The Lyman-alpha emission line is the pivotal spectral feature in both the identification of high-redshift galaxies and the confirmation of candidates. In this respect Ly-alpha promises to realize many of the fundamental goals of galaxy evolution astrophysical cosmology. Unfortunately the line is a resonance one, and suffers a radiation transport that is intricate and complicated -- despite thousands of high-z galaxies having been found through Ly-alpha, it is still not known which physical properties of galaxies fundamentally determine the line visibility and how they intertwine. Galaxies at high-z are typically too faint to study at the necessary levels of detail, and spectral features for benchmark and calibration are redshifted to wavelengths where they are undetectable. To resolve these issues we began a Ly-alpha imaging program, targeting 14 nearby galaxies in HST cycle 18: LARS -- the Lyman-alpha Reference Sample. LARS will consist of a public access data release and will address many aspects of Ly-alpha transport, such as dust-content and characteristics of the stellar population. Without ultraviolet spectroscopy, however, the LARS data-set will have no measurements of the neutral gas kinematics - something that is qualitatively known to be of great significance to Ly-alpha escape. Quantitatively, however, the case is far from resolved. We will finally obtain this information by completing our HST data-set with far-ultraviolet spectroscopy from the Cosmic Origins Spectrograph. With 49 primary orbits dedicated to LARS, and further reliance on 31 orbits of archival data, the award of just 7 more orbits in cycle 19 will allow us to resolve this point. This program will obtain far ultraviolet spectra of 7 starburst galaxies in the nearby Universe with COS. There are two primary goals: 1. to obtain absorption spectra around the low ionization stage metal lines that form in the neutral ISM: SiII 1260 AA; OI 1302; SiII 1304; CII 1334. 2. to obtain emission/absorption spectra of the HI Lyman-alpha at 1216 AA. We were awarded 7 orbits. 1 orbit for each target. We will use the same grating for every galaxy: G130M, although various CENWAVE/FP-POS combinations are adopted. The coordinates given are based upon WFC3/UVIS/F336W imaging, which has been astrometrically corrected against 2MASS, giving an estimated maximum r.m.s. error on our requested pointing of 0.25 arcsec. In one case WFC3 imaging has not yet been obtained, although is scheduled in cycle 18 -- this galaxy is rather compact and we currently enter the 2MASS coordinates for the acquisition. We may tweak this when the WFC3 imaging has been obtained. With these accuracies we rely upon NUV target acquisition with ACQ/IMAGE. Being selected from GALEX catalogs, we have 1500 and 2200 AA magnitudes for all targets. The objects are unresolved by GALEX, and assumed to be stars, but all galaxies are well-resolved in the UV by HST. They all consist of multiple star-forming condensations, knots, etc. Thus the warning offered by the GALEX mode of the Bright Object Tool are extremely conservative and not applicable to our galaxies. The individual knots are, however, spatially compact, sufficiently so for ACQ/IMAGE without much loss of time spectroscopy. Notes on photometry and ETC runs: The definition of conservative means fainter than expected for target acquisition but brighter than expected for bright object safety. For bright object safety we do aperture photometry in 0.5 arcsec (radius) annuli, centring is on, and background subtration is off -- given the resolved nature of our targets, this is double conservative. For target acquisition our photometry is done in 0.25 arcsec (radius) annuli. For all ETC runs in spectrscopic mode, we assume exposure times of 800 s; fluxes are either measured in ACS/SBC/F140LP or extrapolated from WFC3/UVIS/F336W using the beta slope measured by GALEX. The shortest FUV spectroscopic buffer time is over 5000 seconds. We therefore set the buffer time to the exposure time in every case. In 6 of the 7 cases we have orient constraints that are designed to place multiple star forming knots along the dispersion axis. ISM IN EXTERNAL GALAXIES 12 false false 0.0 0.0 false false false SUPPORTED GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(3354)=8.8379e-17 ; beta=-1.18 ; F-CONT(2338)=1.3534e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(3354)=1.7692e-16 ; beta=-0.61 ; F-CONT(2338)=2.2052e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(1528)=5.3137e-16 ; beta=-1.12 ; F-CONT(2338)=3.3000e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(1528)=2.3066e-15 ; beta=-2.13 ; F-CONT(2338)=9.3222e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(1528)=2.6253e-16 ; beta=-0.67 ; F-CONT(2338)=1.9743e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(3354)=5.3254e-16 ; beta=-1.32 ; F-CONT(2338)=8.5778e-16 GALAXY STAR FORMING REGION STARBURST J2000 J2000 F-CONT(1528)=2.7748e-16 ; beta=-1.05 ; F-CONT(2338)=1.7753e-16 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1300 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). 1347563498000 321.29490872832866 (Tic-Visit :proposal-id 12583 :visit-id "02" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:07:12.0" :trans-errors '(:WARNINGS 1 :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3092 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3430 :pcs-gap 0 ) true 1 1 Acquisition time estimates based upon point source in WFC3/UVIS/F336W imaging and UV continuum slope measured by GALEX (FUV/NUV). Could be updated as ACS/SBC imaging arrive, allowing us to interpolated to the COS/NUV channel directly. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. No orient ranges are defined. Given the complex morphology we may as well leave it to chance. According the beta slope measured by GALEX, this galaxy has the reddest UV continuum in the sample. Combined with the relative faintness of the point-sources in F336W, the FUV continuum of this object is the most likely to be weak. The object is located at +62 degrees, and since it has no orient requirement, CVZ visits can easily be scheuled -- 3 to 7 day windows are available every month in cycle 19. As stated in our Phase I proposal, we request the CVZ for this visit. 1341871483000 100.4279882854546 (Tic-Visit :proposal-id 12583 :visit-id "03" :proposal-version -1 :trans-version "20120125" :date "07-Mar-2012 15:21:19.0" :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 330560 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 12583 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 4963 :al-overhead-at-end 0 :internal-dur-at-end 426 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 1 0 Acquisition time estimates based upon point source in WFC3/UVIS/F336W imaging and UV continuum slope measured by GALEX (FUV/NUV). Could be updated as ACS/SBC imaging arrive, allowing us to interpolated to the COS/NUV channel directly. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). 1356992023000 295.0 (Tic-Visit :proposal-id 12583 :visit-id "04" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:07:13.0" :trans-errors '(:WARNINGS 1 :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3092 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3430 :pcs-gap 0 ) true 1 1 Acquisition time estimates based upon point source in both ACS/SBC/F140LP and WFC3/UVIS/F336W imaging. Flux is logarithmically interpolated to 2330 AA. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). 1333354041000 194.68908895329514 (Tic-Visit :proposal-id 12583 :visit-id "05" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:07:15.0" :trans-errors '(:WARNINGS 1 :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3131 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) true 1 1 Acquisition time estimates based upon point source in ACS/SBC/F140LP imaging and UV continuum slope measured by GALEX (FUV/NUV). Could be updated as WFC3/UVIS/F336W imaging arrive, allowing us to interpolated to the COS/NUV channel directly. We have adopted mirror B for the acquisition because photometry in larger apertures gives warnings with mirror A. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). 1335454369000 113.31434615500802 (Tic-Visit :proposal-id 12583 :visit-id "08" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:07:16.0" :trans-errors '(:WARNINGS 1 :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "08" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2890 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3233 :pcs-gap 0 ) true 1 1 Acquisition time estimates based upon point source in both ACS/SBC/F140LP and WFC3/UVIS/F336W imaging. Flux is logarithmically interpolated to 2330 AA. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). (Tic-Visit :proposal-id 12583 :visit-id "09" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:01:36.0" :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "09" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2877 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) true 1 0 Acquisition time estimates based upon point source in WFC3/UVIS/F336W imaging and UV continuum slope measured by GALEX (FUV/NUV). Could be updated as ACS/SBC imaging arrive, allowing us to interpolated to the COS/NUV channel directly. We have adopted mirror B for the acquisition because photometry in larger apertures gives warnings with mirror A. The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Orientation angles are computed so as to arrange multiple point-like sources along the spatial axis. 2 ranges are defined, separated by 180 degrees, which are computed as the position angle of the desired spatial axis (E of N) + 135 degrees (PII manual section 7.2.2 and table 7.4). (Tic-Visit :proposal-id 12583 :visit-id "11" :proposal-version -1 :trans-version "20121031" :date "26-Feb-2013 10:08:52.0" :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 252288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12583 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12583 :visit-id "11" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2887 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3233 :pcs-gap 0 ) false 1 0 Acquisition time estimates based upon point source in both ACS/SBC/F140LP and WFC3/UVIS/F336W imaging. Flux is logarithmically interpolated to 2330 AA.