0 Assigned ID: 314 ----- Attempting Submission 1 (Fri Apr 05 01:24:27 GMT 2019) ----- HST Phase I Proposal 314 (PNLineSurvey.apt) successfully submitted. Receipt: # 314-1 ----- Attempting Submission 2 (Fri Apr 05 16:28:39 GMT 2019) ----- HST Phase I Proposal 314 (PNLineSurvey.apt) successfully submitted. Receipt: # 314-2 ----- Attempting Submission 3 (Fri Apr 05 16:44:21 GMT 2019) ----- HST Phase I Proposal 314 (PNLineSurvey.apt) successfully submitted. Receipt: # 314-3 POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. Resubmission of Phase II w/ new visit (#5) to redo failed F502N & F673N observations plus add F658N. -667295687 ----- Attempting Submission 1 (Wed Jul 24 15:15:42 GMT 2019) ----- HST Phase II Proposal 15953 (PNLineSurveyPhaseII.apt) successfully submitted. Receipt: # 15953-1 ----- Attempting Submission 2 (Fri Feb 14 20:06:05 GMT 2020) ----- The errors/warnings have to w/ images already obtained for this program (w/ quad filter FQ243N). Planetary nebulae (PNe) serve as textbook examples of astrophysical plasmas and shock processes and provide essential tests of theories of stellar evolution and the origin and enrichment of the heavy elements in the universe. HST imaging has established that PNe exhibit a dazzling variety of aspherical morphologies: elliptical; bipolar or multipolar; highly point-symmetric; chaotic and clumpy. The multifaceted PN shaping problem has connections to (and implications for) a wide variety of astrophysical systems: binary star astrophysics; stellar wind interactions and shocks; the physics and chemistry of photoionized plasmas and photon-dominated regions; and enrichment of the ISM in the products of intermediate-mass stellar nucleosynthesis. Yet, as the useful lifetime of HST comes to a close, the tremendous potential of HST/WFC3 to obtain a comprehensive set of near-UV/optical/near-IR emission-line images has yet to be exploited for any PN. Here, we propose the first such comprehensive HST/WFC3 emission-line studies, targeting two of the youngest and most rapidly evolving known PNe, NGC 7027 and NGC 6302. The resulting set of diagnostic emission-line (and line ratio) images will distinguish between photoionization and shock-induced ionization; between ionization fronts and conduction fronts; between active and ``fossil'' shaping processes; and between the action of intrinsic shaping engines (e.g., accretion-disk-driven jets) and extrinsic ``pre-existing conditions'' (e.g., AGB wind inhomogeneities and equatorial density enhancements). Filter suite: We will obtain WFC3 images of each target PN in a dozen filters, notionally organized in these complementary filter sets: * central star photoionization: [Ne IV] + [Ne V] (FQ243N + F343N) * spatial variations of shocks vs. photoionization, optical: [O III] + [S II] + H$\alpha$ + H$\beta$ (F502N + F673N + F656N + F487N) * spatial variations of shocks vs. photoionization, near-IR: [Fe II] + P$\beta$ (F164N/F167N + F128N/F130N) * near-IR (scattered light) dust imaging: F110W + F160W Exposure time and orbit requirements: The IUE-measured $\lambda$2425 [Ne IV] line fluxes of NGC 7027 and NGC 6302 are $4\times10^{-13}$ and $6\times10^{-14}$ erg cm$^{-2}$ s$^{-1}$, respectively. ETC predicts 400 s exposure should reach S/N of 10 in a 5$\times$5 pixel region for FQ243N imaging of NGC 6302 given its line flux. Hence we can obtain high-quality images in this line and the $\lambda$3426 [Ne V] line (for which we assume similar line fluxes) in a single orbit dedicated to imaging of each PN in the FQ243N and F343N filters. Typical maximum exposure times for both nebulae in previous observations through the optical filters that are repeated here (F502N, F656N, F673N; see ``Duplications'') are 400 s for NGC 7027 and 2200--5200 s for NGC 6302. Adopting similar maximum exposure times, and accounting for overheads and time required to obtain a suite of shorter (30--300 s) exposure times through each filter (thereby yielding images that are unsaturated even in the bright central regions of both nebulae), we require two orbits to cover the full optical filter set (F487N, F502N, F656N, F673N) for NGC 7027\footnote{Exposures of NGC 7027 with WFC3 through filters F487N, F502N, and F656N are included in a complementary Cycle 27 Treasury proposal, so we would drop the exposures of NGC 7027 through these 3 filters if the Treasury proposal is successful.} and three orbits to cover these same filters for NGC 6302. For the near-IR image exposure times, the ETC predicts we can reach S/N of 10 in a 5$\times$5 pixel region in $\sim$120 s for F164N imaging of NGC 7027 given its measured total [Fe II] 1.64 $\mu$m line flux of $\sim$$3\times10^{-14}$ erg cm$^{-2}$ s$^{-1}$. This is similar to the times of archival (NICMOS) HST near-IR emission-line (H$_2$ and Br$\gamma$) imaging of this PN. As with these archival observations, we will perform on- and off-line imaging of [Fe II] and of ($\sim$100 times brighter) Pa$\beta$ so we can subtract continuum emission due to near-IR free-free radiation at the cores of each PN. These narrow-band near-IR observations, plus dust (scattered-light) imaging through the broad-band filters F110W and F160W, will require two orbits per PN. We therefore request 5 and 6 orbits, respectively, for the proposed comprehensive WFC3 emission line imaging studies of NGC 7027 and NGC 6302. The PI, Joel Kastner (Rochester Inst. of Technology), has led numerous observational investigations of planetary nebulae over the past 25 years. In particular, he led the most comprehensive surveys of near-IR H_2 and X-ray emission from PNe (Kastner et al. 1996, 2012). He has been among the lead organizers of the series of (eight) "Asymmetrical Planetary Nebula'' conferences almost since its inception. He is supervising co-I Jesse Bublitz, a 4th-year Ph.D. student at RIT, whose thesis research is focused on radio molecular emission line surveys of PNe, including the two targets. Co-I Frank (U Rochester) is the lead developer of AstroBEAR, a powerful adaptive mesh MHD simulation code specifically developed for theoretical studies of PNe. Co-I Balick (U Washington) has a long track record of successful HST imaging of PNe, and has recently authored a series of papers on the structural evolution of bipolar PNe based on the comparison of HST imaging with AstroBEAR simulations. Co-I Blackman (U Rochester) is a leading theorist in the area of PN shaping mechanisms, including jet launching and collimation. Co-I R. Montez (SAO) is an expert in the study of X-ray and UV emission from PNe and evolved stars generally. He was co-lead of the Chandra (X-ray) planetary nebula survey and is a coauthor of the paper on emission-line imaging diagnostics featured in Fig. 4 of this proposal. In addition to the X-ray imaging described in the propsal, the PI and Ph.D. student Bublitz, along with co-I Montez, have obtained IRAM 30 m radio spectra and IRAM/NOEMA radio interferometric imaging for one of the two targets, NGC 7027, in key tracers of irradiation of molecular gas. Bublitz is leading the same team in an ALMA proposal to obtain a similar suite of molecular line images of the other target, NGC 6302. Stellar Physics 6 false false false false false false false SUPPORTED ISM PLANETARY NEBULA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 ISM PLANETARY NEBULA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No FQ243N WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F673N WFC3/IR Imaging No No F128N WFC3/IR Imaging No No F130N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F164N WFC3/IR Imaging No No F167N WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No FQ243N WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F673N WFC3/IR Imaging No No F128N WFC3/IR Imaging No No F130N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F164N WFC3/IR Imaging No No F167N WFC3/IR Imaging No No F160W POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 1 false POS-TARG MOSAIC DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 2 false POS-TARG DITHER DITHER 4 5.183 WFC3-IR-DITHER-BOX-MIN false 74.653 true 0.365 0.572 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 18.528 3 false 1563932525147 /Users/jhkpci/Documents/work/proposal/HST/cycle27/OP-cache/PNLineSurveyPhaseIIrepeatFailed-v01.xml The scheduling data was generated by CASM 27.2. 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