v10308u Hamamatsu Photonics, K.K.,, v10308u Datasheet - Page 2

• Manufacturer Part Number: v10308u
• Description: Image Intensifiers
• Manufacturer: Hamamatsu Photonics, K.K.,

1
Image Intensifier
Image intensifiers (often abbreviated as I. I.) were primarily developed for nighttime viewing and surveillance under
moonlight or starlight. Image intensifiers are capable of detecting and amplifying low-light-level images (weak emissions or
reflected light) for bringing them into view as sharp contrast images. Image intensifier applications have spread from
nighttime viewing to various fields including industrial product inspection and scientific research, especially when used
with CCD cameras (intensified CCD or ICCD). Gate operation models are also useful for observation and motion analysis of
high-speed phenomena (high-speed moving objects, fluorescence lifetime, bioluminescence and chemiluminescence
images). Some major image intensifier applications are introduced here.
Mitochondria inside a nerve system culture cell NG108-15, specificity -
labeled with fluorescent dye MITO TRACKER.
Very-low plasma emission occurring over an ultra-short duration can be ob-
served. (*Plasma emission is superimposed on the PDP electrode. Top left
shows elapsed time after applying a voltage to the each others electrode.
A wide variety of characteristics is presented including spectral response by choosing a photocathode and
window material combination, photocathode size, the number of MCPs (gain) and gate time. You are sure to
find the device that best matches your application from our complete lineup of standard or custom products.
GLow-light-level imaging GMulti-channel spectroscopy GHigh-speed motion analysis
GBioluminescence or chemiluminescence imaging
Feature
PDP (Plasma display panel) emission
ISpectral Response Characteristics
1
Fluorescence imaging
0.47 µs
1.09 µs
WIDE VARIATIONS
BIOTECHNOLOGY
ELECTRONICS
10
10
10
10
10
-1
100
3
2
1
0
0.71 µs
1.37 µs
APPLICATION EXAMPLE
TII B0098EC
-07
-08
200
-03
-02
-01
300
-06
-04
-05
FEATURES
400
OTHER-APPLICATIONS
-74
WAVELENGTH (nm)
500
-71
600
How soot is generated can be observed by viewing low-level scattering
light resulting from laser irradiation.
Star wind from the protostar L1551-IRS5 (red star at upper left),
twinkling in yellowish green when it collides with surrounding gases.
Photo courtesy of National Astronomical Observatory in Japan/In cooperation with NHK (Nihon Hoso Kyokai)
Soot scattering images (taken by image intensifier)
Direct flame images (taken by high-speed shutter camera)
ATDC: After Top Dead Center, θ: Crank angle with respect to ATDC
700
800
No suffix.
-09
Observing engine combustion
Celestial body observation
900
1000
QE = 0.1 %
QE = 50 %
QE = 25 %
QE = 10 %
QE = 1 %
ASTRONOMY
INDUSTRY
1100
NOTE:
Gate operation types may
have slightly lower sensitivi-
ty in the ultraviolet region.