Crimean Astrophysical Observatory
Type of Observation:	Goals:	Instrument Setup:
Active region imaging/measurements	Obtain daily full-disk solar magnetograms seen in chromosheric Na D1-D2 lines, and monitoring of the solar velocity and brightness with 30-second cadence; Obtain daily images of active regions in the HeI line 1083nm and spectra  in  the  range  390-1084 nm to study physical conditions in active regions before and after solar flares.	Regular observations with magneto-optical filter in Na D1-D2 lines, spatial resolution 4.5 arcsec, time resolution 30 seconds; Echelle  spectrograph  for  spectral range 390-660 nm and spectrophotometer for infrared observations.
Flare high resolution imaging	Study nature of linear polarization of H-alpha flare emission	Spectral (and may be monochromatic) observations with linear polarization analyzer

 

OVRO Solar Array
Type of Observation:	Goals:	Instrument Setup:
Active region multi- frequency imaging	Obtain coronal temperature, emission measure, and magnetic field measurements (with ~ 15" resolution)	daily, 43 frequencies, 1-18 GHz, dual polarization, 12 s time resolution, 10 baselines
Flare multifrequency imaging	Determine radio emission mechanism, coronal flare location, radio spectral diagnostics of electron energy distribution and ambient plasma parameters	If flare-triggering available: auto-switch to 10-12 frequencies, 1-18 GHz, Stokes I, 2 s time resolution, 10 baselines. If no flare-triggering: use same sequence as for active regions (12 s time resolution)

 

Itapetinga Radio Observatory
Type of Observation:	Goals:	Instrument Setup:
High time resolution polarimetry	Time variations of the  polarization degree in association to the fast structures present in the intensity profiles of bursts	Instrument characteristics: frequency observation: 7 GHz, full Sun, sensitivity less than 0.5 sfu, 20 ms time resolution, circular polarization modes (R and L)

 

Kitt Peak (National Solar Observatory)
Type of Observation:	Goals:	Instrument Setup:
Active region measurements	Obtain context observations for  the campaign, and high-resolution monitoring of active region magnetic development at chromospheric heights	Regular full disk synoptic observations in the morning (1400-1700 UT -- photospheric and chromospheric magnetogram and 1083 nm spectroheliogram); high-rate chromospheric longitudinal magnetograms (rate depends on size of region)

 

Kitt Peak (National Solar Observatory)
Type of Observation:	Goals:	Instrument Setup:
Active filaments	Put active filament observations in the context of what we know from other observations about the helicity of the region and the eruption.	Scan in the red and blue wings of helium 10830 with a repeat rate of about 2 min for at least four hours per day

 

Baikal Solar Vacuum Telescope (BSVT)
Type of Observation:	Goals:	Instrument Setup:
Impact polarization in solar flares, Active region measurements	Temporal, spatial and spectral distribution of impact polarization during solar flares in H alpha; Spectropolarimetric observations of pores, filigree with high spatial and spectral resolution	BSVT - 760 mm aperture, 40 m focal length, spectrograph with two camera mirror (f1=9.5 m, f2=14m); spatial dispersion 0."24/pixel, 0."37/pixel, detector- CCD camera TEK 512*512

 

El Leoncito Solar Observatory
Type of Observation:	Goals:	Instrument Setup:
Active region and flare imaging	Obtain flare and active region observations at chromospheric heights	H-alpha imager and coronagraph; etails tbd

 

Marshall Space Flight Center
Type of Observation:	Goals:	Instrument Setup:
Active region measurements	Provide shear analyses of vector magnetograms taken near 1300 UT to aid in target selection; Obtain vector magnetograms of target active region throughout day; provide analyzed magnetogram data for extrapolations, electric current calculations; provide co-aligned H-alpha coverage of active region	Magnetograph--6x6 arcmin field of view with 3.2" resolution, taken in Fe I (5250.22 A), fastest cadence one magnetogram every 7 minutes (vector magnetograms and shear maps available on web). H-alpha, co-aligned with magnetograph, 1/2 A bandpass, 3 images per magnetograph image. Video rate recording is possible.

 

Meudon Observatory
Type of Observation:	Goals:	Instrument Setup:
Active region measurements	Obtain chromospheric context observations of active region development	Full disk observations in H-alpha center line, +0.5 A and -0.5 A, with 1 min time resolution, 2" pixel size.
Flare high time resolution spectroscopy	H-alpha line profile changes in 2D; study the dynamics of active regions and flares	Solar Tower, multichannel spectrograph with 9 simultaneous 2D channels, at 0.25 A resolution, with 8' x 5' field of view, 0.5" pixel size, 1 minute time resolution
Impact polarization	Study impact linear polarization during solar flares in H alpha	Stokes parameters integrated over the H alpha profile

 

Nobeyama Radioheliograph
Type of Observation:	Goals:	Instrument Setup:
Full-Sun active region and high time resolution flare radio imaging	Locate non-thermal electron acceleration sites and identify the acceleration machanism.  Search for phenomena in precursor phases just before impulsive onsets.	Standard observing mode: Frequency/Polarization: 17 GHz/I and V, 34 GHz/I; temporal resolution: 1 sec; FOV/HPBW: Full disk/16 arc sec (17GHz), 8 arc sec(34GHz); PFI (5 arc min.) /10 arc sec (17 GHz); and high temproal resolution mode(during bursts): temporal resolution: 100 msec

 

Trieste Astronomical Observatory
Type of Observation:	Goals:	Instrument Setup:
Full-disk, high time resolution, multifrequency radiopolarimetric observations	Analyze radio signatures of energy release fragmentation in flares, e.g. spikes, and radio signatures of flare-accelerated electron beams, such as type III bursts.  Interpret the relevant radio diagnostics of the coronal plasma, in the attempt to characterize by the former the acceleration processes and by the latter the propagation environment.	Daily, 5 frequencies (237, 327, 408, 610, 1420 MHz), circular polarization, 1 ms time resolution, no spatial resolution, two separate multichannel radiopolarimeters

 

Nançay Radioheliograph
Type of Observation:	Goals:	Instrument Setup:
Active region multi- frequency imaging at dm-m waves	Obtain multi-frequency images of the low and middle corona (0.1-0.5 Rs above the photosphere) to identify structures, trace their evolution before flares, and identify sites of electron acceleration in non-flaring active regions.	Daily imaging observations of the whole Sun at five frequencies in the range 150-450 MHz (standard setup: 164, 236.6, 327, 410, 435 MHz; change of frequencies and extension to up to ten frequencies possible).  Stokes Parameters I, V. 8 images/second. Spatial resolution between 0.3' and 6', depending on observed frequency and direction.
Flare multifrequency imaging at sub-second time resolution	Study non thermal energy release in solar flares, the sites of acceleration and the propagation of deka-keV electrons over an extended coronal height range ( 0.1-0.8 Rs above the photosphere), large-scale coronal shock waves and ejecta associated with CMEs. Provide observational constraints for particle injection into interplanetary space	Same as above

 

Big Bear Solar Observatory
Type of Observation:	Goals:	Instrument Setup:
Active region measurements	Obtain vector magnetic field measurements over entire active region with 0.5" image scale, and corresponding H-alpha coverage	10" center bench, video- magnetograph; 26" east bench, H-alpha center line
Flare high time resolution imaging	Obtain chromospheric diagnostics in H-alpha and D3, to study the chromospheric response to electron precipitation	10" east bench, fast (10 ms) He D3 observations of precipitation kernels (2.1 x 2.1 arcmin field of view); 26" benches, H-alpha center line, +0.6 A, and -0.6 A

 

National Astronomical Observatory of Japan, Mitaka/Tokyo
Type of Observation:	Goals:	Instrument Setup:
Active region measurements	Obtain vector magnetic field measurements and corresponding H-alpha and white-light images of target active regions.	The Solar Flare Telescope which is made of a video vector magnetograph and H-alpha and white light imagers. Its aligned field of view is 400"X300", with 0.66" pixel. Magnetograms are taken every 3 minutes. H-alpha images are taken every 30 seconds.

 

Hida Domeless Solar Telescope
Type of Observation:	Goals:	Instrument Setup:
Active region imaging	Study flare energy build-up processes: new flux emergence and magnetic shear developments.  Study flare trigger mechanism: new flux emergence, filament eruption	High resolution imaging with the Domeless Solar telescope (DST) H-alpha 0.0,  H-alpha +0.8, H-alpha -0.8 images: 10 G-band sunspot images: 30s cadence
Flare high time resolution imaging	Study rapid developments of electron- bombarded footpoints of flare loops.	High resolution imaging with the DST H-alpha -1.0 A and G-band images: 1/30s cadence

 

Huairou Solar Station
Type of Observation:	Goals:	Instrument Setup:
Longitudinal and vector magnetograms and velocity maps, H alpha monochromatic images	tbd	tbd

 

Hiraiso Solar Terrestrial Research Center
Type of Observation:	Goals:	Instrument Setup:
H alpha full disk doppler imaging	Obtain full disk H alpha dopplergram with 2K by 2K CCD to observe the chromospheric dynamics and filament eruption at flare and CME.	H alpha center, +0.7A, -0.7A and continuum images are taken every three minutes. Passband of Lyot filter is set at 0.25A. Close-up imaging of target active region with higher cadence is also available in parallel.

 

Sonora Solar Observatory
Type of Observation:	Goals:	Instrument Setup:
Active region and filaments imaging and CCD video recording	Obtain daily from 17 to 22 hrs UT continuous CCD video recording of active regions and filaments with 1/30 s temporal resolution and imaging at the time some event is in progress.	High resolution images in H-Alpha center line, +0.5 and -0.5 A. 1.3" pixel size on a frame of 18' X 11'.

 

RATAN 600 Radiotelescope
Type of Observation:	Goals:	Instrument Setup:
Active region radio spectra with 1D imaging	Obtain the data about temperature, emission measure, magnetic field in active region (before, during and after flare), the study of the appearence of new magnetic flux using fine polarization measurements	Daily - 35 frequencies, 0.955-16.4 GHz, V and I Stokes parameters, 3 azimuths [near 8-00UT, near 9-00 UT (meridian time) and near 10-00 UT]; special alert program - several azimuths (up to 20 with interval 8-9 minutes of time) at the same equipment.

 

Oporto Radiospectrograph
Type of Observation:	Goals:	Instrument Setup:
Radio dynamic spectrographic observations of flares	Obtain measurements of non-thermal electrons in noise storms, electron beams and accelerated at shock waves	Spectral resolution of 1 MHz and a time resolution of  60 ms, within the band 150 to 650 MHz