Millimetron and CII. Andrey Baryshev on behalf of Millimetron contributors SRON and Kapteyn Astronomical Institute

Transcription

1 Millimetron and CII Andrey Baryshev on behalf of Millimetron contributors SRON and Kapteyn Astronomical Institute

2 Herschel true THz space astrophysical facility Launch late 2009 shared with Planck on Arianne V Far-infrared/submm Space Observatory Sun-Earth L2 orbit Credits ESA/Astrium Credits ESA/Astrium C+ Workshop, Lorentz center, Leiden, Feb

3 Hershel heritage (SPIRE) A lot of interesting science is becoming available from Herschel in far infrared region, as in this example of Mkr 231 with broadband SPIRE spectrum. But it is only the beginning.. Millimetron with its larger mirror size and colder mirror it can look much deeper and with higher resolution Markarian 231 region, P. van der Werf at al, SPIRE consortium

4 Herschel heritage (HIFI) NGC 6334 I*, M. Emprechtinger et al, HIFI consortium, Water lines observed by Hershel HIFI delivering a lot of information on the underlying physical processes C+ Workshop, Lorentz center, Leiden, Feb

5 From Herschel to Millimetron Larger mirror size higher resolution Colder mirror temperature higher sensitivity Larger frequency coverage new science in high resolution Advances in detector/instrument technology Focal plane arrays High sensitivity Larger pixel counts Cost effective

6 Millimetron mission Approved mission of Russian Space Agency with approved funding Led by Astro Space Center, PI N. Kardashov (Radioastron) Launch date (as early as possible) Life time 10 years (5 Cold) Orbit Lagrangian L2 Mirror 10 m deployable, <2 THz (>150 micron) 3m central part, <6 THz (>50 micron) Actively cooled to 30K (considering 4K for central part) Closed cycle mechanical coolers, 4K instrumentation package In Russia Launch, Proton-M Satellite Deployable antenna Large mission, 4000 kg, 5000 W Instrumentation is built by international consortium Heterodyne arrays HIFI+ (CII, O, OH etc) Imaging spectrometer <150 micron (similar SPICA BLISS) Imaging spectrometer FTS (3mm 0.3mm) S-VLBI channels (some ALMA bands + VLBI) C+ Workshop, Lorentz center, Leiden, Feb

7 The Orbit (Anti-Solar Lagrangian Point L2) The Observatory s ecliptic latitude varies around the L2 between 55 with period of days C+ Workshop, Lorentz center, Leiden, Feb

8 Deployable petals M1 M2 Solid inner 3.5m 3m dish Sunshields Instrument bay container (4K) Compartment warm units (300K) C+ Workshop, Lorentz center, Leiden, Feb

9 Reflector C+ Workshop, Lorentz center, Leiden, Feb

10 Mirror surface Actuator with Three Degree of Freedom Hinge at One End and Two-Degree-of-Freedom at Other End Actuator at C.O.G. with Rigid Fixation at One Side and Two-Degree-of- Freedom Hinge at Other Side Actuating Mechanism with Hinges C+ Workshop, Lorentz center, Leiden, Feb

11 Navigator platform Electra L as a prototype/ Launched early 2011 RadioAstron is launched and working C+ Workshop, Lorentz center, Leiden, Feb

12 Radioastron Mission (as Prototype) General view of Radioastron in Lavochkin Association Space Earth VLBI (SVLBI) Moon perturbed elliptical orbit apogee km Multi frequency synthesis to improve U-V coverage Wavelength 95 cm 1.35 cm Diameter 10 m (deployable) Mirror surface accuracy 2 mm RMS Pointing accuracy 32 Spacecraft mass 5200 kg Launched summer

13 Millimetron instrumentation Space Earth VLBI instruments, GHz, high spectral resolution, (RadioAstron, ALMA heritage) Ultra high spatial resolution experiment Millimetron High Resolution Spectrometer, GHz, (HIFI heritage) HIFI science and far beyond Millimetron Medium Spectral Resolution Spectrometer, GHz, (SPICA BLISS/SAFARI concept) Similar to SPICA/BLISS science but higher spectral resolution/sensitivity CMB, High-Z umillimetron Imaging Spectrometer Polarimeter, GHz, (dual FTS) niverse, SZ-effect, CMB Polarization (limited area) ASIAA, Taipei, 16 Jan 2013

14 High resolution spectrometer Wide-field Focal-Plane relay required: Re-images central on-axis part FoV Selects sky or calibration source input Maps and distributes FoV to mixer bands Re-imaged FP divided in 3x2 bands: Map any point in FoV to any of the mixer bands CAL (cold) SKY CAL (hot) ASIAA, Taipei, 16 Jan 2013

15 HRS band allocation 8 GHz IF bandwidth, x 16 in peak configuration CH+ CII O ASIAA, Taipei, 16 Jan

16 DSB Noise Temperature (K) Sensitivities (compared with HIFI) 4.8 GHz 1000 Status GHz K! 100 Baseline mixer H mixer V HIFI total Millimetron SIS L HEB 6H Frequency (GHz) C+ Workshop, Lorentz center, Leiden, Feb

17 Optical Design FP relay (2) Folding mirror FP in 2D-BS miror Folding mirror FP out C+ Workshop, Lorentz center, Leiden, Feb

18 Optical Design Mixer cartridge (1) Instrument bay 12K 70K 300K Mixer cartridges LO injected from below C+ Workshop, Lorentz center, Leiden, Feb

19 Optical Design Mixer cartridge (2) Cartridge concept: Balanced or SSB mixer Separate RF/LO ports BS grid or dichroic Dumps for X-pol Single LO beam in LO-MUX by grating Input paraboloid forms imaging pair with splitting optics Pupil plane near entrance of cartridge C+ Workshop, Lorentz center, Leiden, Feb

20 Technology HEB SIS HEMT IF amplifier LO multipliers C+ Workshop, Lorentz center, Leiden, Feb

21 Current ( A ) Noise temperature T N,rec (K ) THz QCL s LO already demonstrated in lab s test 214µm / 153µm 10 m 25 m 670 m 12µm Active Region THz Radiation Active region Metal-metal waveguide QCL (DM QCL), MIT/Sandia, 2.8 THz 1500 µm Surface plasmon QCL (SP QCL) U. Paris 7/Cambridge, 2.8 THz 300 f LO =2.8 THz bolometer nw 300 nw 300 nw 330 nw Voltage (mv ) Gao et al C+ Workshop, Lorentz center, Leiden, Feb

22 FFTS 16 x 8 GHz bandwidth ( W peak) C+ Workshop, Lorentz center, Leiden, Feb

23 C+ and Millimetron 3 CII x K 1300 km/s 4 OI x K 650 km/s 0.01 km/s peak resolution ++ Grating spectrometer (SPICA/BLISS) No atmosphere contribution Cold mirror CII, 1 square degree 1km/s = 160 hr (sorry was indeed mistake there) C+ Workshop, Lorentz center, Leiden, Feb

24 VLBI channels For frequencies >350 GHz contained in high resolution instrument For frequencies <350 GHz ALMA cartridge concept is being adopted HEMT technology will be used ALMA band 1-5 experience is very valuable C+ Workshop, Lorentz center, Leiden, Feb

25 VLBI concept L2 Millimetron is designed to turn away from earth UV baselines from meters till L2 distance W is large, plan to send LO tone to Earth (H-Maser) Orbit is slow (compared to VSOP/Radioastron) Based on Radioastron heritage C+ Workshop, Lorentz center, Leiden, Feb

26 VLBI bands Band Frequency IF Pol TN Comment GHz 4-12 (НЕМТ) H V <20 K GHz 4-12 (НЕМТ) H V <30 K GHz 4-12 (НЕМТ) H V <37 K GHz 4-12 (SIS) GHz 4-12 (SIS) GHz 4-12 (SIS) H V H V H V <50 K <100 K Part of HRS <150 K Part of HRS C+ Workshop, Lorentz center, Leiden, Feb

27 VLBI instruments in container Криоконтейнер РСДБ-1 РСДБ-2 РСДБ-3 Переключающее зеркало Круг фокуса телескопа РСДБ-5 РСДБ-6 РСС РСДБ-4 C+ Workshop, Lorentz center, Leiden, Feb

28 Medium resolution spectrometer polarimeter C+ Workshop, Lorentz center, Leiden, Feb

29 Conclusion Mission of opportunity for astronomical community Addresses several areas of astrophysics C+ (heterodyne, contunuum) Astrochemistry VLBI (event horizon) Extragalactic CMB (S-Z, Polarisation) Needs large international effort to make it possible Millimetron science and technology workshop April Groningen, after ISSTT2013 conference C+ Workshop, Lorentz center, Leiden, Feb