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The Far-Infrared Universe:from the Universe’s oldest light to the birth of
its youngest stars
Jeremy P. Scott, on behalf of Locke D. Spencer
Physics and Astronomy, University of Lethbridge
CAP Congress 2015, University of Alberta
June 17, 2015
1. The Far Infrared
2. Planck
3. Herschel/SPIRE
4. Interferometry
5. Future Work
Contents
Image: ESA-CNES-Arianespace
Introduction
FIR observations offer great potential in the study of star and planetary formation
Observations in the Far-IR (FIR) allow investigation of key science questions of star formation and galaxy evolution.
Success of Spitzer and Herschel, and expectations for ALMA and JWST, stress the need for observations in the FIR Blain et al. 2002, Helmich and Ivison 2009
FIR NIR/VISCMB
Science Drivers• Advances in FIR astronomy from within our own galaxy
to cosmological studies– Protoplanetary discs and planet formation
• Resolving snow line (liquid/ice regions), water dynamics, dust structure / dynamics
– Star Formation• ISM structure and IMF, High mass star formation rate, molecular
tracers (H2O, CO, …), pre-stellar core / filament dynamics– Nearby Universe
• Galaxy dust budget (~low mass vs. supernovae ejecta), dust heating, formation of massive stars, AGN / host galaxy relations
– Evolving Universe• Most of the observable universe is feature-rich in FIR bands
(84%), star formation history, black hole accretion and growth – Early Universe
• Molecular hydrogen, cosmic microwave background
• All of these areas are very well served by advances in FIR technology and observations!
Near/Small
Far/Large
Why space?
Image: NASA
Herschel and Planck:
Europe’s Cosmic Explorers
M31 – the Andromeda Galaxy
In optical light (390-700 nm) In infrared light (24 µm)
Images: NOAO, NASA/JPL-Caltech/K. Gordon (Arizona) Spitzer, Herschel
Far-Infrared (Herschel 250-500µm)
All sky (visible)
www.chromoscope.net
DSS
All-sky (microwave)
Planck
The sky as seen by Planck
Images: ESA
Component Maps
The 2013 Planck Cosmic Microwave Background Temperature Map
Image: ESA
…And Polarization
Star formation in Aquila
Planck + IRAS 100/350/540 m
Planck + IRAS 100/350/540 m
Herschel 70/160/500 m
Star formation in Aquila
Please see my poster tomorrow (Scott et al. DASP poster session, 17 June 2015)
SPIRE FTS Imaging and Spectroscopy
Spencer et al. in prep
SPIRE FTS Frequency Calibration
• Decadal plan for astronomy from the Canadian Astronomy Community
– (2010-2020)– http://www.casca.ca/lrp2010/
• Two FIR/submm recommendations1. Cooled apertures
(increased sensitivity)2. Interferometry (increased spatial resolution)
Angular Resolution
FIR gap
YSO disk at 140 pc
YSO disk at 140 pc
Simulated JWST deep field
YSO disk at 140 pc
• Interferometer
• Baseline/, u, v
• Fourier Spectrometer
• Optical path difference, z
Interferometer Theory
)}({FT
)2exp()()(
zI
dzzizIS
z
L
L
)},({FT
)](2exp[),(),(
, vuI
dudvvyuxivuIyx
vu
Spectral / Spatial Interferometer
• Spectral Resolution– ~1/(2Zmax)
• Angular Resolution– /B
• The spectral and spatial properties of the source are obtained through spectral/spatial Fourier transformation of the observed signal
Nyquist and Cittert-Zernike sampling conditions allow lossless spectral/spatial hyperspectral image reconstruction
Conclusions
• With imaging FTS:
Per pixel
Conclusions
• With spatial/spectral double Fourier:
Per pixel
Current Status / Future Work
• Working on current FIR astrophysics instruments and research/science programs – E.g., Herschel, Planck, BETTII, EBEX,SCUBA-2
• Working on future-generation instrumentation and technologies– E.g., SPICA, FIRI/FISICA
• Working to set up a FIR spatial/spectral interferometry instrument at U of L– develop observing and data processing
techniques and extend FTS processing to FIRI-like applications
– In parallel with international collaborations
