0Assigned ID: 286
----- Attempting Submission 1 (Thu Apr 10 22:46:18 GMT 2014) -----We have shifted the position of visits 4 and 5 to include another transient in the field.
The positional change is 41.3" in X, and 20.8" in Y.1584241431----- Attempting Submission 1 (Thu Jul 17 20:08:59 GMT 2014) -----
----- Attempting Submission 2 (Wed Jan 14 04:06:28 GMT 2015) -----
----- Attempting Submission 3 (Wed Feb 25 04:47:05 GMT 2015) -----Massive stars dying alone: Extremely remote environments of SN2009ip and SN2010jpWe propose an imaging study of the astonishingly remote environments of two recent supernovae (SNe): SN2009ip and SN2010jp. Both were unusual Type IIn explosions that crashed into dense circumstellar material (CSM) ejected by the star shortly before explosion. The favored progenitors of these SNe are very massive luminous blue variable (LBV) stars. In fact, SN2009ip presents an extraordinay case where the LBV-like progenitor was actually detected directly in archival HST data, and where we obtained spectra and photometry for numerous pre-SN eruptions. No other SN has this treasure trove of detailed information about the progenitor (not even SN1987A). SN2010jp represents a possible collapsar-powered event, since it showed evidence of a fast bipolar jet in spectra and a low 56Ni mass; this would be an analog of the black-hole forming explosions that cause gamma ray bursts, but where the relativistic jet is damped by a residual H envelope on the star. In both cases, the only viable models for these SNe involve extremely massive (initial masses of 40-100 Msun) progenitor stars. This seems at odds with their extremely remote environments in the far outskirts of their host galaxies, with no detected evidence for an underlying massive star population in ground-based data (nor in the single shallow WFPC2/F606W image of SN2009ip). Here we propose deep UV HST images to search for any mid/late O-type stars nearby, deep red images to detect any red supergiants, and an H-alpha image to search for any evidence of ongoing star formation in the vicinity. These observations will place important and demanding constraints on the initial masses and ages of these progenitors.We will be obtaining deep WFC3 images in the V (555W), I (814W) and Halpha (665/667N) for two recent SNe 2010jp and 2009IP. Additionally, for SN 2009IP we will also obtain UV (F275W) imaging to look for O star companions. These observations will be taken over 8 orbits; 4 orbits for SN 2009ip, and 4 orbits for SN 2010jp.
For SN 2009ip a full orbit is needed for F275W, two full orbits for Halpha (665N), and one orbit for F814W and F555W.
For SN 2010jp, which is further away with higher extinction, two full orbits are needed for Halpha (657N), an orbit and a half for F555W, and half an orbit for F814W.
There are no timing constraints for our observations, although if possible we would like the visits for each SNe to occur as close to each other as is feasible.HOT STARSDefaultfalsefalsefalsefalsefalseSUPPORTEDSTARSUPERNOVA TYPE IIJ2000J2000STARSUPERNOVA TYPE IIJ2000J2000WFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF657NWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF555WTiming link suitability includes constraints ([Group (01 02 03) Within 7.0 days])Hst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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