0 Assigned ID: 352 ----- Attempting Submission 1 (Fri Apr 07 00:35:52 GMT 2017) ----- HST Phase I Proposal 352 (eta.apt) successfully submitted. Receipt: # 352-1 ----- Attempting Submission 2 (Fri Apr 07 05:54:18 GMT 2017) ----- HST Phase I Proposal 352 (eta.apt) successfully submitted. Receipt: # 352-2 ----- Attempting Submission 3 (Fri Apr 07 20:37:28 GMT 2017) ----- HST Phase I Proposal 352 (eta.apt) successfully submitted. Receipt: # 352-3 FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser 2/15/18 - ROYLE - opened up ORIENT on visit 01 to allow observations to schedule in 2018. PI said removing ORIENT would be acceptable. -391036771 ----- Attempting Submission 1 (Thu Jul 20 18:19:45 GMT 2017) ----- ----- Attempting Submission 2 (Thu Feb 15 20:53:39 GMT 2018) ----- This is a flash warning. Can be ignored. Eta Car is in a bright background Hii region. Although Eta Car has been imaged many times with HST to monitor the central star and the bright Homunculus Nebula, we propose the first WFC3 imaging of Eta Car to study the more extended "Outer Ejecta" from previous eruptions. WFC3 has two key filters that have not been used before to image Eta Car, which will provide critical physical information about its eruptive history: (1) F280N with WFC3/UVIS will produce the first Mg II 2800 image of Eta Car, the sharpest image of its complex Outer Ejecta, and will unambiguously trace shock fronts, and (2) F126N with WFC3/IR will sample [Fe II] 12567 arising in the densest post-shock gas. Eta Car is surrounded by a bright, soft X-ray shell seen in Chandra images, which arises from the fastest 1840s ejecta overtaking slower older material. Our recent proper motion measurements show that the outer knots were ejected in two outbursts several hundred years before the 1840s eruption, and spectroscopy of light echoes has recently revealed extremely fast ejecta during the 1840s that indicate an explosive event. Were those previous eruptions explosive as well? If so, were they as energetic, did they also have such fast ejecta, and did they have the same geometry? The structure and excitation of the Outer Ejecta hold unique clues for reconstructing Eta Car's violent mass loss history. The locations of shock fronts in circumstellar material provide critical information, because they identify past discontinuities in the mass loss. This is one of the only ways to investigate the long term (i.e. centuries) evolution and duty cycle of eruptive mass loss in the most massive stars. These observations aim to obtain an image of the extended Mg II 2800 emission and the [Fe II] 1.2567 um emission of the Outer Ejecta nebulosity around the Homunculus of Eta Carinae. For the MgII 2800 line, we use the WFC3/UVIS F280N filter. For the near-IR [Fe II] emission, we use the WFC3/IR F126N emission line filter and the F130N filter for off-line continuum to subtract. The IR images will use a 4-point dither pattern with a gap in the middel to avoid the central star, which is extremely bright in the IR. Stellar Physics 6 false true false false false false SUPPORTED STAR CIRCUMSTELLAR MATTER EMISSION LINE NEBULA EMISSION LINE STAR ETA CARINAE STAR LUMINOUS BLUE VARIABLE YES This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F280N WFC3/IR Imaging No No F126N WFC3/IR Imaging No No F130N POS-TARG MOSAIC DITHER 2 2.4 WFC3-UVIS-MOS-DITH-LINE false true 0.119 3 85.754 POS-TARG WFC3-UVIS-MOS-DITH-LINE 33.606 1 false POS-TARG MOSAIC MOSAIC 2 94 LINE true true 104 2 40 POS-TARG LINE 134 2 true 1518727934564 /private/var/folders/h2/_3b1kkv56nn2rfp1zrxtm0sc0006z1/T/OPVisit4440576955953720314.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. MgII line emission image of the Outer Ejecta. (Tic-Visit :proposal-id 15289 :visit-id "01" :proposal-version -1 :trans-version "20171009" :date "15-Feb-2018 15:52:14.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1732496 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15289 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 15289 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 4593 :al-overhead-at-end 119 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 1 0 1500574736794 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. FeII and continuum images of Outer Ejecta. (Tic-Visit :proposal-id 15289 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "20-Jul-2017 11:18:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 2228336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15289 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 15289 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 4473 :al-overhead-at-end 0 :internal-dur-at-end 538 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 1 0