FIR/submm astronomy: science, observatories, and perspectives for lunar observatory
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1 FIR/submm astronomy: science, observatories, and perspectives for lunar observatory Prof. Jürgen Stutzki I. Physikalisches Institut der Universität zu Köln Kölner Observatorium für Submm-Astronomie (KOSMA) Co-PI Heterodyne Instrument for the Far-Infrared (HIFI)/ ESA cornerstone mission Herschel Co-PI German Receiver for Astronomy at Terahertz frequencies (GREAT), SOFIA Terahertz Array Receiver (STAR) Stratospheric Observatory for Infrared Astronomy (SOFIA) PI NANTEN2/KOSMA Submm Observatory, Pampa la Bola, Chile Lunar Observatories, Page 1 Nov. 23dr, 2006
2 FIR/submm astronomy: science, observatories, and perspectives the electromagnetic spectrum: the Far-IR spectral range science topics astronomy and instrumentation present missions: operational and/or implemented ground: APEX, NANTEN2, ALMA airborne: SOFIA spaceborne: Herschel perspectives and limitations the angular resolution gap -> interferometry mission studies: Dome C/A Antarctica FIRI/ESPRIT Summary Lunar Observatories, Page 2 Nov. 23dr, 2006
3 FIR/submm astronomy: science, observatories, and perspectives the electromagnetic spectrum: the Far-IR spectral range science topics astronomy and instrumentation present missions: operational and/or implemented ground: APEX, NANTEN2, ALMA airborne: SOFIA spaceborne: Herschel perspectives and limitations the angular resolution gap -> interferometry mission studies: Dome C/A Antarctica FIRI/ESPRIT Summary Lunar Observatories, Page 3 Nov. 23dr, 2006
4 Astrophysics across the electromagnetic spectrum Lunar Observatories, Page 4 Nov. 23rd, 2006
5 Astrophysics across the electromagnetic spectrum Lunar Observatories, Page 5 Nov. 23rd, 2006
6 submm- and far-ir spectral range astrophysical motivation: the cosmos is cold: emission peaks in the submm/fir local/galaxy: molecular clouds, star formation, dusty disks, planets, stellar envelopes, global: active galaxies, galaxy evolution, cosmology (high-z galaxies, cosmic background) the submm/ir has a high density in spectral characteristics atoms (neutral and ions): fine-structure lines, molecules: rotational and ro-vibrational lines, solid state: broad spectral features (silicates, ices), dust emission submm- and FIR-radiation penetrates clouds throughout a galaxy, offers view into galactic nuclei redshift: emission of distant, i.e. cosmologically young, objects shifted into submm-/fir Lunar Observatories, Page 6 Nov. 23rd, 2006
7 submm/far-ir: top science goals census of early, i.e. distant, galaxies broad band flux, spectral energy distribution high angular resolving power with bolometer detectors follow up line observations (strongest cooling lines) line fluxes: imaging spectroscopy at moderate spectral resolution galaxy evolution: tracing the physical and chemical conditions of the interstellar medium multi-line studies, kinematic and dynamic information high sensitivity and moderate to high spectral resolution formation of stars and planetary systems physical and chemical status of proto-planetary disks (dust and gas) ultimate angular resolving power and sensitivity instrument/telescope boundary conditions: direct detection: large and cold telescopes incoherent detection: multi-element interferometer with large collection area Lunar Observatories, Page 7 Nov. 23rd, 2006
8 submm- und far-ir spectral range/ detectors and instruments two fundamental detection methods: incoherent Filter: pre-detection Fabry-Perot Grating, etc. Detector: intrinsic or extrinsic photoconductor bolometer Lunar Observatories, Page 8 Nov. 23rd, 2006
9 submm- und far-ir spectral range/ detectors and instruments and coherent (heterodyne) detection Local Oscillator: FIR-Laser Carcinotron,BWO solid-state multiplier chain Quantum Cascade Laser Mixer: (non-linear element) quantum mixer: SIS-junction quantum mixer: Hot Electron Bolometer Backend: (Filter, post-detection) digital correlator acousto-optical spectrometer digital Fourier transform spectrometer Lunar Observatories, Page 9 Nov. 23rd, 2006
10 direct vs. heterodyne detection direct detection: photon shot noise (background limited) background limited: requires cold telescope multi element interferometry challenging: pre-detection interference heterodyne detection: quantum limit (phase coherence) close to fundamental limit of sensitivity (quantum limit) multi-element interferometry with large collection area feasible (post detection interference) fundamental physics and state-of-the-art-detector performance give: crossover resolution (break-even in sensitivity) in the far-ir: at about 30 km/s line width Both technologies by now can do spectral imaging (3D data cubes) Science areas: global emission from galaxies (continuum and line): direct detection galaxy dynamics and structure; interstellalr medium; star formation heterodyne detectiond Lunar Observatories, Page 10 Nov. 23rd, 2006
11 FIFI-LS Science: C II Data Cube in Interacting Galaxies CII and OI lines Lunar Observatories, Page 11 Nov. 23rd, 2006
12 SOFIA THz Array Receiver: STAR (Graf et al.) 16 pixel (receivers) integrated optics concept beam rotator diplexer mixer unit (8x) beam rotator second generation SOFIA instrument - [CII] 158 μm 1.9 THz - SMART & CHAMP heritage - solid state LO chain (VDI) - Fourier Grating Optics for LO mulitplexing Fourier Grating Mirror Lunar Observatories, Page 12 Nov. 23rd, 2006
13 technological progress: heterodyne sensitivities DSB Noise Temperature (K) projected 1.9 THz GHz GHz QL (1.9 THz) 100 QL (800 GHz) KOSMA Schottky SIS HEB 1980 MMIC QL (100GHz) Time (years) Lunar Observatories, Page 13 Nov. 23dr, 2006
14 FIR/submm astronomy: science, observatories, and perspectives the electromagnetic spectrum: the Far-IR spectral range science topics astronomy and instrumentation present missions: operational and/or implemented ground: APEX, NANTEN2, ALMA airborne: SOFIA spaceborne: Herschel perspectives and limitations the angular resolution gap -> interferometry mission studies: Dome C/A Antarctica FIRI/ESPRIT Summary Lunar Observatories, Page 14 Nov. 23dr, 2006
15 Ground Based submm/fir best ground based site (beyond Antartica): Chile: Atacama: Chajnantor Plateau & Pampa la Bola Future: Chajnantor Summit APEX 12 m telescope ALMA 64 element submm interferometer KOSMA/ NANTEN CCAT 25 m telescope Lunar Observatories, Page 15on Chajnantor summit Nov. 23rd, 2006
16 SOFIA Open Port Cavity Mission Control & Science Operation Section Education & Public Outreach Section Science Instrument Pressure Bulkhead Telescope Cavity Door Telescope 2.7m Cavity Environmental Control System
17 SOFIA: roll-out after painting (Waco: Oct. 2006) SOFIA is alive again, pending final budget decision by Congress end of November Lunar Observatories, Page 17 Nov. 23dr, 2006
18 SOFIA: Stratospheric Observatory for Infrared Astronomy first light Lunar Observatories, Page 18 Nov. 23rd, 2006
19 SOFIA: Stratospheric Observatory for Infrared Astronomy PLANETARY ATMOSPHERES INTERSTELLAR CHEMISTRY MOLECULES IN COMETS first light YSO DISK DYNAMICS PAHs/ORGANIC MOLECULES COMPOSITION OF ISM GRAINS GC GAS DYNAMICS DYNAMICS/COMPOSITION IN YSO OUTFLOWS ISM PHYSICS IN EXTERNAL GALAXIES PLANETARY ATMOSPHERES KBOs, PLANET TRANSITS DEBRIS DISK STRUCTURE Lunar Observatories, Page 19 YSO LUMINOSITIES, SEDs Nov. 23rd, 2006
20 Herschel: ESA cornerstone no. 4: FIR-astronomy space mission Lunar Observatories, Page 20 Nov. 23rd, 2006
21 Herschel spacecraft telescope diameter 3.5 m telescope WFE < 6 µm telescope temp < 90 K telescope emissivity < 4% abs/rel pointg (68%) < 3.7 / 0.3 science instruments 3 science data rate 130 kbps cryostat lifetime 4.0±0.4 years height / width ~ 7.5 / 4 m launch mass ~ 3200 kg power ~ 1500 W orbit large Lissajous around L2 solar aspect angle deg launcher (w Planck) Ariane 5 ECA Lunar Observatories, Page 21 Nov. 23dr, 2006
22 Herschel hardware Lunar Observatories, Page 22 Nov. 23dr, 2006
23 Herschel: Launch and orbit Lunar Observatories, Page 23 Nov. 23dr, 2006
24 FIR/submm astronomy: science, observatories, and perspectives the electromagnetic spectrum: the Far-IR spectral range science topics astronomy and instrumentation present missions: operational and/or implemented ground: APEX, NANTEN2, ALMA airborne: SOFIA spaceborne: Herschel perspectives and limitations the angular resolution gap -> interferometry mission studies: Dome C/A Antarctica FIRI/ESPRIT Summary Lunar Observatories, Page 24 Nov. 23dr, 2006
25 SAFIR? Herschel Herschel ASTRO-F SPITZER Wavelength (µm) SWAS COBE IRAS Planck JWST ISO KAO WISE SOFIA Year Airborne observatories provide temporal continuity and wide spectral coverage, complementing other facilities. Frequency (THz) ODIN Timeline of IR - FIR - Submm Missions
26 The Far-IR Spatial Resolution Gap: Interferometry l/s he sc er H ~ 10 arcsec with micro-k sensitivity FI O A JJW W SSTT ~ arcsecs with few K sensitivity
27 FIRI/ESPRIT: Far-IR Imager Mission study ESPRIT = mission concept for a free-flying sub-millimetre and farinfrared heterodyne space interferometer Exploratory Space Submm Radio Interferometric Telescope Telescopes : N ~ 6 ; free-flying Telescope size : ~ >3.5 m Temperature : ambient (90K) Proj. Baselines : ~ m Freq. range in : THz ( µm) Inst. Bandw. : ~ >4 GHz Angular Res. : 0.02 arcsec (@100 µm) Spectr. Res. : 1 Km/s (@100 µm)
28 FIRI/ESPRIT Science objectives A. Complementary to ALMA: Different frequency range > 950 GHz (ALMA) No atmosphere hindering in phase and transmission B. Imaging water and molecular ions in star forming regions and proto-stellar/proto-planetary disks: H2O, OH, OH+, CH, CH+, CH2+, CH3+, C. Imaging in important atomic fine-structure lines: CII, NII, OI, OIII, Imaging in high excitation lines of CO, HCN, HCO+, etc D. Follow-up on ISO-LWS, SWAS, ODIN, Herschel,
29 Interferometer element linking Free flying Interferometer-elements linking requirements: Ariane launch: 6 elements in single faring 1. Optical metrology for position determination 2. Signal transport between elements for correlation 3. Locking of all the LOs (reference distribution) Design goal is to have all three functions carried out by optical means, using same optical components.
30 Antartic: Dome C Exploration pro: excellent atmosphere low ambient temperature but: challenging logistics Lunar Observatories, Page 30 Nov. 23rd, 2006
31 SUMMARY (1) FIR astronomy: unique and competitive science goals detector, instrument and telescope technologies make rapid progress next step: interferometry (incoherent/coherent) broad band/incoherent: very low thermal background: spaceborne need for new generation of ultra-sensitive detectors high resolution spectroscopy: close to fundamental sensitivity limit multi-element interferometry routinely performed spatial resolution: long wavelength (λ/d): either large single dish telescopes needed and/or multi element interferometry needed Lunar Observatories, Page 31 Nov. 23rd, 2006
32 SUMMARY (2) a lunar-based FIR-observatory? low gravity allows for larger telescopes ADVANTAGE solid foundation allows for easy interferometry implementation thermal environment : uncritical for high spectral resolution, difficult for direct detection systems moderate effort in cryo-/vacuum technology science use case discussion shows: useful minimum configuration is 6 plus interferometer elements, possibly with larger central dish. each greater 6 m diameter, is this feasible? competing with opportunities in Antartic program (Dome C/A) competing with formation free flying space interferometer possible technology demonstration: submm/thz monochromatic source installed on the moon as phase reference for ALMA???? Lunar Observatories, Page 32 Nov. 23rd, 2006
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