This is a disruptive ToO proposal hoping to start observing SN 2023ixf on May 281770008464Assigned ID: 3992
----- Attempting Submission 1 (Sun May 21 02:51:04 GMT 2023) -----The number of orbits used exceeds the number allocatedUpdates:
* Added visit 5 as a make up for the failed visit 4 (as approved by HOPR 92578)-1227494833----- Attempting Submission 1 (Mon May 22 09:46:27 GMT 2023) -----
----- Attempting Submission 2 (Mon May 22 18:07:58 GMT 2023) -----
HST Phase II Proposal 17313 successfully submitted.
Receipt: # 17313-2
----- Attempting Submission 3 (Mon May 22 19:11:54 GMT 2023) -----
----- Attempting Submission 4 (Wed Jul 12 22:42:54 GMT 2023) -----extra orbit approved by HOPR 92578Tracing the UV CSM interaction over the first 50 days in the extremely nearby SN 2023ixf in M101The 2023 May 19 explosion of SN~2023ixf in the nearby (~6.4 Mpc) spiral galaxy M101 has presented us with a once in an HST-lifetime chance to get a comprehensive NUV to NIR dataset of an interacting core collapse supernova. This disruptive DDT ToO will be complementary to an already approved Cycle 30 ToO proposal which has been triggered on this object, and will take over observations 10 days after explosion (ie May 29) and will persist over 5 epochs to 50 days post-explosion. With only a handful of core-collapse supernovae observed in the ultraviolet with HST, and almost all within 3 weeks of explosin, this proposal fills a crucial gap in our knowledge of the evolution of core-collapse supernovae in the ultraviolet. Only with HST can this be done, and only with a SN that is this close can we probe the UV far into time periods when the flux has normally faded significantly.This program is to obtain NUV-NIR spectra with the G230LB, G430L, and G750L gratings of SN 2023ixf, 15, 20, 30, and 50 days after explosion. These epochs correspond to Jun 2, Jun 7, Jun 17, and Jul 7, 2023. Given the current brightness we will use the 52x0.2 arcsec slit at the E1 position for G230LB and G430L and the central position for better fringing for the G750L.K. A. Bostroem extensive experience with the STIS data reduction and the reduction and analysis of core collapse supernovae observations with HST, Swift, and Gemini. Her research focuses on understanding the progenitors of hydrogen-rich CC SNe.
M. Lundquist is an active member of the DLT40 team and specializes in the reduction and analysis of Gemini and Keck. He is currently a staff astronomer at the W. M. Keck Observatory. Prior to joining the DLT40 team, he worked as a Gemini Science Fellow at the Gemini Observatories.
S. Valenti is the co-PI of DLT40. He has worked comprehensively on core collapse supernovae (CC SNe).
D. Sand is the co-PI of the DLT40 survey and an expert in the progenitors of Type Ia SNe and SN environments. He has extensive experience with Swift, and Gemini observations of SNe and their environments.
J. Andrews is an active member of the DLT40 team, has expertise observing with HST/STIS, and is an assistent astronomer the Gemini Observatory. Her research focuses on characterizing the progenitors of core collapse (CC) SNe, specifically focusing on their mass-loss history via circumstellar interaction.
G. Hosseinzadeh is an expert in early interaction in CCSNe and has experience analyzing early UV data. He leads the US team's contribution to the Global Supernova Project, which is already collecting a high candence ground based observing campaign with the Las Cumbres Observatory.
M. Shrestha is a Postdoctoral Research Associate at the University of Arizona. Her research focuses on the transients such as long gamma-ray bursts, core collapse (CC) SNe, and kilonova. She is part of DLT40 and SAGUARO collaboration.
J. Jencson is an active member of the DLT40 team and has extensive experience in reducing an analyzing Swift observations of transients. His research focuses on multi-wavelength studies of hydrogen-rich transients and searches for dust-obscured transients and faint/failed SNe.
J. Pearson is focusing her thesis research on understanding the progenitors and environments of CC SNe and is an active member of the DLT40 team.
S. Wyatt is an active member of the DLT40 team and has extensive experience in studying the diversity of SN~Ia and their progenitor systems.
Y. Dong is an active member of the DLT40 team and has experience analyzing both CC~SNe and SN~I.
N. Meza and Emily Hoang are the newest member of the DLT40 team focusing their theses work on CC~SNe.
D. A. Howell is the PI of the Global Supernova Project, which is already collecting a high candence ground based observing campaign with the Las Cumbres Observatory. He specializes in thermonuclear supernovae and fast transients
Dr. Curtis McCully is an Astrodata Scientist at Las Cumbres Observatory in charge of pipeline processing and has extensive HST data reduction experience; was part of the SN search team for the CLASH and CANDELS legacy HST programs; also lead the HST analysis on the pre-explosion images of the Type Iax SN 2012Z. He is also an expert in spectroscopic reduction techniques.
S. Gomez is a post doc at the Space Telescope Science Institute studying transients including superluminous supernovae and tidal disruption events. He
D. Hiramatsu is an expert on supernova observations and their progenitor and light-curve modeling.
A. Ravi: Aravind P. Ravi has experience working with multi-wavelength spectroscopy of core-collapse supernovae through his work on Type Ic SN 2021krf where the team identified a luminous late-time emission from a central engine and an early onset of dust formation.
A. Filippenko is an expert on core-collapse supernovae and specifically UV observations of core collapse supernovae with HST/STIS
N. Smith is an expert in interacting supernova and their progenitors.
Saurabh Jha studies supernova of all types, most recently focusing on IR observations of Type Ia and core-collapse supernovae with JWSTStellar Physics and Stellar Types0falseSUPPORTEDEXT-STARCIRCUMSTELLAR MATTERSUPERNOVASUPERNOVA TYPE IIJ2000J2000STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751Timing link suitability includes constraints ([02 After 01 by 4.0 to 6.0 days] [03 After 01 by 10.0 to 20.0 days])The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.This is the first visit in the series. Ideal execution date is Jun 2, 15 days after explosion. Supernovae evolve on the order of days in the UV at this phase.1685683109000128.36978567885762(Tic-Visit
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:date "22-May-2023 11:48:52.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17313
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:orbit-number 1
:pcs-time 393
:si-vis-utilization 2544
:al-overhead-at-end 0
:internal-dur-at-end 755
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2942
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)true10TA calculated for S/N of 40 at current brightness (STIS.ta.1857482), checked that this will not come close to saturation at max potential brightness. Expected brightness is V=10.824s per exposure is 60% satuartion of reaches maximum brightness of V=10mag, if expected V=10.8 S/N is still 211 @ central wavelength and S/N of 175 if it stays at current V=11.224s per exposure is 60% satuartion of reaches maximum brightness of V=10mag, if expected V=10.8 S/N is still 120 @ central wavelength and S/N of 100 if it stays at current V=11.2Timing link suitability includes constraints ([02 After 01 by 4.0 to 6.0 days])The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.This is the second visit in the series. It should execute on Jun 7, 20 days after explosion. Supernovae evolve on the order of days in the UV at this phase. Expected brightness is V=11.2, maximum brightness V=101686156297000127.80000000000001(Tic-Visit
:proposal-id 17313
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:proposal-version -1
:trans-version "20220630"
:date "22-May-2023 12:10:45.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17313
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:orbit-number 1
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:dark-offset NIL
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:low-sky "N"
:pcs-visibility 2942
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)true10TA calculated for S/N of 60 at current brightness V=11.2Estimated brightness at this epoch is V=11.2; S/N~100 per exposureEstimated brightness at this epoch is V=11.2; S/N~66Timing link suitability includes constraints ([03 After 01 by 10.0 to 20.0 days])The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.This is the third visit in the series. It should execute on Jun 17, 30 days after explosion. Supernovae evolve on the order of days in the UV at this phase. Expected brightness is V=12.3, maximum brightness V=10. Brightness at this phase is very uncertain - we will monitor and update exposure times as nessesary1686567695000128.3697704961196(Tic-Visit
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:trans-version "20220630"
:date "22-May-2023 12:07:36.0"
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:number-of-orbits 1
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:data-volume 239664
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17313
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:orbit-number 1
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:dark-offset NIL
:dark-utilization 0
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:low-sky "N"
:pcs-visibility 2942
:pcs-gap 0
)true10TA calculated for S/N of 40 at brightness V=12.3Estimated brightness at this epoch is V=12.3; S/N~10 per exposureEstimated brightness at this epoch is V=12.3; S/N~65 per exposureEstimated brightness at this epoch is V=12.3; S/N~45The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.This is the fourth visit in the series. It should execute on Jul 7, 50 days after explosion. Supernovae evolve on the order of days in the UV at this phase. Expected brightness is V=12.3, maximum brightness V=10. Brightness at this phase is very uncertain - we will monitor and update exposure times as nessesary1688741892000114.88813855861753(Tic-Visit
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:date "22-May-2023 12:02:22.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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(Tic-Orbit
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:dark-offset NIL
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)true10TA calculated for S/N of 40 at brightness V=12.3Estimated brightness at this epoch is V=12.3; S/N~10 per exposureEstimated brightness at this epoch is V=12.3; S/N~65 per exposureEstimated brightness at this epoch is V=12.3; S/N~45The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode./private/var/folders/6l/54htg8p52b762n_6mhsb13v80000gn/T/OPVisit16266474157775816571.xmlThis is a repeat of Visit 4 due to GS failure. It should be executed as soon as possible as this is a time varying source and the UV is fading with time(Tic-Visit
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:trans-version "20230418"
:date "12-Jul-2023 15:33:43.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 239664
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
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(Tic-Orbit
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:orbit-number 1
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:si-vis-utilization 2548
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:internal-dur-at-end 755
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2942
:pcs-gap 0
)true10TA calculated for S/N of 40 at brightness V=12.3Estimated brightness at this epoch is V=12.3; S/N~10 per exposureEstimated brightness at this epoch is V=12.3; S/N~65 per exposureEstimated brightness at this epoch is V=12.3; S/N~45