Theoretical models of galaxy formation predict that feedback from supernovae plays a crucial role in regulating star formation in low-mass galaxies. Efficient feedback, with large outflow rates, is needed in these models to account for the low-efficiency of galaxy formation in low-mass halos. Current constraints on mass outflow rates in this low mass regime are very sparse and the best estimates are uncertain by orders of magnitude. In order to test feedback models, we selected a unique sample of z=1 star-forming galaxies, near background quasars, that show direct evidence of strong outflows: they show large velocities (200-500 km/s) from the low-ionization absorption lines. The advantage in using background quasars over traditional galaxy spectra is that the kinematics and location of the cool gas can be determined accurately. The one missing ingredient in order to determine accurate mass outflow rates is the total gas column density. Therefore, we propose to measure the total gas column density and empirically determine the ouflow rates in low-mass (sub-L*) star-forming galaxies using COS/G230L given the redshift of our sources. With these data we will answer the fundamental question: Are the mass outflow rates higher than the star-formation rates as predicted by theory? Our sample is unique: for each quasar-galaxy pair, 
we have deep IFU kinematics of the galaxy and the line-of-sight kinematics with high-resolution
 optical spectroscopy. Our results will be a huge step forward and provide a strong bench mark for models. In order to determine accurate mass outflow rates in star-forming galaxies, we need to measure the total gas column density for the outflowing gas probed by the background quasars. Given the redshift of our sources, we must use NUV spectroscopy with COS/G230L. The low resolution grating is sufficient as we expect absorptions of a few AA, i.e. not mAA. Our pilot study is made of the best 3 sources from our sample. Hence, the scope of this project is very focused. For J0302, we aim to detect and measure the HI absorption line at 2215AA. For J1422, we aim to detect and measure the HI absorption line at 2331AA. For J0147, we aim to detect and measure the HI absorption line at 2480AA. NA Standard. COSMOLOGY 12 false 0.0 0.0 false false false false SUPPORTED EXT-MEDIUM ABSORPTION LINE SYSTEM ABSORPTION LINE SYSTEM - EXTRAGALACTIC WIND J2000 J2000 NUV=18.5 EXT-MEDIUM ABSORPTION LINE SYSTEM ABSORPTION LINE SYSTEM - EXTRAGALACTIC J2000 J2000 NUV=19.9 EXT-MEDIUM ABSORPTION LINE SYSTEM ABSORPTION LINE SYSTEM - EXTRAGALACTIC J2000 J2000 NUV=20.5 COS/NUV Spectroscopic No No G230L 3360 COS/NUV Spectroscopic No No G230L 3360 STIS/NUV-MAMA Spectroscopic No No G230L 2376 The scheduling data was generated by CASM 19.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 12522 :visit-id "01" :proposal-version -1 :trans-version "20110509" :date "31-Aug-2011 13:49:25.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "32" :si-bright-earth-limb-angle 20.0 :data-volume 208864 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12522 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12522 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2911 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) true 1 0 we are looking at HI absorption line at 2215 we are looking at HI absorption line at 2215 The scheduling data was generated by CASM 19.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 12522 :visit-id "02" :proposal-version -1 :trans-version "20110509" :date "31-Aug-2011 13:49:28.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "32" :si-bright-earth-limb-angle 20.0 :data-volume 487184 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12522 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12522 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2900 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3234 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3012 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3234 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3012 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3234 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3012 :al-overhead-at-end 0 :internal-dur-at-end 390 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3234 :pcs-gap 0 ) false 4 0 we are looking at HI absorption line at 2321 The scheduling data was generated by CASM 19.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 12522 :visit-id "03" :proposal-version -1 :trans-version "20110509" :date "31-Aug-2011 13:49:40.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 3079408 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12522 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12522 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2912 :al-overhead-at-end 0 :internal-dur-at-end 180 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 324 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 324 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 324 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12522 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 586 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) true 5 0 target has r=18mag we are looking at HI absorption line at 2480 we are looking at HI absorption line at 2480 we are looking at HI absorption line at 2480 we are looking at HI absorption line at 2480 we are looking at HI absorption line at 2480