TES Bolometer
Basics principles of bolometer
Bolometer is a thermal detector which absorbs photons and converts their energy to heat, which is detected by a very sensitive (resistance)
thermometer.
● Thermometer and absorber are connected
to heat sink by thermal conductance.
● Incoming photon’s energy is converted to heat in the absorber.
● Temperature rise is detected by measuring the change of resistivity of the thermometer.
Normally the thermometer is made of semiconductor e.g. Ge.
In our case, it is superconducting film operated near its transition temperature:
“Superconducting Transition Edge Sensor (TES) bolometer”
TES Bolometer
http://web.mit.edu/figueroagroup/ucal/ucal_tes/index. html
● SCUBA2 (Submillimeter
Common-User Bolometer Array) on
James Clerk Maxwell Telescope (JCMT), Hawaii.
● MUSTANG, a 90 GHz
bolometer on the 100 m Green Bank radio telescope (GBT)
TES Bolometer Arrays – detector
proposed performance
Waveband
:
• Band A: 30-57μm
• Band B: 57-106 μm
• Band C: 106-210 μm
WavelengthCoverage :
30-210 μm
Readout :
multiplexed SQUID
Linearity :
Good linearity with feedback to the
readout SQUIDs
Cosmic raysusceptibility :
Absorber has low
cross section
NEP :
~ 1 x 10
-19W/√Hz
Base Operating Temperature :
100-mK for
detector elements
Dynamic range :
Fundamentally linked to NEP
and limited to ~ 10000 @ 1x10
-19Various prototype TES detectors are being tested and developed at Cardiff/SRON/Cambridge/JPL
TES Bolometer Arrays For SPICA
Long narrow leg structures (left)
Staggered leg structures (right)
SRON: Astrophysics Detector Workshop
SRON have successfully tested a device at 205 mK. The results
