Changed the proposal type to GO/DD.-433108327Assigned ID: 1176
----- Attempting Submission 1 (Wed Nov 13 21:32:40 GMT 2019) -----
HST Phase I Proposal 1176 (RAqr_TOO_pi_submitted.apt) successfully submitted.
Receipt: # 1176-1
----- Attempting Submission 3 (Thu Nov 14 20:45:51 GMT 2019) -----
HST Phase I Proposal 1176 (RAqr_TOO_pi_submitted_v2.apt) successfully submitted.
Receipt: # 1176-3FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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 high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
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.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserThis submission revises the FLASH level from 11 to 20 based on Jay's latest recommendation in order to better account for the increased CTE losses in the instrument.2088420684----- Attempting Submission 1 (Tue Nov 26 13:18:35 GMT 2019) -----
HST Phase II Proposal 16055 (RAq_TOO_16055_pii_v5.apt) successfully submitted.
Receipt: # 16055-1
----- Attempting Submission 2 (Tue Nov 26 23:54:38 GMT 2019) -----
HST Phase II Proposal 16055 (RAq_TOO_16055_pii_v5.apt) successfully submitted.
Receipt: # 16055-2
----- Attempting Submission 4 (Sat Nov 30 12:22:21 GMT 2019) -----
----- Attempting Submission 5 (Mon Dec 02 13:22:43 GMT 2019) -----
----- Attempting Submission 6 (Tue Dec 31 05:33:33 GMT 2019) -----
HST Phase II Proposal 16055 (16055_3visits_v1.apt) successfully submitted.
Receipt: # 16055-6
----- Attempting Submission 7 (Tue Dec 31 15:56:32 GMT 2019) -----The Quad filter observations are taken using small dithers which do not impact take the source out of the quad filters
field-of-view, and these same observations were successfully used in Prop 14847 with this target in 2017. This
proposal also only uses 1 Quad filter anymore on the same AMP as the rest of the exposures to minimize slews
between exposures so dual-guide stars can be more readily used.UNEXPECTED EARLY PERIASTRON PASSAGE AND ECLIPSE IN THE SYMBIOTIC SYSTEM R AQRWe propose ToO/DDT HST WFC3 observation of the R Aqr symbiotic system to obtain high S/N multiwavelength - UV to Optical - images of the binary environment and of the ejecta resulting from the recent - earlier then expected - periastron passage of the WD accretor. This observation is critical for studying this phenomenon (observable only about twice a century, with the next periastron passage expected in about 40 years). The effects of the periastron passage will include enhanced accretion and mass ejections and very likely new jet formation.We request a total of 3 orbits, in 1 visit.
We plan to carry out HST WFC3/UVIS imaging of R Aqr, using the 4-point dither mode in several filters. This approach will allow us to reach the maximum resolution of 0.025''/pixel and also assist in cosmic ray removal. This will nearly double the number of pixels covering the regions of interest. Furthermore, better sampling of the PSF will allow further enhancement in the resolution using deconvolution techniques such as Richardson-Lucy or EMC2.
We have selected a set of filters to separate line and continuum emission , and to distinguish shocked from photoionized emission. The high-resolution images obtained in the spectral lines e.g., CII] 2326angstroms(A), Mg II 2800A, [OII] 3726A, [OIII] 5007A, H-alpha, and [SII] 6731A, will provide information on the ionization state of the gas. The CII] line can also help determine the (dust) extinction and it is sensitive to carbonatious grain-depletion. The Mg II 2800A line is expected to have a resonant scattering component and will also provide information on the ionization state of the gas. The [OII] 3726A line is a density indicator (the line is bright when the density is low). Furthermore, the [OII] 3726A/[CII] 2326A ratio is a good indicator of temperature and density characteristics of the gas. The SII] 6731A/H-alpha ratio will allow us to identify shocked vs. ionized gas emission, e.g., the ratio will be >=0.4 for shocked gas, and smaller for photoionized gas.
The exposure times are based on the online WFC3 ETC calculations as verified by the 2017 WFC3 observations of R Aqr. We optimize the efficiency of the observing time by using subarray readouts (1024x1024 readout) to minimize the overheads, while still providing a >=40''x40'' field of view. The Phase II proposal was generated using the latest APT based on the desired exposure times to avoid saturation and on the use of dither patterns, and makes the most efficient use of the observing time.
We are requesting non-disruptive ToO observations of R Aqr. We request observing within few weeks after the formal activation (of at all possible), other wise , not later then January. In the event a reduced gyro mode will need to be used for this proposal, it will not have any significant impact as long as the target is in the HST field-of-regard when the observations need to be taken in order to catch this time-sensitive behavior of the target since we have no roll constraints for our observations.The expertise of our team is complementary (multiwavelength observations
and analysis, and theoretical modeling) which will allow us to achieve
the goals of our proposal.
Dr. Margarita Karovska: Scientific expertise in multiwavelength
observational studies and modeling of interacting binaries including
symbiotic systems. High-resolution imaging expertise (including
deconvolution techniques) allowing to achieve maximum resolution (e.g.,
previous HST observations including of R Aqr, CH Cyg, Mira, and other
interacting systems).
Warren Hack: Imaging software and data processing expertise (e.g.,
primary developer of the Drizzlepac
package). He has been applying novel
dithered-images combination techniques and PSF simulations, allowing to
reach the finest resolution achievable with the HST (e.g., previous HST
studies of symbiotics R Aqr, CH Cyg, Mira, HM Sge).
John Raymond: Extended expertise in modeling of plasma characteristics
of a wide range of astrophysical sources , including symbiotics (of the
central source and of the jet-structures - based on previous HST
observations)Stellar Physics0falseSUPPORTEDSTARACCRETION DISKINTERACTING BINARYJETSYMBIOTIC STARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF373NWFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoFQ437NWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoFQ232NPOS-TARGDITHER0.145LINEfalsefalse446.86SPIRAL2falseThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode./private/var/folders/0b/qbp4bysx6vdbfxvp_xw3dyxw00023y/T/OPVisit17978404650531406964.xml(Tic-Visit
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