The Planck Mission and Ground-based Radio Surveys
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1 The Planck Mission and Ground-based Radio Surveys Russ Taylor University of Calgary Kingston Meeting UBC, November 2003 Current state of that art in ground-based radio surveys How Planck factors into the Galactic science Plans for advancing ground-based radio surveys before Planck Can ground-based radio surveys enhance Planck data products and also advance CMB/cosmology science Prospects toward the end of the decade Kingston Meeting UBC, November 2003
2 22 MHz 408 MHz spectral index -2.3 > beta > MHz 19 GHz (7 degree resolution) Platania et al. 1998, ApJ, 505, 473. Mean beta = -2.8
3 Haslam et al. (1982) 408 MHz Angular resolution 35 arc-minutes Anchor for spectral index images Striping Global zero level uncertainty Hartmann and Burton (1997) 1420 MHz spectral line Angular resolution 35 arc-minutes
4 The International Galactic Plane Survey Dominion Radio Astrophysical Observatory National Research Council of Canada Australia Telescope Compact Array Commonwealth Science and Industrial Research Organisation Very Large Array U.S. National Radio Astronomy Observatory The International Galactic Plane Survey Consortium Canadian Universities University of Calgary University of Alberta University of British Columbia University of Toronto University of Montreal University of Waterloo Queen s University Université Laval University of Western Ontario University of Manitoba St Mary s University International Organizations California Institute of Technology University of California, Berkeley Five Colleges Radio Astronomy Observatory University of New Mexico Cambridge University Hamburger Sternwarte Commonwealth Science and Engineering Resear Organisation Onsala Space Observatory University of Minnesota University of Sydney Max Planck Institut fur Radioastronomie National Radio Astronomy Observatory NRC of Canada, Herzberg Institute of Astrophysics Dominion Radio Astrophysical Observatory Canadian Astronomical Data Centre
5 IGPS grew out of a collaboration between CGPS and SGPS IGPS: CGPS I and II, SGPS I and II, VGPS SGPS CGPS VGPS SGPS International Galactic Plane Survey HI SURVEYS: CGPS VGPS SGPS unobserved CGPS SGPS VGPS
6 International Galactic Plane Survey Northern Hemisphere HI and CO Surveys HI CGPS Latitude Extension CGPS VGPS SGPS CO FCRAO Cepheus Survey FCRAO OGS BU-FCRAO GRS IGPS grew out of a collaboration between CGPS and SGPS 1420 MHz Continuum (free-free and synchrotron) IGPS: CGPS I and II, SGPS I and II, VGPS SGPS CGPS HI Line V LSR = -41 km/s VGPS SGPS
7 CGPS Sample Radio Continuum Products: MW1 mosaic 21 cm 74 cm 21 cm Polarised Intensity 21 cm Polarisation Angle Cygnus radio/ir composite July 2001 Sky & Telescope
8 Polarised Intensity of MW1 Stokes I Polarized Intensity Diffuse Polarized Emission: CGPS I 8
9 Polarised signal from foreground Faraday rotation Milky Way at Radio (21 cm)
10 Atomic Hydrogen Image from DRAO 7-element Interferometer, Penticton Dominion Radio Astrophysical Observatory equivalent diameter equals 600m Similar step as COBE to WMAP Planck Resolution HFI Approaching IGPS class resolution
11 Planck Resolution LFI Resolution at low frequencies much poorer than HFI bands The Evolution of Matter Planck-IGPS connection Radio submm Increasing radiation wavelength
12 Planck IGPS Science (It s about the dust) Diffuse HI to molecules Dust tracer of molecules Sources and sinks of dust (local and global) Dust processing versus gas environment and kinematics Heating and cooling (dust SED) Energization and transport (disk-halo exchange, shocks, turbulenc) Relationship to magnetic-fields Exploration away from the disk IGPS high latitude extension Atomic hydrogen gas Northern Sky from Leiden/Dwingeloo
13 HI Structure to High Latitudes Arcminte-scale HI structures extend to high latitudes V= -10 km/s V= -16 km/s V= -33 km/s High Latitude Polarimetry Combined effects of : synchrotron emissivity syncrotron polarisation ionized gas Galactic magnetic field Stokes I Stokes Q Stokes U
14 DRAO-Planck Deep Field Observation An high sensitivity, high photometric precision arcminute resolution image of the diffuse radio continuum and HI emission in the Galactic Halo 1.5 years of observations! begin early 2004 completion ~ 2007 Continuum sensitivity ~50 microjy/beam (3 mk at 1420 MHz continuum at 2 ) HI sensitivity 0.1 K at 2.6 km/s area ~10 square degrees noise and photometric accuracy across Simulated DRAO Deep Field Noise Power Map image uniform to 10-4 Full spatial frequency coverage Two frequencies of radio continuum full polarimetry HI spectral line emission Joint Planck DRAO DF Galactic ISM Science structure and conditions of Galactic halo ISM characteristics of synchrotron radiation on arcminute scales gas dust relationship (HI and ionized gas association with dust) dust magnetic field relationship low-frequency radiation from dust synchrotron/spinning dust emission self-consistent model of Faraday screen effect including free-free emission, synchrotron emission and magnetic fields (note the point sources will provide probes of the RM to extragalactic sources)
15 What can the IGPS and DRAO DF do for Planck? Low-frequency foreground for Planck CMB deconvolution at highest angular resolution possible with Planck ( l to ~ 2000) Highly sensitive and precise arc-minute scale measurement of the Galactic foreground emission at GHz wavelengths synchrotron intensity synchrotron spectral index free-free intensity polarized intensity HI column = proxy for dust emission? Calibration patch/proof of Planck spectral deconvolution algorithm DRAO DF: Ancillary observations 1. VLA higher resolution image to identify and measure parameters of compact sources to be removed, leaving the diffuse emission map. 2. matching resolution continuum and survey at higher frequencies (for better spectral deconvolution with three bands) 8 GHz survey with 100m class dish
16 DRAO DF: Where? Declination > 30 degrees Region from WMAP with 23 GHz associated dust emission Region containing known HI and dust over a range of intensities Range of HI velocity components? within Planck Deep Integration area near ecliptic poles? Regions of lowest dust and HI column (cleanest window on the extragalactic sky) Match to other Deep Field projects? Galactic ALFA Consortium
17 GALFACTS (GALFA Continuum Transit Survey) Pilot Study proposed for spring 2004 Full polarimetry ν/ν ~ 0.3 The Canadian Large Adaptive Reflector An innovative Canadian radio telescope design. The world s largest telescope. Prototype for the Square Kilometre Array
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