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[Possible EIS Core Team Studies (2009-Dec-01)|http://docs.google.com/Doc?docid=0AdazsPAS3_6xZGNzZHFiOWhfMTY2ZjQ3cG1oZGQ&hl=en&invite=CIDL2K4H]\\

Possible EIS Core Team Studies\\ 
__Quiet Sun__\\ 
!1. Evolution of X-ray bright point – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de]) \\ 
- point to a quiet region with an X-ray bright point near disk centre\\ 
- run IUU_SLOT_136x400_Q65 (ID # 292) for context \\ 
- data volume: 12.1 Mbit; duration: 15m 41s\\ 
- run SK_QS_34x168c (ID # 295) for BP study; data volume: 2.1 Mbit; dur: 3m 49s\\ 
- run for 3 hours or longer \\ 
- SOT: support with magnetograms (3 min cadence) and Ca II H filtergrams to track evolution of magnetic fields in the photosphere\\ 
__2. Coronal/TR Doppler & photosphere transverse magnetic features and cancellation events – Yokoyama ([yokoyama.t@eps.s.u-tokyo.ac.jp|mailto:yokoyama.t@eps.s.u-tokyo.ac.jp])__\\ 
- QS near the disk centre, if possible, include an XBP in FOV for alignment\\ 
- observation structure similar to the Muglach programme\\ 
- run studies in the order: three times (a) - n times (b) – three times (a)\\ 
- a) Study: quiet_sun_slot (#210); 40x512 slot image as context; volume: 1.4Mbits, \\ 
- duration: 1.5min, rate:16.4kbps\\ 
- three images should be taken before and after program b)\\ 
- b) Study: sta_loop_context_lo (#278); vol: 23.3Mbits, dur: 34min, rate: 34kbps\\ 
- repeat n times to fit into available data volume\\ 
- EXPOSURE: 30s, RASTER: 60 steps, SLIT: 2", STEP: 2" FOV: 120"x248"\\ 
__SOT __support: FG/NFI: NaI/IV 2-wavelength filter (mandatory)\\ 
  - 1st priority on the high cadence (at least < 60sec).\\ 
  - 2nd priority on the longer coverage (>2-3hrs continuous coverage; \\ 
  - Interuptions by SAAs and S/C nights are OK.)\\ 
  - 3rd priority on the FOV (at least, larger than 100arcsec^2)\\ 
- SP: fast mapping, FOV: same as FG/NFI (mandatory)\\ 
- FG/BFI: CaII/G-band (lowest priority, can be omitted)\\ 
__XRT __support: FOV: cover the same FOV as SOT Filters: low-temperature filter-pair; Cadence: <5min\\ 
!3. QS Brightenings – Bewsher ([d.bewsher@rl.ac.uk|mailto:d.bewsher@rl.ac.uk]), Young \\ 
EIS to point at quiet Sun region near disk centre \\ 
run following studies:\\ 
PRY_slot_context_v3 (dur: 3min; vol: 3 Mbit) once at start of observation\\ 
tr_bright_lo (dur: 6min; vol: 1.5 Mbit) repeatedly to fill available time slot\\ 
PRY_slot_context_v3 again, once at end of observation\\ 
run tr_bright_lo for minimum of 4h; longer if possible\\ 
request SOT and XRT to observe EIS FoV: 20” x 144”\\ 
SOHO/CDS involvement desirable; __advise schedule to Bewsher__\\ 
!4. Search for Evidence of Wave Activity in the Solar Corona - Bewsher ([dbewsher@uclan.ac.uk|mailto:dbewsher@uclan.ac.uk]), Harrison ([richard.harrison@stfc.ac.uk|mailto:richard.harrison@stfc.ac.uk])\\ 
run__ __rah_line_narrow; duration: 1 h 5 m 20 s; data volume: 24 Mbits\\ 
run for 6 hour min (~ 144Mbits); longer if possible; repeat to fill time slot\\ 
point to the off limb ‘quiet’ solar corona above the equator; solar y = 0; limb should be in the fov;  planner should maximise the altitude observable\\ 
request SOT and XRT to observe EIS fov (238 x 256”)\\ 
__CDS involvement essential,__ __advise schedule to Bewsher – note email change__\\ 
__5. X-ray Bright Points Onset – Brown __([dsbrown@uclan.ac.uk|mailto:dsbrown@uclan.ac.uk])__, Bewsher ([dbewsher@uclan.ac.uk|mailto:dbewsher@uclan.ac.uk]) __\\ 
EIS to point at quiet Sun region near disk centre \\ 
target QS magnetic fragments as seen by SOT with little/no emission in the corona\\ 
run the following studies:\\ 
PRY_slot_context_v2 (dur 3 min; vol 3 Mbit) once at start of observation\\ 
dob_bp_slit_raster (dur 33m 50s; vol 7 Mbit) or dob_bp_slot_raster (dur 2m 13s; vol 7 Mbit); repeat to fill available time slot\\ 
PRY_slot_context_v2 at end of observations\\ 
run dob_bp_****_raster for minimum 4h; run both studies on different days\\ 
request SOT and XRT to observe EIS FoV: 120x160" (dob_bp_slit_raster) or 160x160" (dob_bp_slot_raster)\\ 
TRACE/CDS involvement desirable; __advise schedule to Brown  and Bewsher__\\ 
!6. Coronal Jets – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil]), Ugarte-Urra \\ 
measure DEM in jet reconnection region\\ 
run slot_context_lite_v1 before/after IUU_SCAN_STEPS_002 in N- polar CH\\ 
place raster (slit: 368") so that part covers adjacent Quiet Sun\\ 
run for as long as possible outside of eclipse\\ 
!7. Quiet Sun diagnostics/evolution - Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto:iugarte@ssd5.nrl.navy.mil]) \\ 
point to a generic quiet Sun region (solar tracking). Two study sequences:\\ 
a) run NRL_QSCH_30X400_90s2 multiple times (3 at least)\\ 
b) run IUU_SLOT___488x512__ as context\\ 
run HPW019AR__1x400_45s (sit-and-stare) for 2 hours\\ 
run IUU_SLOT___488X512__ as context\\ 
Note: ideally run sequences one after the other on the same pointing. \\ 
sequences can run independently of each other if  needed. \\ 
SOT magnetograms and XRT C_poly or Al_poly observations desirable,\\ 
      matching EIS cadence (1-2 min) in sequence b)\\ 
!8. Coronal Hole Density Measurement – Young ([peter.young.ctr.uk@nrl.navy.mil|mailto:peter.young.ctr.uk@nrl.navy.mil]) \\ 
polar or equatorial CH\\ 
select pointing based on EIT 195 images; choose darkest part of CH\\ 
accurate warm pixel removal essential for CH data\\ 
run REGCAL071 and REGCAL072 on the same day; also context study\\ 
study sequence is: REGCAL071; REGCAL072; PRY_slot_context_v2 ;\\ 
run on mid-latitude extension to N-polar CH\\ 
Note 1: repeat PRY_CH_density to fill time slot; vol: 20 Mbit; data rate: 5.2 kbps\\ 
Note 2: for large dark CH areas, stitch two or more repeats of PRY_CH_density\\ 
!9. Eclipse Spectral Atlas - Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\ 
obtain reference spectra for general science during Hinode eclipse season\\ 
run PRY_slot_context_v3 (5 Mbits) and Eclipse_raster_v2 (99 Mbits)\\ 
observe any target\\ 
run PRY_slot_context_v3 once\\ 
follow by one run of Eclipse_raster_v2 (total duration: 54mins) \\ 
start PRY_slot_context_v3 10 mins after end of Hinode orbital night\\ 
repeat for consecutive day-time periods depending on available data volume\\ 
!10. Properties in Solar Wind Source Regions – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil]) Ko ([yko@ssd5.nrl.navy.mil|mailto:yko@ssd5.nrl.navy.mil]) \\ 
target: equatorial or low-latitude coronal hole within ± 400 latitude; Polar CH extensions also possible if within ± 400; observe with CH at central meridian\\ 
run a) YKK_EqCH_02n around the centre of the coronal hole\\ 
run b) YKK_EqCH_02n between the centre and East CH boundary\\ 
run c) YKK_EqCH_02w at E CH boundary partly covering the 'visible' CH, partly covering adjacent AR or QS to the East\\ 
run context raster slot_context_q50 covering FOV of the a, b and c rasters\\ 
default pointing: Sun center X=0", Y=0"; slit field-of-view to cover the solar equator;  if CH does not reach latitude zero cover lowest latitude reached\\ 
if all three studies not possible in time available, run b) followed by c)\\ 
contact Yuan-Kuen Ko ([yko@ssd5.nrl.navy.mil|mailto:yko@ssd5.nrl.navy.mil]) to agree final pointing\\ 
__see Core HOP 146; use these original studies for on-disc CHs only__\\ 
__11. Quiet sun dynamics study – Muglach __\\ 
- run studies in the order: three times (a) - n times (b) – three times (a)\\ 
       - a) Study: quiet_sun_slot (#210); 40x512 slot image as context\\ 
       - three images should be taken before and after program b)\\ 
       - b) Study: KM-qs-study-low (#315)\\ 
       -  run in areas of quiet Sun, also plage or moderately active regions possible\\ 
       - slit should at least be partially on the disk\\ 
       - avoid large, well developed ARs and coronal holes \\ 
       - study for small-scale short-term variation of QS structures in cool EIS lines.\\ 
       - repeat n times to fit into available data volume; at least for 30 min\\ 
       - EXPOSURE: 20s, RASTER: Scanning, 4 steps, SLIT: 2", STEP: 2"\\ 
         FOV: 10"x464"\\ 
       - if n = 30 for (b), data volume is 70 Mbits; run (b) for longer if volume available\\ 
Co-observing: - SOT:\\ 
1) magnetograms in either Fe I or Na I, in 60s cadence (or less if telemetry allows).   \\ 
    SOT to run > 15 min before EIS start and at least 15 min after EIS end.\\ 
2) SP scans of the target regions valuable additions but lower priority than 1.\\ 
3) BFI images in G-Band can be added; lower priority than 1 and 2.\\ 
4) XRT: filtergrams in the thinnest filter(s)\\ 
!12. Filament Evolution – Green ([lmg@mssl.ucl.ac.uk|mailto:lmg@mssl.ucl.ac.uk])\\ 
-    Observe an on-disc filament\\ 
-    Run \\ 
          - cme_slot_red_lkh for approx 30 min; data vol: 18 Mbit; context\\ 
          - cme_slit_red_lkh to fill available time; 34 min has data vol: 31 Mbit\\ 
          - cme_slot_red_lkh for approx 30 min; data vol: 18 Mbit; context\\ 
__-    Run if suitable quiescent filament is available on disc__\\ 
!13. Interchange Reconnection at CH Boundaries – Baker ([db2@mssl.ucl.ac.uk|mailto:db2@mssl.ucl.ac.uk]), Van Driel ([lidia.vandriel@obspm.fr|mailto:lidia.vandriel@obspm.fr]) search for closed/open field interactions at CH boundaries with adjacent activity\\ 
run dhb_polar_scan_Q90 (ID #294); \\ 
check with proposers for pointing details\\ 
__run for small closed structures at CH boundaries or inside on-disc CHs__\\ 
__------------------------------------------------------------------------------------------------------EIS CORE HOP 80: Polar Coronal Hole Observation – Gabriel ([alan.gabriel@ias.u-psud.fr|mailto:alan.gabriel@ias.u-psud.fr]), Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk])__\\ 
__EIS CORE HOP 130: Multi-temperature Full Disk Slot Scans - Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto:iugarte@ssd5.nrl.navy.mil]), Brooks ([dhbrooks@ssd5.nrl.navy.mil|mailto:dhbrooks@ssd5.nrl.navy.mil]) __\\ 
__EIS CORE HOP 146: Solar Wind Source Regions During Solar Minimum Conditions – Kuen Ko ([yko@ssd5.nrl.navy.mil|mailto:yko@ssd5.nrl.navy.mil]), Mariska ([mariska@nrl.navy.mil|mailto:mariska@nrl.navy.mil])__\\ 
__EIS CORE HOP 137: Evolution of Network Boundary Elements: Possible Connections to the Corona – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil])__\\ 
__------------------------------------------------------------------------------------------------------B. Active Region, Flare, CME__\\ 
__Useful AR context studies for before/after main AR observation are: __\\ 
__PRY_slot_context_v3 or PRY_slot_contextLITE__\\ 
__1. Active Region Studies – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil]), Mariska __\\ 
Studies HPW017AR_30x400_30s2, HPW018AR300x400_30s2 and   \\ 
select as appropriate for AR ToO\\ 
use PRY_slot_context___v3__ or PRY_slot_context __LITE __before/after selected HPW\\ 
check with Harry Warren re ASRC for raster expansion\\ 
!2. AR dynamics and CME watch – Young, Ugarte-Urra \\ 
40” slot for large FoV, high cadence AR images in a wide Te range to i) examine loop morphology ii) detect CME initiation. \\ 
run either i) PRY_slot_context___v3__ (AR dynamics, includes diagnostics) or ii) PRY_slot_context__LITE__ (488”x488”; 3.5min); (CME watch, low TLM, extended hours)\\ 
repeat to fill available time slot \\ 
-     run for 3 hours, preferably longer\\ 
!3. Active Region Studies – Warren__ ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil]),__ Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto:iugarte@ssd5.nrl.navy.mil]) \\ 
-     observe the large dispersing AR near CM\\ 
-     run a large raster with HPW018\\ 
-     run a fast scan with IUU_SCAN_STEPS_002 for several hours\\ 
__4. Loop morphology and oscillations - de Moortel ([ineke@mcs.st-and.ac.uk|mailto:ineke@mcs.st-and.ac.uk]), Bewsher ([d.bewsher@rl.ac.uk|mailto:d.bewsher@rl.ac.uk]), Young __\\ 
relatively quiescent (non-flaring) coronal loop system either on disk or limb.\\ 
point to loops in the active region.\\ 
run PRY_footpoints_lite (dur: 28min; vol: 55 Mbit), sta_loop_slot_lo (dur: 39min; vol: 22 Mbit).\\ 
-     study sequence is: \\ 
      -     PRY_footpoints_lite once at beginning of a period \\ 
      -     sta_loop_slot_lo at the same pointing\\ 
-     repeat sta_loop_slot_lo to fill available time slot.\\ 
__run on any quiescent AR; advise schedule to de Moortel__\\ 
!5. Pre-flare activity monitoring - Wallace ([ajw2@mssl.ucl.ac.uk|mailto:ajw2@mssl.ucl.ac.uk])\\ 
point to a flaring AR to search for features that precede flares\\ 
run Flare0_slit_AJW; (dur: 50m 34s; vol: 2.9 Mbits; size: 180” x 320”)\\ 
scanning raster; slit: 2”; step:2”; exposure: 30s; 89 steps.\\ 
run repeatedly on a flaring AR to fill available time allocation.\\ 
!6. Search for Active Region outflows – Culhane ([jlc@mssl.ucl.ac.uk|mailto:jlc@mssl.ucl.ac.uk]), Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk])\\ 
-     observe AR outflows at opposite boundaries of the large dispersing AR near CM\\ 
-     run HPW015_DETAILED_MAP_1_45s_200x360 twice; two separate pointings\\ 
-     total data volume: 662 Mbits; duration: 2 x 2h 44 m or 5h 28 m total\\ 
-     __check pointing positions with proposers__\\ 
!7. AR Temperature Diagnostic – Mason ([hm11@damtp.cam.ac.uk|mailto:hm11@damtp.cam.ac.uk])\\ 
run cam_ar_temp_lite_v2\\ 
target: temperature structure of active regions on the limb\\ 
centre raster at the active region core.\\ 
exposure time: 30s; raster: scanning; slit: 2"; step Size: 2", FOV: 360"X400";\\ 
raster duration: 1h40m46s \\ 
!8. High cadence observations of AR transient brightenings and microflares - Mason ([hm11@damtp.cam.ac.uk|mailto:hm11@damtp.cam.ac.uk])\\ 
run cam_artb_lite_v2\\ 
run on AR to study transient brightenings and microflares at very high cadence\\ 
raster centre should be at polarity inversion line.\\ 
raster: scanning; slit: 2", step size: 2"; FOV: 40"X120"\\ 
raster duration: 4m32 seconds\\ 
run as many times as possible and at least for 3-4 hours continuous \\ 
__9. CME onsets - Bewsher ([danielle.bewsher@stfc.ac.uk|mailto:danielle.bewsher@stfc.ac.uk]), Harrison__\\ 
algorithm to detect CME-related dimming\\ 
point above limb __at AR if it develops __with part of limb in FoV\\ 
if AR present, centre raster y-direction on the AR; null evaluation in AR absence\\ 
run cmeo_slit_lo; minimum 5 rasters; Duration: 4.2 h; Volume: 13 Mbit __or__\\ 
run cmeo_slot_lo; min duration: 5 h; Volume: 10 Mbit\\ 
algorithm uses difference imaging so minimum durations __must__ be available\\ 
!10. CORE EIS Flare Study – Milligan ([ryan.o.milligan@nasa.gov|mailto:ryan.o.milligan@nasa.gov])\\ 
run FLR001_flare_study; \\ 
exposure: 5s; raster: scanning; slit: 2”; step: 2”; FoV: 80” x 120”; raster time: 5m\\ 
run for 2 hr; data volume: 36 Mbit\\ 
target: any AR with significant flare probability\\ 
!!!C. Test and Calibration Studies \\ 
__1. EIS slit calibration – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])__\\ 
-      Obtain co-spatial data in the 1", 2" and 40" slits for various calibration tests (slit   \\ 
       widths, tilt, intensity calibration)\\ 
-      run CALIB_slit_slot_v1\\ 
-      study includes three separate rasters; each must be individually pointed\\ 
-      point off-limb above the quiet Sun at the equator (either limb)\\ 
-      make two separate adjacent entries of calib_slit_slot_v1 on the timeline\\ 
-      select Solar-X position 50-60” above limb; same for each of the rasters in both  \\ 
       study entries\\ 
-      select Y position with the YIP input rather than the solar-Y position\\ 
-      set the YIP entry to 511 for each of the three rasters in first study entry \\ 
-      for the second study entry, set YIP to 1 for each of the three rasters\\ 
__-      __data volume: 54 Mbits.\\ 
__2. EIS velocity calibration – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de])__\\ 
__-     __Determine__ __the slit tilt and curvature in full Y height for velocity calibration\\ 
-     execute raster scans at three positions with 1" and 2" slits\\ 
-     run ID 375 SK_DEEP_5x512_SLIT1 – the  1" slit study, with Y initial positions\\ 
      #1 YIP=1; #2 YIP=256; #3 YIP=512\\ 
-     run ID 376 SK_DEEP_10x512_SLIT2 – the  2" slit study, with Y initial positions\\ 
      #4 YIP=1; #5 YIP=256; #6 YIP=512\\ 
-     six consecutive rasters require total time ~ 60min and data volume ~ 45Mbits\\ 
-     target: quiet region near disk center (0", 0"); shift EIS FOV ±200" in E-W \\ 
      direction to avoid ARs; do not run if ARs in target area;\\ 
-     keep the same mirror initial position (MIP) for all rasters.\\