0 Assigned ID: 778 ----- Attempting Submission 1 (Fri Apr 05 21:19:41 GMT 2019) ----- 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 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 Added one orbit of data-taking to 15955_19 because that opportunity added a forth orbit. 561433687 ----- Attempting Submission 1 (Fri Sep 27 19:51:47 GMT 2019) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 2 (Thu Oct 03 17:07:16 GMT 2019) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 3 (Mon Oct 21 21:16:01 GMT 2019) ----- HST Phase II Proposal 15888 (pureparallel_phase_II.apt) successfully submitted. Receipt: # 15888-3 ----- Attempting Submission 4 (Mon Oct 21 21:17:18 GMT 2019) ----- ----- Attempting Submission 5 (Mon Oct 28 19:53:38 GMT 2019) ----- HST Phase II Proposal 15888 (pureparallel_phase_II.apt) successfully submitted. Receipt: # 15888-5 ----- Attempting Submission 6 (Thu Oct 31 14:10:40 GMT 2019) ----- ----- Attempting Submission 7 (Fri Dec 13 15:30:48 GMT 2019) ----- We expect nebulosity and extended emission in the observed region, which will fill out the charge traps and avoid CTI. This should help to bring the background level up to 12 without longer LAMP flashes for the three WFPC exposures that report problems.. A pure-parallel search for faint stuff in star forming regions Star forming regions contain many resolved structures, ranging from disks around individual stars to narrow and wide binaries to large-scale outflows, bubbles and shock fronts traversing the entire cloud. In many cases, optical high-resolution imaging is the best tool to find and study these objects. We propose a pure-parallel survey, where no primary orbits are allocated and instead or observations are performed on whatever happens to be in the field-of-view of the WFC3 or ACS when other programs use STIS or COS on targets in star forming regions. In this way, we can survey a large area to discover (i) previously unresolved companions, (ii) jets and outflows from young stars and (iii) irradiated and evaporating disks. Typically, such imaging studies are done in the most "interesting" regions close to the most massive and brightest stars. Our survey can complement that by imaging more "typical" parts of the cloud. We will use a combination of broad-band filters to detect nebulosity and identify and separate point sources as well as narrow-band filters in emission lines typically seen from irradiated disks, jets, and outflows. This is a program to carry out pure-parallel observations of star forming regions in our galaxy. We designed a pure-parallel survey, where no primary orbits are allocated and instead or observations are performed on whatever happens to be in the field-of-view of the WFC3 or ACS when other programs use STIS or COS on targets in star forming regions. In this way, we can survey a large area to discover (i) previously unresolved companions, (ii) jets and outflows from young stars and (iii) irradiated and evaporating disks. Typically, such imaging studies are done in the most "interesting" regions close to the most massive and brightest stars. Our survey can complement that by imaging more "typical" parts of the cloud. We will use a combination of broad-band filters to detect nebulosity and identify and separate point sources as well as narrow-band filters in emission lines typically seen from irradiated disks, jets, and outflows. As such, we aim for a combination of broad-band and narrow band filters. Narrow band images trace instead the rich phenomenology typical of these regions. In particular, in high-mass star-forming regions, [O iii] is a good tracer of hot nebular gas, either radiatively or collisionally excited, whereas in low-mass star-forming regions, [O iii] 5007 Ang only traces shock excitation (jets and HH objects). The soft-UV flux typical of these regions supports the complex chemical networks typical of PDR regions, which includes [O i] emission from the photodissociation of water molecules. WFC3 has a larger choice of narrow-band filters, and, if we have the opportunity (see below) we propose to add observations in [O i] 6300 Ang and two lines in the UV that are unique to HST /WFC3 because they are inaccessible from the ground (Mg ii 2800 Ang and [Ne v] 3426 Ang) as well as additional broad-band WFC2 V images. In particular, Mg ii 2800 Ang has been shown to be strong, even stronger than Halpha in jets from low-mass stars (Coffey et al. 2007). If we have only one orbit with a specific pointing, we will perform imaging with the WFC3 because it is located closer to the STIS or COS FOV. In a star-forming region, a STIS or COS observation is most likely centered on a bright, active star and thus observing closer to it increases the chances to find irradiated cloud or outflow features. However, it is typical for FUV spectroscopic observations to last for more than one orbit. In those cases, we may have access to more than one parallel orbit with almost the same pointing. We use the extra orbits for additional observations with ACS/WFC and to observe in other filters in the WFC3. ACS has a FOV a few arcmin away from WFC3. The ACS is equipped with fewer filters than the WFC3 and thus there would be little use to add another orbit for a second set of filters in the ACS. In general, if we have more than three orbits with the same pointing, we plan to repeat the cycle of three orbits (WFC3, ACS, and WFC3 with other filters) observations to detect fainter features and to take advantage of multiple dither positions (if the primary observation dithers); taking multiple exposures in each filter will also mitigate against cosmic rays. We selected five opportunities from the list provided to us and, following the general strategy above, selected WFC3 and ACS obsrvations. The time available in ech orbits varies widely and so does the duration and spacing of the buffer dumps in the primary instrument. We fiddeled with the exposure times by hand to place our buffer dumps between the primary buffer dumps. In some cases, that limits the number of exposures we cna take in a single orbit, e.g. in parallel observations 9 we cannot squeeze a buffer dump between the primary dumps and are thus forced to limit ourselves to two exposures per orbit, such that the buffer can be dumped in occulation. The proposal may observe a wide variety of phenomena depending on which primary targets in star forming regions our observatiosn can be scheduled with. Thus, we built a team that has expertize in different areas, listed here: PI Guenther: WFPC3 PSF modelling, SEDs, microjets, accretion modelling Co-I Principe: high-contrast imaging of dust around low-mass stars (e.g. SPHERE on the VLT looking for cavities in the envelope, hour-glass shaped outflows etc.) Co-I Schneider: jets (high-mqass and low-mass), X-rays Co-I Gomex de Castro: resolved and unresolved binaries, surveys Co-I Manara: extinction from spectrsocopy or photometry Co-I Bacciotti: Jet imaging Co-I Robberto: performed a study of the Orion Nebula cloud with very similar filters and coverage, thus he really knows everything we're going to get from targeting high-mass star forming regions Co-I Wolk: multi-wavelength surveys and source classification Stellar Physics 6 false false false false false false false SUPPORTED WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F502N ACS/WFC Imaging No No F625W ACS/WFC 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