0 Assigned ID: 111 ----- Attempting Submission 1 (Wed Apr 09 18:23:23 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 2 (Wed Apr 09 19:56:51 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 3 (Wed Apr 09 21:36:49 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 4 (Thu Apr 10 00:57:21 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 5 (Thu Apr 10 11:56:28 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 6 (Thu Apr 10 12:02:32 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 7 (Thu Apr 10 21:57:44 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 8 (Fri Apr 11 00:43:43 GMT 2014) ----- HST Phase I Proposal 111 (WN3O3.apt) successfully submitted. ----- Attempting Submission 9 (Fri Apr 11 00:46:33 GMT 2014) ----- Changed acqusitions to dispersed light to avoid safety concerns and corrected comments. -1171289394 ----- Attempting Submission 1 (Sun Jul 06 23:33:24 GMT 2014) ----- HST Phase II Proposal 13780 (WN3O3PII.apt) successfully submitted. ----- Attempting Submission 2 (Thu Jul 17 23:44:49 GMT 2014) ----- HST Phase II Proposal 13780 (WN3O3PII.apt) successfully submitted. ----- Attempting Submission 3 (Tue Oct 07 19:52:35 GMT 2014) ----- HST Phase II Proposal 13780 (WN3O3PII.apt) successfully submitted. ----- Attempting Submission 4 (Tue Oct 07 19:53:51 GMT 2014) ----- The Nature of Newly Discovered Wolf-Rayet Stars in the LMC We have recently discovered five Wolf-Rayet (WR) stars in the LMC which might be naively classified as "WN3+O3 V." However, such a pairing is unlikely for a number of reasons: (a) O3 V stars are very rare, as they are the hottest and most luminous of the dwarfs; (b) the absolute visual magnitudes of our stars are quite faint (Mv=-3) compared to even an O3 V star by itself (Mv=-5.5); (c) these stars do not exhibit radial velocity variations, although our data on this are admittedly limited; and (d) such a pairing would be hard to understand from a stellar evolution point of view, since a massive star will evolve out of the O3 V phase in about a million years, while it takes several million years to form a WN star. We are forced to conclude that we have discoverd a new class of WRs. We have excellent optical spectra with Magellan, and our modeling of these data suggest a very high effective temperature (70,000 K), strongly enhanced nitrogen, and a very low mass-loss rate. However, these physical parameters are poorly constrained by the optical data alone, and we now seek UV spectra that will contain lines that will better determine the temperatures, and the important resonance lines that provide crucial diagnostics of the stellar winds. The results of this modeling will allow us to understand the nature of these objects, and where they fit in the evolution of massive stars. If they are the products of single star evolution, they indicate we have some fundamental misconceptions. If they are the products of binary evolution, how do we explain the absence of any companions? We can only address these questions by having reliable stellar parameters and abundances. Overview: We will observe each of these three WN3/O3V stars using COS/FUV and the G140L grating in the standard two settings (G140L/1105, G140L/1280) for complete wavelength coverage in the FUV. Each star will be observed in a 2-orbit visit. Target Acquisitions: Our coordinates have been measured directly from our survey frames; all three targets are also listed in the GSC-II with coordinates that agree to <0.1". The only complication is that our targets are too bright for acquisition through the Primary Science Aperture with Mirror A. We therefore do PEAKXD and PEAKD in dispersed light. Exposure times have been estimated by (a) our preliminary CMFGEN 100K model, (b) flux distribution of an O3 V star, and (c) a 120,000 black-body, all with good agreement. HOT STARS Default false true false false false SUPPORTED EXT-STAR WOLF RAYET WOLF RAYET - WN J2000 J2000 B-V=0.03, U-B=-1.02 EXT-STAR WOLF RAYET WOLF RAYET - WN J2000 J2000 B-V=-0.25, U-B=-1.03 EXT-STAR WOLF RAYET WOLF RAYET - WN J2000 J2000 B-V=-0.16, U-B=-0.87 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1105 /Users/massey/Dropbox/cycle22/OP-cache/WN3O3PII-v01.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13780 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "07-Oct-2014 12:49:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1043840 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13780 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13780 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3280 :al-overhead-at-end 0 :internal-dur-at-end 410 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3614 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13780 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3389 :al-overhead-at-end 0 :internal-dur-at-end 404 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3614 :pcs-gap 0 ) true 2 0 Buffer-time returned is 550 sec both by using our CMFGEN model a input to the ETC (622040) and by using a 100,00 K black body with V=16.0 and E(B-V)=0.13 with LMC reddening law. 360 is roughly 2/3rds of that. We obtain a buffer-time of 712-714 sec either with a 100K black-body or with our CMFGEN model; we have taken 2/3rds of that and used 470 sec. /Users/massey/Dropbox/cycle22/OP-cache/WN3O3PII-v02.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13780 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "07-Oct-2014 12:49:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1009024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13780 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13780 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3237 :al-overhead-at-end 0 :internal-dur-at-end 401 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13780 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3349 :al-overhead-at-end 0 :internal-dur-at-end 404 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) true 2 0 Buffer-time returned is 550 sec both by using our CMFGEN model a input to the ETC (622040) and by using a 100,00 K black body with V=16.0 and E(B-V)=0.13 with LMC reddening law. 360 is roughly 2/3rds of that. We obtain a buffer-time of 712-714 sec either with a 100K black-body or with our CMFGEN model; we have taken 2/3rds and used 470 sec. /Users/massey/Dropbox/cycle22/OP-cache/WN3O3PII-v03.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13780 :visit-id "03" :proposal-version -1 :trans-version "20140605" :date "07-Oct-2014 11:57:18.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1009024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13780 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13780 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3237 :al-overhead-at-end 0 :internal-dur-at-end 401 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13780 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3349 :al-overhead-at-end 0 :internal-dur-at-end 404 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) true 2 0 ETC estimates BUFFER-TIME of 532 sec using our CMFGEN 100K model. 2/3rds of this is 350 sec. Decreased to 150sec to be conservative We obtain a buffer-time of 712-714 sec either with a 100K black-body or with our CMFGEN model; we have taken 2/3rds of that and used 470 sec.