=> The conventions of title: HEADERyyyymmdd-Index => brief descriptions
HEADER: qs (Quite Sun); ar (Active Region); hop (Hinode Operation Plan); test (Test studies)
yyyymmdd: the date when the study is added; For "hop" and "test" header, it may be different
For example: ar20100417-13 => Nanoflare heating of coronal loops
=> study qs20091216-09 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04
=> study ar20100329-12 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04
HEADER: qs (Quite Sun); ar (Active Region); hop (Hinode Operation Plan); test (Test studies)
yyyymmdd: the date when the study is added; For "hop" and "test" header, it may be different
For example: ar20100417-13 => Nanoflare heating of coronal loops
=> study qs20091216-09 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04
=> study ar20100329-12 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04
Table of Contents
- Available EIS Core Team Studies
- A. Quiet Sun
- qs20091216-01 => Evolution of X-ray bright point
- qs20091216-02 => Coronal/TR Doppler & photosphere transverse magnetic features and cancellation events
- qs20091216-03 => QS Brightenings
- qs20091216-04 => Search for Evidence of Wave Activity in the Solar Corona
- qs20091216-05 => X-ray Bright Points Onset
- qs20091216-06 => Coronal Jets
- qs20091216-07 => Quiet Sun diagnostics/evolution
- qs20091216-08 => Coronal Hole Density Measurement
- qs20091216-10 => Properties in Solar Wind Source Regions
- qs20091216-11 => Quiet sun dynamics study
- qs20091216-12 => Filament Evolution
- qs20091216-13 => Interchange Reconnection at CH Boundaries
- B. EIS HOP Obs.
- hop-a => EIS CORE HOP 80
- hop-b => EIS CORE HOP 130
- hop-c => EIS CORE HOP 146
- hop-d => EIS CORE HOP 137
- hop-e => EIS CORE HOP 131 (ToO)
- hop-f => EIS CORE HOP 150 (ToO)
- hop-g => EIS CORE HOP 160 (ToO)
- hop-h => EIS CORE HOP 163 (ToO)
- C. Active Region, Flare, CME
- ar20091216-01 => Active Region Studies
- ar20091216-02 => AR dynamics and CME watch
- ar20091216-03 => Active Region Studies
- ar20091216-04 => Active Region Abundance Variations
- ar20091216-05 => Pre-flare activity monitoring
- ar20091216-06 => Search for Active Region outflows
- ar20091216-07 => AR Temperature Diagnostic
- ar20091216-08 => High cadence observations of AR transient brightenings and microflares
- ar20091216-09 => CME onsets
- ar20091216-10 => CORE EIS Flare Study 1
- ar20091229-11 => CORE EIS Flare Study 2
- ar20100417-13 => Nanoflare heating of coronal loops
- ar20100423-14 => Active Region Transient Brightening Lite
- ar20100423-15 => Multi-temperature Observation of Sigmoids
- ar20100426-16 => Outflows from Small Active Regfions
- ar20100622-17 => AR Temperatures and Flows Optimized for Eclipse Observing
- ar20101109-18 => Dynamic events at the limb with EIS and AIA
- ar20110120-19 => AR Loop footpoint studies using the bright point trigger
- ar20110209-20 => Search for slow mode oscillations in coronal loops
- D. Synoptic and Other Studies
- syo20100504-01 => EIS Spectral Atlas Synoptic Programme
- syo20100713-02 => Full CCD Study to Measure Relative Wavelengths
- E. Test and Calibration Studies
- test-01 => EIS slit calibration
- test-02 => EIS velocity calibration
- test-03 => EIS Slot Deconvolution Test
Available EIS Core Team Studies#
A. Quiet Sun
#
qs20091216-01 => Evolution of X-ray bright point#
– Kamio (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 292 | IUU_SLOT_136x400_Q65 | details | Example fits |
| 295 | SK_QS_34x168c | details | Example fits |
qs20091216-02 => Coronal/TR Doppler & photosphere transverse magnetic features and cancellation events#
– Yokoyama (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 210 | quiet_sun_slot | details | Example fits |
| 278 | sta_loop_context_lo | details | Example fits |
qs20091216-03 => QS Brightenings#
– Bewsher (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 251 | tr_bright_lo | details | Example fits |
qs20091216-04 => Search for Evidence of Wave Activity in the Solar Corona#
– Bewsher (dbewsher@uclan.ac.uk), Harrison (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 337 | rah_line_narrow | details | Example fits |
qs20091216-05 => X-ray Bright Points Onset#
– Brown (dsbrown@uclan.ac.uk), Bewsher (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 285 | dob_bp_slit_raster | details | Example fits |
| 284 | dob_bp_slot_raster | details | Example fits |
qs20091216-06 => Coronal Jets#
– Warren (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 354 | PRY_slot_contextLITE | details | Example fits |
| 358 | IUU_SCAN_STEPS_002 | details | Example fits |
qs20091216-07 => Quiet Sun diagnostics/evolution#
– Ugarte-Urra (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)
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)
| Study ID | Acronym | ||
|---|---|---|---|
| 322 | NRL_QSCH_30X400_90s2 | details | Example fits |
| 378 | IUU_SLOT_488x512 | details | Example fits |
| 336 | HPW019AR_1x400_45s | details | Example fits |
qs20091216-08 => Coronal Hole Density Measurement#
– Young (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 ;
-- PRY_CH_density
-- 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
-- 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 ;
-- PRY_CH_density
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 249 | PRY_slot_context_v2 | details | Example fits |
| 268 | PRY_CH_density | details | Example fits |
qs20091216-10 => Properties in Solar Wind Source Regions#
– Warren (hwarren@nrl.navy.mil), Ko (yko@ssd5.nrl.navy.mil)
-- target: equatorial or low-latitude coronal hole within ± 40o latitude; Polar CH extensions also possible if within ± 40o; 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) to agree final pointing
-- see Core HOP 146; use these original studies for on-disc CHs only
-- 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
) to agree final pointing-- see Core HOP 146; use these original studies for on-disc CHs only
| Study ID | Acronym | ||
|---|---|---|---|
| 330 | YKK_EqCH_02n | details | Example fits |
| 329 | YKK_EqCH_02w | details | Example fits |
| 249 | PRY_slot_context_v2 | details | Example fits |
qs20091216-11 => 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)
-- 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)
| Study ID | Acronym | ||
|---|---|---|---|
| 210 | quiet_sun_slot | details | Example fits |
| 315 | KM-qs-study-low | details | Example fits |
qs20091216-12 => Filament Evolution#
– Green (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 254 | cme_slot_red_lkh | details | Example fits |
| 255 | cme_slit_red_lkh | details | Example fits |
qs20091216-13 => Interchange Reconnection at CH Boundaries#
– Search for closed/open field interactions at CH boundaries with adjacent activity
– Baker (db2@mssl.ucl.ac.uk), Van Driel (lidia.vandriel@obspm.fr)
-- 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
-- check with proposers for pointing details
-- run for small closed structures at CH boundaries or inside on-disc CHs
| Study ID | Acronym | ||
|---|---|---|---|
| 294 | dhb_polar_scan_Q90 | details | Example fits |
B. EIS HOP Obs.
#
hop-a => EIS CORE HOP 80#
Polar Coronal Hole Observation
– Gabriel (alan.gabriel@ias.u-psud.fr), Harra (lkh@mssl.ucl.ac.uk)
hop-b => EIS CORE HOP 130#
Multi-temperature Full Disk Slot Scans
– Ugarte-Urra (iugarte@ssd5.nrl.navy.mil), Brooks (dhbrooks@ssd5.nrl.navy.mil)
hop-c => EIS CORE HOP 146#
Solar Wind Source Regions During Solar Minimum Conditions
– Kuen Ko (yko@ssd5.nrl.navy.mil), Mariska (mariska@nrl.navy.mil)
hop-d => EIS CORE HOP 137#
Evolution of Network Boundary Elements: Possible Connections to the Corona
– Warren (hwarren@nrl.navy.mil)
hop-e => EIS CORE HOP 131 (ToO)#
Helioseismology Observations of Coronal Holes with SOT
– Harra (lkh@mssl.ucl.ac.uk), Zharkov (sz2@mssl.ucl.ac.uk), Sekii (sekii@solar.mtk.nao.ac.jp)
Note: ToO is for "Targets of Opportunity"
hop-f => EIS CORE HOP 150 (ToO)#
Flows during a filament eruption
– Harra (lkh@mssl.ucl.ac.uk), Culhane (jlc@mssl.ucl.ac.uk), Demoulin, Mandrini, Kliem, Williams
Note: ToO is for "Targets of Opportunity"
hop-g => EIS CORE HOP 160 (ToO)#
Long-term Evolution of AR from Flux Emergence through Decay
– Del Zanna (GDelZanna@spd.aas.org), van Driel-Gesztelyi (lvdg@mssl.ucl.ac.uk)
Note: ToO is for "Targets of Opportunity"
hop-h => EIS CORE HOP 163 (ToO)#
Variations in Line Width Across kG Magnetic Field Patches in Coronal Holes
– Harra (lkh@mssl.ucl.ac.uk), Tsuneta, Ito, Shiota
Note: ToO is for "Targets of Opportunity"
C. Active Region, Flare, CME
#
Useful AR context studies for before/after main AR observation are: PRY_slot_context_v3 or PRY_slot_contextLITE
ar20091216-01 => Active Region Studies#
– Warren (hwarren@nrl.navy.mil), Mariska
-- Studies HPW017AR_30x400_30s2, HPW018AR300x400_30s2 and
-- HPW019AR_1x400_45s2
-- select as appropriate for AR ToO
-- use PRY_slot_context_v3 or PRY_slot_contextLITE before/after selected HPW
-- check with Harry Warren re ASRC for raster expansion
-- HPW019AR_1x400_45s2
-- select as appropriate for AR ToO
-- use PRY_slot_context_v3 or PRY_slot_contextLITE before/after selected HPW
-- check with Harry Warren re ASRC for raster expansion
| Study ID | Acronym | ||
|---|---|---|---|
| 355 | HPW017AR_30x400_30s2 | details | Example fits |
| 356 | HPW018AR300x400_30s2 | details | Example fits |
| 357 | HPW019AR_1x400_45s2 | details | Example fits |
| 353 | PRY_slot_context_v3 | details | Example fits |
| 354 | PRY_slot_contextLITE | details | Example fits |
ar20091216-02 => AR dynamics and CME watch#
– Young (pyoung@ssd5.nrl.navy.mil), Ugarte-Urra (iugarte@ssd5.nrl.navy.mil)
-- 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_contextLITE (488”x488”; 3.5min); (CME watch, low TLM, extended hours)
-- repeat to fill available time slot; run for 3 hours, preferably longer
-- run either i) PRY_slot_context_v3 (AR dynamics, includes diagnostics) or ii) PRY_slot_contextLITE (488”x488”; 3.5min); (CME watch, low TLM, extended hours)
-- repeat to fill available time slot; run for 3 hours, preferably longer
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 354 | PRY_slot_contextLITE | details | Example fits |
ar20091216-03 => Active Region Studies#
– Warren (hwarren@nrl.navy.mil), Ugarte-Urra (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
-- run a large raster with HPW018
-- run a fast scan with IUU_SCAN_STEPS_002 for several hours
| Study ID | Acronym | ||
|---|---|---|---|
| 356 | HPW018AR300x400_30s2 | details | Example fits |
| 358 | IUU_SCAN_STEPS_002 | details | Example fits |
ar20091216-04 => Active Region Abundance Variations#
– Ko (yko@ssd5.nrl.navy.mil)
-- target: young AR of less than 3 days; search for any abundance evolution
-- FoV to cover centre of the AR
-- run study twice a day; separate runs by 12 hours; run for 7 consecutive days until AR west limb passage or decay - subject to TLM limitations
-- run YKK_ARabund01; raster scanning: 2” slit and 3” step; exposure: 45s; FOV: 194"x280; duration: 53 m 19s; Data: DCPM/64Mbit.
-- run PRY_slot_contextLITE for context after each raster
-- FoV to cover centre of the AR
-- run study twice a day; separate runs by 12 hours; run for 7 consecutive days until AR west limb passage or decay - subject to TLM limitations
-- run YKK_ARabund01; raster scanning: 2” slit and 3” step; exposure: 45s; FOV: 194"x280; duration: 53 m 19s; Data: DCPM/64Mbit.
-- run PRY_slot_contextLITE for context after each raster
| Study ID | Acronym | ||
|---|---|---|---|
| 381 | YKK_ARabund01 | details | Example fits |
| 354 | PRY_slot_contextLITE | details | Example fits |
ar20091216-05 => Pre-flare activity monitoring#
– Wallace (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.
-- 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.
| Study ID | Acronym | ||
|---|---|---|---|
| 286 | Flare0_slit_AJW | details | Example fits |
ar20091216-06 => Search for Active Region outflows#
– Culhane (jlc@mssl.ucl.ac.uk), Harra (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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 243 | HPW015_DETAILED_MAP | details | Example fits |
ar20091216-07 => AR Temperature Diagnostic#
– Mason (hm11@damtp.cam.ac.uk)
-- run cam_ar_limb_lite_v2
-- target: temperature structure of active regions on the limb
-- centre raster at the active region core.
-- exposure time: 45s; raster: scanning; slit: 2"; step Size: 2", FOV: 322"X376";
-- raster duration: 2h13m15s; Data volume: 186 Mbits;
-- target: temperature structure of active regions on the limb
-- centre raster at the active region core.
-- exposure time: 45s; raster: scanning; slit: 2"; step Size: 2", FOV: 322"X376";
-- raster duration: 2h13m15s; Data volume: 186 Mbits;
| Study ID | Acronym | ||
|---|---|---|---|
| 377 | cam_ar_limb_lite_v2 | details | Example fits |
ar20091216-08 => High cadence observations of AR transient brightenings and microflares#
– Mason (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
-- run context study PRY_slot_context_v3 before and after
-- 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
-- run context study PRY_slot_context_v3 before and after
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 360 | cam_artb_lite_v2 | details | Example fits |
ar20091216-09 => CME onsets#
– Bewsher (danielle.bewsher@stfc.ac.uk), Harrison(Richard.Harrison@stfc.ac.uk)
-- 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
-- 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
| Study ID | Acronym | ||
|---|---|---|---|
| 279 | cmeo_slit_lo | details | Example fits |
| 280 | cmeo_slot_lo | details | Example fits |
ar20091216-10 => CORE EIS Flare Study 1#
– Milligan (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 as long as possible with available TLM; data volume: 37 Mbit/hr
-- target: any AR with significant flare probability
-- see http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html for further details
-- exposure: 5s; raster: scanning; slit: 2”; step: 2”; FoV: 80” x 120”; raster time: 5m
-- run for as long as possible with available TLM; data volume: 37 Mbit/hr
-- target: any AR with significant flare probability
-- see http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html
for further details| Study ID | Acronym | ||
|---|---|---|---|
| 363 | FLR001_flare_study | details | Example fits |
ar20091229-11 => CORE EIS Flare Study 2#
– Hara (hara@solar.mtk.nao.ac.jp)
-- study used to search for flow structures in flares
-- run HH_Flare_180x160_v2 (ID # 390)
-- exposure: 8s; raster: scanning, sparse; slit: 2”; step: 5”; FoV: 180” x 160”;
-- raster time: 6m 36s, data volume: 4.7 Mbit
-- with compression (JPEG85) study should run at 757 Mbit in 16h 30m
-- see http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html for further details
-- run HH_Flare_180x160_v2 (ID # 390)
-- exposure: 8s; raster: scanning, sparse; slit: 2”; step: 5”; FoV: 180” x 160”;
-- raster time: 6m 36s, data volume: 4.7 Mbit
-- with compression (JPEG85) study should run at 757 Mbit in 16h 30m
-- see http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html
for further details| Study ID | Acronym | ||
|---|---|---|---|
| 390 | HH_Flare_180x160_v2 | details | Example fits |
ar20100417-13 => Nanoflare heating of coronal loops#
– Klimchuk (james.a.klimchuk@masa.gov), Patsourakos (spatsurakos@gmail.com), Young (pyoung@ssd5.nrl.navy.mil)
-- test theory that coronal loops are bundles of unresolved, impulsively-heated strands by searching for spectral signatures in the wings of hot (5MK) emission lines
-- run PRY_slot_context_v3 (4.9 Mbits, 3min 29s), nanoflare_sas_v1 (82.5 Mbits, 31min 24s)
-- run sequence: PRY_slot_context_v3, then nanoflare_sas_v1, finally PRY_slot_context_v3
-- run nanoflare_sas_v1 multiple times with raster repeats to fill available time
-- AR pointing for nanoflare_sas_v1 to be at lower legs of loops
-- select inner part of AR; not perimeter “fan” loops
-- choose side of AR with legs oriented along line-of-sight to maximize Doppler shift due to field-aligned flows
-- prefer ARs near disk center
-- for wavelength calibration, position hot loops towards either bottom or top of slit; ensure that the opposite side of the slit observes a quiet Sun region.
NOTE: for pointing confirmation, please send screen grab from eis_image_tool to all three study authors showing suggested pointing. See http://tiny.cc/43rcc for typical pointing examples
-- run PRY_slot_context_v3 (4.9 Mbits, 3min 29s), nanoflare_sas_v1 (82.5 Mbits, 31min 24s)
-- run sequence: PRY_slot_context_v3, then nanoflare_sas_v1, finally PRY_slot_context_v3
-- run nanoflare_sas_v1 multiple times with raster repeats to fill available time
-- AR pointing for nanoflare_sas_v1 to be at lower legs of loops
-- select inner part of AR; not perimeter “fan” loops
-- choose side of AR with legs oriented along line-of-sight to maximize Doppler shift due to field-aligned flows
-- prefer ARs near disk center
-- for wavelength calibration, position hot loops towards either bottom or top of slit; ensure that the opposite side of the slit observes a quiet Sun region.
NOTE: for pointing confirmation, please send screen grab from eis_image_tool to all three study authors showing suggested pointing. See http://tiny.cc/43rcc
for typical pointing examples| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 392 | nanoflare_sas_v1 | details | Example fits |
ar20100423-14 => Active Region Transient Brightening Lite#
– Mason (hm11@damtp.cam.ac.uk)
-- run cam_artb_cds_a_lite
-- observe on-disc active region close to disc centre; study AR transient brightening and density structure
-- raster to be centred on AR core or polarity inversion line
-- exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 200" x 400"
-- raster duration: 21m09s; data volume: 108 Mbits
-- run context study PRY_slot_context_v3 before and after
-- observe on-disc active region close to disc centre; study AR transient brightening and density structure
-- raster to be centred on AR core or polarity inversion line
-- exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 200" x 400"
-- raster duration: 21m09s; data volume: 108 Mbits
-- run context study PRY_slot_context_v3 before and after
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 361 | cam_artb_cds_a_lite | details | Example fits |
ar20100423-15 => Multi-temperature Observation of Sigmoids#
– Mason (hm11@damtp.cam.ac.uk)
-- run cam_sigmoid_study_v1
-- observe temperature structure of cooling plasma in sigmoidal structures on newly reconnected flux rope field lines
-- select small to medium size ARs; the AR should be in the centre of the raster
-- exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 400" x 400"
-- raster duration: 41m33s; data volume: 125 Mbits
-- repeat to fill available time slot; minimum of 4 repeats preferred (needs 500 Mbits)
-- observe temperature structure of cooling plasma in sigmoidal structures on newly reconnected flux rope field lines
-- select small to medium size ARs; the AR should be in the centre of the raster
-- exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 400" x 400"
-- raster duration: 41m33s; data volume: 125 Mbits
-- repeat to fill available time slot; minimum of 4 repeats preferred (needs 500 Mbits)
| Study ID | Acronym | ||
|---|---|---|---|
| 374 | cam_sigmoid_study_v1 | details | Example fits |
ar20100426-16 => Outflows from Small Active Regfions#
– Young (pyoung@ssd5.nrl.navy.mil)
-- observe small ARs simultaneously with QS regions to obtain accurate outflow velocities
-- run PRY_loop_velocity
-- duration: 4h33m; volume:230 Mbits
-- position AR near top or bottom of slit; see example at *http://tiny.cc/qccji*
-- ensure that any fan loops visible in 171 Å images are contained within raster
-- avoid complex ARs
-- run PRY_loop_velocity
-- duration: 4h33m; volume:230 Mbits
-- position AR near top or bottom of slit; see example at *http://tiny.cc/qccji
*-- ensure that any fan loops visible in 171 Å images are contained within raster
-- avoid complex ARs
| Study ID | Acronym | ||
|---|---|---|---|
| 388 | PRY_loop_velocity | details | Example fits |
ar20100622-17 => AR Temperatures and Flows Optimized for Eclipse Observing#
– Warren (harry.warren@nrl.navy.mil)
-- run hpw021_vel_120x512v1
-- duration should allow it to be run between eclipses; can be run multiple times to cover a larger area; avoid SAA.
-- target: active region
-- full slit is taken; position active region near top or bottom of slit so that there is ample quiet Sun for velocity calibration.
-- exposure time: 60s; raster: scanning; slit: 1"; step Size: 2", FOV: 120"x512";
-- raster duration:1h4m58s; data volume: 135 Mbits
-- duration should allow it to be run between eclipses; can be run multiple times to cover a larger area; avoid SAA.
-- target: active region
-- full slit is taken; position active region near top or bottom of slit so that there is ample quiet Sun for velocity calibration.
-- exposure time: 60s; raster: scanning; slit: 1"; step Size: 2", FOV: 120"x512";
-- raster duration:1h4m58s; data volume: 135 Mbits
| Study ID | Acronym | ||
|---|---|---|---|
| 420 | hpw021_vel_120x512v1 | details | Example fits |
ar20101109-18 => Dynamic events at the limb with EIS and AIA#
– Young (pyoung@ssd5.nrl.navy.mil)
-- pointing should be above the limb, preferably an active region; quiet Sun or prominence cavity also acceptable
-- sequence: first run PRY_slot_context_v3, then PRY_sit_stare_1 (repeat for several hours), then PRY_slot_context_v3
-- XRT: high cadence, long duration, Y-coverage: 512”; spatial resolution: 1-2” preferred
-- SOT: Ca II and/or H-alpha, with high cadence, long duration preferred over spatial resolution
-- sequence: first run PRY_slot_context_v3, then PRY_sit_stare_1 (repeat for several hours), then PRY_slot_context_v3
-- XRT: high cadence, long duration, Y-coverage: 512”; spatial resolution: 1-2” preferred
-- SOT: Ca II and/or H-alpha, with high cadence, long duration preferred over spatial resolution
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 443 | PRY_sit_stare_1 | details | Example fits |
ar20110120-19 => AR Loop footpoint studies using the bright point trigger#
– Young (pyoung@ssd5.nrl.navy.mil)
-- observe AR on the disc with bright loop footpoints (check AIA 171 image)
-- target region near central meridian preferred
-- run Hunter_loop_fe8 (ID: 445, 3.1 Mbits, 24min); set response study to be Cool_loop_response
(ID: 444, 268 Mbits, 2hr 52m)
-- BP trigger parameters are given in the Hunter_loop_fe8 study description, but change the Xthresh
value to 5000 (instead of 5460)
-- target region near central meridian preferred
-- run Hunter_loop_fe8 (ID: 445, 3.1 Mbits, 24min); set response study to be Cool_loop_response
(ID: 444, 268 Mbits, 2hr 52m)
-- BP trigger parameters are given in the Hunter_loop_fe8 study description, but change the Xthresh
value to 5000 (instead of 5460)
| Study ID | Acronym | ||
|---|---|---|---|
| 445 | Hunter_loop_fe8 | details | Example fits |
| 444 | Cool_loop_response | details | Example fits |
ar20110209-20 => Search for slow mode oscillations in coronal loops#
– Wang (tongjiang.wang@nasa.gov), Mariska (john.mariska@nrl.navy.mil)
-- pointing is to a possibly flare-productive active region on the limb.
-- for Study A, 1/3 FOV on the disk and 2/3 FOV off the limb.
-- for Studies B and and C, the slit center position is set about 30-50 arcsec above the AR on the
limb (close to the AR core)
-- run PRY_slot_contextLITE (ID #354); Study A
-- run Hot_loop_osci_1_v2 (ID #417); Study B, repeating for up to 5 hrs
-- run PRY_slot_contextLITE (ID #354); Study A
-- run Hot_loop_osci_2_v2 (ID #418); Study C, repeating for up to 5 hrs
-- run PRY_slot_contextLITE (ID #354); Study A
-- runs can be done in two parts: A B A as one part and A C A as the second part.
-- each sequence above should be run uninterrupted (preferably use chained studies)
-- for Study A, 1/3 FOV on the disk and 2/3 FOV off the limb.
-- for Studies B and and C, the slit center position is set about 30-50 arcsec above the AR on the
limb (close to the AR core)
-- run PRY_slot_contextLITE (ID #354); Study A
-- run Hot_loop_osci_1_v2 (ID #417); Study B, repeating for up to 5 hrs
-- run PRY_slot_contextLITE (ID #354); Study A
-- run Hot_loop_osci_2_v2 (ID #418); Study C, repeating for up to 5 hrs
-- run PRY_slot_contextLITE (ID #354); Study A
-- runs can be done in two parts: A B A as one part and A C A as the second part.
-- each sequence above should be run uninterrupted (preferably use chained studies)
| Study ID | Acronym | ||
|---|---|---|---|
| 354 | PRY_slot_contextLITE | details | Example fits |
| 417 | Hot_loop_osci_1_v2 | details | Example fits |
| 418 | Hot_loop_osci_2_v2 | details | Example fits |
D. Synoptic and Other Studies
#
syo20100504-01 => EIS Spectral Atlas Synoptic Programme#
– Young (pyoung@ssd5.nrl.navy.mil), Warren, Mason, Del Zanna
-- run twice each month; in the first and third full weeks of the month
-- run PRY_slot_context_v3; Duration: 3min 29s; Data volume: 5 Mbit
-- follow with either Atlas_30s (34min, 257 Mbit), or Atlas_60s (65min, 257 Mbit)
-- pointing to be specified by email to CO at start of observing week by P. Young
-- in absence of specific target, CO is free to choose any solar feature on- or off-disc
-- *NOTE: use Atlas_30s only if an AR is forecast to produce M-class or greater flares; use Atlas_60s for all other targets*
-- run PRY_slot_context_v3; Duration: 3min 29s; Data volume: 5 Mbit
-- follow with either Atlas_30s (34min, 257 Mbit), or Atlas_60s (65min, 257 Mbit)
-- pointing to be specified by email to CO at start of observing week by P. Young
-- in absence of specific target, CO is free to choose any solar feature on- or off-disc
-- *NOTE: use Atlas_30s only if an AR is forecast to produce M-class or greater flares; use Atlas_60s for all other targets*
| Study ID | Acronym | ||
|---|---|---|---|
| 353 | PRY_slot_context_v3 | details | Example fits |
| 403 | Atlas_30 | details | Example fits |
| 404 | Atlas_60 | details | Example fits |
syo20100713-02 => Full CCD Study to Measure Relative Wavelengths#
– Warren (hwarren@nrl.navy.mil)
-- run HPW020_VEL_FULLs1 (ID # 413)
-- full CCD sit-and-stare study; Duration: 45 min; Data volume: 243 Mbits.
-- prefer run above limb on AR 11087; EIS pointing: x = R_Sun + 15 arc sec, y = 0
-- full CCD sit-and-stare study; Duration: 45 min; Data volume: 243 Mbits.
-- prefer run above limb on AR 11087; EIS pointing: x = R_Sun + 15 arc sec, y = 0
| Study ID | Acronym | ||
|---|---|---|---|
| 413 | HPW020_VEL_FULLs1 | details | Example fits |
E. Test and Calibration Studies
#
test-01 => EIS slit calibration#
– Young (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_v2 (ID # 389)
-- 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_v2 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: 35 Mbits
-- duration: 56m.
-- run CALIB_slit_slot_v2 (ID # 389)
-- 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_v2 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: 35 Mbits
-- duration: 56m.
| Study ID | Acronym | ||
|---|---|---|---|
| 389 | CALIB_slit_slot_v2 | details | Example fits |
test-02 => EIS velocity calibration#
– Kamio (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.
-- 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.
| Study ID | Acronym | ||
|---|---|---|---|
| 375 | SK_DEEP_5x512_SLIT1 | details | Example fits |
| 376 | SK_DEEP_5x512_SLIT2 | details | Example fits |
test-03 => EIS Slot Deconvolution Test#
– Sun (js2@mssl.ucl.ac.uk)
-- Develop method to deconvolve EIS slot data
-- Two studies:
* js2_decon_slot_sc_LT (ID # 429): data volume: 3.71Mbits; duration: 1m51s
* js2_decon_ref_vel_LT (ID # 430): data volume: 87.87Mbits; duration: 47m37s
-- Instructions for planner:
- Run study (ID # 429) first, then consecutively run study (ID # 430), then run study (ID # 429) again.
- It's prefer that the slot study (ID # 429) repeats a few times,
eg. study429 (x6), study430 (x1), study429 (x6)
-- Target:
- simple active region;
- FoV to cover AR edge to detect outflows;
- both rasters to have identical pointing
-- Run during SAA-free interval preferred
-- Two studies:
* js2_decon_slot_sc_LT (ID # 429): data volume: 3.71Mbits; duration: 1m51s
* js2_decon_ref_vel_LT (ID # 430): data volume: 87.87Mbits; duration: 47m37s
-- Instructions for planner:
- Run study (ID # 429) first, then consecutively run study (ID # 430), then run study (ID # 429) again.
- It's prefer that the slot study (ID # 429) repeats a few times,
eg. study429 (x6), study430 (x1), study429 (x6)
-- Target:
- simple active region;
- FoV to cover AR edge to detect outflows;
- both rasters to have identical pointing
-- Run during SAA-free interval preferred
| Study ID | Acronym | ||
|---|---|---|---|
| 429 | js2_decon_slot_sc_LT | details | Example fits |
| 430 | js2_decon_ref_vel_LT | details | Example fits |