BasyouhuC200005(D) ver.1.00 SD Japanese Special Discretionary Time RCP in May (to Aug.), 2000

2. Schedule file

3. Test running, please...

	After reading the explanation of the sounding mode below,
	please run this RCP before the May. DT(May 3) if possible
	although only a few DT days left before them(or no days left...).
	Please test this RCP with the 2 options, -df and -nf
	at your radar site.
	(It's good enough for this RCP to run just for 10 to 15 min or so.)
	And please report any problem to me ASAP if any.
	Please make sure again that you specify '-df' and '-nf'
	options for your test run as describled above.
	You can see display task's display or 'errlog' file to check
		if intt is correct or not, and
		if beam sequence and freqency setting are correct or not.
	This RCP will output time/bmnum/start_freq/scan for each beam 
	in errlog file ONLY IF you specify higher verbose level
	by '-v N' (N=2,3,4...) command line option to this RCP(default:N=1).

	Many thanks for your great efforts to check and run this RCP!!

4. Sounding mode

	This BasyouhuC200005 is a modified version of Basyouhu scan
	which ran for our Special Time in Feb.,1998, Jan. to Aug., 1999,
	and Jan. to Mar., 2000.
	(If any of you cannot perform intt=3 on your radar, let me know soon.)
	For most radars for most days, various Basyouhu scans will be made
	to get (1 to) 3 high time resolution special camping beams data with
	optimized high time resolution global convection data simultaneously.
	intt=3sec,frang=180km,mpinc=2400,rsep=45km as usual,
	but no GPS synchronization.
	(If intt=4sec is much much better than intt=3sec to get much echoes,
	 please don't hesitate to change it by -it option...)

	CP=5249

	Detailed beam sequences for all the radars will be shown below...

5. Beam sequence

	Each beam sequence for each radar is almost completely different
	from ones for the other modes/radars.

	I try to summarize all the sequences here...

###############################################################################
===============================================================================
Kodiak:forward scan :rsep=45,intt=3 spec= 8      w/ global scan(sb=1 eb=15)
					8 just for a center beam
    1, 8,5, 8,9, 8,13, 8,3, 8,7, 8,11, 8,15, 8,2, 8,6, 8,10, 8,14,8,4, 8,12, 8
 (N 1,   5,   9,   13,   3,   7,   11,   15,   2,   6,   10,   14,  4, 8,12   )
 (S    8,   8,   8,    8,   8,   8,    8,    8,   8,   8,    8,   8,   8,    8)
===============================================================================
Sas   :forward scan :rsep=45,intt=3 spec= 10     w/ global scan(sb=1 eb=15)
					10 for RIT
    1,10,5,10,9,10,13,10,3,10,7,10,11,10,15,10,2,10,6,10,14,10,4,10,8,10,12,10
 (N 1,   5,   9,   13,   3,   7,   11,   15,   2,   6,10,14,   4,   8,   12   )
 (S   10,  10,  10,   10,  10,  10,   10,   10,  10,  10,   10,  10,   10,  10)
===============================================================================
PrinceGeorge : NotReadyYet...
===============================================================================
Kap   :backward scan:rsep=45,intt=3 spec= 6      w/ global scan(sb=14 eb=0)
					6 for RIT
    14, 6,10, 6,2, 6,12, 6,8, 6,4, 6,0, 6,13, 6,9, 6,5, 6,1, 6,11, 6,7, 6,3, 6
 (N 14,   10, 6,2,   12,   8,   4,   0,   13,   9,   5,   1,   11,   7,   3,  )
 (S     6,    6,   6,    6,   6,   6,   6,    6,   6,   6,   6,    6,   6,   6)
===============================================================================
Goose :forward scan :rsep=45,intt=3 spec= 2,11   w/ global scan(sb=0 eb=15)
					2 for SPA, 11 for STF
    0,11,4, 2,8,11,12, 2,6,11,10,2,14,11,1, 2,5,11,9, 2,13,11,3, 2,7,11,15, 2
 (N 0,   4,   8,   12, 2,6,   10,  14,   1,   5,   9,   13,   3,   7,11,15   )
 (S   11,   2,  11,    2,  11,   2,   11,   2,  11,   2,   11,   2,  11,    2)
===============================================================================
IceW  :backward scan:rsep=45,intt=3 spec= 5,6    w/ global scan(sb=15 eb=0)
					5(or4) for SPA, 6 for STF
    15, 6,11, 5,7, 6,3, 5,13, 6,9, 5,1, 6,14, 5,10, 6,2, 5,12, 6,8, 5,4, 6,0, 5
 (N 15,   11,   7,   3,   13,   9, 5,1,   14,   10, 6,2,   12,   8,   4,   0   )
 (S     6,    5,   6,   5,    6,   5,   6,    5,    6,   5,    6,   5,   6,   5)
===============================================================================
IceE  :forward scan :rsep=45,intt=3 spec= 2,4,6  w/ global scan(sb=0 eb=14)
					4 for ZHO, (5 for LYR)
     0, 2, 8, 4,12, 6,10, 4,14, 2, 1, 4, 5, 6, 9, 4,13, 2, 3, 4, 7, 6,11, 4
 (N  0,    8, 4,12, 6,10,   14, 2, 1,    5,    9,   13,    3,    7,   11   )
 (S     2,    4,    6,    4,    2,    4,    6,    4,    2,    4,    6,    4)
===============================================================================
Fin   :backward scan:rsep=45,intt=3 spec= 2,4,6  w/ global scan(sb=14 eb=0)
					4(or5) for ZHO (9 for LYR)
    14, 2,10, 4,12, 6, 8, 4, 0, 2,13, 4, 9, 6, 5, 4, 1, 2,11, 4, 7, 6, 3, 4
 (N 14, 2,10,   12, 6, 8, 4, 0,   13,    9,    5,    1,   11,    7,    3,  )
 (S     2,    4,    6,    4,    2,    4,    6,    4,    2,    4,    6,    4)
===============================================================================
###############################################################################
===============================================================================
Halley:forward scan :rsep=45,intt=3 spec= 1,3,6  w/ global scan(sb=0 eb=14)
					3 for SPA (12 for STF)
     0, 1, 4, 3, 8, 6,12, 3, 2, 1,10, 3,14, 6, 5, 3, 9, 1,13, 3, 7, 6,11, 3
 (N  0,    4,    8,   12,    2,   10,   14, 6, 5,    9, 1,13,    7,   11, 3)
 (S     1,    3,    6,    3,    1,    3,    6,    3,    1,    3,    6,    3)
===============================================================================
Sanae :backward scan:rsep=45,intt=3 spec= 7,5,3  w/ global scan(sb=15 eb=1)
					5 for SPA (12 for STF)
    15, 7,11, 5,13, 3, 9, 5, 1, 7,14, 5,10, 3, 6, 5, 2, 7,12, 5, 8, 3, 4, 5
 (N 15, 7,11,   13, 3, 9, 5, 1,   14,   10,    6,    2,   12,    8,    4   )
 (S     7,    5,    3,    5,    7,    5,    3,    5,    7,    5,    3,    5)
===============================================================================
SyowaS:backward scan:rsep=45,intt=3 spec= 5,3,1  w/ global scan(sb=14 eb=0)
					3 for SPA (4 for STF)
    14, 5,10, 3, 6, 1, 2, 3,12, 4, 8, 3, 4, 1, 0, 3,13, 5, 9, 3,11, 1, 7, 3
 (N 14,   10,    6,    2,   12,    8,    4,    0,   13, 5, 9,   11, 1, 7, 3)
 (S     5,    3,    1,    3,    5,    3,    1,    3,    5,    3,    1,    3)
===============================================================================
SyowaE:forward scan :rsep=45,intt=3 spec= 5,7,9  w/ global scan(sb=0 eb=14)
					7 for ZHO (9 for LYR)
     0, 7, 4, 5, 8, 7,12, 9, 2, 7, 6, 5,10, 7,14, 9, 1, 7,13, 5, 3, 7,11, 9
 (N  0,    4,    8,   12,    2,    6,   10,   14, 9, 1,   13, 5, 3, 7,11   )
 (S     7,    5,    7,    9,    7,    5,    7,    9,    7,    5,    7,    9)
===============================================================================
Kerg. :backward scan:rsep=45,intt=3 spec= 4,6,8  w/ global scan(sb=14 eb=0)
					6 for ZHO (10 for LYR)
    14, 8,10, 6, 2, 4,12, 6, 0, 8,13, 6, 9, 4, 5, 6, 1, 8,11, 6, 7, 4, 3, 6
 (N 14,   10, 6, 2, 4,12,    0, 8,13,    9,    5,    1,   11,    7,    3   )
 (S     8,    6,    4,    6,    8,    6,    4,    6,    8,    6,    4,    6)
===============================================================================
TigerT:backward scan:rsep=45,intt=3 spec= 5,7,9  w/ global scan(sb=14 eb=0)
					5 for DRV (11 for another cusp region)
 #ifdef BACKWARDS
TigerT:backward scan:rsep=45,intt=3 spec= 5,7,9  w/ global scan(sb=14 eb=0)
    14, 7,10, 9, 6, 7, 2, 5,12, 7, 8, 9, 4, 7, 0, 5,13, 7, 1, 9,11, 7, 3, 5
 (N 14,   10,    6,    2,   12,    8,    4,    0, 5,13,    1, 9,11, 7, 3   )
 (S     7,    9,    7,    5,    7,    9,    7,    5,    7,    9,    7,    5)
 #else
TigerT:forward scan :rsep=45,intt=3 spec= 5,7,9  w/ global scan(sb=0 eb=14)
     0, 7, 4, 5, 8, 7,12, 9, 2, 7, 6, 5,10, 7,14, 9, 1, 7,13, 5, 3, 7,11, 9
 (N  0,    4,    8,   12,    2,    6,   10,   14, 9, 1,   13, 5, 3, 7,11   )
 (S     7,    5,    7,    9,    7,    5,    7,    9,    7,    5,    7,    9)
 #endif
===============================================================================
###############################################################################

  * N : will (be able to) be treated as normal beams
  * S : will (be able to) be treated as special beams

6. Notes

'vlptm' is now not good for any beam sequences which include camping beams.
This is because vlptm regards any beams with scan!=0 as start_beam
which means any special camping beam whose scan value is negative
will be regarded as a start_beam and which is meaningless.
If you change vlptm code a bit you might get much more proper vec files
for some of special programs including Basyouhu...
A line 277 in vlptm.c both in Radops2000 version 4.01 and version 4.10,
	if (scan && (bmbak != -1)) { ....
shuold be modified to
	if ((scan==1) && (bmbak != -1)) { ....
(or	if ((scan>0) && (bmbak != -1)) { ....   (this is my favorite...)).
I strongly recommend you to adopt this fix
to get proper vec files even when we do any other mode than normal_scan.
(before grid files officially become used for the ISTP KP data
 or before next Radops is available.)
How do Mike and Rob think about this?

7. SuperDARN time allocation request
sent to SD scheduling working group

> Date: Mon, 6 Mar 2000 17:50:56 +0900
> To: darn-swg
> From: Natsuo Sato
> Subject: NIPR SD request (May)

Dear Catherine and Scheduling WG,

Thanks for your arrangement of SuperDARN scheduling.
I am attaching here the NIPR requests for Time Allocation in May.
One request is the DT request, and the other is the operation period 
when High Time Common Mode will run.

NIPR is planing that the same request will apply in June, July and August 
during austral winter season.

Best regards,
Natsuo

########################
# ==== Request -1 ==== #
########################

SUPERDARN TIME ALLOCATION REQUEST (from NIPR: No1)

MONTH:	May 2000

PERIOD (DATES, TIMES):
	4 days requested.
	Best optical observing conditions at S. Pole, Zhongshan and AGOs 
	in Antarctica are 1-9 and 27-31 May around new moon periods 
	(new moon is 4 May and 2 June)
	Note that the same request will apply in June, July and August.

RADARS:	Syowa South, Syowa East, Kerguelen, Halley, Sanae and Tiger in the 
	southern hemisphere and CUTLASS in the northern hemisphere.

CLASS (Special time, Discretionary time): DISCRETIONARY

INSTITUTE: 
	NIPR/BAS/ Univ.Natal/CNRS/ La Trobe Univ./ Univ. Leicester 

PI:	N. Sato

SCIENTISTS: 
	N. Sato, H. Yamagishi, A. S. Yukimatu, M. Watanabe, 
	M. Pinnock, D. Walker, Jean-Paul Villain, Jean-Claude CERISIER, 
	Peter L Dyson and Mark Lester

COLLABORATORS (Outside of SD): 
	M. Ejiri, S. Okano, M. Taguchi and M. Okada (NIPR; S. Pole Optical) 
	+ R. Liu & H. Yang (Chinese Polar Institute; Zhongshan Digisonde 
	and Optical) + Antarctic AGO experimenters.

PROGRAMME TITLE: 
	Study on the radar and optical signatures of the dayside phenomena 
	in the cusp region and their geomagnetic conjugacy

SCIENTIFIC CASE: 
	The field of view of Syowa South, Halley and Sanae radars cover over 
	South Pole Station, where NIPR's and AGO's monochromatic all-sky 
	auroral imagers are working. Syowa East and Kerguelen radars cover 
	over Chinese Zhongshan Station, where NIPR's all-sky CCD camera 
	(6300 or 5577 A), panchromatic all-sky camera and scanning photometers 
	(6300, 5577 and 4278 A) and Chinese Digisonde are operating. Both of 
	South Pole and Zhongshan are located at the cusp region (~75 degree), 
	but about 6 hours different in MLT. The Tiger radar, which covers more 
	equatorward and more different local time from other southern 
	hemisphere SuperDARN radars, provides the relationship between 
	dayside and nightside phenomena. 
	Quasi-periodic (QP) variations of optical aurora are the outstanding 
	characteristics in the dayside cusp region. The mechanism of such 
	quasi-periodic variation is still an open question. The candidate 
	mechanism would be MHD wave, FTE, plasma pressure pulse, etc. 
	Simultaneous observations of optical aurora with monochromatic 
	wavelength and radar aurora are very important method to solve this 
	problem. Coordinated observations with HF radars in both hemispheres, 
	all-sky imagers and digisonde at different local time would clarify 
	the IMF dependence, propagation characteristics and local time 
	dependence for such quasi-periodic phenomena.
	The observations from the conjugate regions (Syowa East-Kerguelen and 
	CUTLASS over Zhongshan) are very valuable for this scientific aim; 
	for example, the time difference between the two hemispheres in the 
	response to an IMF Bz, By and Bx changes.

EXPERIMENT OBJECTIVES:
	High time resolution velocity for one to three beams from each radar 
	crossing over S. Pole, Zhongshan and AGOs and its conjugate region. 
	Background flow conditions with full beam scans with higher time 
	resolution. This operation enables us to compare the spatial and 
	temporal variations between radar and optical auroras. 

REASONS FOR TIME PERIOD REQUESTED
(Supporting campaigns, instrumentation, geophysical conditions): 
	Optimum conditions for S. Pole, Zhongshan and AGOs optical observation 
	during new moon periods (new moon in May is 4).

COULD EXPERIMENT BE RUN AT ANOTHER TIME (YES/NO): 
	NO (it is possible to shift within following period)
	No moon light interference periods are 1-10 and 27-31 May and a new 
	moon is 4 May. Therefore the best period is the 4 days around 4 May.

RADLANG PROGRAMMES TO BE RUN AND BRIEF DESCRIPTION OF SOUNDING MODE:
	All radars run one to three camping beam (high time resolution) 
	with global scan.

= END OF FORM =

#########################################################
# ====== REQUEST-2  (Additional request from NIPR) ==== #
#########################################################

SUPERDARN TIME ALLOCATION REQUEST (Additional request from NIPR)

	** Though this is a Common mode allocation request, 
	   I (NIPR) want to arrange SWG to allocate the High Time Common Mode 
	   during the following period if it is possible ****

MONTH:	May 2000

PERIOD (DATES, TIMES): 
	4 days requested as High Time Resolution Common Mode (4 days period is 
	a standard duration as HTR, in my understanding).
	The periods of the best optical observing conditions over Antarctica 
	are 1-10 and 27-31 May around new moon periods (new moon is 4 May)
	(Note that the same request will apply in June, July and August.)

RADARS:	All SuperDARN radars

CLASS (Special time, Discretionary time): 
	High Time Resolution Common Mode.

INSTITUTE: All

PI:	All PI (proposed by N. Sato)

COLLABORATORS (Outside of SD): 
	M. Ejiri, S. Okano, M. Taguchi and M. Okada (NIPR; S. Pole Optical) 
	+ R. Liu & H. Yang (Chinese Polar Institute; Zhongshan Digisonde and 
	Optical) + Antarctic AGO experimenters.

PROGRAMME TITLE: 
	Study on the radar and optical signatures of the dayside phenomena 
	in the cusp region and their geomagnetic conjugacy

SCIENTIFIC CASE: 
	The field of view of Syowa South, Halley and Sanae radars cover over 
	South Pole Station, where NIPR's and AGO's monochromatic all-sky 
	auroral imagers are working. Syowa East and Kerguelen radars cover over
	Chinese Zhongshan Station, where NIPR's all-sky CCD camera (6300 or 
	5577 A), panchromatic all-sky camera and scanning photometers (6300, 
	5577 and 4278 A) and Chinese Digisonde are operating. Both of South 
	Pole and Zhongshan are located at the cusp region (~75 degree), but 
	about 6 hours different in MLT. The Tiger radar, which covers more 
	equatorward and more different local time from other southern 
	hemisphere SuperDARN radars, provides the relationship between dayside 
	and nightside phenomena. 
	Quasi-periodic (QP) variations of optical aurora are the outstanding 
	characteristics in the dayside cusp region. The mechanism of such 
	quasi-periodic variation is still an open question. The candidate 
	mechanism would be MHD wave, FTE, plasma pressure pulse, etc. 
	Simultaneous observations of optical aurora with monochromatic 
	wavelength and radar aurora are very important method to solve this 
	problem. Coordinated observations with HF radars in both hemispheres, 
	all-sky imagers and digisonde at different local time would clarify 
	the IMF dependence, propagation characteristics and local time 
	dependence for such quasi-periodic phenomena.
	The observations from the conjugate regions (Syowa East-Kerguelen and 
	CUTLASS over Zhongshan) are very valuable for this scientific aim; 
	for example, the time difference between the two hemispheres in the 
	response to an IMF Bz, By and Bx changes.

EXPERIMENT OBJECTIVES:
	The operation of full beam scan with higher time resolution (High Time
	Resolution Common Mode) can be possible to compare the spatial and 
	temporal variation between radars and optical auroras and their 
	geomagnetic conjugacy. 

REASONS FOR TIME PERIOD REQUESTED 
(Supporting campaigns, instrumentation, geophysical conditions): 
	Optimum conditions for S. Pole, Zhongshan and AGOs optical observation 
	during new moon periods (new moon in May is 4).

COULD EXPERIMENT BE RUN AT ANOTHER TIME (YES/NO): 
	NO (but it is possible to shift within following period)
	No moon light interference periods are 1-10 and 27-31 May. 

RADLANG PROGRAMMES TO BE RUN AND BRIEF DESCRIPTION OF SOUNDING MODE:
	All radars run with High Time Resolution Common Mode.

== END OF FORM ==

8. Explanation of sounding mode (2)

> Date: Wed, 19 Apr 2000 12:57:32 -0700
> From: Natsuo Sato
> Subject: Summary of May DT

Dear PIs of all of the Southern Hemisphere and CUTLASS radars,
(M. Pinnock, D. Walker, Jean-Paul Villain, Jean-Claude CERISIER, 
Peter L Dyson and Mark Lester-sama)

Thanks for your (Mike, Mark and Peter-san's) suggestion and approval 
about the proposal of NIPR May DT plan.
In order to arrange the RCP by Sessai for this experiment soon, 
I want to summarize the plan in the followings. 
If you have comment and suggestion, please tell me as soon as possible.

1) Summary of the special beams at each station

	All radars run three camping beams with global scan.
	The special beam N at each station is as follows;

	Syowa East: N=7, N-2, and N+2
	Syowa South: N=3, N-2, and N+2
	Kerguelen: N=6, N-2, and N+2
	Halley: N=3, N-2, and N+3 (!!)
	Sanae: N=5, N-2, and N+2
	Tiger: N=7, N-2, and N+2
	Iceland East: N=4, N-2, and N+2
	Finland: N=4, N-2, and N+2
 
	where N is the highest time resolution beam (may be 12-sec 
	sampling time with 3-sec integration) which is directed over 
	Zhongshan and South Pole or their conjugate point except Tiger. 
	On the other hand, N-2/N+2 or N+3 are the beams with the second 
	highest time resolution (24-sec sampling with 3-sec integration).

2) The RCP operates with Basyohu.

3) Priority for the usage for this DT data
	Each PIs of this collaboration is available to use own data 
	immediately and freely, I believe.

	(As Mike-san pointed out, the SuperDARN agreement is a problem for 
	 such collaborative DT project. That is, the SD agreement says that 
	 the PI of the radar has sole use of DT period data for 4 years.
	 But of course I am not the PI of other radars who has made the 
	 request for this DT period, for me!!).
	This issue may be discussed at coming SD workshop.

Thanks for your collaboration.

Best wishes,
Natsuo



That's it.
Many thanks in advance!

Regards,
Sessai