UV Line Emission from Million Degree Gas in a Galaxy Cluster Core

ORBITAL VISIBILITY OVERRUN INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS ORBITAL VISIBILITY OVERRUN INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN INEFFICIENT ORDERING OF FP-POS POSITIONS The remaining 5 orbits were re-allocated between 1 STIS orbit, to recover from a previous failed acquisition during Visit 01, and 4 COS/NUV orbits, to obtain an upper limit or detection of CIV. We increased the exposure time on the acquisition from 2 to 60 seconds. The COS/FUV observation detected only Lyman alpha (but clearly successful acquisition). The previous COS/NUV observation detected continuum, but the wavelength range missed the redshifted CIV wavelength (2110 Ang). The conservative COS acquisition strategy is identical to the previously successful COS visits. The STIS scientific goal is to obtain an accurate Halpha measurement of the knot to compare to the Lyman alpha detection, as well as assess the velocity width of the optical emission emission lines. The COS science goal is to place a limit on any CIV emission to <10% of the Lyman Alpha detection. Further attempts to detect OVI, which is utterly missing in the FUV spectrum, will not have nearly the same scientific impact. 547535991 ----- Attempting Submission 2 (Tue Jul 01 22:43:31 GMT 2014) ----- Selecting the Fixed targets folder and running Target Confirmation Tool did not do anything. When only the "Targets" folder was selected, the tool attempted to export target but complete stalled. I did not change the targets, the target RA and Dec and information are untouched from the previous submission. The warnings are about inefficient order for COS FP-Pos, which is an unavoidable warning given the number of exposures. UV Line Emission from Million Degree Gas in a Galaxy Cluster Core Progress in understanding the nature of galaxy formation and feedback in massive halos depends critically on knowing whether the source of the star-forming gas in Brightest Cluster Galaxies is cooling and condensation out of the hot ambient medium or whether it enters the central galaxy already in cold form. We will study UV and optical line emission from the knots of a powerful star-forming brightest cluster galaxy from the CLASH MCT cluster sample in order to place definitive limits on the presence of intermediate temperature (10^5-6 K) gas in the center of a massive galaxy that is forming stars at ~100 solar masses per year. We have chosen a galaxy cluster at z~0.35 to enable the first ever simultaneous measurement of O VI, N V, and C IV from a cluster core. We will compare the observed UV line ratios to those predicted by competing model for steady nonequilibrium cooling, thermal conduction, and cooling mediated by turbulent mixing. We plan to acquire STIS (H-alpha, NII) and COS spectroscopy OVI, Lyman-alpha, CIV) of UV-bright knots in the Brightest Cluster Galaxy of a moderate redshift cluster RXJ1532+3021. We have in hand rest-frame UV images f rom the MCT CLASH program so we can accurately position the knots in the STIS aperture. We have a mild constraint that we would like the knots in the COS aperture to be not aligned along the dispersion direction. ISM IN EXTERNAL GALAXIES Default false true false false false SUPPORTED CLUSTER OF GALAXIES COOLING FLOW EMISSION LINE NEBULA NUCLEUS RICH CLUSTER STAR FORMING REGION The GSC2 coordinates are similar, with larger error budget 0.2". The target, Knot A in the proposal, is GSC2.2 star N13303016375, at 233.224095 + 30.349857. The STIS PA restrictions place the STIS long slit is oriented approximately N/S, and will include Knot B and possibly Knot C (farther south). The restrictions on the COS PA are to avoid lining up Knot A and B (N/S) along the dispersion direction: assumes the dispersion axis "x" is the U3 axis - 45 degrees. It is unlikely both of these knots will be in the sweet spot of the COS aperture simulatenously, however, so even this weak restriction on COS scheduling is probably unnecessary. J2000 J2000 CLUSTER OF GALAXIES COOLING FLOW EMISSION LINE NEBULA NUCLEUS RICH CLUSTER STAR FORMING REGION The GSC2 coordinates are similar, with larger error budget 0.2". The target, Knot A in the proposal, is GSC2.2 star N13303016375, at 233.224095 + 30.349857. I've provided a position that is 0.1" North of the actual position to avoid centering on Knot B, 0.5" to the south of Knot A. The STIS PA restrictions place the STIS long slit is oriented approximately N/S, and will include Knot B and possibly Knot C (farther south). The restrictions on the COS PA are to avoid lining up Knot A and B (N/S) along the dispersion direction: assumes the dispersion axis "x" is the U3 axis - 45 degrees. It is unlikely both of these knots will be in the sweet spot of the COS aperture simulatenously, however, so even this weak restriction on COS scheduling is probably unnecessary. J2000 J2000 STIS/CCD Spectroscopic No No G750M 8825 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G140L 1280 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1404254337978 The allowed orientations put all 3 knots in the slit. The two allowed ranges are 180 degrees different from each other. 1395168272000 229.20974435240896 (Tic-Visit :proposal-id 13367 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "01-Jul-2014 18:38:57.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 166112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13367 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13367 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2901 :al-overhead-at-end 121 :internal-dur-at-end 246 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3041 :al-overhead-at-end 121 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 2 1 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1404251826158 The allowed orientations put all 3 knots in the slit. The two allowed ranges are 180 degrees different from each other. (Tic-Visit :proposal-id 13367 :visit-id "05" :proposal-version -1 :trans-version "20140605" :date "01-Jul-2014 17:57:06.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 92496 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13367 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13367 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2923 :al-overhead-at-end 0 :internal-dur-at-end 603 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1404251734480 The orient constraint is in place simply to avoid lining up Knot A and B (almost directly north-south) along the dispersion direction. A long IMAGE/acquisition is in place because the Lyman alpha flux is uncertain by a factor of 2 or so. The orient constraint is intended to keep the cross-dispersion direction in roughly a north-south orientation. (Tic-Visit :proposal-id 13367 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "01-Jul-2014 17:55:34.0" :trans-errors '(:WARNINGS 2 :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 548256 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13367 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13367 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2919 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 4 0 This acquisition is slight offset to ensure the aperture centers on Knot A rather than Knot B. Both will be in the aperture. All of the acquisition images, summed, will be a high-resolution map of the Lyman Alpha emission line nebula in the center of this BCG, should be really nice. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. I think FP-POS hits all 4 recommended dither positions but if this is wrong, I'll need to redo each exposure to do so. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1404254346780 The orient constraint is in place simply to avoid lining up Knot A and B (almost directly north-south) along the dispersion direction. A long IMAGE/acquisition is in place because the Lyman alpha flux is uncertain by a factor of 2 or so. The orient constraint is intended to keep the cross-dispersion direction in roughly a north-south orientation.I am considering switching to grating G160M, 1589 central wavelength to avoid source overlap in the cross dispersion (Perp to dispersion) direction. 1403857144000 158.987792969 (Tic-Visit :proposal-id 13367 :visit-id "03" :proposal-version -1 :trans-version "20140605" :date "01-Jul-2014 18:39:05.0" :trans-errors '(:WARNINGS 3 :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 722272 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13367 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13367 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2917 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 5 1 This acquisition is slight offset to ensure the aperture centers on Knot A rather than Knot B. Both will be in the aperture. All of the acquisition images, summed, will be a high-resolution map of the Lyman Alpha emission line nebula in the center of this BCG, should be really nice. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. I think FP-POS hits all 4 recommended dither positions but if this is wrong, I'll need to redo each exposure to do so. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. I think FP-POS hits all 4 recommended dither positions but if this is wrong, I'll need to redo each exposure to do so. The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1404254349124 The orient constraint is in place simply to avoid lining up Knot A and B (almost directly north-south) along the dispersion direction. A long IMAGE/acquisition is in place because the Lyman alpha flux is uncertain by a factor of 2 or so. The orient constraint is intended to keep the cross-dispersion direction in roughly a north-south orientation 1402343193000 158.987792969 (Tic-Visit :proposal-id 13367 :visit-id "04" :proposal-version -1 :trans-version "20140605" :date "01-Jul-2014 18:39:08.0" :trans-errors '(:WARNINGS 4 :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 478672 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13367 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13367 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2922 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3045 :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 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13367 :visit-id "04" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 4 3 This acquisition is slight offset to ensure the aperture centers on Knot A rather than Knot B. Both will be in the aperture. All of the acquisition images, summed, will be a high-resolution map of the Lyman Alpha emission line nebula in the center of this BCG, should be really nice. The NUV COS acquisition is somewhat shorter to allow for longer NUV spectrum exposure. Ideally this visit happens after Visit 2 OR Visit 3 (either one) ; if acquisition should be longer, we wouldn't want this visit to be the first COS visit of the program. Buffer time adjusted to be shorter than actual exposure time, to minimize the read-out time between exposures. Buffer time adjusted to be 100s shorter than actual exposure time, to minimize the read-out time between exposures. I think FP-POS hits all 4 recommended dither positions but if this is wrong, I'll need to redo each exposure to do so.