0 Assigned ID: null ----- Attempting Submission 1 (Wed Jun 20 00:47:58 GMT 2018) ----- Submission failed due to error communicating with the submission server. Please retry in a few minutes. If this error persists please contact the help desk at help@stsci.edu Assigned ID: 6 ----- Attempting Submission 1 (Wed Jun 20 00:48:24 GMT 2018) ----- 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 Please correspond about this 15596 Phase 2 submission with Co-I Morse at jamorse@boldlygo.org. Thanks, -JM Second submission shortens the longest exposure times in order to fit the whole sequence into a 53 min orbit in order to expedite scheduling. The ORIENTs available during days 18.200-206 will be fine. 811055558 ----- Attempting Submission 1 (Fri Jul 06 16:04:12 GMT 2018) ----- HST Phase II Proposal 15596 (15596-Phase2.apt) successfully submitted. Receipt: # 15596-1 ----- Attempting Submission 2 (Fri Jul 06 18:40:30 GMT 2018) ----- The FLASH=2.0 level was used successfully on our 15289 program. The source is extended and will accumulate sufficient counts/pixel in important regions. In cycle 25, time was awarded to obtain a UV image of Mg II 2800 emission in the nebula around the massive star Eta Carinae, using the F280N filter with WFC3/UVIS. 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 the nebulosity around Eta Carinae. That image revealed strong Mg II emission, but with very unexpected morphology. The Mg II is essentially anticorrelated with the other line emission seen previously in H-alpha, [N II], or [Fe II] emission. The Mg II emission provides an entirely new view of Eta Carinae, 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. To accomplish the originally stated goal of using Mg II as a diagnostic of shocks in the ejecta, we need to understand the alignment of the Mg II emission as compared to other tracers like H-alpha, and the Mg II image needs to be continuum subtracted to separate line emission from dust-scattered starlight. This DD proposal requests images in the F336W (continuum subtraction) and F658N ([N II]) filters at the current epoch. This is urgently needed because the nebula is expanding rapidly and differentially; WFPC2 images from more than a decade ago are inadequate for proper alignment. These additional images (1 orbit) will permit a quantitative analysis of the shock conditions that give rise to the separation of Mg II and H-alpha, and will allow us to separate shocked gas from photoionized ejecta. We also request a very short exposure in F280N to patch saturated pixels in the existing F280N image. Our proposed observations have two immediate objectives: (1) to obtain F336W and F658N images at the present epoch to align with our new F280N Mg II image, and (2) to obtain a pair of very short exposures in the F280N lter to patch saturated pixels around the bright central star. F336W and F658N: We will image continuum emission from Eta Car at blue/near-UV wavelengths (F336W) and H+[N ii] 6583 line emission from shocked gas (F658N). We will use a similar observing strategy as in previous sequences of images taken with WFPC2 in 1999 and 2001, with a range of integration times to accommodate the factor of > 10^5 in dynamic range between the central star and the faintest structures in the extended nebula. In the longest exposures needed to see the fainter outer condensations in the nebula, the central star and its immediate surroundings will badly saturate and bleed onto adjacent pixels. The range of shorter exposure times are necessary to provide unsaturated images that can be used to patch the overexposed sections of the images. For F336W and F658N, a suitable series of exposures can be obtained in one orbit, including overheads. For WFC3, the red sensitivity is similar to WFPC2, but blue sensitivity is signifcantly better. We will therefore use a similar range of exposures in the F658N filter, and somewhat shorter exposures in F336W than in previous cycles. The main requirement is to achieve good signal to noise in the fainter outer regions of the nebula to compare with the F280N emission. F280N short exposures: We will also obtain two short-exposure images in the F280N filter, with exposure times of a few to tens of seconds. The purpose of these images is to patch the saturated pixels in the F280N image obtained in March 2018. A central region of roughly 20x200 pixels was badly saturated with bleeding onto adjacent pixels around the central star. For this program, we had obtained a CR-split pair of images with a total exposure time of about 3900 s, because we were primarily interested in detecting faint outer MgII emission. Not knowing what to expect, we maximized the exposure time in one orbit. To carefully register the F280N image with the F336W and F658N images proposed here, and to investigate the morphology of any MgII emission or absorption near the central star that may be different from the continuum emission, we need unsaturated exposures of the central star in the F280Nfilter. Stellar Physics 0 false AVAILABLE EXT-STAR EJECTA EMISSION LINE NEBULA ETA CARINAE STAR LUMINOUS BLUE VARIABLE YES This object was generated by the targetselector and retrieved from the SIMBAD database. In previous cycles we noted that special catalog ZZZQ may be needed because GSC is poor in this field. It does not appear that the predecessor program 15289 used the special catalog. Visit 1 of 15289 successfully imaged with WFC3 through the F280N UVIS filter, but Visit 2 appears to have had tracking issues with a couple of exposures in the IR channel. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F658N POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false 1530902186739 /private/var/folders/zy/h8hf71px5pz3x_q44vg9cw780000gp/T/OPVisit8289278365160430389.xml The scheduling data was generated by CASM 26.0. 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 previous F280N images. Please duplicate this orientation (or use 349.08 degrees) if possible. (Tic-Visit :proposal-id 15596 :visit-id "01" :proposal-version -1 :trans-version "20180409" :date "06-Jul-2018 14:36:26.0" :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 565824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15596 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15596 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2854 :al-overhead-at-end 170 :internal-dur-at-end 655 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3449 :pcs-gap 0 ) true 1 0