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.Re-submission with use of BLADE=A for shortest exposures based on recommendation from PC in order to preserve
the primary goal of this proposal; namely, the highest possible resolution view of this active object.
set mode to available, approved by team lead
visit 02 is HOPR repeat of visit 01
In addition, the shorter exposure times in visit 02 were adjusted to better match the increasingly brighter source (now going brighter than V=8.75).570305298----- Attempting Submission 1 (Thu Sep 05 20:59:34 GMT 2019) -----
HST Phase II Proposal 16000 (mw560_chandra_cy27_pii.apt) successfully submitted.
Receipt: # 16000-1
----- Attempting Submission 2 (Tue Sep 17 20:48:31 GMT 2019) -----
----- Attempting Submission 3 (Wed Sep 18 15:20:07 GMT 2019) -----
----- Attempting Submission 4 (Wed Feb 19 13:31:26 GMT 2020) -----
----- Attempting Submission 5 (Fri Feb 21 18:13:53 GMT 2020) -----Our observations are of a point source with limited extended emission expected which will in no way be impacted by the use of the Quad filter. We have used this filter before with no issues on previous proposals
The use of the BLADE=A option is required, as recommended by our Contact Scientist, in order to preserve the spatial
resolution needed for the science of this variable and active object.EVOLUTION OF RECENTLY DISCOVERED SPATIALLY RESOLVED JET/OUTFLOW IN THE SYMBIOTIC MWC 560We propose to carry out coordinated Chandra, HST, and XMM observations of the MWC 560 symbiotic interacting binary system, as a follow-up to the 2016 Chandra discovery of an extended jet/outflow. When combined, these observations will result in a comprehensive picture of the central source and the dynamic jet/outflow from as close as few hundred AU from its source, to the region of its interaction with the circumbinary environment into which the jet propagates. We will determine its evolution and origin, including association with powerful past outbursts in the system.We plan HST observations (in Cycle 27) using WFC3 high-spatial resolution imaging in several spectral lines and the continuum. This would allow us to unambiguously study the components of the system, including the ejected material (jet/outflow) and the core. We request a total of 4 orbits, in 1 visit. The selected set of filters (see table below) will separate line and continuum emission, to distinguish shocked from photoionized gas, and to determine the shock speed and the nature of the photoionizing continuum. Difference and ratio maps will reveal changes in local physical conditions. We plan to carry out the observations in a dither mode to improve the sampling of the PSF, and to deal with cosmic rays. The pixel size for WFC3 is 0.04 arcsecond/pixel. We plan to use a standard dither pattern which fractionally samples the pixels across the detector; namely, the WFC3-UVIS-DITHER-BOX pattern as described in https://hst-docs.stsci.edu/display/HPIOM/7.3+WFC3+patterns#id-7.3WFC3Patterns-W-UDitherbox. This pattern has steps in pixels of (0, 0), (4.0, 1.5), (2.5, 4.0), and (-1.5, 2.5). This will allow us to reach 0.025 arcsecond/pixel when combining the dithered images using the {\it drizzle} software, doubling the number of pixels covering the regions of interest. We will use a combination of long and short exposure times to compensate for the high contrast between the red-giant and surrounding emission(s). This technique was used effectively in a number of observations (e.g., symbiotics CH Cyg and R Aqr). The exposure times were estimated using the latest version of the online Exposure Time Calculator assuming a combined red-giant plus white-dwarf spectrum normalized to V=9.5 with E(B-V)=0.18. The reddening estimate was determined with the use of the Pan-STARRS 1 3D Dust Mapping online tool. Given the variable nature of this system, we set the exposure times conservatively to minimize the chance of saturation while still allowing to observe the object in the selected filters even when it is up to a magnitude brighter. We request use of the UVIS 1K subarray readout modes in order to minimize readout overhead times and buffer memory usage. This increases the number of total exposures we can get in each orbit while still providing a sufficient field-of-view which covers the extended emission. The overheads listed in the online Phase-1 proposal instructions are 2.1 min/exposure (2.4 min for the first exposure). To this are added the times for guide star acquisition for each orbit (6 min x 4 orbits=24 min) and 1 min efficiency/orbit (4 min). These overheads added to the combined exposure times for a 4-point dither pattern for each filter result in a final total of ~200 min, which is enough to fit into the time available in 4 orbits for ~216 min, with 54 minutes per orbit, based on the visibility charts provided by ``Available Science Time and Visibility Tool''. The sets of exposures can be split across the orbits to maximize efficiency. The Cycle 27, APT shows good visibility of the target over extended periods in 2019/2020. {Summary of HST/WFC3 Observations} {FILTERS and EXPOSURES for Visit 2} F280N MgII -- 4 x 360 s plus 4 x 10 s exp. F275W cont. -- 4 x 15 s exp. F336W cont. -- 3 x 10 s exp. F373N [OII] -- 4 x 90 s exp. plus 4 x 3 s exp. FQ437N [O III] -- 4 x 10 s F502N [O III] -- 4 x 1s plus 4 x 10 s plus 4 x 120 s exp. plus 2 x 550s exp. F547M cont.-- 4 x 0.5 s exp. F656N H-alpha -- 4 x 1 s plus 4 x 30 s plus 2 x 360 s exp. F673N [S II] -- 4 x 1 s plus 4 x 30 s exp.Stellar Physics6falsefalsefalsefalsefalsefalse0.00.0falseAVAILABLEEXT-STARACCRETION DISKJETSYMBIOTIC STARThis object was generated by the targetselector and retrieved from the SIMBAD database.V694-MONDR1-3054628260437829760J2000J2000WFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF373NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoFQ436NWFC3/UVISImagingNoNoFQ437NWFC3/UVISImagingNoNoF547MPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.158158889900058.47859760273849(Tic-Visit
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