Transcript Bolometers evolution - Fysik och Teknisk Fysik Chalmers/GU
New Generation Submillimeter telescopes for an Era after Planck and Herschel missions
V.D. Gromov, N.S. Kardashev
Astro Space Center, P.N. Lebedev Physical Institute , Moscow , Russia
Outline
ASC projects Golden Era of Submillimeter Astronomy (THz/FIR, Astrophisics/Cosmology Exp./Theory) Current projects: Spitzer, Astro-F, Planck, Hershel, ALMA, APEX New generation projects: Cryogenic Submillimeter telescopes Sensitivity gap between radioastromy and IR - X ray Extraterestrial background gap, most distant objects detection New generation detectors: antenna-copled bolometers Conclusions. Need in observationa tests of detectors
Lebedev Physical Institute Astro-Space Center
Space Projects
Submillimetron and Millimetron
Submillimetron project participants
Millimetron Project
Telescope diameter -12 m Spectral region 0.2 - 3 mm Mirror cooling T = 4 K Presented at 36-th Liege Int. Astrophys. Colloqium "From Optical to Millimetric Interferometry: Scientific and Technological Challenges", July 2001. Proc., pp. 99-102 V. Gromov, N. Kardashev, "Space Submillimeter interferometer” .
Submillimeter telescope module docked to Russian Segment of the ISS for service and instruments replacement
RSCE
S.P. Korolev Rocket Space Corp. Energia Leonid Gorshkov Sergey Stoiko Andrey Adov Submillimeter telescope module Russian segment of the ISS
Submillimer Sky Survey Project
•
Telescope diameter: D=0.6 m .
Submillimeter Telescope bay (shields not shown) •
Wavelengths: submillimeter bands: 0.2- 2 mm .
Antenna of docking system Aggregates compartment •
Cooling: telescope - 5K, detectors - 0.1-0.25 K .
•
Detectors: bolometer arrays 10 -18 W/Hz 1/2
Docking assembly Pressurized compartment Solar panels Nonpressurized compartment •
Sensitivity of the telescope 3-12 mJy (integration time = 1 s).
•
Angular resolution
= 1’ - 10'
Spitzer
( SIRTF , Space InfraRed Telescope Facility ) 3-180 SIRTF is lifted into space aboard a Boeing Delta II Heavy rocket in the early morning of August 25, 2003, Cape Canaveral Air Force Station.
Herschel (FIRST) and Planck mission 2007
Scientific objectives
• Full-sky survey in submillimeter and millimeter wave region with polarization and variability data • Catalog of all-sky submm point sources at tens mJy level (high sensitivity limited by confusion and extraterrestrial background in its spectral minimum ) • Photometric spectra (SED), and their variability, high redshift evaluations • Syunyaev-Zeldovich effect (SZ cosmology) • Foreground sources for CMBA analysis • Quiet sources obscured by dust, not generating high energy particles manifesting in radio and X-ray • Cold object of Solar system, Kuiper belt, Oort cloud
WMAP satellite
WMAP has detected evidence that first stars ignited 200 million years after the Big Bang.
Results: Universe is 13.7 1% billion years Old Big Bang The geometry of the
Universe is flat.
The matter of which we are made is only
4%
of the Universe
Dark ages
10 5 l.y.
CMB 10 9 l.years
10 10 light years
Super young galaxies: redshift measurements in photometric (bolometric) submm survey Starburst galaxy model of Efstathiou, Rowan-Robinson & Siebenmorgen (2000, MNRAS). Spectral band of Submm sky survey photometer of Gromov et al. (2003, 3 d ESA MMW workshop)
Next Generation Submillimeter-wave (Terahertz) cryogenically cooled space telescope concepts
1
Small mirror Full sky survey
2
Large deployable reflector Selected sources imaging ASC/RSCE: Submillimetron NASA: CIRCE Survey of InfraRed Cosmic Evolution ASC: Millimetron NASA: SAFIR Single Aperture Far InfraRed observatory
10 -5 I , W/m 2 sr
Extraterrestrial background
10 -6 10 -7 10 -8 10 -9 10 -2 Brightness
I
,
(from bottom to top). 10 -1 for
b>60 o , 30
, mm
o
10 0
o , 10
10 1
o
and
b= 0, l=180 o
10 -2 I , W/m 2 sr 10 -3 10 -4 10 -5 10 -6 10 -7 10 -8 10 -9 10 -2 10 -1
Cooled mirror background
10 0 10 1 , mm Telescope mirrors T = 80, 40, 20, 10, 5, 4, 3, and 2 K - thin curves from top to bottom ( =0.01); dashed curve =0.04, T= 5 K. Thick solid curve shows extraterrestrial background for comparison.
But why 4K?
Because it makes a big difference!
A 4K scope is background-limited (zodi @ <200µm, CMB @ >200µm) At these wavelengths, point source sensitivity is more dependent on temperature than on aperture!
Photon noise
(Bose-Einstein statistics)
Power detector
, signal ~ <|E 2 |>:
(direct detector, bolometer, photon counter).
Noise Equivalent Power: NEP 2 ~< n 2 >= <
n
> ( 1 +
Linear detector
, signal ~ E(t):
(RF amplifier, mixer receiver).
Noise temperature T noise ~
1/2
)
At low background <
n
>
<< 1 .
Moor law for astronomy
Astronomical bolometers evolution
from simple cell to full function separation
CEB-STJ bolometer (An)(Ab+Hc)(Hc+Ts) Antenna-coupled bolometers TES, KID (An)(Ab+Ts+Hc)
Composite bolometer (An+Ab)(Ts) (Hc) Bolometer F. Low (An+Ab+Ts) (Hc) Hot electron InSb bolometer “all in one” (An+Ab+Ts+Hc) An-antenna, Ab-absorber, Ts-t o sensor, Hc - heat conductor
Antenna-coupled bolometers
no limitation on sensor size
The calculated sensitivity is almost two orders of magnitude higher than that of the best available direct detectors of millimeter and submillimeter radiation operated at the same temperature.
TES - Transition Edge Sensor: 1990-Nahum M.; Richards P .
SIN: Superconductor-Insulator-Normal metal sensor 1993 - Nahum M.; Richards P.L.; Mears C.A.
SIN demonstration NEP = 3x10 April - November - M.Nahum, J.Martinis (NIST) Andreev reflection -18 W Hz -1/2 "Andreev detector“ - ASC + KIPP 1995 CEB - Cold Electron Bolometer (NHEB, CCNHEB) L.Kuzmin, Chalmers 1998
NEP comparision CMB COBE/FIRAS SCUBA bolometer array. CMB anisotropy. (BOOMERANG,MAXIMA)
NEP bol =10 -14
W/Hz 1/2 .
NEP bol =10 -16
W/Hz 1/2 .
NEP bol =2·10 -17
W/Hz 1/2 Spider-Web Bolometer Andreev Bolometer.
NEP bol =10 -17
W/Hz 1/2 .
NEP bol =10 -18
W/Hz 1/2 .
Nanometric bolometer at temperature of milli-Kelvins
as subject for "Andreev physics”, a mesoscopic region, where dominate Andreev reflection, Andreev conductance, Andreev interferometry, Andreev current, Andreev levels, Andreev scattering, Andreev tunneling, Andreev channels, Andreev orbit, Andreev states and even Andreev billiard .
Antarctic station Vostok
Computed atmospheric transmission, zenith, mean winter t=-70 o C, w = 0 .2 mm, H=3488 m a.s.l..
Burova et. al, P. Astron. J., 15, 339 (1986)
Peak Terskol, 3100 m a.l.s.
BTA 6 meter telescope, Russia
ALMA, 5000 m a.s.l.
COBE
(COsmic Background Explorer) Sky mapping in radio and 10 IR bands 1.25 -240 m with resolution 42 . Nov. 1989.
COBE satellite had a total mass of 2270 kg, a length of 5.49 m, and a diameter of 2.44 m with Sun-Earth shield and solar panels folded (8.53 m with the solar panels deployed).
IRAS – discovery of IR sky
Survey = 12, 25, 60, 100 m
ISO (Infrared Space Observatory)
• Nov.
1995, 0.6 m, T=3 K.
• IR bands 2.5 -240 selected sources m, 5" resolution, pointing to • For comparision, main Submillimetron bands: 0.3-1 mm.
IRIS (Astro-F)
Infrared Imaging Surveyor 2005 0.7 m resolution 30-50" at 50-200 m.
Second IR sky survey
Lagrange Points of the Earth-Sun system
(not drawn to scale!).
1AU =150 million km. Lagrange points L1 and L2 are located approximately 1.5 million kilometers from the Earth
Detector Assembly Bolometers filled arrays characteristics:
response time = 10 ms temperature = 300 mK NEP = 5.10
-17 W/Hz 1/2
(
m
) 100 - 700 pixel FWHM 25 arcsec
# of pixels Pixel size
16x32 1.5 mm Size of array 24x48 mm 2 2000 72 arcsec 6x12 4.3 mm 26x52 mm 2
25 arcmn
Focal plane FOV of array 6.7x13.3‘ 2 7.2x14.4‘ 2
CIRCE
initiative of Infrared Astrophysics group of GSFC/NASA • 2011 , survey confusion limited full sky 2m, T=5 K, 0.1-0.5 mm with 13" resolution.
• Warm launch, radiative cooling + liquid Helium, 0.1 K ADR cooling of bolometer arrays.
• TES bolometers
SAFIR
The Single Aperture Far Infrared Observatory [email protected]
Parameter
Aperture Temperature Wavelength Diffraction limit Lifetime
Requirement
~10m 4K <20 500+µm ≥40µm (1”) >5 years
Science Targets
distant galaxies circumstellar disks Galaxy @ z=5 coolant line emission (JWST, ALMA overlap) circumstellar disks distant galaxies Productivity, time variability!
Point sources sensitivity
10 3 Noise Equivivalent Flux Density, mJy/Hz 1/2 (>10 6 objects in survey with 60-cm cold mirror) 10 2 IRAS SIRTF/MIPS Hershel/SPIRE Plank/HFI Quantum limit for heterodyne detector with =10 GHz 10 1 ISO-PHT IRIS SUBMILLIMETRON 10 0 10 -1 10 -2 10 -1 , mm 10 0 10 1
Spectra of a sturburst galaxy at different redshifts
Interstellar Dust Fractal Model
(Ned Wright, UCLA)
Bolometer technology
–
Terahertz measurements – Astro-applicatons
ASC-FIAN (Lebedev Physical Institute, Moscow) RSCE (Korolev Space Corp.) Chalmers University of Technology
SPB 0209 WMAP