procyon: New Candidate for the Dynamo Clinical TrialThis is the first year of a joint Chandra/HST program to follow the evolution of the high-energy (X-ray and UV) activity cycles of the nearby mid-F subgiant Procyon. This bright star has high-energy attributes that are similar to the Sun, yet it is a hotter star, at the edge of the region in the H-R diagram where surface convection occurs (the power source for stellar magnetic activity). The HST part is to record STIS UV spectra of the bright star on a semi-annual basis at high echelle resolution and high S/N, especially to capture the FUV Fe XII 124,134 nm coronal forbidden lines, which can tie together the non-simultaneous Chandra X-ray and HST pointings; as well as to record other key high-energy species like Si IV, C IV, and N V. The latter display Doppler-shifted, bimodal distorted emission profiles that signify high-powered dynamics in the interface regions of the stellar atmosphere between the super-hot corona (>1 MK) and the cold photosphere (<6000 K). The associated flows are a hot topic in contemporary solar physics, and one focus of a new space-based solar imaging spectrometer called IRIS. The solar and stellar FUV views are strongly complementary. The HST part of the program has two general objectives: (1) follow changes in the FUV spectra associated with any slowly evolving X-ray activity cycle of Procyon; and (2) combine the multiple epochs of echelle spectra to provide the highest possible S/N for identifying weak, but diagnostically important, emission lines (absorption, in some cases), and for decomposing the high-temperature line profiles (e.g., Si IV, C IV) into multiple dynamical components (which are though to be symptomatic of coronal heating and cooling processes).The proposed STIS observations of Procyon are straightforward. There are two identical visits of two orbits each, with a BETWEEN constraint specified to ensure scheduling at about a half-year separation, which is adequate timing to follow starpot cycle variations (which occur on timescales of roughly a decade).
In each visit, the optically bright target is acquired by direct imaging with the CCD through the F25ND5 filter. The remainder of the first orbit is occupied by a high-res FUV echelle exposure with setting E140H-1307 through the 0.2x0.2 photometric aperture. A peak-up is not needed because the CCD ACQ is accurate enough for centering in the photometric slot. The second orbit begins with a second high-res FUV echelle exposure, now with E140H-1489, but again through the 0.2x0.2 aperture. Together, these two settings cover the range from below Lyman Alpha (121 nm) out to beyond the C IV doublet at 155 nm, where the rising F-type photospheric continuum begins to overwhelm the faint subcoronal emission line spectrum. The two settings overlap in the key 140 nm region which contains the prominent Si IV doublet, as well as a density-sensitive multiplet of semi-permitted O IV. At the end of the second orbit, a brief NUV high-res echelle exposure is taken with setting E230H-2762 to capture the important chromospheric emission doublet of Mg II at 280 nm. Owing to the brightness of Procyon at these wavelengths, the observation must be taken through the ND2 slit, which requires a prior peak-up (in this case in dispersed light with G430M-4451).COOL STARS12falsefalsefalsefalse0.00.0SUPPORTEDSTARF3-F9NOThe target coords for epoch 2016.5 were taken from SIMBAD, in the ICRS frame.ALP-CMIJ2000J2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode./Users/ayres/Documents/SUPERIOR-OCT2014/PROPs/HST-CYC23/apt/OP-cache/GO-14350-AlpCMi-v10.xmlThe BETWEEN range given below is about 6 months prior to the narrower (3-day) visibility window in OCT 2016. This is the only pair of six-month-separated visibilities in Cycle 23, consistent with the desired starspot cycle monitoring interval.(Tic-Visit
:proposal-id 14350
:visit-id "10"
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:trans-version "20150609"
:date "19-Sep-2015 12:06:12.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 262544
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
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(Tic-Orbit
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:internal-dur-at-end 113
:dark-offset NIL
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:low-sky "N"
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(Tic-Orbit
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)false20Castelli-Kurucz Model:F5V; V=+0.37; Optimum SNR = 95; time to sat 3.2 sInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 2 ks at Si IV 139 nm gives peak SNR~25 (per resol) with 0.2x0.2 aperture; no LCR or GCR issuesInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 2 ks at Si IV 139 nm gives peak SNR~35 (per resol) with 0.2x0.2 aperture; no LCR or GCR issuesdispersed light peak-up assuming Castelli-Kurucz Model F5V, V=+0.37 mag: in 0.1 s, 479k e- with ND2 slitInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 750 s at Mg II 279 nm gives peak SNR~32 (per resol) with ND2 aperture; no LCR or GCR issuesThe scheduling data was generated by CASM 23.2.CASM was run in Phase II mode./Users/ayres/Documents/SUPERIOR-OCT2014/PROPs/HST-CYC23/apt/OP-cache/GO-14350-AlpCMi-v11.xmlThe BETWEEN range given below for the narrow OCT visibility window is approximately 6 months after the broader window in APR 2016.(Tic-Visit
:proposal-id 14350
:visit-id "11"
:proposal-version -1
:trans-version "20150609"
:date "19-Sep-2015 12:06:32.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 262544
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
:proposal-id 14350
:visit-id "11"
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(Tic-Orbit
:proposal-id 14350
:visit-id "11"
:orbit-number 1
:pcs-time 333
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:al-overhead-at-end 0
:internal-dur-at-end 113
:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3213
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(Tic-Orbit
:proposal-id 14350
:visit-id "11"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 2991
:al-overhead-at-end 0
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)false20Castelli-Kurucz Model:F5V; V=+0.37; Optimum SNR = 95; time to sat 3.2 sInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 2 ks at Si IV 139 nm gives peak SNR~25 (per resol) with 0.2x0.2 aperture; no LCR or GCR issuesInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 2 ks at Si IV 139 nm gives peak SNR~35 (per resol) with 0.2x0.2 aperture; no LCR or GCR issuesdispersed light peak-up assuming Castelli-Kurucz Model F5V, V=+0.37 mag: in 0.1 s, 479k e- with ND2 slitInput=special ETC file for ALP-CMI from ASTRAL catalog; exposure time= 750 s at Mg II 279 nm gives peak SNR~32 (per resol) with ND2 aperture; no LCR or GCR issues