0 Assigned ID: 280 ----- Attempting Submission 1 (Thu Apr 04 22:15:11 GMT 2019) ----- HST Phase I Proposal 280 (eta.apt) successfully submitted. Receipt: # 280-1 ----- Attempting Submission 2 (Thu Apr 04 22:25:04 GMT 2019) ----- FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE We removed BLADE=A on some of the WFC3 exposures. We have used this before, but APT gave error messages this time and said it is not allowed. Resubmission - changed slit width for Visit 02 to 0.5 arcsec slit. Removed autowavecal and inserted GO wavecal. 47769443 ----- Attempting Submission 1 (Mon Jul 22 21:43:23 GMT 2019) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 2 (Mon Feb 01 19:39:55 GMT 2021) ----- ----- Attempting Submission 3 (Wed Feb 03 23:29:33 GMT 2021) ----- We have used the same FLASH=2.0 setting before for WFC3 observations. For STIS, the target is intentionally outside the aperture. We center on the target and then place the slit ata small offset to move the bright central star out of the slit. In Cycle 25, a UV image of Mg II 2800 emission in the nebula around the massive star Eta Carinae was obtained using the F280N filter with WFC3. This was the first WFC3 imaging of Eta Car, the first image of Mg II around a massive star, and the first deep UV image of its nebulosity. That image revealed strong Mg II emission, but with unexpected morphology. Mg II is anticorrelated with any other line emission features seen previously in typical tracers like Halpha, [N II], or [Fe II] emission. Mg II emission provides an entirely new view of Eta Car, revealing a significant reservoir of additional ejecta mass and kinetic energy outside the main bipolar nebula, which has been invisible in all other imaging filters used so far. The MgII emission is probably resonance scattering of near-UV starlight, tracing dense warm neutral gas that is unshocked. Since it is outside the main bipolar nebula, it may hold critical clues about the acceleration of the ejcta and the mass loss and instability of the star in the decades leading up to the eruption that cannot be ascertained any other way. We therefore propose to obtain a second epoch of imaging for proper motions, and deep STIS spectroscopy of the extended MgII emission in order to measure its expansion speed and its 3D structure. The measured ratio of the MgII doublet will trace the optical depth of the line and test our hypothesus that it is resonance scattering, allowing a rough mass estimate of this material. Combined with velocities from proper motions and spectra, these observations will therefore constrain the kinetic energy that this material adds to the total energy budget of Eta Carinae's eruption. This program has two observational goals. One is to obtain a second epoch of imaging in the WFC3/UVIS F280N, F336W, and F658N filters in order to measure proper motions of Mg II 2800 AA emission, near-UV continuum, and [N II] emission as compared to previous epochs. Toward this goal, we duplicate as closely as possible our previous observation. The second observational goal is to obtain long-slit STIS spectra of Mg II 2800 AA line from ejecta immediately outside the bipolar Homunculus nebula in order to measure radial velocities along the slit, and hence, 3D kinematics in conbination with proper motions. The WFC3 imaging uses two CVZ orbits (one for a deep F280N image, and one for both F336W and F658N). The STIS spectra use 4 CVZ orbits, with two different slit positions (2 orits each). Both team members are experts in studying Eta Carinae, and both have extensive previous experience reducing and analyzing HST imaging and spectroscopy. Both Smith and Morse were co-investigators on the Eta Car Treasury project, and both have been PI on previous awarded HST studies of Eta Car. Dr. Nathan Smith has written over 30 refereed first author papers about Eta Carinae and its nebula, and has extensive experience with both HST imaging and spectroscopy. His PhD thesis used STIS to study Eta Carinae's nebula, and he has used HST STIS to study Eta Car and a number of other massive evolved stars with circumstellar nebulae since then. He is an expert in massive star evolution and mass loss, supernovae, and stellar eruptions. Dr. Jon Morse has also authored several papers on Eta Car using HST data, has extensive experience with analysis of UV and optical emission line spectroscopy and imaging, and was the project scientist for the COS spectrograph. He is an expert in UV and optical line emission shock diagnostics, massive star outflows, supernova remnants, and protostellar jets. Stellar Physics 6 false false true false false false false SUPPORTED STAR CIRCUMSTELLAR MATTER ETA CARINAE STAR YES This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F658N WFC3/UVIS Imaging No No F336W STIS/CCD Spectroscopic No No G230MB 2794 POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 2 false POS-TARG DITHER 0.173 LINE 0.112 false true 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 4 false 1612375696746 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. Any ORIENT could suffice for these observations, however duplicating the orientation of program 15289 UVIS F280N observations would be helpful for data analysis and directs the diffraction spikes and CCD saturation bleeding away from important outer emission. The image header states that PA_V3 = 169.08 degrees for the March 2018 F280N images. Please duplicate this orientation (or use 349.08 degrees) if possible. 1581481852000 345.9 (Tic-Visit :proposal-id 15823 :visit-id "04" :proposal-version -1 :trans-version "20200619" :date "03-Feb-2021 11:08:16.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3785856 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15823 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 15823 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 10307 :al-overhead-at-end 0 :internal-dur-at-end 47 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 2 0 1612394860416 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. STIS spectrum with slit oriented roughly along polar axis (Tic-Visit :proposal-id 15823 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "03-Feb-2021 16:27:40.0" :trans-errors '(:WARNINGS 6 :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 92992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15823 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 15823 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 10267 :al-overhead-at-end 122 :internal-dur-at-end 400 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) false 2 0 1612375732771 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. STIS spectrum with slit oriented roughly perpendicular to the polar axis 1590801015000 95.0 (Tic-Visit :proposal-id 15823 :visit-id "03" :proposal-version -1 :trans-version "20200619" :date "03-Feb-2021 11:08:52.0" :trans-errors '(:WARNINGS 4 :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 148208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15823 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 15823 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 10435 :al-overhead-at-end 75 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 2 0