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/VIS CMB

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 ( nm) In infrared light (24 µm) Images: NOAO, NASA/JPL-Caltech/K. Gordon (Arizona) Spitzer, Herschel Far-Infrared (Herschel µm)

All sky (visible) 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 –( ) – Two FIR/submm recommendations 1.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

Spectral / Spatial Interferometer Spectral Resolution – ~1/(2Z max ) 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

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