0 Assigned ID: 1074 ----- Attempting Submission 1 (Fri Apr 08 23:53:19 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-1 ----- Attempting Submission 2 (Sat Apr 09 00:07:14 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-2 ----- Attempting Submission 3 (Sat Apr 09 00:24:55 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-3 ----- Attempting Submission 4 (Sat Apr 09 00:36:25 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-4 ----- Attempting Submission 5 (Sat Apr 09 01:02:56 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-5 ----- Attempting Submission 6 (Sat Apr 09 01:09:32 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-6 ----- Attempting Submission 7 (Sat Apr 09 03:59:37 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-7 ----- Attempting Submission 8 (Sat Apr 09 04:02:33 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-8 ----- Attempting Submission 9 (Sat Apr 09 04:09:57 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-9 ----- Attempting Submission 10 (Sat Apr 09 04:19:56 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-10 ----- Attempting Submission 11 (Sat Apr 09 04:32:34 GMT 2016) ----- HST Phase I Proposal 1074 (safe24.apt) successfully submitted. Receipt: # 1074-11 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 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. 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 INEFFICIENT ORDERING OF FP-POS POSITIONS 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. 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. 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. 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 INEFFICIENT ORDERING OF FP-POS POSITIONS 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. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Second submission version, assuming request to add two short G140L exposures is granted. BOT flags COS/NUV exposures as exceeding local healts based on GALEX data. The local and global health has been verified for all exposures using existing HST images with ACS/SBC and WFPC2, and the ETC. Target coordinates have been refined vz submission 1 975446958 ----- Attempting Submission 1 (Wed Jul 20 16:21:53 GMT 2016) ----- HST Phase II Proposal 14806 (saf24_p2_v2.apt) successfully submitted. Receipt: # 14806-1 ----- Attempting Submission 2 (Fri Jul 22 01:22:43 GMT 2016) ----- WARNINGS: Inefficient ordering of FP-POS positions. This I do not understand, as I always use increasing FP-POS If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE: The taget coordinates are known accurately. COS FUV PSA science exposures with extended targets have special calibration limitations.: We are aware of this, but our science will not be impacted. SAFE: Star clusters, lyman Alpha and Feedback in Eso338-04 The Lyman alpha line is a widely used probe of the distant universe. However, being a resonant line it is prone to scattering on neutral hydrogen. Hence the radiative transport through galaxies sensitively depends on the structure, kinematics and dust content of the ISM, which in turn are strongly affected by feedback from massive star formation. Imaging observations have demonstrated that Lyman alpha emission from galaxies is dominated by a large scale diffuse component. Here we propose a multi aperture COS study of, ESO338-04, the nearest and brightest Lyman alpha galaxy. From this, we will deduce the Lyman alpha profile - in which the scattering history is imprinted - and how it varies across the galaxy, and for the first time probe the dominant diffuse component. Low ionisation metallic absorption lines will be used to study the neutral ISM kinematics along several sight lines and determine the outflow geometry. We will add two STIS slits from which we will study the Lyman alpha and H-beta profile on top of the brightest clusters at superb spatial and spectral resolution. The result will be the first spatially resolved study combining neutral ISM kinematics and Lyman alpha profiles in a galaxy, from which we will build a realistic model of that accounts for the Lyman alpha emission from the entire galaxy. The data and results will have a strong legacy in the JWST and ELT era for interpreting Lyman alpha spectroscopy of high redshift sources when the UV window offered by HST has closed. the observations are split in 5 visits: 3 COS visits of duration 4 orbits each, and 2 STSI visits of duration 3 orbits each. Each visit have different ORIENT constraints, selected for optimum dispersion direction (COS) or slit angle (STIS). The brightest central cluster (a.k.a. cluster #23) is used for acquisition in all visits. For the COS visits, we obtain G130M spectra on multiple locations. For those containing bright continuum sources (bright apertures) we also obtain a short NUV image, to secure that the pointing is accurate. Each COS observation employs cenwave 1300 and 4 FP positions. The STIS visits have orient angles selected so that the STIS slit covers bright star clusters. For CCD observations with G430M we use CR-SPLIT=2 and a pattern with 2 positions along the slit to get a total of 4 exposures. For G140M we take 3 positions offset along the slit using normal pos-targ commands. For G140L we obtain a single short exposure per visit. Galaxies 12 false true false false false false SUPPORTED STELLAR CLUSTER EMISSION LINE NEBULA GLOBULAR CLUSTER NO Brightest central star cluster in ESO 388-04 = Bright Aperture (B The coordinates have been determined in an ACS/WFC/F550W image that has been matched to 2MASS and the uncertainties in position quoted above is the resulting RMS from this match, using 21 stars. We have checked these stars for proper motion and the RMS of the proper motions over the 10 year time difference between 2MASS and the ACS image is approx 0.2 arcsec, hence smaller than the position uncertainty, but making a significant contribution to the total error budget. Hence we feel confident that a ACQ/IMA is adequate. J2000 mag_1500_AB = 16.7 STELLAR CLUSTER EMISSION LINE NEBULA GLOBULAR CLUSTER NO Bright Aperture 2 = BA2 J2000 mag_1500_AB = 18.7 STELLAR CLUSTER EMISSION LINE NEBULA GLOBULAR CLUSTER NO Bright aperture 3 (BA3) J2000 mag_1500_AB = 17.8 STELLAR CLUSTER EMISSION LINE NEBULA GLOBULAR CLUSTER NO Bright aperture 4 (BA4) J2000 mag_1500_AB = 18.3 STELLAR CLUSTER EMISSION LINE NEBULA GLOBULAR CLUSTER NO Bright aperture 5 (BA5) J2000 mag_1500_AB = 18.9 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 1 (FA1) - Diffuse region J2000 mag_1500_AB = 19.8 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 2 (FA2) - Diffuse region J2000 mag_1500_AB = 19.5 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 3 (FA3) - Diffuse region J2000 mag_1500_AB = 20.4 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 4 (FA4) - Diffuse region J2000 mag_1500_AB = 18.2 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 5 (FA5) - Diffuse region J2000 mag_1500_AB = 18.2 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 6 (FA6) - Diffuse region J2000 mag_1500_AB = 19.8 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 7 (FA7) - Diffuse region J2000 mag_1500_AB = 21.1 STELLAR CLUSTER EMISSION LINE NEBULA YOUNG ASSOCIATION YES Faint Aperture 8 (FA8) - Diffuse region J2000 mag_1500_AB = 20.2 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1055 STIS/FUV-MAMA Spectroscopic No No G140M 1222 STIS/CCD Spectroscopic No No G430M 4961 POS-TARG DITHER 0.5070 LINE false false 2 90.0 STIS-ALONG-SLIT 1 false /private/var/folders/cq/d7nv4pb90n96h7hfy8bvzt2r0000gn/T/OPVisit3094037147404451355.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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It takes into account the slight extension of the source (FWHM=0.065" as measured from several passbands in WFPC2/PC images) which in effect reduces the peak pixel intensity with COS/NUV to 59% of that for a pure point source. Buffer time accounts for total flux in aperture (cluster 23 + background) Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture /private/var/folders/cq/d7nv4pb90n96h7hfy8bvzt2r0000gn/T/OPVisit2448419855066299599.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 14806 :visit-id "0C" :proposal-version -1 :trans-version "20160601" :date "22-Jul-2016 03:21:21.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 374688 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14806 :visit-id "0C" :obset-id "0C" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14806 :visit-id "0C" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2972 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14806 :visit-id "0C" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3082 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14806 :visit-id "0C" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3084 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14806 :visit-id "0C" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3082 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) true 4 0 Buffer time accounts for total flux in aperture (cluster 23 + background) Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture Buffer time accounts for total flux in aperture /private/var/folders/cq/d7nv4pb90n96h7hfy8bvzt2r0000gn/T/OPVisit3137049382068733907.xml The scheduling data was generated by CASM 24.2. 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