AstroNote 2020-74

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DRAFT
2020-04-02 01:43:12
Type: Object/s-Data/Analysis
HST Ultra-rapid Observations of SN 2020fqv
Authors: Georgios Dimitriadis, David A. Coulter, Ryan J. Foley, Charles D. Kilpatrick, Cesar Rojas-Bravo, Matthew R. Siebert (UC Santa Cruz), Susana E. Deustua, Ori D. Fox, Crystal L. Mannfolk, Armin Rest, Ryan Ridden-Harper, David R. Soderblom, Lou G. Strolger (STScI), Qinan Wang (JHU), Maria R. Drout (University of Toronto), Saurabh W. Jha (Rutgers), Daniel Kasen (UC Berkeley), Patrick L. Kelly (University of Minnesota), Anthony L. Piro (The Observatories of the Carnegie Institution for Science)
Source Group: UCSC
Abstract:
We report ultra-rapid ToO STIS and COS UV observations with the Hubble Space Telescope and Swift UV observations of the young and nearby SN 2020fqv. The first epoch of HST UV spectroscopy is scheduled to occur on 3 April 2020 starting at 05:28 UT, with a total of 5 epochs of HST spectroscopy over the span of ~3 weeks. We encourage additional and simultaneous follow-up observations at all wavelengths, especially considering the limited resources currently available.

Following the discovery (TNS Astronomical Transient Report #65714) by the ALeRCE team using public ZTF data and classification (TNS Classification Report #6435; ATel #13605) of SN 2020fqv as a young, nearby (D ~ 20 Mpc) core-collapse supernova, located in an active TESS sector and with spectroscopic indications of circumstellar interaction, we triggered ultra-rapid ToO STIS and COS UV observations with the Hubble Space Telescope under the Cycle 27 program "Ultra-Rapid UV Spectroscopy of an Interacting Supernova Discovered by TESS" (GO-15876; PI Foley). The first epoch of HST UV spectroscopy is scheduled to occur on 3 April 2020 starting at 05:28 UT. There will be a total of 5 epochs of HST spectroscopy over the span of ~3 weeks. An up-to-date schedule is available at https://www.stsci.edu/cgi-bin/get-visit-status?id=15876

We have also triggered our Swift Cycle 15 program "Young Supernova Experiment" (GI-1518200; PI Foley) to obtain high-cadence UV light curves of this SN.

We encourage additional and simultaneous follow-up observations at all wavelengths, especially considering the limited resources currently available.

We are especially thankful to the dedicated STScI staff who enabled this program and quickly scheduled the observations.  We also thank the Swift staff and PI Cenko for promptly executing our program.

Show current TNS values
CatalogNameReported RAReported DECReported Obj-TypeReported RedshiftHost NameHost RedshiftRemarksTNS RATNS DECTNS Obj-TypeTNS Redshift
TNS2020fqv12:36:33.266+11:13:54.04SN II0.007522NGC 45680.00752212:36:33.261+11:13:53.96SN IIb0.007522

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Final