0 Assigned ID: 1329 ----- Attempting Submission 1 (Mon Jan 25 19:17:57 GMT 2021) ----- HST Phase I Proposal 1329 successfully submitted. Receipt: # 1329-1 FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. We have increased the FLASH for the WFC3 observations and adjusted the exposure times accordingly. 853930011 ----- Attempting Submission 1 (Tue Feb 16 15:38:51 GMT 2021) ----- HST Phase II Proposal 16492 successfully submitted. Receipt: # 16492-1 ----- Attempting Submission 3 (Mon Feb 22 13:47:14 GMT 2021) ----- HST Phase II Proposal 16492 successfully submitted. Receipt: # 16492-3 ----- Attempting Submission 4 (Tue Feb 23 20:28:35 GMT 2021) ----- HST Phase II Proposal 16492 successfully submitted. Receipt: # 16492-4 ----- Attempting Submission 5 (Wed Feb 24 15:33:52 GMT 2021) ----- FLASH warnings are ignored as these are the levels suggested by the WFC3 team. FP-POS positions are chosen to ensure that they are cycled through sequentially over the two orbits. The accuracy of the COS target positioning should not require an acquisition image as the source is extended. We have taken into consideration the additional COS limitations. SOFIA and HST Multi-wavelength Study of the Symbiotic Mira HM Sge To showcase the capabilities of evolved-star science using the instrument modes of SOFIA and the Hubble Space Telescope (HST), we propose to use FORCAST and EXES aboard SOFIA, and WFC3 and COS aboard HST to probe the quickly-evolving symbiotic system HM Sge. We will use SOFIA to probe the dust and the kinematics of the dense circum-stellar material, and HST to map the gas in the inner nebula and probe the shocked emission. These observations will provide a public dataset that can be used to anchor future observations of HM Sge, a post-outburst symbiotic Mira that displays a wide and diverse range of active astrophysical phenomena. The observations will also demonstrate the possibilities for future observations of other evolved-star systems. With WFC3 we are targeting the F502N([O iii]), F656N(Halpha), and F658N([N ii]) filters with three short exposures to image the inner nebula around the symbiotic system, and then a longer exposure (also F658N;[N ii]) that will saturate at the core, but that will capture the morphology of the more extended surrounding nebula. We will also do three pointings with COS, one on the central system, and two on the previously identified shocked regions to the North and South. For each of these pointing we will use the G140L/800 and G230L/2950 gratings. PI Goldman is an expert in AGB stars. Co-I Sankrit is an expert in symbiotic systems and and instrument scientist for COS. Co-I Montiel is an instrument scientist for EXES. Co-I Richter is the PI of EXES. Co-I Karnath is an instrument scientist for FORCAST. Stellar Populations and the Interstellar Medium 0 false SUPPORTED STAR AGB STAR SYMBIOTIC STAR YES Co-ordinates and proper motions from SIMBAD, which uses GAIA DR2. V magnitude as listed in SIMBAD ; however AAVSO data shows that V varies between 11.5 and 12.5. J2000 J2000 STAR EMISSION LINE NEBULA YES STAR EMISSION LINE NEBULA YES WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F658N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F658N COS/FUV Spectroscopic No No G140L 800 COS/NUV Spectroscopic No No G230L 2950 POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.145 LINE false false 4 46.86 SPIRAL 2 false /private/var/folders/zs/hqh_d0sd35n8y1_8wq6t9qw00001q_/T/OPVisit4565095638651615354.xml The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16492 :visit-id "01" :proposal-version -1 :trans-version "20200619" :date "24-Feb-2021 10:22:24.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1368880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16492 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16492 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2773 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16492 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 126 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 2 0 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /Users/sgoldman/Documents/document_archive/Proposals/symbiotics_sofia/OP-cache/hm_sge_sofia_hst_sub_feb23-v02.xml The input spectrum used for all ETC calculations is one constructed from IUE observations obtained on October 20, 1992, SWP46012 and LWP24119. ACQ/IMAGE: The continuum from the central source is expected to be the main contributor to the flux for the NUV acquisition, and therefore a point source is assumed for the calculation. The line emission, however, is likely to be distributed, and we have increased the S/N to 40 to examine the spatial extent of this emitting region. Spectroscopy: We are mainly interested in the line emission from compact, but extended sources. The total flux has been measured by IUE. In the spectroscopy ETC calculations, we are assuming a point source to be conservative for Bright Object Protection. (Tic-Visit :proposal-id 16492 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "23-Feb-2021 13:17:57.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1426368 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16492 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16492 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2763 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16492 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 0 :internal-dur-at-end 407 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 2 0 The input spectrum used for the ETC calculation was constructed from IUE observations obtained on October 20, 1992, SWP46012 and LWP24119. The continuum from the central source is expected to be the main contributor to the flux, and therefore a point source is assumed for the calculation. The line emission, however, is likely to be distributed, and we have increased the S/N to 40 to examine the spatial extent of this emitting region.