0Assigned ID: 3686
----- Attempting Submission 1 (Fri Mar 25 23:10:35 GMT 2022) -----
HST Phase I Proposal 3686 successfully submitted.
Receipt: # 3686-1
----- Attempting Submission 2 (Fri Mar 25 23:45:50 GMT 2022) -----
HST Phase I Proposal 3686 successfully submitted.
Receipt: # 3686-2
----- Attempting Submission 3 (Fri Mar 25 23:47:36 GMT 2022) -----This pattern is not used in this proposal.
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browserUpdated timing constraints.-369479223----- Attempting Submission 1 (Thu Jul 14 13:44:44 GMT 2022) -----
----- Attempting Submission 2 (Thu Oct 06 17:07:04 GMT 2022) -----
----- Attempting Submission 3 (Wed Dec 07 21:59:09 GMT 2022) -----New Flash values recommended by CS.Towards a Comprehensive Search for Surviving Companions to Stripped-Envelope SupernovaeThe mass-loss mechanism for stripped-envelope supernovae (SESNe) remains debated, but indirect evidence is mounting in support of binary stars. It wasn't until 2014, however, that the community obtained the first direct post-explosion detection of a surviving companion to a SESN (Type IIb SN 1993J). Since then, there have been four more, including the first fully stripped Type Ib/c SN 2013ge this past year. The field is now past the point of targeting individual systems one at a time. A statistically complete companion-mass distribution (including deep upper limits) can provide important constraints on the underlying physics used in binary evolution models (e.g., winds, rotation, metallicity, nuclear burning instabilities), which in turn has far-reaching implications in all of astrophysics, including merger sources for gravitational waves. Building the proper dataset is a slow process given the small number of viable candidates each year (considering distance, extinction, etc.). Here we propose optical+UV observations at the sites of the two most viable SESNe targets of this year to detect (or place meaningful limits on) any surviving companion. 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. We also propose ongoing monitoring of SN 2013ge. 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
- When scheduled, please have CS contact PI to finalize pos_tag based on final orientation
- EXPTIME (actual):
-SN 2016coi (9 orbit)
-F275W (13803 s)
-F336W (8082 s)
-F438W (1000 s)
-F555W (700 s)
-SN 2017gax (9 orbit)
-F275W (13803 s)
-F336W (8082 s)
-F438W (1000 s)
-F555W (700 s)
-SN 2013ge (4 orbits)
-F336W (8082 s)
-F555W (700 s)
- FLASH = varies with aim of minimizing photon transfer losses and read noise
- Note prior email to Sylvia. Hope all is well. Tis the night before Phase 2's are due, and I need a clue. We are wondering about Flash settings.
- Here is the situation:
*We are trying to detect a single, very faint source (surviving star from a supernova). We only care about one position, not the entire field.
*We have placed the pointing in the center of the UVIS2-512C-CTE aperture, so that will help with the CTE.
*We are not sure what the background from the galaxy looks like, but it may contribute to the flux slightly (or not at all).
*It is easy to adjust the Flash value in APT to turn the warning off, but we are hoping we aren't adding too much noise unnecessarily, as this source is faint.
- 4 pt WFC3-UVIS-DITHER-Box
-We use 4 POS TARGS instead
*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.
Dr. Justin Pierel, Dr. Melissa Shahbandeh, and Dr. Sebastian Gomez are postdocs at STScI working with PI Fox. All are expert observers with extensive HST data reduction and analysis experience.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDEXT-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/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF555WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseTiming link suitability includes constraints ([Group (01 02) Within 1.0 days] [02 After 01 by at most 5.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1669320370000292.03131(Tic-Visit
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