Hi,
We are submitting only the 7 visits allocated by the DD process. We have deleted or moved some of the visits to correspond to the allocated 7 orbits.
We have placed orientations and acceptiable dates for the observations into the phase 2. If there are any problems please contact me (dzurek@amnh.org).
Thank you
Dave----- Attempting Submission 5 (Wed May 04 16:06:23 GMT 2011) -----Ionization and Light Echoes in the T Pyxidis NebulaContrary to published predictions, the famous prototype recurrent nova T Pyxidis unexpectedly commenced a new outburst on 2011 April 14 UT --- its first outburst since 1966. T Pyx is unique among recurrent novae in being surrounded by a nebula, representing material ejected during previous eruptions, which is well resolved into thousands of sub-arcsecond features in HST images. The outburst offers the opportunity to make two unique measurements. (1) A direct geometric determination of the distance to T Pyx (a highly controversial subject), based on imaging polarimetry of the knots --- a technique already validated for the light echo around V838 Monocerotis. (2) A determination of the 3D structure of the nebula, based on the ionization echo that will sweep out into the nebula, causing each individual knot to develop strong Halpha emission when first illuminated by the nova. Our proposed observations consist of Halpha imaging with WFC3, and broadband polarimetric imaging with ACS. Our results will 1) Allow a determination of the distance, and hence the true luminosity and mass accretion rate onto the white dwarf in T Pyx. This is essential for determining if T Pyx (and other recurrent novae) will exceed the Chandrasekhar limit and erupt as a type Ia SN. 2) Allow a direct test of the most detailed numerical modeling of nova explosions ever done. Recently predicted features and geometries in the ejecta must be present, and will be observed by HST for the first time, if, and only if our state-of-the-art models of novae are correct.
The wave of illumination and ionization will pass through the entire nebula within the next few months, so it is crucial to begin the HST observations as soon as possible.We request the first Halpha observation to be made as soon as possible, nominally about 7-10 days after the outburst begins. After that, images should be obtained at about 14, 24, 38, 58, 86, 109, 155, 190, and 225 days after April 14. (The gap between 109 and 155 days is due to T Pyx being too close to the Sun during that interval.) We also request two visits for the polarimetric imaging, at about 20 and 30 days after April 14.ISM AND CIRCUMSTELLAR MATTER0false0.00.0falsefalsefalsefalseSUPPORTEDISMEJECTASHELLJ200009 04 41.5000-32 22 47.50J2000WFC3/UVISImagingNoNoF656NACS/WFCImagingNoYesF606WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseThe scheduling data was generated by CASM 19.0.CASM was run in Phase II mode./private/var/folders/vw/vwvqK9d7GOOBvWlI3odYiU+++TI/-Tmp-/OPVisit783154935935309378.xml130309209700088.14595811763121(Tic-Visit
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