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For detailed information, please contact kawabata @ bao.go.jp. |
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| 101 cm reflecting telescope |
| *Basic structure: |
A reflector with a Cassegrain focus (F/12)
and a Fork type equatorial mounting. |
| *Focus: |
By selecting from four focus options, five
observational modes are possible. |
| *Regulation system: |
The telescope and all other instruments
are controlled by a computer network. |
| *Optical capability: |
Hartmann constant is about 0.54 arcsec. |
| *Pointing accuracy: |
The telescope analysis has improved automatic
pointing accuracy to 6 arcsec. |
|
| Astronomical observation and astro-photography
using 101 cm reflecting telescope. |
| *Astronomical observation: |
Specific
ocular (eyepiece) with Cassegrain focus is used. |
| *Taking photos: |
1/2 scale optical Nasmyth focus is used. |
| *Taking video images: |
A
color-CCD video camera (manufactured by Ikegami)
is attached to specific eyepieces. |
|
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|
| Astronomical observation by direct imaging |
Observation by direct imaging is possible
using large format (1K) cooled CCD
(F/12 and field of view of seven arcmin) |
| *Connected optical system: |
The system is composed of a reducer (removable), filter
turret (6 colors), and the apparatus for offset guide with IICCD.
|
| *Filters: |
Filters of B, V, R, I and Hƒ¿ are available. |
| *CCD camera: |
Liquid nitrogen-cooled CCD camera (Astrocam for direct imaging),
ST-6(SBIG) or CV-16II (Mutoh) is available.
|
|
Observable range of field
| Camera |
Number of pixcel |
Pixcel size |
Field of view(F/12) |
Field of view(F/6 with reducer) |
| Astrocam |
1242x1152 |
22.5x22.5µm |
8x7.5 arcmin |
14 arcmin
(circular field)
|
| CV-16(II) |
1536x1024 |
9x9µm |
3.9x2.6 arcmin |
7.8x5.2 arcmin |
|
| Astronomical spectroscopy |
| The physical properties of celestial objects,
such as their motion and temperature, can be determined
by spectral analysis of the light radiated by
the object. A spectrograph divides the light into
component wavelengths (like a rainbow) for analysis.
|
| *Spectrograph: |
Spectrograph with a standard diffraction
grating is used. |
| *CCD camera: |
Liquid nitrogen-cooled CCD camera (Astrocam
for spectrograph) is used. |
| *Characteristics of wavelength sensitivity of spectrograph: |
It should be referred for astronomical spectroscopy. |
|
Specifications of spectrograph now in use
| Grating |
Camera |
Order |
Dispersion |
wavelength range |
λ/Δλ |
| 300 grooves/mm |
200 mm(F/3, fluorite lens) |
1 |
162 Å/mm |
4400 Å |
1500 |
| 1800
grooves/mm |
400
mm (F/6, fluorite lens) |
1 |
13
Å/mm |
360
Å |
15000 |
|
| Astronomical photometry |
| The structure of multiple stars or variable
stars is studied by measuring changes in light
intensity. |
| *Photometer: |
Photoelectric photometer with photo-multiplier
is used. High-speed photoelectric photometry is
also possible. Sub-photometer is now under adjustment. |
| *Filter: |
Filters of U, B, V, y, and b are available. |
|
| Cooled CCD cameras available: |
| The physical properties of celestial objects, such as their motion and temperature, can be determined by spectral analysis of the light radiated by the object. A spectrograph divides the light into component wavelengths (like a rainbow) for analysis. |
|
| CCD camera |
Pixel size |
Number of pixel |
Cooling system |
Note |
| *Astrocam for direct imaging |
22.5x22.5
(µm) |
1242x1152
(pixel) |
liquid nitrogen-cooled |
|
| *Astrocam for spectrograph |
27x27
(µm) |
256x1024
(pixel) |
liquid nitrogen-cooled |
UV coating |
| *CV-16II(Mutoh) |
9x9
(µm) |
1536x1024
(pixel) |
Peltier thermoelectric cooling module |
E chip |
| *ST-6(SBIG) |
23x27
(µm) |
375x242
(pixel) |
Peltier thermoelectric cooling module |
|
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