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(NoRH) is a radio telescope dedicated to observe the Sun. "Helio"
means the Sun, "graph" means an imaging telescope. It consists of
84 parabolic antennas with 80 cm diameter, sitting on lines of 490
m long in the east/west and of 220 m long in the north/south. Its
construction took 2 years and cost 1.8 billion yen. The first
observation was in April, 1992 and the daily 8-hours observation
has been done since June, 1992. Frequency 17GHz (Right and left
circular polarization), 34GHz (only intensity) Field of view
Solar full disk Spatial resolution 10 arcsec (17GHz), 5 arcsec
(34GHz) Temporal resolution 0.1 sec (Event), 1 sec (Steady)
As the NoRH is a radio interferometer, original data are sets of
correlation values of all the combination of antennas. They
correspond to the spatial Fourier components of the brightness
distribution of the solar disk. In most cases, it is necessary to
synthesize images from the original raw data. To maximize the data
use, we prepare images, indices and other related materials
routinely and put them on our Web page. This Web page is to help
the scientists in the world to look for interesting phenomena
detected by the NoRH and to start the actual analysis using the
original data set. Software for image synthesis and analyses are
prepared. Image synthesis and analyses can be done remotely through
the Internet. This data and images can also be used for science
education. We are glad if our images are of any help in education
at schools, universities, and public.
Nobeyama Radioheliograph
(NoRH) is a radio telescope dedicated to observe the Sun. "Helio"
means the Sun, "graph" means an imaging telescope. It consists of
84 parabolic antennas with 80 cm diameter, sitting on lines of 490
m long in the east/west and of 220 m long in the north/south. Its
construction took 2 years and cost 1.8 billion yen. The first
observation was in April, 1992 and the daily 8-hours observation
has been done since June, 1992. Frequency 17GHz (Right and left
circular polarization), 34GHz (only intensity) Field of view
Solar full disk Spatial resolution 10 arcsec (17GHz), 5 arcsec
(34GHz) Temporal resolution 0.1 sec (Event), 1 sec (Steady)
As the NoRH is a radio interferometer, original data are sets of
correlation values of all the combination of antennas. They
correspond to the spatial Fourier components of the brightness
distribution of the solar disk. In most cases, it is necessary to
synthesize images from the original raw data. To maximize the data
use, we prepare images, indices and other related materials
routinely and put them on our Web page. This Web page is to help
the scientists in the world to look for interesting phenomena
detected by the NoRH and to start the actual analysis using the
original data set. Software for image synthesis and analyses are
prepared. Image synthesis and analyses can be done remotely through
the Internet. This data and images can also be used for science
education. We are glad if our images are of any help in education
at schools, universities, and public.
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Just five years after George Ellery Hale founded the Mount Wilson
Solar Observatory with a grant from the Carnegie Institution of
Washington, designs for a long-focal-length tower telescope were
completed. In 1908, Hale discovered magnetic fields in sunspots
(using the 60-foot solar tower built in 1907) by applying the
principle of Zeeman splitting, where a spectral line will usually
be split up into several components in the presence of a magnetic
field. This was a discovery of great import. In order to study the
Zeeman splitting of sunspots more precisely, Hale needed a
telescope with a larger image scale and a spectrograph with a
greater linear dispersion than the 60-foot could provide. Because
of this, funds were provided by the Carnegie Institution of
Washington, and in 1909, the construction of the 150-foot solar
tower was begun.
Mt. Wilson
Just five years after George Ellery Hale founded the Mount Wilson
Solar Observatory with a grant from the Carnegie Institution of
Washington, designs for a long-focal-length tower telescope were
completed. In 1908, Hale discovered magnetic fields in sunspots
(using the 60-foot solar tower built in 1907) by applying the
principle of Zeeman splitting, where a spectral line will usually
be split up into several components in the presence of a magnetic
field. This was a discovery of great import. In order to study the
Zeeman splitting of sunspots more precisely, Hale needed a
telescope with a larger image scale and a spectrograph with a
greater linear dispersion than the 60-foot could provide. Because
of this, funds were provided by the Carnegie Institution of
Washington, and in 1909, the construction of the 150-foot solar
tower was begun.
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The Big Bear Solar Observatory (BBSO) exploits the excellent
climatic conditions of Big Bear Lake to study the Sun, source of
life on Earth. The observatory is located in the middle of Big Bear
Lake to reduce the image distortion which usually occurs when the
Sun heats the ground and produces convection in the air just above
the ground. Turbulent motions in the air near the observatory are
also reduced by the smooth flow of the wind across the lake instead
of the turbulent flow that occurs over mountain peaks and forests.
These conditions, combined with the usually cloudless skies over
Big Bear Lake and the clarity of the air at 2,000 meters (6,750
feet) elevation, make the observatory a premier site for solar
observations. The observatory was built by the California Institute
of Technology in 1969. Management of the observatory, and an array
of solar radio telescopes at Owens Valley Radio Observatory (OVRO)
in Owens Valley, California, was transferred to the New Jersey
Institute of Technology on July 1, 1997. Funding for the operation
of the observatory is from the National Aeronautics and Space
Administration (NASA), the National Science Foundation (NSF), the
United States Air Force, the United States Navy and other agencies.
BBSO
The Big Bear Solar Observatory (BBSO) exploits the excellent
climatic conditions of Big Bear Lake to study the Sun, source of
life on Earth. The observatory is located in the middle of Big Bear
Lake to reduce the image distortion which usually occurs when the
Sun heats the ground and produces convection in the air just above
the ground. Turbulent motions in the air near the observatory are
also reduced by the smooth flow of the wind across the lake instead
of the turbulent flow that occurs over mountain peaks and forests.
These conditions, combined with the usually cloudless skies over
Big Bear Lake and the clarity of the air at 2,000 meters (6,750
feet) elevation, make the observatory a premier site for solar
observations. The observatory was built by the California Institute
of Technology in 1969. Management of the observatory, and an array
of solar radio telescopes at Owens Valley Radio Observatory (OVRO)
in Owens Valley, California, was transferred to the New Jersey
Institute of Technology on July 1, 1997. Funding for the operation
of the observatory is from the National Aeronautics and Space
Administration (NASA), the National Science Foundation (NSF), the
United States Air Force, the United States Navy and other agencies.
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