Subject: Re: HIGH CADENCE IMAGING CAMPAIGN Date: Thu, 11 Apr 2002 12:04:17 +0200 From: Andreas Magun Organization: IAP, University of Bern, Switzerland To: Richard Canfield CC: mbianda@irsol.ch Hallo Dick, you might be interested in the observations with a fast H-alpha camera and a fast magnetic field imager that are occasionally carried out at IRSOL in Locarno (Switzerland). The digital camera acquires 20 solar images per second with 640x480 pixels over a FOV of approx 3 arc minutes. The H-alpha camera has been built by a german group (Dr. Kuevler) and is used for solar flare observations at IRSOL by Michele Bianda. We, at Bern, are involved in data analysis and interpretation. The magnetic field imager is a project of ETHZ (Stenflo). I have forwarded your e-mail to Michele Bianda, who is doing the observations. He will contact you for more datails. kind regards Andreas On Thursday 11 April 2002 06:56, you wrote: > The RHESSI team seeks collaborators at ground-based and space-based > observatories to participate in a High Cadence Imaging Campaign. RHESSI > is capable of making high-quality hard and soft X-ray movies with a > cadence of 2 seconds (half spin) and even down to 10s of ms for intense > events, and seeks collaborators at observatories working in other > spectral bands (H-alpha, radio, EUV, continuum, ...) who can make > observations at similar cadence. > > Please contact me by telephone or e-mail to discuss imaging observations > you can achieve with a temporal cadence of at least 2-4 seconds: > > 1. What field of view can you observe at this cadence? (RHESSI sees the > full Sun, but we presume that observations will be aimed at a specific > active region chosen by the Max Millennium Chief Observer) > > 2. What spectral bandpass(es) can you observe? (RHESSI's bandpass is > limited by both detector response and source strength but usually covers > from 3 keV to 17 MeV. Thus, it is interesting to make observations over > a broad range of flare sizes from small soft X-ray B and C flares to M > and X gamma-ray flares). > > 3. In what UT time range and seasons can you observe? (RHESSI > observations are continuous, interrupted only by night in Low-Earth > Orbit and SAA). > > 4. Can you participate in a Target-of-Opportunity campaign at very short > notice, or must we pick a fixed schedule? (RHESSI would welcome > collaborators in either campaign mode, since both have unique advantaqes > and disadvantages). > > 5. If we must pick a fixed schedule, how far in advance must fixed dates > be chosen (RHESSI requires no advanced notice since it is expected to be > continuously operating in the same near-autonomous mode.) > > Of course, we are interested in non-imaging data at high cadence and > lower-cadence imaging data as well, but in response to this message I > would most urgently like to hear about the high-cadence imaging > discussed above. > > I look forward to hearing from you. > > Dick > > Department of Physics E-mail: canfield@physics.montana.edu > Montana State University Telephone: (406) 994-5581 > P.O. Box 173840 Fax: (406) 994-4452 > Bozeman, MT 59717-3840 USA http://solar.physics.montana.edu/canfield > ====================================================================== > FedEx etc: Physics Dept, EPS 264, Montana State Univ, Bozeman MT 59717 > ====================================================================== Subject: Re: HIGH CADENCE IMAGING CAMPAIGN Date: Fri, 12 Apr 2002 13:46:36 +0100 From: "Michele Bianda" To: "Richard Canfield" CC: "Philippe Jetzer" , "Gerd Dr. Kuveler" , "Prof. Jan Olof Stenflo" , "Andreas Magun" Dear Richard Canfield, Our institute (IRSOL, Istituto Ricerche Solari in Locarno, Switzerland) started observations intended to be run in parallel with HESSI. The project involves: the ETH Zurich (Jan Stenflo), the FHS Wiesbaden in Germany (Gerd K\"uveler), Bern (Andreas Magun), and us. One of our goals is to investigate the impact polarization in Ha with the ZIMPOL polarimeter (Stenflo). A flare detector system, developed at the FHS Wiesbaden, can be used to store Ha images, and probably this is what you are interested at. Andreas is involved with the elaboration of this data. For more informations on this system you can contact Gerd K\"uveler, head of the team who realised it. "Gerd Dr. Kuveler" The ZIMPOL and the FHS Wiesbaden system can work independently, but generally informations are exchanged to decide if data need to be stored or can be overwrite (a 15 minutes, or more, buffer is used). About your questions: >1. What field of view can you observe at this cadence? 640x480 pixels over a FOV of approx 3 arc minutes Ha images at a 10 to15 images/sec >2. What spectral bandpass(es) can you observe? 0.6 A at 6563 A, temperature tunable (for the moment a Day Star filter is used) >3. In what UT time range and seasons can you observe? In all seasons. The sun culminates at ~ 11:20 UT and we can observe about 12 hours in summer and about 5 hours in the shortest winter days. >4. Can you participate in a Target-of-Opportunity campaign at very short > notice, or must we pick a fixed schedule? Generally yes, but not always. The flare observations project is not the only one running at IRSOL, and the optical layout needs to be configurated for this observations. It will be possible for us to notice you: when other projects are scheduled (then no observation is possible), when we are already observing with the full system, and when could be possible to start the system after 30 - 40 minutes. One of the problems here in Locarno is related with the very small amount of personnel. > 5. If we must pick a fixed schedule, how far in advance must fixed dates > be chosen It could be possible to define observing campaigns within few weeks (2-3) in advance. IRSOL was former, till 1984, the G\"ottingen University external observatory; now it is operated by a private foundation. The 45 cm Gregory Coude Telescope in Locarno is the twilling of the VGT in Tenerife, Canary Islands. The Locarno observatory is placed at 500 m above sea level, then the seeing is not a particular god one. Please let me know if you need more informations, we are without doubt very interested to collaborate with you working on high cadence imaging projects. Yours sincerely, Michele Bianda ******************** Istituto Ricerche Solari Locarno (IRSOL) via Patocchi 6605 Locarno-Monti Switzerland e-mail: mbianda@irsol.ch Tel. + Fax: ~41 91 743 42 26 ************ Andreas Magun wrote: > > Hallo Dick, > > you might be interested in the observations with a fast H-alpha camera > and a fast magnetic field imager that are occasionally carried out at IRSOL > in Locarno (Switzerland). The digital camera acquires 20 solar images per > second with 640x480 pixels over a FOV of approx 3 arc minutes. > > The H-alpha camera has been built by a german group (Dr. Kuevler) and > is used for solar flare observations at IRSOL by Michele Bianda. We, at Bern, > are involved in data analysis and interpretation. The magnetic field imager > is a project of ETHZ (Stenflo). > > I have forwarded your e-mail to Michele Bianda, who is doing the observations. > He will contact you for more datails. > > kind regards > > Andreas > > On Thursday 11 April 2002 06:56, you wrote: > > The RHESSI team seeks collaborators at ground-based and space-based > > observatories to participate in a High Cadence Imaging Campaign. RHESSI > > is capable of making high-quality hard and soft X-ray movies with a > > cadence of 2 seconds (half spin) and even down to 10s of ms for intense > > events, and seeks collaborators at observatories working in other > > spectral bands (H-alpha, radio, EUV, continuum, ...) who can make > > observations at similar cadence. > > > > Please contact me by telephone or e-mail to discuss imaging observations > > you can achieve with a temporal cadence of at least 2-4 seconds: > > > > 1. What field of view can you observe at this cadence? (RHESSI sees the > > full Sun, but we presume that observations will be aimed at a specific > > active region chosen by the Max Millennium Chief Observer) > > > > 2. What spectral bandpass(es) can you observe? (RHESSI's bandpass is > > limited by both detector response and source strength but usually covers > > from 3 keV to 17 MeV. Thus, it is interesting to make observations over > > a broad range of flare sizes from small soft X-ray B and C flares to M > > and X gamma-ray flares). > > > > 3. In what UT time range and seasons can you observe? (RHESSI > > observations are continuous, interrupted only by night in Low-Earth > > Orbit and SAA). > > > > 4. Can you participate in a Target-of-Opportunity campaign at very short > > notice, or must we pick a fixed schedule? (RHESSI would welcome > > collaborators in either campaign mode, since both have unique advantaqes > > and disadvantages). > > > > 5. If we must pick a fixed schedule, how far in advance must fixed dates > > be chosen (RHESSI requires no advanced notice since it is expected to be > > continuously operating in the same near-autonomous mode.) > > > > Of course, we are interested in non-imaging data at high cadence and > > lower-cadence imaging data as well, but in response to this message I > > would most urgently like to hear about the high-cadence imaging > > discussed above. > > > > I look forward to hearing from you. > > > > Dick > > > > Department of Physics E-mail: canfield@physics.montana.edu > > Montana State University Telephone: (406) 994-5581 > > P.O. Box 173840 Fax: (406) 994-4452 > > Bozeman, MT 59717-3840 USA http://solar.physics.montana.edu/canfield > > =================================================================== > > FedEx etc: Physics Dept, EPS 264, Montana State Univ, Bozeman MT 59717 > > ===================================================================