minor fixes.751231958Assigned ID: 800
----- Attempting Submission 1 (Fri Apr 11 20:52:53 GMT 2014) -----
HST Phase I Proposal 800 (proposal_submitted.pdf.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 20:58:17 GMT 2014) -----ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONSChanged COS acquistion image exposure times to 30 sec.128038290----- Attempting Submission 1 (Tue Jul 22 06:11:47 GMT 2014) -----
----- Attempting Submission 2 (Wed Apr 22 18:41:12 GMT 2015) -----
----- Attempting Submission 3 (Thu Apr 23 01:11:33 GMT 2015) -----As to the warning about the PF-POS positions being inefficiently ordered, we there are 4 PF-POS positions to be divided over 5 orbits. I am requesting all 4 PF-POS positions for the first orbit and then one each for the following four orbits.The First UV Spectra of a Hydrogen-Rich Superluminous SupernovaThere is a rare class of supernovae with peak luminosities ten times greater than a typical Type Ia supernovae in the optical and hundreds of times greater in the UV. Some of these "superluminous" supernovae (SLSNe) show evidence for hydrogen in their spectra, and some do not. There are now spectroscopically confirmed examples of these hydrogen poor SLSN-I out to redshift 1.6, but, surprisingly, there are no confirmed examples of any hydrogen-rich SLSN-II above redshift 0.4 even through SLSN-II can have peak luminosities comparable to or greater than SLSN-I. As a result, we have no rest-frame UV spectra of SLSN-II, the spectral range most critical for understanding the nature of these events and for verifying their utility as potential probes of the high redshift universe. Here we propose to obtain the first UV spectra of a SLSN-II. These data will serve as a guide to enable higher redshift SLSN-II to be identified and they will stand as a local reference to compare against these future, high-redshift discoveries against. HST is uniquely suited to these observations, which need to take place before our window into the UV universe closes.We will obtain UV spectroscopy of one, hydrogen-rich superluminous supernova (SLSN-II). We have requested one, disruptive ToO trigger in order to rapidly (Delta t < 10 days) respond to new SLSN-II discoveries to be made during Cycle 22. We may choose targets from publicly available sources, but we expect the best SLSN-II will come from the Intermediate Palomar Transient Factory (iPTF). We will trigger our ToO observations only on spectroscopically confirmed targets, and we will first request Swift UV photometry to verify the brightness of the targets in the NUV (this data will also help streamline bright-object checking for the MAMA detectors).
We will divide our allocated orbits between COS and STIS. We propose to acquire FUV spectra with the COS G140L grating, and NUV spectra with the STIS G230L grating. The exact division will be dictated by the redshift of the target, which will not be known until just prior to activation of or disruptive ToO observation. The goal is to obtain the broadest possible coverage of the rest frame UV light with S/N > 10. For a nearby, low-redshift source, we expect to use most of our orbits for COS and the remainder for STIS. However, we could use all allocated orbits for STIS if the target is sufficiently redshifted.
We have estimated exposure times using black body fits to Swift NUV observations of two previous SLSN-II discovered by PTF. We find that a relatively bright, nearby SLSN-II could be detected at S/N > 10 over a broad range in 27000s (10 orbits assuming 45 minutes on source per orbit. Four more orbits with STIS would deliver S/N > 10 across in the NUV as well. The COS and STIS observations could be performed together or could take place within about 5 days of each other (COS first). For a more distant source we would use the full orbit allocation just for STIS as this would cover essentially the whole rest-frame UV range of interest.HOT STARS12RegularfalsetruefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVAJ2000low-redshift SLSN-IICOS/FUVSpectroscopicNoNoG140L1105STIS/NUV-MAMASpectroscopicNoNoG230L2376The scheduling data was generated by CASM 23.0.CASM was run in Phase II mode./private/var/folders/pk/hvspwx654yggwxqn0f3n4r5w0000gr/T/OPVisit4873443117691165070.xml(Tic-Visit
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