This proposal for HST's 29th anniversary has been discussed with the Director's Office since last summer. Although we have a short fuse to conduct these observations and prepare the press release by April, we have good schedulability in Feb and March 2019 and do not require disruptive scheduling.1355453719Assigned ID: 622
----- Attempting Submission 1 (Thu Dec 20 20:06:20 GMT 2018) -----Updates: Feb. 13, 2019
Compared coordinates from Simbad's webpage to APT's Simbad generator. Positional offset between the two are ~0.144", well within the blind pointing uncertainty.
Updated the coordinate reference frame to ICRS to avoid all of the small aperture warnings.
Repacked all of the STIS orbits. Exposure times were increased in some cases and addtional shallow exposures were added whenever concerns of saturation arose.
Updated all STIS ETC IDs as well.
I changed the WFC3 expsosure times, but not the visit structure. I merged some small dithers into the POS TARGs along with the offset and gap dithers. We will likely have further revisions to our STIS visits later, and we are still verifying whether our target coordinates and proper motions are ICRS and consistent.-235623286----- Attempting Submission 1 (Sat Jan 12 03:05:38 GMT 2019) -----
----- Attempting Submission 2 (Thu Jan 17 19:48:35 GMT 2019) -----
----- Attempting Submission 3 (Sat Feb 02 17:16:26 GMT 2019) -----
----- Attempting Submission 4 (Thu Feb 14 07:24:02 GMT 2019) -----Spectroscopy and Imaging of the Southern Crab NebulaWe will obtain WFC3 imaging of the Southern Crab Nebula (also known as WRAY-16-47 and Hen 2-104) with four narrowband filters to detect key nebular emission features. We will also obtain high-quality STIS spectra, which will cover the core of the nebula and one of the bright limbs of the ejecta.We will obtain high S/N images of the Southern Crab Nebula with 4 narrowband filters to detect key nebular emission features (F502N, F656N, F658N, F673N). This target has a bright central region, with much fainter extended structure, so there is some chance the central region may saturate in our long exposures. To mitigate this, we will also obtain some short exposures with these narrowband filters. This will ensure that we have unsaturated images of the central region, which should show nebular expansion relative to earlier WFPC2 images from 1999-2003. We will also obtain short exposures with two broadband filters (F475W, F606W) for continuum subtraction and star colors across the entire field. Each filter will consist of multiple dithered exposures which will be drizzle-combined to eliminate chip gaps, hot pixels, and cosmic rays. We specify a desirable WFC3 pointing with an orientation available in March 2019. We place the target on WFC3 chip 2 (UVIS2-FIX, with a slight offset applied) to avoid having window ghosts (internal reflections caused by other stars in the field) fall on the nebula. We use POS TARGs to merge this offset with dithers for the chip gap and improved sampling. The WFC3 went into safemode at the time of our Phase II program submission. So in an early version of this program we included alternate ACS imaging as ON HOLD visits to be used in case WFC3 is unavailable before our window closes at the end of March 2019. WFC3 later came out of safemode and these backup ACS visits have been removed, but could be swapped back in for the WFC3 visits if needed.
We will also obtain high-quality G430M and G750M spectra with STIS, which will cover the core of the nebula and one of the bright limbs of the ejecta. In order to maximize signal to noise in the spectrum, we will use a 0.5" slit (52x0.5). The velocities in the nebula are low enough that we do not expect using a smaller slit to reveal signicant structure in the 2-D spectrum, so we will sacrifice spectral resolution to maximize the number of photons from the extended source. The two gratings will allow us to construct a high quality spectrum spanning from H-beta to around 6700A. We estimate that 7 orbits should be sufficient to obtain high quality spectra in both G430M and G750M using the 0.5" slit. We will include CR-SPLITs for cosmic ray removal, and dithering for hot pixel filtering during data processing. There are limited observations of this target in the archive, but they are sufficient to enable detailed integration time calculations. A STIS spectrum taken with the G750M grating for HST program 9050 (PI Balick) at a short exposure of 280s shows prominent features include H-alpha and the [NII] doublet, as well as He I 6678 and the [SII] doublet at 6717A and 6731A to the right of He I 6678. Even in this short exposure, the diffuse emission from H-alpha and the [NII] doublet is visible, extending above and below the central star along the spatial direction. Flux measurements in each line are also available from ground based spectra (de Freitas Pacheco & Costa, 1996) which cover the range 3600-7000A. We specify a desirable orientation of the STIS slit (52x0.5) which is available before April 2019.Stellar Physics3falseSUPPORTEDSTARCIRCUMSTELLAR MATTEREMISSION LINE NEBULASYMBIOTIC STARYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000WFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF658NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF606WSTIS/CCDSpectroscopicNoNoG430M4961STIS/CCDSpectroscopicNoNoG430M5216STIS/CCDSpectroscopicNoNoG430M5471STIS/CCDSpectroscopicNoNoG750M5734STIS/CCDSpectroscopicNoNoG750M6252STIS/CCDSpectroscopicNoNoG750M6581STIS/CCDSpectroscopicNoNoG750M6768ACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WPOS-TARGDITHER0.761655LINEfalsetrue390.0STIS-ALONG-SLIT3falseThe scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode./private/var/folders/_b/k1329bs53yg68lrswlm3cqwm0001dl/T/OPVisit2898979236356089454.xml(Tic-Visit
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)true40Halpha will saturateShallow exposure for Halpha to not saturate