0Assigned ID: 308
----- Attempting Submission 1 (Thu Mar 05 21:45:13 GMT 2020) -----
HST Phase I Proposal 308 successfully submitted.
Receipt: # 308-1
----- Attempting Submission 2 (Fri Mar 06 16:10:22 GMT 2020) -----
HST Phase I Proposal 308 successfully submitted.
Receipt: # 308-2
----- Attempting Submission 3 (Fri Mar 06 16:33:02 GMT 2020) -----
HST Phase I Proposal 308 successfully submitted.
Receipt: # 308-3
----- Attempting Submission 4 (Fri Mar 06 22:52:03 GMT 2020) -----0----- Attempting Submission 1 (Tue Jun 30 21:52:38 GMT 2020) -----Towards a Comprehensive Search for Surviving Companions to Stripped-Envelope SupernovaeWe propose optical+UV observations at the sites of nearby stripped-envelope supernovae (SNe) to search for expected surviving binary companions from the progenitor systems. Directly measuring the photometry (or deep upper limits) of SN companions provides a critical constraint on the underlying physics in binary evolution models, which in turn has far-reaching implications in all of astrophysics. While a number of binary star models exist, the detailed physics remain unconstrained (e.g., winds, rotation, metallicity, nuclear burning instabilities). Current models predict that the majority of stripped-envelope SNe (i.e., IIb, Ib, and Ic) have a close binary companion, but the expected endpoints for these companions vary based on the physics of the binary interaction and evolution. An unbiased, comprehensive, statistically complete sample of direct companion observations is necessary to measure the actual binary fraction and stellar type. To date, however, only several candidate detections exist. Our program will build a meaningful sample by providing robust detections (or deep upper limits) of the most viable candidates out to a reasonable detection limit (~20 Mpc). NUV (F275W/F336W) imaging offers an optimum detection strategy for the expected hot, blue stellar companions, while optical imaging can rule out shock interaction contributions and probe less likely, but possible, cooler star companions. Given HST's time horizon, the degrading UV response on WFC3, and the requisite waiting period to allow the SN to fade before conducting a companion search, now is the time to take full advantage of HST's unique UV capabilities.WFC3:
- Use entire array to aquire fiducial stars for alignment purposes
- Use 512_UVIS2_CTE aperture to minimize photon transfer losses for 12fh and 13ge only
- When scheduled, please have CS contact PI to finalize pos_tag based on final orientation
- EXPTIME (actual):
-SN 2012fh (3 orbits)
-F275W (5246 s)
-F336W (2364 s)
-SN 2016coi (1 orbit)
-F555W (2381 s)
-SN 2017gax (1 orbit)
-F555W (2614 s)
-SN 2013ge (9 orbits)
-F275W (13803 s)
-F336W (8082 s)
-F438W (1000 s)
-F555W (700 s)
- FLASH = varies with aim of minimizing photon transfer losses and read noise
- To be safe
- 4 pt WFC3-UVIS-DITHER-Box
-Provides optimal 4-step sampling of the PSF; produces spacings of >1 column for removal of hot columns
- remove CR and hot pixels
*Scheduling constratints for 16coi and 17gax*
Although we did not specifically mention scheduling constraints in the original proposal, the goal of observing 16coi and 17gax is to observe the SN position (astrometry) before it fades. We estimated a flux based on a decline rate somewhere towards the middle of Cycle 28. Therefore, scheduling these targets earlier in the cycle is a huge benefit since the late time decay of such SNe remains somewhat uncertain. We therefore request the added scheduling constraints for 16coi and 17gax (only one orbit each).
*Impact of Gyros*
We have considered the impact of reduced gyro operations on our program. The only problematic observation is SN 2013ge, which has 9 orbits requested. We were able to successfully reduce this target to 4 visits, each with 2-3 orits per visit. The only condition is that all filters must be obtained in the same orientation for several reasons, including time variablility and optimized sampling and reductions. Therefore, we have added this constraint.Our team consists of experts ranging from theory to observation.
PI Dr. Ori Fox is an expert in observations of SN companions with HST. He led the HST/COS paper on detecting the companion to SN 1993J (Fox et al. 2014) and was PI of the HST/WFC3 program that led to papers on the companions to SN 2002ap (Co-I Zapartas et al. 2017a) and SN 2001ig (Co-I Ryder et al. 2018).
For Observations, Data Reduction, Analysis, and Interpretation: Dr. Jennifer Andrews is an expert observer and works heavily on SNe. With approved time on MMT, she will any necessary supporting ground-based observations. Ms. K. Azalee Bostroem is an expert on HST data, as she used to work at STScI as a Research Instrument Analyst. Dr. Maria Drout is an expert in stripped-envelope SNe. Professor Alex Filippenko has approved time on Keck and Lick that can provide for any necessary supporting ground-based observations. Professor Pat Kelly has long studied the properties of host galaxies of SNe. Dr. Jon Mauerhan is an expert on spectropolarimetry and has much experience regarding the properties of massive stars. Mr. Nathan Miles is an expert on HST/WFC3 data, as he currently works at STScI as a Research Instrument Analyst. Professor Dan Milisavljevic is an expert in SN theory and observations. Dr. Stuart Ryder is an expert in binary companion observations. Professor Nathan Smith is an expert in the properties and evolution of massive stars, and on spectroscopy of SNe. Dr. Schuyler Van Dyk is an expert in HST photometry of SNe and in the study of stripped-envelope SNe. Dr. WeiKang Zheng is an expert at CCD imaging and photometry of SNe, both ground-based and HST; he will construct multifilter light curves of the object. Dr. Ben Williams is an expert in local stellar populations, which is an important aspect of our study in case we need to disentangle line of sight coincidences.
For Theory and Interpretation: Professor Selma de Mink is an expert in SN population synthesis theory and modeling. Dr. Niharika Sravan is an expert in binary modeling. Dr. Emmanouil Zapartas is an expert in population synthesis theory and modeling.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IBJ2000J2000EXT-STARSUPERNOVA TYPE IBThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARSUPERNOVA TYPE IBThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARSUPERNOVA TYPE IBThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX3false/private/var/folders/0b/qbp4bysx6vdbfxvp_xw3dyxw00023y/T/OPVisit2080405297235726870.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.1610548290000286.2422577230618(Tic-Visit
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