0Assigned ID: 2965
----- Attempting Submission 1 (Thu Mar 24 11:48:06 GMT 2022) -----
HST Phase I Proposal 2965 successfully submitted.
Receipt: # 2965-1
----- Attempting Submission 2 (Thu Mar 24 23:37:19 GMT 2022) -----
HST Phase I Proposal 2965 successfully submitted.
Receipt: # 2965-2
----- Attempting Submission 3 (Fri Mar 25 15:34:33 GMT 2022) -----
HST Phase I Proposal 2965 successfully submitted.
Receipt: # 2965-3
----- Attempting Submission 4 (Fri Mar 25 18:01:41 GMT 2022) -----
HST Phase I Proposal 2965 successfully submitted.
Receipt: # 2965-4
----- Attempting Submission 5 (Fri Mar 25 18:16:19 GMT 2022) -----May 22: Resubmission - PI added a GAIN=4 property to all 4 exposures in the visit 5
May 20: Re-Submitting on behalf of the PI.
This rapid ToO necessitates a disruption of regular HST operations.
Therefore we will work together with the STScI team to do everything operationally possible to facilitate a swift trigger, which will greatly improve the scientific impact of this observation.
The PI’s mobile number is +972528631854 and will be available 24 hours a day throughout the execution of this proposal.
If no answer is given by the first PI please conact the Co-PI at +972547688876
Reason for Activation:
SN2023ixf is an infant SN that has recently been discovered by Koichi Itagaki (https://www.wis-tns.org/object/2023ixf) and is at most a day old. The SN host is M101 at the extremely nearby distance of 7 Mpc. The SN shows a strong g-r ~ -0.11 color, magnitude difference suggesting it to be hot, peaking in the UV. The SN optical magnitude is currently 14.05 at r-band and 13.94 at g-band as measured by photometry from the Liverpool telescope in La Palma, adhering to the magnitude constraint in our proposal.
Rapid spectroscopy obtained by the SPRAT spectrograph on board the 2.0 meter Liverpool telescope in La Palma telescope revealed strong flash features including narrow Balmer lines, He II λ4686, N III λ4634&4641 doublet, as well as other narrow lines commonly found in infant SNe surrounded by CSM.
We, therefore, request to activate our rapid disruptive ToO to obtain UV flash spectroscopy for this Supernova.
This is an extremely nearby SN, and to my knowledge, it is the nearest type II exhibiting flash features ever discovered. Such SNe are only discovered once per decade. It is likely the best candidate we will have for this program.
Scheduling Requirements:
According to our proposal, we wish for the first visit to occur as soon as operationally possible, ideally within 2 days.
We fiducially suggest visits 2 and 3 that to be spaced at about 10 and 20 hours after visit 1, however a 20 hour cadence would also suffice.
Lastly, we ask that visit 4 be scheduled 2-3 days after visit 3 and visit 5 be scheduled 2-3 days after visit 4.247471481----- Attempting Submission 1 (Thu Jul 14 13:28:41 GMT 2022) -----
----- Attempting Submission 2 (Sat May 20 01:58:38 GMT 2023) -----
----- Attempting Submission 3 (Sat May 20 16:01:42 GMT 2023) -----
----- Attempting Submission 4 (Mon May 22 18:50:49 GMT 2023) -----visit planner ranExplosions in Real-Time: Rapid UV Supernova Flash SpectroscopyRapid UV spectroscopy of an infant supernova explosion offers compelling science returns and can only be carried out by HST. UV spectra provide a unique insight into the first days of the explosion, a way to determine the initial metallicity and surface composition of the exploding star as well as a probe of the final year of mass loss leading to the terminal SN event, tracing the final stages of pre-explosion stellar evolution. Constraining such progenitor properties of SNe could pave the path to answer the 2020 Decadal Survey question on what powers the diversity of explosive phenomena across the elecromagnetic spectrum. This is only possible with HST in rapid ToO mode. A successful campaign to study an infant stellar explosion in the UV from its very start would benefit from preparations undertaken by STScI.This rapid ToO necessitates a disruption of regular HST operations, we propose to make full use of this disruption, and undertake a series of 5 visits.
The first visit should occur as soon as operationally possible. Therefore ideally we would want to have an activation time of 2-3 days after trigger. However, in case this is not possible, in some cases we would be able to achieve our science goals even with a 5 day activation time.
We fiducially suggest visits 2 and 3 that to be spaced at about 10 and 20 hours after visit 1 (i.e a 10 hour cadence from the first visit). However, the exact spacing will depend on HST tecnical constraints, and a more relaxed and uneven cadance between all 3 first visits is possible with a range between 10-24 hours between visits, optimized to avoid SAA and that conforms to scheduling constraints, and should provide useful science as well.
Within the first 3 visits we plan a 5-orbit sequence interspersing a joint optical blue (G430L) and red (G750L) orbit among 4 UV (G230LB) orbits. This will allow to monitor the UV evolution of the spectrum on an orbit timescale.
Should there be a critical operational need for shorter visits, we would be able to compliment a 4-orbit UV-only visit with high quality spectra from ground instruments.
In the next 2 visits we propose to have the B/R visit at the end of 2-3 consecutive UV orbits (longer UV and shorter optical exposures with time), based on previous work showing that within days the UV emission drops, while the optical is on the rise. Visits 4-5 then follow 2 - 3 and 4 - 5 days later, with the goal of mapping the CSM distribution by observing the UV lines disappear. These late visits will be shorter (4 and 3 orbits, of which one split among B and R grisms in each visit), as their main goal could be achieved using just the strongest lines.Trigger day - working with STScI: Experience shows that good planning and solid groundwork are the key to successful rapid spectroscopic follow-up campaigns. We build our strategy on the combined legacy and demonstrated success of previous ground-based work with PTF/ZTF as well as previous HST UV SN spectroscopy ToO programs. In this new era of SN studies, where the relevant timescales are ~1 hour (instead of the traditional day), we require a team that is available around the clock to identify a target, rapidly obtain and analyze critical follow-up observations (ground-based spectroscopy, Swift UV photometry), and promptly communicate with STScI personnel. To facilitate this we have set up two sister operational teams around the globe, the ``Eastern hemisphere'' (Israel and Europe, led by coPI Gal-Yam) and ``Western hemisphere'' (US; led by a Co-I Cenko) teams, each led by a person with extensive experience in managing such rapid follow-up campaigns, and including experts in design and rapid analysis of follow-up spectroscopic data and Swift photometry, as well as, importantly, persons with extensive experience in operations, trigger and analysis of HST/STIS ToO UV SN spectroscopy as part of previous successful programs. As the sun never sets on our operational network, at the day of trigger STScI staff can rely on having at their disposal a science team available immediately to provide all necessary information, guidance and scientific decisions, with experienced members in such interactions from previous cycles. The full composition of our teams is as follows: Eastern team: Gal-Yam (coPI, lead, STIS ToO spectroscopy), Ben-Ami (STIS UV spectroscopy), Yaron, Schulze, Perley, Bruch (rapid spectroscopy), Ofek, Soumagnac, Irani (Swift); Western team: Cenko (US lead; Swift expert), Nugent, Neill (rapid spectroscopy), Yan (STIS ToO spectroscopy).
Progess report: This proposal follows in the steps of approved (cycle 22-23) proposals; no data obtained. We have initiated the trigger verification process numerous times (most recently for iPTF16abc, ATEL #8909; young Ia) and we have triggered once (on iPTF15ayt, flash Type II), with that trigger rejected by STScI due to scheduling conflict. We will remain cautious in using this precious resource. Our successful trigger has demonstrated in full the operational setup, including a Gemini spectrum analyzed within 2.5h from event discovery, as well as work with STScI personnel on activation timelines. We further benefit from experience from recent successful activations of HST UV spectroscopy programs targeting transients on slower time scales (e.g., by co-Is Yan and Perley).Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IINOThis is a once in a decade nearby SN.J2000STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751POS-TARGDITHER0.5LINEfalsefalse390.0STIS-ALONG-SLIT1falsePOS-TARGDITHER0.5LINEfalsefalse290.0STIS-ALONG-SLIT2falseThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.1684730774000152.3(Tic-Visit
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