0 Assigned ID: 591 ----- Attempting Submission 1 (Fri Apr 10 17:15:23 GMT 2015) ----- HST Phase I Proposal 591 (cyc23_m87.apt) successfully submitted. Receipt: # 591-1 ----- Attempting Submission 2 (Fri Apr 10 19:33:01 GMT 2015) ----- HST Phase I Proposal 591 (cyc23_m87_submit_1x.apt) successfully submitted. Receipt: # 591-2 ----- Attempting Submission 3 (Fri Apr 10 21:23:15 GMT 2015) ----- 0 ----- Attempting Submission 1 (Thu Jul 23 13:00:36 GMT 2015) ----- As the nearest galaxy with an optical jet, M87 affords an unparalleled opportunity to study extragalactic jet phenomena at the highest resolution. We have previously obtained HST images of the jet with unprecedented resolution which show detailed shock structures as well as numerous unresolved condensations over the first few arcseconds of the jet. Our previous HST monitoring observations have found superluminal motion at speeds up to 6c in many of these features, and showed the formation of new emission regions and rapid variability. The STIS/NUV instrument presents a unique opportunity to measure proper motions in the M87 jet with a single highly stable, high resolution detector across a 19 yr timebase. We will use these new data, together with existing STIS/NUV data, to map the velocity field of the jet with much higher accuracy than previously possible. This will allow us to measure the bulk deceleration of the jet, transverse motions, accelerations / decelerations of individual features, and numerous fainter jet features. We will use this to test models for the structure and kinematics of relativistic jet flows, synchrotron emission regions, and AGN in general. We will obtain STIS NUV F25QTZ images of the jet using a setup which closely duplicates our previous monitor observations. Sub-exposures will be dithered to improve PSF sampling by the 0.024" pixels and minimize detector artifacts. ACCUM mode is used for greatest consistency with past monitoring observations. We do not expect any bright object issues for either the M87 nucleus or jet, but a WFC3 observation (Visit 1) is included prior to STIS NUV-MAMA (Visit 2) for added safety; Visit 2 is ON-HOLD pending results of the WFC3 observation. WFC3 observations are made 30 to 100 days prior to the STIS MAMA observations. Filters F225W, F475W, and F814W are used. A sub-array near the C amplifier is used to reduce data volume issues and CTE effects. A POST-FLASH of 12 electrons is used. Bright object discussion for STIS NUV-MAMA: We have used an identical observation (same mode and filter) taken in May 2013 to perform a baseline check of the MAMA-NUV count rate. The brightest feature in image oc1w01w8q.flt was the nucleus which had a total of 70207 counts in 590 sec, or 119 counts/sec, or F(lambda)=7.4e-16 erg cm-2 s-1 A-1. With these inputs the ETC gives the brightest pixel as 30 counts/sec (STIS.im.733860). The nucleus is in fact resolved, and the observed brightest pixel was 11 counts/sec in that image. Both of these values are well below the limit of 100 counts/sec. We also note the target was observed in January and June 2015 in program 13759 using the same mode without incident (those data are proprietary). The M87 jet has been previously seen to produce a bright flare with an e-folding (factor 3) rise time ~1 year. Hence, as added precaution, we have scheduled the WFC3 F225W observation 30 - 120 days prior to the STIS NUV MAMA observation. These data will be reduced promptly, and an updated flux and ETC run will be provided prior to the STIS NUV MAMA observation. The STIS NUV-MAMA observation is ON-HOLD pending the WFC3 result. AGN/QUASARS 12 false false false false 0.0 0.0 SUPPORTED GALAXY ELLIPTICAL JET RADIO GALAXY J2000 J2000 GALAXY ELLIPTICAL JET RADIO GALAXY Position in Knot F near middle ot the jet. J2000 J2000 WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F814W STIS/NUV-MAMA Imaging No No F25QTZ POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false 1437653321438 Timing link suitability includes constraints ([02 After 01 by 30.0 to 120.0 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /Users/biretta/Desktop/M87_Cycle23_14256/OP-cache/14256-v01.xml ORIENTs chosen to place jet along diagonal of sub-array, so as to get more of the jet. Target is M87-JET which is near Knot F in the middle of the jet; this keeps it centered on the detector at different ORIENTs. (Tic-Visit :proposal-id 14256 :visit-id "01" :proposal-version -1 :trans-version "20150609" :date "23-Jul-2015 08:08:41.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 213904 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14256 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14256 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2627 :al-overhead-at-end 83 :internal-dur-at-end 270 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2988 :pcs-gap 0 ) true 1 0 ETC calculation based on expected flux in single WFC3 pixel in F225W for bright region of Knot A. ETC calculation based on expected flux in single WFC3 pixel in F475W for bright region of Knot A. ETC calculation based on expected flux in single WFC3 pixel in F814W for bright region of Knot A. 1437652838254 Timing link suitability includes constraints ([02 After 01 by 30.0 to 120.0 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /Users/biretta/Desktop/M87_Cycle23_14256/OP-cache/14256-v02.xml Visit 2 is on hold pending fluxes from Visit 1 and check of bright object issues. Nominally it should schedule 30 to 120 days after Visit 1. Both visits have ORIENT constraints. STIS NUV-MAMA ORIENT chosen to match prior epochs of monitoring observations. POS TARG used to place middle of jet near center of detector. Dithering used to improve PSF sampling and remove any detector artifacts. ACCUM used for greatest consistency with prior observations. (Tic-Visit :proposal-id 14256 :visit-id "02" :proposal-version -1 :trans-version "20150609" :date "23-Jul-2015 08:00:38.0" :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 278320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14256 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14256 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2653 :al-overhead-at-end 0 :internal-dur-at-end 450 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2988 :pcs-gap 0 ) true 1 0 Visit 2 is on hold pending Bright Object check based on F225W fluxes from Visit 1. ETC calculation based on May 2013 STIS NUV F25QTZ observation of the M87 nucleus (brightest feature), assuming it is unresolved, gives 30 counts/sec. In reality the nucleus is slightly extended, and the actual observered count rate for brightest pixel was 11 counts/sec. Both numbers are well below brightest pixel limit of 100 counts/sec. For added safety against flaring behavior in the jet, an F225W image will be taken in Visit 1 approx 30 to 120 days before the STIS NUV-MAMA visit.