0
Assigned ID: 558
----- Attempting Submission 1 (Fri Apr 05 17:23:56 GMT 2019) -----
HST Phase I Proposal 558 (tess.apt) successfully submitted.
Receipt: # 558-1
----- Attempting Submission 2 (Fri Apr 05 22:49:27 GMT 2019) -----
This target is not used in this proposal.
-Re-submission. The number of total orbits in this submission matches the request in Phase I.
-We will continue working with STScI staff to optimize the triggering strategy.
-Updated with ETC IDs for STIS/NUV-MAMA and COS/FUV.
-Removed timing constraints, added them as comments in each visit section
-Added COS ACQ PEAKXD step before PEAKD for visits 4 and 5, using same instrument parameters as PEAKD
-Rerun Orbit/Visit planners and Target Confirmation tool
-Added New Obset for the first exposure to each orbit, for the first 3 STIS visits (Visits 01, 02 and 03)
-Added Visits 14 and 15, set them to "on hold". These are equivalent to Visits 04 and 05, but using image acquisition for the COS exposures
-Added Qinan Wang and Ryan Ridden-Harper as Phase II contacts
-Rerun Orbit/Visit planners
-Added/updated ETC runs for various exposures
-Re-adjusted buffer times
-Re-adjusted acquisition exposure times
-Rerun Orbit/Visit planners
-Added possible target: SN 2020fqv
-New exp time for COS dispersed-light ACQ : 32 sec
-Updated parameters for visits 04, 05
-New visit 25, replacement for failed visit 05
-1126387592
----- Attempting Submission 1 (Fri Jul 19 20:31:08 GMT 2019) -----
----- Attempting Submission 2 (Tue Jul 23 15:30:08 GMT 2019) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 3 (Wed Mar 11 02:44:05 GMT 2020) -----
----- Attempting Submission 4 (Thu Mar 12 16:29:55 GMT 2020) -----
HST Phase II Proposal 15876 successfully submitted.
Receipt: # 15876-4
----- Attempting Submission 5 (Thu Mar 12 17:56:37 GMT 2020) -----
----- Attempting Submission 6 (Sat Mar 14 00:15:17 GMT 2020) -----
----- Attempting Submission 7 (Sat Mar 28 21:13:35 GMT 2020) -----
----- Attempting Submission 8 (Wed Apr 01 18:45:04 GMT 2020) -----
----- Attempting Submission 9 (Wed Apr 01 20:20:31 GMT 2020) -----
----- Attempting Submission 10 (Tue Apr 14 19:28:04 GMT 2020) -----
We will update after discussions with STScI staff.
Ultra-Rapid UV Spectroscopy of an Interacting Supernova Discovered by TESS
The supernova (SN) community has a spectacular opportunity. Through July 2020, TESS will observe a large fraction of the sky with a 30-min cadence. In Cycle 27, TESS will detect ~60 (or more) SNe within hours - perhaps even minutes - of explosion. Such data have proven to be a unique window to the details of the SN explosion, progenitor, and circumstellar (CS) environment. We are devoting significant ground-based resources to search for and follow these SNe.
We propose to take advantage of these emergent SNe and exquisite TESS light curves to study 1 SN in detail with HST. For the first few days after a SN explosion, one can potentially see signs of the SN interacting with its CS environment (e.g., a wind, accretion disk, companion star) that are not present later in its evolution. For instance, the large UV flux from a SN shock breakout will ionize CS gas. As the gas recombines over the following days, it produces excess broad-band flux and reveals the CSM (and thus progenitor) composition through emission lines. While early optical data can be illuminating, its utility is limited. However, UV spectra can greatly enhance our understanding of SN progenitor systems, including progenitor composition, CS environment, and the existence of a binary companion. Our program will observe a single TESS SN that shows signs of early interaction.
Because of the ephemeral nature of the interaction signatures, this program requires an ultra-rapid ToO. The combination of TESS photometry, ground-based data, and HST UV spectra will be a completely unique and defining data set. As the TESS prime mission ends during Cycle 27, this may be our only opportunity for such a program.
This is an ultra-rapid ToO. We will observe a TESS supernova that shows indications of interaction. Our first epoch should be scheduled as quickly as possible. The second and third epochs will be spaced by ~1 day. Our 4th epoch should be scheduled as quickly as possible to use COS and the STIS MAMA. The final epoch should be obtained ~1 week after the 4th visit.
PI Foley and his team are supernova experts, having led over a dozen supernova-related HST programs. PI Foley has published 58 journal articles using HST data with 10 focusing on UV spectra of supernovae. CoIs Dimitriadis, Drout, Fox, Jha, Kelly, Kilpatrick, and Rest are PhD astronomers and skilled supernova observers. CoIs Kasen and Piro are supernova theorists who will assist in interpretting the data. CoI Dimitriadis led a paper analyzing the K2 light curve of SN 2018oh, which showed signs of interaction. CoI Rest is leading an effort to (1) search for SNe in TESS sectors, (2) produce accurate TESS light curves for these objects, and (3) independently find SNe in TESS data alone. Our team is using Pan-STARRS, ATLAS, Swope, Nickel, RATIR, du Pont, Shane, APO, SOAR, Magellan, Gemini, and Keck to observe these events (in addition to using public data). CoIs Coulter, Rojas-Bravo, and Siebert are graduate students working with Foley. CoI Ridden-Harper is a PhD student who will start a postdoc with Rest in the Fall. CoI Wang is a graduate student working with Rest.
Stellar Physics
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SUPPORTED
STAR
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J2000
STAR
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TESSSN
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G230LB
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G430L
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G230LB
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G130M
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G160M
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G230L
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G130M
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G160M
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Spectroscopic
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G230L
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
true
4
0