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2. Overview of IFUs & science results
• Selected IFUs, science highlights & datacube visualization
• Brief overview of the major topics in astronomy
• Data formats in (optical & infrared) astronomy
IFUs
• Optical– SAURON, VIMOS, FLAMES, GMOS, PPAK
• Infrared– SINFONI, OSIRIS
• Many more exist– TIGER, OASIS, IMACS, NIFS, GNIRS, ...
• Near future– MUSE, KMOS, VIRUS
• Space based– NIRSpec, MIRI (both on JWST)
LensletsLenslets + FibresFibresSlicer
Astronomy 101
• Seeing: typically < ~1 arcsec for ground based telescope– telescope diffraction limit < 0.1 arcsec for D > 10 cm
• Redshift:
• IFU ⇒ complex data ⇒ complex data reduction and analysis ⇒ complex physics
Lenslet array: SAURON
SAURON • 1600 square lenslets• 0.94”/lenslet (33”x41” field) • 4810-5400 Angstrom range• R ~ 1500
Bacon et al.
Lenslet array: OSIRIS
OSIRIS • > 1000 square lenslets• AO corrected• 1- 2.5 micron range• R ~ 3800
Larkin et al.
Distant galaxies: SSA22a
Paraview rendering
Bower et al. 2004
Spatially resolved observations of the diffuse Lyman alpha halo around a proto-galaxy
SSA22b (z = 3.09)
VolView rendering
Observational evidence for feedback process: crucial ingredient of galaxy formation scenarios.
Lenslet array + fibres: VIMOS
VIMOS • 6400 square lenslets• 0.67”/lenslet (54”x54” field) • 3500-9000 Angstrom range• R ~ 300 - 1500
VIMOS March ‘02
VLT 1st Gen. Instrument: FLAMES-IF
10
Active galaxy: Seyfert 1.9
• Nearby AGN (z~0.1)
• Interacting/merging(?) with companion
• Triggered jet activity
10
FLAMES - deployable IFUs
FLAMES (d-IFUs)• 15 d-IFU spectroscopy• 20 μ-lenses (2”x3” field)• 0.37-0.95 μm range• R ~ 1.1x 104
• λ/Δλ = 9.5; εF ~ 68%
VLT 1st Gen. Instrument: FLAMES-IF
10
Multiplexed IFU observations of intermediate redshift galaxies
Flores et al. 2006
• Observed 35 galaxies
• Texp = 8 - 13 hours
• z: 0.4 to 0.7
• No TF evolution in in ‘regular’ galaxies
Tully-Fisher at z=0.6
GMOS-IFU
GMOS-IFU• 0.2”/lenslet (5”x7” field)• 0.4-1.0 μm range• R ~ 1.1x 104
• λ/Δλ = 9.5; εF ~ 68%
Allington-Smith et al.
VLT 1st Gen. Instrument: FLAMES-IF
10
GMOS IFU observations of the prototypical Seyfert 2 NGC 1068
Complex emission-line profiles in the galaxy’s nucleus
GMOS IFU datacube of Hbeta in NGC 1068 + disk model
Slicers: Sinfoni
SINFONI• 250 – 100 - 25 mas slice width• 8”x8”- 3”x3”- 0.8”x0.8” field• 32 x 64 spaxels• 1.1-2.45 μm range• R : 1.5x103 (H+K) / 3x103 (H) /
4x103 (K)
SINFONI Jul. ‘04
High-z galaxiesRotation curves and dynamical evolution of galaxies at z=2, Förster Schreiber et al, 2006
As SAURON survey but for distant, hence young galaxies
Fibres: PPAK
PPAK • 331+36 non-contiguous fibres• 2.7”/fibre (74”x65” field)• 0.35-0.90 μm range• R ~ 5000
Roth et al.
PPAK
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
NGC 488
Long-slit data
Probe of secular evolution and appears to correlate with Hubble type
Summary of IFU applications
• Planets (searches for)
• Dense stellar clusters (eg. globular clusters)
• Galactic centre
• Planetary Nebulae
• Nearby galaxy: mass distribution, stellar population, central black holes
• Active galaxies (AGN): central engine, jet activity, feedback
• Distant galaxies: young galaxies, gravitational arcs, Ly-alpha galaxies
• Cosmology
File format(s)
• FITS is the standard in astronomy– Header + data– Reference:
• A potential alternative for IFU data is Euro3D – Based on the FITS standard
Major scientific objectives (of all new facilities, eg. ELT, JWST)
• The end of dark ages: first light and re-ionization• The assembly of galaxies• The birth of stars and the proto-planetary systems• The planetary systems and the birth of life
The end of the dark ages: first light and reionization
• What are the first galaxies?• When did reionization occur?
– Once or twice?• What sources caused reionization?
The assembly of galaxies• What are the physical processes that determine galaxy
properties?• How did the heavy elements form?• Can we test hierarchical formation and global scaling
relations?• What about ‘active’ galaxies (AGN)?
The birth of stars and protoplanetarysystems
• How do clouds collapse?• How does environment affect star-formation (and vice-versa) ?• What is the low-mass IMF (stars planets)?
Deeply embedded protostar
Agglomeration & planetesimals Mature planetary system
Circumstellar disk
David Hardy
The planetary systems and the origins of life
• How do planets form?• Are circumstellar disks like our Solar System?• How are habitable zones established?
Simulated JWST imageFomalhaut at 24 microns
Spitzer imageRobert Hurt
• Extra-solar giant planets– Coronagraphy
• Spectra of circumstellar disks, comets and KBOs• Spectra of icy bodies in outer Solar System
TitanMalfait et al 1998
The planetary systems and the origins of life