Thermal Equilibration and Cosmic-Ray Acceleration in Astrophysical Shocks: UV Spectra of the SN1006 Remnant

0 Assigned ID: 311 ----- Attempting Submission 1 (Fri Apr 10 00:11:13 GMT 2015) ----- HST Phase I Proposal 311 (sn1006.apt) successfully submitted. Receipt: # 311-1 ----- Attempting Submission 2 (Fri Apr 10 20:31:42 GMT 2015) ----- HST Phase I Proposal 311 (sn1006.apt) successfully submitted. Receipt: # 311-2 ----- Attempting Submission 3 (Fri Apr 10 21:50:01 GMT 2015) ----- HST Phase I Proposal 311 (sn1006.apt) successfully submitted. Receipt: # 311-3 The number of orbits used exceeds the number allocated A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Hi Paule, I think I have correctly changed ACCUM to TIME-TAG and put in a buffer time of 10,000 sec for lack of a better number, and I have added the ETC number COS.sp.759821. Please let me know if this looks OK. 6/28/16 - PC added alternate visits and target to potentially observe new position with improved proper motion 112330549 ----- Attempting Submission 1 (Thu Jul 16 20:33:46 GMT 2015) ----- HST Phase II Proposal 14228 (sn1006.apt) successfully submitted. Receipt: # 14228-1 ----- Attempting Submission 2 (Wed Dec 30 20:49:08 GMT 2015) ----- ----- Attempting Submission 3 (Tue Jun 28 20:53:35 GMT 2016) ----- Submission failed due to error communicating with the submission server. Please retry in a few minutes. If this error persists please contact the help desk at help@stsci.edu ----- Attempting Submission 4 (Tue Jun 28 20:54:57 GMT 2016) ----- I am ingoring the warning about inefficient order of FP positions because I was told to do so last time around, because it seems impossible to avoid if the last orbit of each visit is to have a different FP position, and because the overhead is trivial. I am ignoring the warning about extended object calibration because the intensities are not really important for this project and because we calibrated the instrumental line profile for an extended object in the COS PSA in our previous work on the Cygnus Loop (Raymond et al. 2015). I am ignoring the warnings about target acquisition because the object is faint and extended, so it would not be possible to peak up the counts. Thermal Equilibration and Cosmic-Ray Acceleration in Astrophysical Shocks: UV Spectra of the SN1006 Remnant Two outstanding questions about the physics of interstellar shock waves are 1) the degree of thermal equilibration among electrons and different ions and 2) efficiency of transfer of energy from the thermal plasma to energetic particles---cosmic rays. Those questions are closely related in that both processes depend upon plasma turbulence in the shock. The degree of thermal equilibration is also important for diagnostics of shock speed based on measured electron or proton temperatures. We propose to observe a fast shock in SN1006 to measure the kinetic temperatures of He, C and N from the widths of the He II, C IV and N V line profiles. It is known from HUT and FUSE observations that the plasma behind a 2300 km/s shocks in SN1006 is far from equilibrium, with He, C and O temperatures roughly mass-proportional (4, 12 and 16 times the proton temperature, respectively), rather than approximately equal to the proton temperature as full equilibration would dictate. By contrast, the He and C temperatures ARE close to equilibrium with the protons in a 350 km/s shock in the Cygnus Loop. However, the existing measurements for SN1006 are quite uncertain, and only one other measurement of ion temperatures in a fast collisionless shock exists. The proposed observation will tighten the constraints on thermal equilibration by factors of 4 to 6. SN1006 is the only Galactic SNR with fast shocks and low enough reddening to be observable in the UV, and we have identified a filament twice as bright and 25% faster than the region studied previously. Thus spectroscopy with COS provides a unique opportunity to attack this problem. We wish to obtain a COS spectrum with the G140L grating (1105 center) of a fast shock wave in the supernova remnant SN1006. We will spend the full 15 orbit allocation on this one position because it is very faint. The objective is to measure the widths of the He II, C IV and N V lines to determine the kinetic temperatures of those ions. ISM AND CIRCUMSTELLAR MATTER 12 false true false false false false SUPPORTED ISM EMISSION LINE NEBULA SHOCK FRONT SNR YES The position and proper motion are based on an H alpha image obtiained at Gemini in April 2015. That image has better seeing that the ones we used before, and we used it to refine the position and proper motion. We also estimate that the He II and C IV emission peak about 0.56" behind (SE from) the H alpha filament, and we itake that into account in the target position given. Because the target is faint and extended, it will not be possible to peak up the couunts diring acquisition. As noted in the Phase I proposal, there is an 8th magnitude star, HD132689, about 60" SW of the target position. Because it is a cool giant, it should be faint in the UV, but it might affect the planning for the acquistion. I am ignoring the warnings about inefficient ordering of FP positions because last time around I was told to do so. I am ignoring the warnings about target acquisition because this is an extended target that is to faint to show up as a significant increase in the count rate. J2000 J2000 5.3e-15 erg/(cm2 s arcsec2) in C IV 1550 A line ISM EMISSION LINE NEBULA SHOCK FRONT SNR YES The position and proper motion are based on an H alpha image obtiained at Gemini in April 2015. That image has better seeing that the ones we used before, and we used it to refine the position and proper motion. We also estimate that the He II and C IV emission peak about 0.56" behind (SE from) the H alpha filament, and we itake that into account in the target position given. Because the target is faint and extended, it will not be possible to peak up the couunts diring acquisition. As noted in the Phase I proposal, there is an 8th magnitude star, HD132689, about 60" SW of the target position. Because it is a cool giant, it should be faint in the UV, but it might affect the planning for the acquistion. I am ignoring the warnings about inefficient ordering of FP positions because last time around I was told to do so. I am ignoring the warnings about target acquisition because this is an extended target that is to faint to show up as a significant increase in the count rate. J2000 J2000 5.3e-15 erg/(cm2 s arcsec2) in C IV 1550 A line COS/FUV Spectroscopic No No G140L 1105 1467147118381 /Users/royle/Documents/Cycle 23/OP-cache/14228-v01.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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