Should be final version 185594302 Assigned ID: 58 ----- Attempting Submission 1 (Sun Apr 02 02:32:00 GMT 2017) ----- HST Phase I Proposal 58 (ngc6231.apt) successfully submitted. Receipt: # 58-1 ----- Attempting Submission 2 (Tue Apr 04 02:11:43 GMT 2017) ----- For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. fRemoved unnecessary SITS peak up exposures, corrected the coordinates for CPD-41 7725 and changed the target acquisition strategies for CL* NGC6231 BVF44 (target 10, visit 10) and NGC 6231 217 (target 11, visit 11) to avoid exceeding count rate maxima. Fixed Orient limits for Target 10 Updated STIS target ACQ configurations, as requested. -240380162 ----- Attempting Submission 1 (Fri Jul 14 17:23:02 GMT 2017) ----- ----- Attempting Submission 2 (Mon Jun 04 01:26:41 GMT 2018) ----- ----- Attempting Submission 3 (Tue Jun 26 18:22:41 GMT 2018) ----- ----- Attempting Submission 4 (Thu Oct 25 14:40:10 GMT 2018) ----- Forced to use only FP3 and 4 to expose both segments Can use overlap of CENWAVEs to reduce S/N for region of interest. Origin of the high velocity gas in NGC 6231 It is well known that clusters of massive stars are influenced by the presence of strong winds, that they are sources of diffuse X-rays from shocked gas, and that this gas can be vented into the surrounding region or the halo, forming a critical element in the process of galactic feedback. However, the details of how these different environments interact and evolve are far from complete. Recently, Massa (2017) showed that the peculiar C IV 1550 Ang absorption seen in several otherwise normal main sequence B stars in NGC 6231 is not intrinsic to the stars. Instead, this absorption, which extends to more than -2000 km/s, is due to intervening carbon rich, high speed gas in the cluster environment. In this proposal, we seek to identify the origin of the high speed gas. The proposed observations will enable us to determine whether it is due to the outer wind of the WC star WR79, or to a collective cluster wind, enriched by carbon from the wind of WR79. If it is due to the wind of WR79, then the new data will furnish a novel, less model dependent estimate of the mass loss rate of a WC star. If it is due to a collective wind from the cluster, then we could be witnessing an important stage of galactic feedback. In either case, the proposed observations will provide a unique and significant insight on how massive, open clusters evolve -- insight that can only be obtained through UV spectroscopy. We will use 12 orbits to observe 12 main sequence B stars (BVs) to map the flow of the high speed gas in NGC 6231. STIS must be used for 9 of the targets because they are too bright for COS. These will be observed with the STISE140M. The remaining 3 will be observed with COS. Two COS settings are needed to observe the absorption and to determine the stellar parameters. G160M CENWAVE 1589 will covers the high speed absorption we intend to model. G130M CENWAVE 1291 covers the N v and Si iv resonance lines and several Si II and III stellar lines needed to determine the physical parameters of the BVs. These stellar lines will be used to select spectra to represent the intrinsic BV spectra in the vicinity of C IV. Good S/N is needed to determine the find good stellar matches and to search for systematic deviations from the simple model of the absorption caused by the flow. Due to the turbulent nature of the flow, only modest spectral resolution (~50 km/s) is needed for the analysis. Therefore, the high resolution STIS or COS spectra can be binned for increased S/N. Stellar Physics 6 false true false false false false SUPPORTED STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. CPD-41D7725 J2000 J2000 STAR B0-B2 V-IV NO This star has a listed proper motion of (-102.2, 52.1) mas/yr, or more than 0.1 arc sec/yr. At the distance of the cluster (consistent with its spectral type and reddening), that would imply a tangential velocity of around 100,000 km/s. This has been ignored, and assumed to be the result of an erroneous measurement. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B0-B2 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B6-B9.5 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR B3-B5 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G130M 1291 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 C:\Users\derck\OneDrive\Documents\OP-cache\latest-v01.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 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ORIENT restriction imposed to avoid Cl* NGC6231 SS108 from possibly falling into the PSA during the ACQ/IMAGE 1531908524000 74.3252547404868 (Tic-Visit :proposal-id 15206 :visit-id "10" :proposal-version -1 :trans-version "20171009" :date "25-Oct-2018 10:26:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 487136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15206 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15206 :visit-id "10" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2965 :al-overhead-at-end 0 :internal-dur-at-end 388 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3298 :pcs-gap 0 ) true 1 0 C:\latex\proposals\hst\hst17\OP-cache\most_recent-v11.xml The scheduling data was generated by CASM 25.2. 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