Target SUPERNOVA1: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA2: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA3: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA4: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA5: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA6: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Target SUPERNOVA7: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.0Assigned ID: 5702
----- Attempting Submission 1 (Tue Mar 26 21:53:17 GMT 2024) -----Generic targets for Flex Thursday programThis target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDSNew flexible thursday target submission (10/06/2025)
Target check for ToO-5 on ZTF25ABVBCZT.-625125759----- Attempting Submission 1 (Thu Aug 15 16:55:38 GMT 2024) -----
----- Attempting Submission 2 (Sat Jan 25 16:41:48 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-2
----- Attempting Submission 3 (Mon Jan 27 20:33:28 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-3
----- Attempting Submission 4 (Mon Feb 10 15:39:36 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-4
----- Attempting Submission 5 (Mon Feb 10 23:40:01 GMT 2025) -----
----- Attempting Submission 6 (Tue Feb 11 05:25:38 GMT 2025) -----
----- Attempting Submission 7 (Mon May 05 22:34:10 GMT 2025) -----
----- Attempting Submission 8 (Mon Jun 16 18:28:16 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-8
----- Attempting Submission 9 (Mon Jun 16 20:36:52 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-9
----- Attempting Submission 10 (Tue Jul 29 04:38:01 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-10
----- Attempting Submission 11 (Tue Jul 29 15:36:25 GMT 2025) -----
----- Attempting Submission 12 (Mon Sep 08 19:41:18 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-12
----- Attempting Submission 13 (Tue Sep 09 14:47:31 GMT 2025) -----
----- Attempting Submission 14 (Mon Oct 06 19:09:15 GMT 2025) -----
HST Phase II Proposal 17807 successfully submitted.
Receipt: # 17807-14
----- Attempting Submission 15 (Mon Oct 06 19:15:48 GMT 2025) -----RoundingFlash Thursday: Early-time UV Spectroscopy of Type II Supernovae with HSTUltraviolet (UV) spectroscopy of type II supernovae (SNe II) in the first week post-explosion remains a largely uncharted observational phase space. Following red supergiant shock breakout, early-time UV emission harbors unique information on the structure and composition of the most local progenitor environment; this being detectable through narrow emission lines (aka. IIn-like or "flash features") that arise from shock ionization of local circumstellar material (CSM). Furthermore, UV spectroscopy of young core-collapse SNe encapsulates the interplay of density, ionization, and temperature within the outermost layers of SN ejecta. Here we propose UV/optical spectral observations with the HST STIS CCD through the Flex Thursday ToO program to obtain up to 7 spectra of SNe II in the first week after explosion. This program will increase the number of SNe II with early UV spectroscopy by more than a factor of 2, enabling precise constraints to be placed on the diversity of red supergiant atmospheres and SN II ejecta structure through the use of radiation hydrodynamics and nLTE radiative transfer codes (e.g., HERACLES, CMFGEN). Furthermore, this program will be essential preparation for the planned launch of the Ultraviolet Explorer (UVEX) telescope and its study of SNe II through UV spectroscopy.ToO program through flex thursdayPI Wynn Jacobson-Galan has led a successful Flexible Thursday program during Cycle 31 and has extensive experience analyzing and reducing HST data. Mr. Jacobson-Galan is a graduate student with burgeoning expertise on the late-time light curves of supernovae observed with HST (2 published papers) and "flash spectroscopy" supernovae (4 published papers). Co-PI K. Das is a graduate student at Caltech supervised by professor M. Kasliwal (Co-PI of ZTF and lead of the ZTF EMGW group) and staff astronomer Dr. C. Fremling (PI of the ZTF Bright Transient Survey). His thesis focuses on the study of core collapse supernovae on the low mass end. He has institutional access to both the Palomar and Keck observatories, in order to obtain complimentary ground-based spectroscopy to the UV observations proposed here. Prof. Raffaella Margutti is a leading expert on x-ray and radio observations of interacting supernovae. Dr. Luc Dessart is one of the world's leading experts on radiative transfer codes (CMFGEN) and hydrodynamics simulations (HERACLES). Drs. Armin Rest, Charles Kilpatrick, Ori Fox, and Matthew Siebert have significant experience in reduction and analysis of HST/WFC3, ACS, and WFPC2 imaging data, including the prime instruments used in these proposed observations. Profs. Mansi Kasliwal, Adam Miller, Jesper Sollerman, Ryan Foley and Ryan Chornock are an expert in transient surveys and follow up of all types of explosive transients. Mr. Qinan Wang and Kyle Davis will assist with data reduction and analysis of all targets obtained through these programs. Co-I Dr. Miller has previously led the physics of SNe Ia subgroup within ZTF and is an expert in the study of the early evolution of SNe Ia. He has experience working with STIS data and will lead and assist in the interpretation of UV spectra of SNe Ia. Co-I Dr. D. Rubin has completed several cosmology analyses using SNe Ia including analysis of rest-frame UV SN spectra. He also has experience with STIS UV spectroscopy. Co-I Dr. A. Fruchter has substantial experience using HST to study explosive transients, in particular supernovae and gamma-ray bursts, and is a long-term member of the scientific staff of STScI. Co-I Prof. A. Gal-Yam has direct experience with directing search efforts for young SNe, and performing rapid HST UV observations (through disruptive ToOs). He is a leading expert on young SN physics, including being the pioneer of ground-based 'flash' spectroscopy. Co-I E. Zimmerman is part of A. Gal-Yam's team, and has experience with HST and Swift UV observations (imaging and spectroscopy) and the overall analysis of young core-collapse SNe.
Our team has proprietary access to ZTF, a fast-cadence wide-area optical survey that is very well-suited to finding very young SNe. We have more than a decade of accumulated experience in identifying and following up very young SNe from both ground-based facilities and space-based ones (HST, Swift). We have access to a variety of robotic follow-up resources to help rapidly confirm the nature of any candidate transients, including the Palomar 60-inch telescope and the Liverpool Telescope; plus target-of-opportunity programs on classical facilities such as Palomar and Keck.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalseSUPPORTEDSTARSUPERNOVA TYPE IIJ2000EXT-STARSUPERNOVAJ2000EXT-STARSUPERNOVAJ2000EXT-STARSUPERNOVAJ2000EXT-STARSUPERNOVAJ2000EXT-STARSUPERNOVAToOToOToOToOToOToOToOSTIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1746785707000267.7328749218863(Tic-Visit
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