0Assigned ID: 5670
----- Attempting Submission 1 (Tue Mar 26 21:20:29 GMT 2024) -----
HST Phase I Proposal 5670 successfully submitted.
Receipt: # 5670-1
----- Attempting Submission 2 (Tue Mar 26 21:23:40 GMT 2024) -----
HST Phase I Proposal 5670 successfully submitted.
Receipt: # 5670-2
----- Attempting Submission 3 (Tue Mar 26 23:49:09 GMT 2024) -----
HST Phase I Proposal 5670 successfully submitted.
Receipt: # 5670-3
----- Attempting Submission 4 (Tue Mar 26 23:52:51 GMT 2024) -----Split this into 12 1-orbit visits and a time constraint to have all observations obtained within 1 week.2024718574----- Attempting Submission 1 (Fri Aug 16 13:52:31 GMT 2024) -----
----- Attempting Submission 2 (Thu Sep 04 15:44:54 GMT 2025) -----Adding Armin Rest to list of Co-I's. Thank you!A Deep Search for the Surviving Companion to the SN 2016gkg ProgenitorBinary physics is an area of growing interest given the implications on a wide range of stellar systems, including merger sources for gravitational waves. Identification of progenitors to stripped-envelope supernovae (SESNe) offers a direct approach to constraining binary evolution scenarios. While the pathway by which SESN progenitor stars lose their envelope remains ambiguous (single vs. binary models), growing evidence suggests most SESN progenitors (>50%) are in binary systems. In just the past few years, the number of direct detections of surviving companions has grown to five. While exciting, the sample is still too small to make statistically meaningful conclusions about either the population or the binary physics itself. Increasing the sample size is slow given the small number of viable candidates, which means that each new data point is significant. Here we propose deep WFC3/UVIS optical+UV observations of the only relevant target for Cycle 32: SN 2016gkg at <26 Mpc. Similar to other companion searches, we aim to detect or place meaningful limits on any surviving companion. We also include one orbit to obtain F555W astrometry on the recent SESN 2023mut for potential future follow-up studies. This experiment will take advantage of HST's unique UV capabilities and will help build a statistically significant sample that will affect our fundamental understanding of binary evolution. The combined low likelihood of future events and HST's expected lifetime make these observations all the more critical.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 iPTF13bvn (12 orbits)
-F336W (17500 s)
-F555W (13500 s)
- FLASH = varies with aim of minimizing photon transfer losses and read noise
- 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.
-For dithering, we use 5 different POS TARGS instead
*Impact of Gyros*
We have considered the impact of reduced gyro operations on our program, which has 12 orbits requested. We were able to successfully reduce this target to 4 visits, each with 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 the constraint that all be scheduled within 1 day of each other.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 Types6falsetruefalsefalsefalsefalseSUPPORTEDEXT-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/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF555WWFC3/UVISImagingNoNoF555WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseTiming link suitability includes constraints ([Group (01 02 03 04 06 07 08 09 10 11 12 13) Within 7.0 days])The scheduling data was generated by CASM 33.1.CASM was run in Phase II mode./private/var/folders/yh/kl4y3s1x3_j3ywy3qq67g3vc0001kc/T/OPVisit11926333819611845267.xml(Tic-Visit
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