A New Dual Perspective of Mutli-phase Galaxy Outflows

0 Assigned ID: 330 ----- Attempting Submission 1 (Fri Apr 10 02:05:29 GMT 2015) ----- HST Phase I Proposal 330 (hstGo2015.apt) successfully submitted. Receipt: # 330-1 If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE 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. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE 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. We have (1) modified the TA time for Visits 2 and 3 to 540s (2) modified the 1st orbits on-target times of Visits 2 and 3 to 1526s (3) removed the holds on Visits 2 and 3 -2090776228 ----- Attempting Submission 1 (Thu Jul 23 23:27:32 GMT 2015) ----- ----- Attempting Submission 2 (Wed Jul 20 20:12:56 GMT 2016) ----- The warning are on of three types: coordinates, extended object, and use of FP POS. We have reviewed these and taken them into to account to the best of our ability. A New Dual Perspective of Mutli-phase Galaxy Outflows We propose the first multi-phase outflow study of the only system where both a galaxy (z=0.2) exhibits metal-line absorption back-illuminated by itself (down-the-barrel) AND transversely by a background quasar. The quasar sight-line is at a projected distance of 58 kpc along the galaxy minor axis; ideal orientation for outflows. We have already analyzed the outflow in the cool gas phase, traced by MgII absorption, in Kacprzak et al. (2014, ApJL,792,L12). Here we request 15 orbits to obtain COS/G130M spectra of BOTH the quasar and the galaxy to study the multi-phase outflows from two perspectives: down-the-barrel of the galaxy and at 58 kpc away probed by the quasar sight-line. We will probe the physics and kinematics of HI (full Lyman series), OVI, FeII, CIII, CII, NIII, and NII absorption from the galaxy and the quasar sight-lines. We will use our established models to further interpret the observed transverse gas-galaxy kinematics, spatial relationships, and ionization conditions, metallicities, outflow mass rates, loading factors and masses. Our proposed observations will provide the first dual multi-phase outflow analysis of its kind and will provide the community with a unique view into the physical properties and processes of gaseous outflows. We planned 15 orbits to obtain COS/G130M/1222 spectra. We planned three visits. Due to the nature of target 1, which is an extended galaxy nucleus, we were approved for a hold on Visits 2 and 3 following Visit 1. We explain this below. All observations are through the PSA. VISIT 1: 5 orbits on fixed target #2 VV2000-J165931.9+373528 (QSO) We used three indepenent sources for the astrometric position of the QSO; they all agree within 0.1". For orbit 1, we acquire the target with ACQ/IMAGE/MIRROR-B for 148 sec to obtain S/N=40. We the use the remainder of orbit 1 to obtain the COS spectrum at FP-POS=3. For orbits 2-4, we continue the COS observations. For each subsequent orbit we move the FP-POS in the order 4, 1, 2. At the start of orbit 5, we slew the telescope to target #1 and obtain an 843 sec image using MIRROR A, which according to the COS image target acquisition ETC delivers S/N=40 (assuming the object fills the aperture). This image will be used to verify that the ACQ/IMAGE for Visits 2 and 3 will produce the optimal pointing on this extended and possibly clumpy target. Implementing this at the beginning of the orbit saves on OSM2 rotation (a total of 70 seconds saved). Within 30 days (and no more than 120 days) of obtaining this image, we will report back the coordinates for the pointing for target 1 and file an updated Phase II plan. Following the image, we slew the telescope back to target 2 and complete orbit 5 with a COS spectrum of target 2 using FP-POS=3. VISIT 2: 5 orbits on fixed target #1 GALEX-J165930.3+373526-GALAXY We used three indepenent sources for the astrometric position of the Galaxy; they all agree within 1". This relative error is likely due to the extended nature of the emitting region. For orbit 1, we currently are stating that we will acquire the target with ACQ/IMAGE/MIRROR-A for 843 sec to obtain S/N=40. However, since we will be using the image taken during orbit 5 of visit 1, we may modify the acquisition of the target. Once the target is acquired, we plan to use the remainder of orbit 1 to obtain the COS spectrum at FP-POS=3. For orbits 2-5, we continue the COS observations. For each subsequent orbit we move the FP-POS in the order 4, 1, 2, and 3. VISIT 3: 5 orbits on fixed target #1 GALEX-J165930.3+373526-GALAXY Though we have a total of 10 orbits on target 2, we break the observations into two 5-orbit visits in order to allow avoidance of the SAA. For orbit 1, we currently state that we will acquire the target with ACQ/IMAGE/MIRROR-A for 843 sec to obtain S/N=40. However, we will adopt the method that we employ for visit 2, once we have analyzed the image obtained during orbit 5 of visit 1. We the use the remainder of orbit 1 to obtain the COS spectrum at FP-POS=3. For orbits 2-5, we continue the COS observations. For each subsequent orbit we move the FP-POS in the order 4, 1, 2, and 3. QUASAR ABSORPTION LINES AND IGM 12 false false false false false false SUPPORTED GALAXY BULGE WIND YES This object was generated by the targetselector and retrieved from the GALEX database. The half light radius of the galaxy is 1.53 arcsec. J2000 J2000 GALEX fuv_flux 16.54+/-3.97 uJy, nuv_flux 30.71+/-4.48 uJy; Flambda = 2.15e-16 erg cm^-2 s^-1 A^-1 at 1600 Ang GALAXY QSO NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALEX FUV COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G130M 1222 1469044957952 /Users/cwc/Desktop/OP-cache/pid14264-v1A.xml Timing link suitability includes constraints ([2A After 1A by 35.0 to 120.0 days] [3A After 1A by 35.0 to 120.0 days]) The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 1467827209000 136.26299225076872 (Tic-Visit :proposal-id 14264 :visit-id "1A" :proposal-version -1 :trans-version "20160601" :date "20-Jul-2016 14:02:36.0" :trans-errors '(:WARNINGS 8 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 522000 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14264 :visit-id "1A" :obset-id "1A" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14264 :visit-id "1A" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2934 :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 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "1A" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "1A" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "1A" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "1A" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 331 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) true 5 0 This image will be used to verify that the ACQ/IMAGE of VIsits 2 & 3 will produce the desired pointing. It's actually faster to do this first, because it saves on OSM2 rotation (70 seconds) 1469044960224 /Users/cwc/Desktop/OP-cache/pid14264-v2A.xml Timing link suitability includes constraints ([2A After 1A by 35.0 to 120.0 days]) The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14264 :visit-id "2A" :proposal-version -1 :trans-version "20160601" :date "20-Jul-2016 14:02:39.0" :trans-errors '(:WARNINGS 7 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 452336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14264 :visit-id "2A" :obset-id "2A" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14264 :visit-id "2A" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "2A" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "2A" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "2A" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "2A" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 407 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) true 5 0 WE HAVE NOW REMOVED THE HOLD Previous Comments: We would like to take a PSA MIRROR A image at the end of Visit 1 (5 orbits) in order to optimize the target acquisitions for Visits 2 and 3. We use the GALEX FUV flux (16.54 micro Jy) corresponding to f_lambda 1.06e-16 and ran the ETC to demonstrate that this is safe to do. The issue is that Visits 1 and 2 are for COS spectra of an extended galaxy nuclear region, for which we know the total flux, but we do not know how clumpy or the degree of flux variations across the nuclear region. In order to optimize the COS spectrum of this object, we would like to determine the optimal location on the nucleus to center the COS PSA. 1469044930646 /Users/cwc/Desktop/OP-cache/pid14264-v3A.xml Timing link suitability includes constraints ([3A After 1A by 35.0 to 120.0 days]) The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14264 :visit-id "3A" :proposal-version -1 :trans-version "20160601" :date "20-Jul-2016 14:02:08.0" :trans-errors '(:WARNINGS 7 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 452336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14264 :visit-id "3A" :obset-id "3A" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14264 :visit-id "3A" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "3A" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "3A" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "3A" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14264 :visit-id "3A" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 407 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) true 5 0 WE HAVE NOW REMOVED THE HOLD: Previous Comments: We would like to take a PSA MIRROR A image at the end of Visit 1 (5 orbits) in order to optimize the target acquisitions for Visits 2 and 3. We use the GALEX FUV flux (16.54 micro Jy) corresponding to f_lambda 1.06e-16 and ran the ETC to demonstrate that this is safe to do. The issue is that Visits 1 and 2 are for COS spectra of an extended galaxy nuclear region, for which we know the total flux, but we do not know how clumpy or the degree of flux variations across the nuclear region. In order to optimize the COS spectrum of this object, we would like to determine the optimal location on the nucleus to center the COS PSA.