OVRO Solar Array
Contact: Dale E. Gary, NJIT
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)

 
Big Bear Solar Observatory
Contact: Haimin Wang, NJIT or Bill Marquette, BBSO
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

 
Siberian Solar Radio Telescope
Contact: Alexander Altyntsev, SSRT
Type of Observation: Goals: Instrument Setup:
Active region imaging Obtain microwave images of the full Sun and to determine temporal evolution of coronal temperature and distribution of circular polarization in the active region before the flare. Daily, 5.72 GHz, Stokes I and V, 20 min time resolution, 21" spatial resolution.
Flare high time resolution imaging Study of the fragmented energy release in solar flares. Diagnostics of plasma parameters in flare loops. During flares: One dimensional scans of the full Sun disk  with time resolution down to 14 ms (Stokes I and V). Two dimensional images of flare region with time resolution down to fractions of min.

 
IZMIRAN
Contact: Boris Ioshpa, IZMIRAN
Type of Observation: Goals: Instrument Setup:
Active region measurements Observe simultaneously the longitudial magnetic fields and radial velocity in the FeI 5253A line and  the radial velocity in
nonmagnetic FeI 5567A line. Obtain some magnetic and velocity maps throughout the day with the rate one map per half hour - one hour (rate depends on size of region and number of maps), provide analyzed magnetogram data for extrapolations.
 Longitudial magnetograph taken in Fe I (5253 A),  one magnetogram and velocity map (with the compensation of 5-min oscillations) every half hour;  tachometer in the nonmagnetic FeI 5567A line.

 
Kitt Peak (National Solar Observatory)
Contact: Jack Harvey, NSO
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)

 
Marshall Space Flight Center
Contact: Mona Hagyard, MSFC
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
Contact: Jean-Marie Malherbe, Observatoire de Paris
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

 
Alfred University H-alpha Video System
Contact: F. David Toot, Alfred U
Type of Observation: Goals: Instrument Setup:
Active region and flare high time resolution imaging Study chromospheric response to electron precipitation at high time resolution Field of view 10x10 arcmin. H-alpha center line imaging at video cadence, using 0.6 A filter.

 
RATAN 600 Radiotelescope
Contact: Vladimir Bogod, Ratan
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.

 
Nobeyama Radioheliograph
Contact: Kiyoto Shibasaki, NRO
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

 
HAO Mauna Loa Observatory
Contact: Joan Burkepile, HAO
Type of Observation: Goals: Instrument Setup:
Full-disk/limb/coronal images Obtain coronal structure and large-scale eruptions/restructuring associated with flares/CMEs Halpha disk and limb images (every 3 minutes between
~17:00 and 22:00) and white light coronal images (~1.1 to 2.7 Rsun every 3 minutes)

 
Nançay Radioheliograph
Contact: Nicole Vilmer, Meudon
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

 
Kharkov Astronomical Observatory
Contact: Gennady Marchenko, Kharkov State U
Type of Observation: Goals: Instrument Setup:
Active region and flare in the He 10830 and Balmer continuum To obtain images in the He 10830 and Balmer continuum during of flare evolution. Full disk images with ~8" resolution in He 10830 and Balmer continuum and precontinuum; one image every 5-10 minutes.

 
Crimean Astrophysical Observatory
Contact: N.N. Stepanian, CRAO
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

 
National Astronomical Observatory of Japan, Mitaka/Tokyo
Contact: Takashi Sakurai, NAOJ
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.

 
Oporto Radiospectrograph
Contact: A. S. de Magalhaes, U Porto
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

 
Hiraiso Solar Terrestrial Research Center
Contact: Maki Akioka, NRC
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. 

 
Trieste Astronomical Observatory
Contact: Mauro Messerotti, TAO
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

 
Mees Solar Observatory
Contact: Barry Labonte, Mees Solar Obs, IfA
Type of Observation: Goals: Instrument Setup:
Active region and flare measurements Record the evolution of magnetic fields and structure.  If major flares occur, spectral diagnostics of chromospheric heating. IVM vector magnetic field movies (2 min. cadence, 0.5 arcsec pixels, 4.5 x 4.5 arcmin FOV) MCCD H-alpha imaging spectra, using the KPR01 program to study preflare and eruptive events if the major flare probability stays low, but switching to the JPW05 program if major flares are likely. These have similar spectral and spatial resolutions, but JPW05 uses a smaller FOV to gain higher cadence.

 
San Fernando Observatory
Contact: Gary Chapman, CSUN
Type of Observation: Goals: Instrument Setup:
Active region imaging Obtain vector magnetic field measurements in photosphere Vector magnetic fields measured with the VSSHG

 
Hida Observatory
Contact: Hiroki Kurokawa, Kyoto University
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

 
PHOENIX Radio Spectrometer
Contact: Arnold Benz, ETH, Zurich
Type of Observation: Goals: Instrument Setup:
Full-disk, high time resolution, broadband spectral radiopolarimetric observations Coherent radio emissions of energy release (e.g. spikes) and of propagating and trapped electrons.  Diagnostics of the acceleration process and of the plasma of propagation and trapping. Daily 0430 - 1600 UT: 200 - 800 MHz; Daily 1630 - 1900 UT: 0.9 - 4.0 GHz

 
Ondrejov Observatory
Contact: Petr HEINZEL or  Karel JIRICKA Ondrejov Obs
Type of Observation: Goals: Instrument Setup:
Active region and flare high cadence optical spectroscopy Chromospheric response to particle-beams precipitation at high temporal resolution, heating and flows at different chromospheric layers Multiline optical spectrograph, range from Ca II H+K up to H-alpha. Video mode: CCD video-cadence (25 frames/sec) spectra in H-alpha, D3 (or H-beta) and Ca II 8542 lines plus 0.5 A H-alpha video cadence filtrograms. Full spectrum mode: 5 cameras covering many chromospheric and photospheric lines, time resolution down to a few sec (on film) plus video H-alpha 0.5 A slit-jaw filtergrams. Both modes can run simultaneously
Whole-Sun radio spectra and flux measurements Energy release signatures in flares with emphasis on spikes and type III bursts, shock waves, and particle beam acceleration. Analysis of effects of particle beams' bombardment of solar atmosphere layers and the study of these
layers' responses in comparison with optical (H-alpha) and X-ray observations
Daily single frequency flux at 3 GHz with 10 ms time resolution.  Spectra 0.8-2.0 and 2.0-4.4 GHz, each with 256 frequency channels and 100 ms time resolution.  Only flares are archived - for list and gif see our web page
sunkl.asu.cas.cz/~radio

 
Sac Peak Coronal Photometer
Contact: Dick Altrock, NSO
Type of Observation: Goals: Instrument Setup:
Active region coronal emission line imaging Obtain coronal temperature Daily observations of the corona above the limb with the Emission Line Coronal Photometer in Fe XIV, Fe X and Ca XV

 
Very Large Array Radiotelescope
Contact: Rob Willson, Tufts University
Type of Observation: Goals: Instrument Setup:
Burst dual-frequency radio imaging Image nonthermal bursts associated with underlying activity Friday, June 18 about 2030-0030 UT using the 74 and 327 MHz systems at the VLA.  Full disk coverage.

 
Brazilian Solar Spectroscope
Contact: Francisco Fernandes, INPE
Type of Observation: Goals: Instrument Setup:
Broadband spectral radio observations Observations of radio emissions, in particular decimetric bursts and fine structures (type III, spikes, patches) as a diagnostics of the particle acceleration process and of  plasma emission. Full disk, high time and spectral resolutions, with 9 m diameter antenna, in the interval 200-2500 MHz, with rrequency resolution 3 MHz and time resolution: 10 - 1000 ms.

 
Kanzelhoehe Solar Observatory
Contact: Wolfgang Otruba, KSO, or Michael Steinegger, Univ. Graz
Type of Observation: Goals: Instrument Setup:
Full-disk H-alpha imaging and full-disk magnetograms Obtain full-disk H-alpha images and full-disk magnetograms for monitoring the activity level of the Sun With the solar patrol telescope H-alpha images (656 nm) are obtained at least once every day if weather permits (a cadence of 1 minute is planned for the future ). A temperature-controlled Lyot-filter (FWHM=0.07 nm) and a 1K x 1K CCD camera (8 bit) are used. Full-disk magnetograms are obtained at least once per day with the magneto-optical filter (MOF) operated in the Na-D line. Image size is 512 x 512 pixels (2 bytes).

 
Kodaikanal Observatory
Contact: K. M. Hiremath, Indian Institute of Astrophysics
Type of Observation: Goals: Instrument Setup:
Flaring active region Monitor sunspot motion associated with flares; monitor chromospheric activity in H-alpha & Ca-IIK line Photoheliograph in white light at time resolution of every one hour with the help of 6 inch refraction telescope and spectroheliograph in H-alpha & Ca-IIK line center with 1 min time resolution