Target REDSNIA-1: 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 REDSNIA-2: 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: 968
----- Attempting Submission 1 (Fri Mar 06 23:59:27 GMT 2020) -----
HST Phase I Proposal 968 successfully submitted.
Receipt: # 968-1ToO targets do not need to be scheduled at this point.This phase II is for a ToO program with a generic target to be replaced by the appropriate supernovae when found.
The observations are based on those successfully used for SN2017erp for program 14665.
ToO response time only included for the first visit of each of the two ToO activitations.
This phase II has the second target of the two cycle program.-453603036----- Attempting Submission 1 (Sat Jun 27 21:05:57 GMT 2020) -----
HST Phase II Proposal 16221 successfully submitted.
Receipt: # 16221-1
----- Attempting Submission 2 (Tue Jun 30 02:52:01 GMT 2020) -----
----- Attempting Submission 3 (Fri Mar 19 19:11:55 GMT 2021) -----
----- Attempting Submission 4 (Mon Mar 22 21:39:23 GMT 2021) -----
----- Attempting Submission 5 (Thu Jul 29 17:34:59 GMT 2021) -----Red or Reddened Supernovae? Understanding the Ultraviolet Differences of Normal Standard CandlesConstraining systematic uncertainties is critical to accurately and confidently use type Ia supernovae as precise cosmological distance indicators. The two dominant astrophysical systematics in optical-based studies are dust reddening and intrinsic color differences. Swift ultraviolet observations of even the most normal type Ia supernovae show a large dispersion in colors, consistent with contributions from both intrinsic differences and dust reddening. The four sets of high-quality ultraviolet spectra with the Hubble Space Telescope do not yet fully sample this distribution, but comparisons among them reveal a complexity which requires the contribution of multiple effects. We request a series of ultraviolet spectroscopy of one more type Ia supernovae. These will be chosen based on early Swift photometry to be of the undersampled red variety, allowing us to measure the wavelength dependence of the intrinsic color and/or host galaxy reddening by comparison with the existing samples. We will determine the source of the differences and constrain the effect they have on the optical measurements used in cosmological measurements. The spectra will also be a significant fraction of the local comparison sample against which we can compare the rest-frame ultraviolet spectra of higher redshift type Ia supernovae.This program will trigger on two type Ia supernovae which appear to be intrinsically red or reddened by dust based on early observations including UV data from Swift UVOT. HST will obtain multi-epoch STIS ultraviolet spectroscopy at four epochs separated by about 5 days.Dr. Peter J. Brown is an expert in the ultraviolet properties of supernovae, and has led three previous HST programs for UV spectroscopy. He is the PI of the NASA-funded Swift Optical Ultraviolet Supernova Archive and leads the Swift observations of supernovae in the UV. He is a member of the Global Supernova Project and Carnegie Supernova Project consortia which will provide complementary optical and near-infrared photometry and spectroscopy.
Peter Milne has experience working with the UVOT light curves of type Ia supernovae.He has published three studies that utilize the UVOT sample of SN~Ia photometry (Milne et al. 2010, 2013, 2015). He led the team that discovered the existence of the NUVB/NUVR bi-modality in normal SNe~Ia. He is currently preparing a paper on sub-groups within narrow-peaked SNe~Ia. He runs the Super-LOTIS telescope and is a member of the AzTEC project, and will assist with the coordination of ground-based, Swift, and HST observations.Large Scale Structure of the UniverseIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IAred supernova IaSTIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300Timing link suitability includes constraints ([06 After 05 by 4.0 to 6.0 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./private/var/folders/lm/1s7yhzbn56l3gt6dp_gzhtgc0000gn/T/OPVisit6084473296362256058.xml(Tic-Visit
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