Opportunities for Dust Polarization Surveys
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1 Opportunities for Dust Polarization Surveys C. Darren Dowell JPL/Caltech This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 1/30
2 Outline magnetic fields in interstellar clouds observational and theoretical approaches dust composition, shape, and alignment sensitivity comparison survey approaches 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 2/30
3 Magnetic Field Strengths in Interstellar Clouds 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 3/30
4 Galactic Field in A V 1 Medium optical polarimetry 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 4/30
5 Galactic Field in A V 10 Medium BICEP: southern sky at λ = 2 mm, 1º resolution 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 5/30
6 Galactic Field in A V 100 Medium FIR-bright cloud cores: no B angle correlation with Gal. plane data from Dotson et al. (2000, 2008) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 6/30
7 Measuring Magnetic Fields In addition to the usual problems with line-of-sight averaging and unresolved structure: vector B = (B x, B y, B los ) B los : Zeeman, Faraday rotation tan -1 (B y /B x ): synchrotron, dust polarization 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 7/30
8 Measuring Magnetic Fields In addition to the usual problems with line-of-sight averaging and unresolved structure: vector B = (B x, B y, B los ) B los : Zeeman, Faraday rotation tan -1 (B y /B x ): synchrotron, dust polarization (B x2 +B y2 ): dust polarization via Chandrasekhar-Fermi approach? 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 8/30
9 WMAP all-sky synchrotron map 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 9/30
10 Berkhuijsen (1997) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 10/30
11 complementarity of synchrotron and dust mapping Blue: Spitzer 8 µm red: Bolocam/CSO 1.1 mm purple: VLA 20 cm Bally et al. (2009) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 11/30
12 complementarity of synchrotron and dust polarization µm Chuss et al. (2003) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 12/30
13 Far-IR polarimetry is an excellent tracer of magnetic fields at densities up to 10 6 cm -3. B vec Orion Core L183 Dark Cloud B vec Rao et al. (1998) Ward-Thompson et al. (2000) Schleuning (1998) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 13/30
14 Tests of Cloud and Core Formation Theory with FIR Polarimetry Ordered structures flow along field lines tidal shear swept-up shells accretion disks Large features resulting from instabilities Dispersion in field Chandrasekhar-Fermi approach 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 14/30
15 Far-IR polarimetry tests geometrical models of magnetic fields: protostars hourglass field in protostellar envelope NGC 1333 IRAS 4A B vec observation w/ interferometer: Girart, Rao, & Marrone (2000) model: Fiedler & Mouschovias /11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 15/30
16 Far-IR polarimetry tests geometrical models of magnetic fields: cloud cores Schleuning (1998); Houde et al. (2004) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry Kirby (2008) 16/30
17 Far-IR polarimetry tests geometrical models of magnetic fields: cloud formation swing amplifier effect magneto-jeans instability Kim & Ostriker (2001) Kim & Ostriker (2006) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 17/30
18 Magnetic Field Strength from Chandrasekhar-Fermi Method strong field: small dispersion weak field: large dispersion Falceta-Gonçalves, et al. (2008) B = x ρ 1/2 Δv / Δθ x: Ostriker et al.(2001); Padoan et al. (2001); Heitsch et al. (2001); Falceta-Goncalves et al. (2008) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 18/30
19 Magnetic Field Strength from Chandrasekhar-Fermi Method strong field: small dispersion weak field: large dispersion Falceta-Gonçalves, et al. (2008) B 80 µg B = x ρ 1/2 Δv / Δθ x: Ostriker et al.(2001); Padoan et al. (2001); Heitsch et al. (2001); Falceta-Goncalves et al. (2008) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 19/30
20 Grain Alignment & Composition current theory of grain alignment (Lazarian et al.): Paramagnetic relaxation no longer needed. Instead, radiative torques on asymmetric grains will do. Alignment with polarization perpendicular to field still applies. Observational tests possible. Vaillancourt et al. (2008) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 20/30
21 Into the Next Decade optical/near-ir: big surveys of starlight polarization FIR: BLASTpol: mapping full molecular clouds SOFIA: precision application of Chandrasekhar-Fermi submm: Planck: all-sky polarization survey ALMA: great for circumstellar dust? radio: EVLA, GBT 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 21/30
22 HAWCpol/SOFIA started Oct on JPL internal funds permanent upgrade to HAWC good for sources up to ~8 3/11/09 observation bands 53, 89, 155, 216 µm angular resolution 5 22 arcsec field of view arcmin2 polarization modulation technique quartz half-wave plate, 15 rpm minimum flux density to achieve σ(p) = 0.2% in 5 hour integration 9, 6, 6, 5 Jy minimum column density to achieve σ(p) = 0.2% in 5 hour integration AV = 1, 2, 5, 4 systematic error goal δp < 0.2%; δθ < 2 C. D. Dowell, Keck Institute/Dust Polarimetry 22/30
23 Required Polarization Sensitivity typical degree polarization = 3% typical intrinsic dispersion = σ(θ) = 3, σ(p) = 0.3% photometric signal-to-noise of 500 Hildebrand et al. (1999) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 23/30
24 BLASTpol sensitivity to extended emission Far-IR polarimetry is 10 6 faster from space. 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 24/30
25 Giant Steps MIDEX-class FIR polarization survey SAFIR polarimeter SPIRIT polarimeter EPIC (CMBPol) with extended highfrequency coverage SKA 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 25/30
26 Dedicated Polarization Survey M4: 0.2 m cold telescope PIREX/M4 (Clemens, P.I.; Goodman; Jones) satellite proposed to NASA 1990, 1993, 1996 possible reasons for non-selection: Polarimetry not a scientific priority for NASA. Difficult for a cryogenic mission to compete on the NASA SMEX playing field. Unsuccessful Origins Probe proposal to study FIR polarimeter and C + heterodyne spectrometer on m telescope (Dowell, Langer et al.) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 26/30
27 MIPS 24 µm (Gordon et al.) with SAFIR/CALISTO: 5 hours integration time (10 4 detectors) 5 = 20 pc resolution at λ = 100 µm likely detection of polarization wherever A V > 0.3 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 27/30
28 EPIC Polariza,on Mapping coverage map, σ(p) 0.3% Planck/350GHz 5 EPIC/850GHz 4K, 1 EPIC/850GHz 40K, 5 EPIC/850 GHz can make accurate polariza,on maps with 10 8 resolu,on elements. 3/11/09 28 C. D. Dowell, Keck Ins,tute/Dust Polarimetry
29 Enabling Technologies for Space Far-IR Polarimetry polarization-sensitive detectors polarization modulation low-power cryogenic rotating quartz half-wave plate scan modulation only (Boomerang Planck) Good polarimeters usually make good cameras. NEP = W Hz -1/2 is adequate for detectors. 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 29/30
30 Antenna-Coupled 200 µm TES Detector work by Peter Day et al. (JPL/Caltech) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 30/30
31 If nuclear and gravitational forces were the only forces at work in the universe, the broad pattern of cosmic evolution would be one of gradual thermal degradation punctuated by occasional explosive events. The cosmos would resemble the serene and monotonous heavens of classical conception. There is, however, a cosmic agitator: the magnetic field. Although only a small part of the available energy in the universe is invested in magnetic fields, they are responsible for most of the continual violent activity of the cosmos, from auroral displays in the earth's atmosphere to stellar flares and X-ray emission, and the massing of clouds of interstellar gas in galaxies. E. Parker, Scientific American (1983) 3/11/09 C. D. Dowell, Keck Institute/Dust Polarimetry 31/30
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