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New Generation Submillimeter telescopes for an Era after Planck and Herschel missions

Submillimetron and Millimetron Projects. 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

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New Generation Submillimeter telescopes for an Era after Planck and Herschel missions

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  1. Submillimetron and Millimetron Projects New Generation Submillimeter telescopesfor an Era after Planck and Herschel missions V.D. Gromov, N.S. Kardashev Astro Space Center, P.N. Lebedev Physical Institute , Moscow, Russia

  2. 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

  3. Lebedev Physical Institute Astro-Space CenterSpace Projects Submillimetron and Millimetron

  4. Submillimetron project participants

  5. Millimetron Project Telescope diameter -12 m Spectral region 0.2 - 3 mm Mirror cooling T = 4 K Presented at36-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”.

  6. Submillimeter telescope module docked to Russian Segment of the ISS for service and instruments replacement Russian segment of the ISS RSCE S.P. Korolev Rocket Space Corp. Energia Leonid GorshkovSergey StoikoAndrey Adov Submillimeter telescope module

  7. Submillimer Sky Survey Project • Telescope diameter: D=0.6 m . • Wavelengths: submillimeter bands: 0.2- 2 mm . • Cooling: telescope - 5K, detectors - 0.1-0.25 K . • Detectors: bolometer arrays 10-18 W/Hz1/2 • Sensitivity of the telescope 3-12 mJy (integration time = 1 s). • Angular resolution = 1’ - 10' Submillimeter Telescope bay (shields not shown) Antenna of docking system Aggregates compartment Solar panels Docking assembly Nonpressurized compartment Pressurized compartment

  8. 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.

  9. Herschel (FIRST) and Planck mission 2007

  10. 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

  11. Results: Universe is 13.7  1% billion years Old The geometry of the Universe isflat. The matter of which we are made is only 4% of the Universe WMAP satellite Big Bang WMAP has detected evidence that first stars ignited 200 million years after the Big Bang.

  12. Dark ages 105 l.y. CMB 109 l.years 1010 light years

  13. 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, 3d ESA MMW workshop)

  14. Next Generation Submillimeter-wave (Terahertz)cryogenically cooled space telescope concepts 1 2 Small mirrorFull sky survey ASC/RSCE: Submillimetron NASA: CIRCESurvey of InfraRed Cosmic Evolution Large deployable reflectorSelected sources imaging ASC: Millimetron NASA: SAFIRSingle Aperture Far InfraRed observatory

  15. Extraterrestrial background Brightness I, for b>60o, 30 o<b<60 o, 10 o<b<30 o, and b= 0, l=180 o(from bottom to top).

  16. Cooled mirror background 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.

  17. 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!

  18. Photon noise (Bose-Einstein statistics) Power detector, signal ~ <|E2|>: (direct detector, bolometer, photon counter).Noise Equivalent Power: NEP2 ~<n2>= <n> (1 + <n>) Linear detector, signal ~ E(t): (RF amplifier, mixer receiver).Noise temperature Tnoise ~ <E2> ~ (<n> + 1/2) <n> - mean number of photons in quantum state. At low background <n> << 1 .

  19. Moor law for astronomy

  20. from simple cell to full function separation Astronomical bolometers evolution 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-to sensor, Hc - heat conductor

  21. Antenna-coupled bolometersno 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 sensor1993 - Nahum M.; Richards P.L.; Mears C.A.SIN demonstration NEP = 3x10-18 W Hz -1/2April - November - M.Nahum, J.Martinis (NIST) Andreev reflection "Andreev detector“ - ASC + KIPP 1995 CEB - Cold Electron Bolometer (NHEB, CCNHEB)L.Kuzmin, Chalmers 1998

  22. CMB COBE/FIRAS NEPbol=10-14 W/Hz1/2. SCUBA bolometer array. NEPbol=10-16 W/Hz1/2. CMB anisotropy. NEPbol=2·10-17 W/Hz1/2(BOOMERANG,MAXIMA) Spider-Web Bolometer NEPbol=10-17 W/Hz1/2. Andreev Bolometer. NEPbol=10-18 W/Hz1/2. Nanometric bolometer at temperature of milli-Kelvinsas 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. NEP comparision

  23. Antarctic station Vostok Computed atmospheric transmission, zenith, mean winter t=-70oC, w = 0 .2 mm, H=3488 m a.s.l.. Burova et. al, P. Astron. J., 15, 339 (1986)

  24. Peak Terskol, 3100 m a.l.s.

  25. BTA 6 meter telescope, Russia

  26. ALMA, 5000 m a.s.l.

  27. Sky mapping in radio and IR bands 1.25 -240 m with resolution 42. Nov. 1989. COBE (COsmic Background Explorer) 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).

  28. IRAS – discovery of IR sky Survey = 12, 25, 60, 100 m

  29. Nov.1995,0.6 m, T=3 K. IR bands 2.5 -240 m, 5" resolution, pointing to selected sources For comparision,main Submillimetron bands: 0.3-1 mm. ISO(Infrared Space Observatory)

  30. 2005 0.7 m resolution 30-50" at  50-200 m. Second IR sky survey IRIS (Astro-F)Infrared Imaging Surveyor

  31. 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

  32. Snoopy Detector Assembly Bolometers filled arrays characteristics: • response time = 10 ms • temperature = 300 mK • NEP = 5.10-17 W/Hz1/2 25 arcmn Focal plane

  33. 2011,2m, T=5 K, confusion limited full sky survey  0.1-0.5 mm with 13" resolution. Warm launch, radiative cooling + liquid Helium, 0.1 K ADR cooling of bolometer arrays. TES bolometers CIRCEinitiative of Infrared Astrophysics group of GSFC/NASA

  34. SAFIR The Single Aperture Far Infrared ObservatoryHarold.Yorke@jpl.nasa.gov

  35. (>106 objects in survey with 60-cm cold mirror) Point sources sensitivity Quantum limit for heterodyne detector with =10 GHz

  36. Spectra of a sturburst galaxy at different redshifts

  37. Interstellar Dust Fractal Model (Ned Wright, UCLA)

  38. ASC-FIAN (Lebedev Physical Institute, Moscow) RSCE (Korolev Space Corp.) Bolometer technology – Terahertz measurements – Astro-applicatons Chalmers University of Technology

  39. Links SPB 0209 WMAP

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