0Assigned ID: 474
----- Attempting Submission 1 (Fri Aug 17 23:05:46 GMT 2018) -----I copied over the visits from Cycle 26, GO 18541. The log (below) seems to think this has been submitted previously
as a cycle 27 Prop 15873... but it has not.
The one difference from cycle 26 is that there is time for another offset, to +100mas.
Also please check the Special requirements where I tried to space out the 4 visits during the accessibility
times fo my targets. I am not going into Auguat 2020; we may have a HOPR then... (we have two visits scheduled
for August 2019 and September 2019.
I ran the target confirmation tool and there is an enormous black dot... appears to be Betelgeuse
Ran the BOT and Galex is happy.
These comments still apply; this submission corrects typos in the year; and also gives
a broader range of between dates.
Most Warnings occur becuase I am offsetting from the ACQ/Peakup and software appears concerned that I am
losing the target... but the target is large ( 120 mas diameter ...not a point source) and we are scanning the star with a STIS slit..
We did not specifiy an ORIENT angle but indicated by pos-offset moving the slit perpendicular to the long axis of the slit.
We do not care about the orientation, just so long as we scan across the extended stellar disk..-387484472----- Attempting Submission 1 (Wed Nov 28 19:28:24 GMT 2018) -----
----- Attempting Submission 2 (Mon Dec 10 20:57:01 GMT 2018) -----
----- Attempting Submission 4 (Wed Feb 27 15:14:55 GMT 2019) -----
----- Attempting Submission 5 (Tue Jul 16 20:01:17 GMT 2019) -----
----- Attempting Submission 6 (Thu Jul 18 19:06:51 GMT 2019) -----Focus on BetelgeuseMultiple ultraviolet spectra of the nearby red supergiant,
Betelgeuse, using STIS will enable spatially resolved measures
of chromospheric structure and mass inflows and outflows. An HST
campaign of 3 cycles will be complemented by multi-frequency
photometry, spectroscopy, interferometry, and polarimetry at radio,
infrared, and optical wavelengths in order to map surface structures
and their variability, and the extended outer atmosphere over both
the short (400-day) and long secondary (2000-day) periods of this
supergiant. These observations, coupled with detailed modeling
and simulations, will probe the structure, the dynamics, and the
mass loss from Betelgeuse in unprecedented detail and provide crucial
insights into the atmospheric physics and wind-driving mechanisms
of red supergiants.We plan raster scans with STIS, medium resolution E230M grating using the small slit (0.1X0.03") centered on the red supergiant Betelgeuse (HD 39801). The raster scans (perpendicular to the long axis of the slit) with STIS using E230M (2707A) will be at the centered position, +/-25 mas, +/-50 mas, +/- 75 mas, and +100 mas.. The pattern is expected to be -75mas, -50mas, -25 mas, 0, +25mas, +50mas, +75mas +100 mas from the peakup in the small aperture.. The visit begins with an acquisition, then a first ACQ/PEAKUP in the 0.2X0.09 aperture using the dispersed spectrum (G230LB), followed by a spiral ACQ/PEAKUP using slit 0.1X0.03. Then offsets are made from the final peakup position as described above.
We are scheduling 4 visits of 3 orbits each during the times ot target accessibility. Hopefully: November 2019, Jan. 2020, March 2020, April 2020Stellar Physics6falsefalsetruefalsefalsefalse4trueSUPPORTEDSTARM III-INOparallax from Harper et al. 2017, AJ, 154, 11BETELGEUSEJ2000J2000STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707Timing link suitability includes constraints ([02 After 01 by 30.0 to 60.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.8 exposures at 8 positions on UV disk: offset -75, -50 -25, 0 +25,+50,+75,+100 mas with the 0.1X0.03 slit1574947483000302.6261504323201(Tic-Visit
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)true30Supposed to be a 3-pt linear peakup, telescope returned to central dwell positionspiral in 0.1X0.03Timing link suitability includes constraints ([02 After 01 by 30.0 to 60.0 days] [03 After 02 by 28.0 to 45.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.8 exposures at 9 positions on UV disk: offset -75, -50 -25, 0 +25,+50,+75 +100 mas with the 0.1X0.03 slit157935202400055.21283237832631(Tic-Visit
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