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Key Scientific Goals: Galaxy Formation and Evolution

Future Far Infrared Space Facilities Matt Griffin School of Physics and Astronomy Cardiff University.

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Key Scientific Goals: Galaxy Formation and Evolution

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  1. Future Far Infrared Space FacilitiesMatt GriffinSchool of Physics and AstronomyCardiff University

  2. • Resolve of the FIR background into individual galaxies and study their internal structure spectroscopically- Star formation to z > 5 - Role of AGN in galaxy evolution - Assembly of Milky-Way type galaxies • Observe the birth and death of the first stars - Formation from primordial material - First injection of heavy elements into proto-galaxies Key Scientific Goals: Galaxy Formation and Evolution

  3. • Direct observation of all stages of star and planetary system formation • Imaging and spectroscopy of dust, ice, and gas - Disk accretion and gas dissipation - Dust mineralogy - Physical and chemical structure of disks - Decoupling of proto-planetary material from the star-forming gas in the centre - Prebiotic chemistry Key Scientific Goals: Planetary System Formation

  4. Sensitivity and Wavelength Coverage • Warm telescope limits sensitivity • Wavelength gap - 30-60 mm not covered by JWST or Herschel

  5. Thermal Backgrounds

  6. SPICA Launch ~ 2018 • 3-m telescope at 4.5 K - Diffraction-limited at 5 mm - l = 5 – 200+ mm • Instruments - MIR Camera & Spectrometer - Coronagraphic capability - FIR Camera & Spectrometer (SAFARI)- 3.5” at 50 μm - l/Dl 3; ~ 1000 • Spectroscopy of nearby and high-z galaxies • Formation of planetary systems

  7. SPICASensitivity Lines x 15 + whole band simultaneously Continuum

  8. 100 Herschel 10 10-m 1 JWST 30-m 0.1 ALMA 1-km interferometer 0.01 Angular Resolution 100 1000 10 Wavelength (mm) Beam Size (arcseconds) HST 1

  9. Fine Structure Lines as Probes of Metallicity Kohno et al

  10. [OIV] / [SIII] [NeV] / [SIII] Fine Structure Lines as Probes of UV Field Spinoglio et al.

  11. Fine Structure Lines as Probes of Gas Density λ Critical Density (μm) (cm-3) [OIII] 51.8 5 x 102 [OIII] 88.4 3x103 [OIV] 25.9 9x103 [SIV] 10.5 4x104 [NeV]14.3 1x105 [NeVI] 15.6 2x105 [NeIII] 15.6 3x105 [NeII] 12.8 6x105 Normalised line intensity nH (cm-3) Dasyra et al. (2011) Line flux predictions based on photoionization models of Netzer et al. 1996

  12. Spectroscopy of High-z Galaxies SAFARI SAFARI SAFARI accretion fusion

  13. Size (arcsec.) Redshift Extragalactic Angular Resolution NGC 1068 Galaxy disk ~ 20 arcmin Starburst ring ~ 30” AGN ~ 5”

  14. Role of Black Holes in Galaxy Formation • Black hole hidden by metals and dust from its conception as surrounding gas forms stars • Need to resolve the reprocessed FIR emission from accretion and SF both spectrally and spatially

  15. Dust, Ice, and Gas in Protplanetary Systems Dust mineralogyand ice Oxygen chemistry and water HD142527

  16. Protoplanetary Disk Structure FIR important for  Grain size and growth  Grain composition Gaps and spirals from forming planets  Gas disk structure and composition

  17. Debris Disks and ExoplanetSignatures 18

  18. SPIRIT SPECS

  19. Instrument • Module • Telescope • Module 20

  20.  Proposed in 2007 for Cosmic Vision (led by Rob Ivison and Frank Helmich) Well received scientifically Two or three cold apertures with central beam combiner Double Fourier spatial-spectral interferometer Baseline up to 1 km l = 25 – 400 mm 0.02” resolution at 100 mm (= 1 AU at 50 pc) l/Dl = 5000 PACS 5-s; 10 hrs ESI 5-s; 10 hrs

  21. New ESA Call for Large Missions  L-class missions = “pillars” - L1 already selected (JUICE) for launch in 2022 - L2 and L3 launches envisaged in 2028 and 2034  L-class mission envelope ~ €1B cost to ESA - Max contribution from other agency = 20% Selection process - Call for science themes now issued - 20-page white papers: ~ 16 pages on science; ~ 4 pages on straw-man mission concept(s) - Senior Review Committee will select science themes for L2 and L3 - Call for mission proposals for L2 in 2014 - Call for L3 mission proposals ~ end of this decade

  22. ESA Call for Large Misisons PACS 5-s; 10 hrs ESI 5-s; 10 hrs

  23.  EU FP-7 programme, started Jan. 2013 •  Objectives: - Update science case for space-borne FIR interferometry - Define corresponding mission concept and requirements - Develop end-end simulator - Assess and advance key technology areas

  24. Plans for FIR Interferometer White Paper(s)  Direct detection science/concept being coordinated by Rob Ivison and Giorgio Savini  Heterodyne concept being coordinated by Frank Helmichand Andrey Baryshev PACS 5-s; 10 hrs ESI 5-s; 10 hrs

  25. Plans for FIR Interferometer White Papers PACS 5-s; 10 hrs ESI 5-s; 10 hrs

  26. Conclusions • High sensitivity, high angular resolution FIR facilities areneeded as an essential complement to ALMA- Formation of planetary systems - Physics of the ISM in distant galaxies - Relationship between AGN and their host galaxies • SPICA is the next step, with a huge increase in sensitivity and spectroscopic power • A FIR interferometer will be proposed as a potential L-class ESA mission

  27. 29

  28. Breaking Confusion with Spectroscopy Photometry @ 120 μm Slice @ 63.2 μm Slice @ 58.3 μm Sources with lines at different redshift appear in different wavelength “slices”

  29. SPICA FIR 900 hour spectral survey SPICA FIR Herschel PACS

  30. Debris Disks ESI 5-s; 10 hrs • Vega-like detectable to ~ 10 kpc • Solar-like zodiacal cloud to > 1 kpc- How typical is the solar system? Greaves et al., ESLAB, May 2010

  31. • Imaging spectroscopy of structure in - High-z galaxies - Planet-forming disks Telescopes cooled to 4 K FIR Interferometer (FIRI) Baseline up to 1 km

  32. Formation of planetary systems 34

  33. SAFARI Imaging FTS Simultaneous Spatial and Spectral Multiplexing Full spectra of 7- 10 sources/field 35 Images Rosenbloom, Oliver, Smith, Raab private communication

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