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Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds - - PowerPoint PPT Presentation

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Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds A&A (submitted), arXiv: 1506.06660 Mike Peel Jodrell Bank Centre for Astrophysics, University of Manchester on behalf of the Planck Collaboration Overview Total

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Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds

A&A (submitted), arXiv: 1506.06660

Mike Peel Jodrell Bank Centre for Astrophysics, University of Manchester

  • n behalf of the Planck Collaboration
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Overview

Mike Peel, NAM, Llandudno, July 2015

10 30 100 300 1000

Frequency (GHz)

10

  • 1

10 10

1

10

2

Rms brightness temperature (µKRJ)

CMB Thermal dust Free-free Synchrotron 30 44 70 100 143 217 353 545 857 S p i n n i n g d u s t

CO 1-0

Sum fg

10 30 100 300 1000

Frequency (GHz)

10

  • 1

10 10

1

10

2

Rms brightness temperature (µK)

CMB Thermal dust Synchrotron 30 44 70 100 143 217 353 Sum fg

Total intensity Polarization Dominated by Galactic emission at nearly every frequency Need to understand them well to subtract them. Also interesting in their own right!

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Overview

Mike Peel, NAM, Llandudno, July 2015

(a) (b) (c) (d)

Synchrotron Hɑ Thermal Dust 30GHz foregrounds

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  • 1. Many previous attempts at component separation
  • 2. Spinning dust predicted 1957 …
  • 3. By-product of CMB maps

Mike Peel, NAM, Llandudno, July 2015

Motivation

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Free-free emission

Mike Peel, NAM, Llandudno, July 2015

50 40 30 20 10 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

50 40 30 20 10 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

350 340 330 320 310 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

350 340 330 320 310 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

300 290 280 270 260 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

300 290 280 270 260 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

7.0 15.0

240 230 220 210 200 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

4.5 10.0

240 230 220 210 200 l [degree]

  • 4
  • 2

2 4 b [degree]

  • 1.0

4.5 10.0

RRLs (Alves et al.) Commander free-free

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Free-free emission

Mike Peel, NAM, Llandudno, July 2015

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Hɑ scattering

Mike Peel, NAM, Llandudno, July 2015

Residual Ha after subtracting mean correlation Traces scattered light? 28+-12% 36+-12% (after dust absorption correction)

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Anomalous Microwave Emission

Mike Peel, NAM, Llandudno, July 2015

Commander AME solution

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AME correlations

Mike Peel, NAM, Llandudno, July 2015

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New AME regions

Mike Peel, NAM, Llandudno, July 2015

AME Thermal dust Planck 28.4GHz - CMB

2 3 5 6 7

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Emissivities

Mike Peel, NAM, Llandudno, July 2015

Region . . . . . . . . AME/545 GHz AME/100 µm AME/τ353 [µK (MJy sr1)1] [µK (MJy sr1)1] [µK 106] R1: Perseus . . . . . 24 ± 7 12.3 ± 1.9 1.5 ± 0.9 R2: Plume . . . . . 47 ± 6 18 ± 2 7.7 ± 1.0 R3: R CrA . . . . . 36 ± 14 50 ± 12 4.1 ± 1.8 R4: ρ Oph . . . . . . 40 ± 9 4.6 ± 0.9 2.2 ± 1.2 R5: Musca . . . . . 59 ± 8 26 ± 3 6.9 ± 1.0 Chamaeleon . 74 ± 8 22 ± 2 11 ± 1.1 R6: Orion . . . . . . 47 ± 5 20 ± 2 4.7 ± 0.6 R7: λ Orionis . . . 104 ± 11 25 ± 3 15 ± 1.8 Entire sky . . . . . . 65 ± 7 22 ± 2 8.3 ± 0.8 |b| > 10 . . . . . . . 70 ± 7 21 ± 2 9.7 ± 1.0 XV: Perseus . . . . . . . 24 ± 4 . . . XV: ρ Oph . . . . . . . . 8.3 ± 1.1 . . . XV: Mean . . . . . . . . . 32 ± 4 . . . D06: Kp2 mask . . . . . 21.8 ± 1.0 . . . D06: Region mean . . . 25.7 ± 1.3 . . .

Emissivities against 545/t353 vary by factor of 2

  • v. high emissivity in λ Orionis

…

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Synchrotron emission

Mike Peel, NAM, Llandudno, July 2015

Synchrotron spectrum based on Galprop (Orlando & Strong 2013)

As

10 30 100 300 KRJ @ 408 MHz

Amplitude based on Haslam 408MHz

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Comparison with WMAP

Mike Peel, NAM, Llandudno, July 2015

Synchrotron is not 1:1 - two populations due to spectral indices

Run Sync Free-free AME a r a r a r MCMC-c base 0.50 0.62 0.68 0.77 . . . . . . MCMC-e sdcnm 0.52 0.92 0.77 0.87 4.91 0.75 MCMC-f fs 0.52 0.62 0.80 0.77 3.18 0.67 MCMC-g fss 0.55 0.62 0.77 0.78 3.14 0.70 MEM 0.34 0.84 0.76 0.79 2.18 0.86 MCMC-c base 0.12 0.74 0.91 0.83 . . . . . . MCMC-e sdcnm 0.61 0.99 0.67 0.98 2.71 0.91 MCMC-f fs 0.13 0.78 1.09 0.89 4.71 0.86 MCMC-g fss 0.15 0.77 1.06 0.93 3.22 0.88 MEM 0.19 0.90 1.01 0.97 2.36 0.93

a>1 = commander > WMAP Trust values if r≳0.9

AME systematically higher Free-free about the same Synchrotron lower, however:

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LMC/SMC

Mike Peel, NAM, Llandudno, July 2015 (a) Synchrotron

10 20 30 40 50

µK at 30 GHz (b) Free-free

10 100 1000

cm−6 pc (c) Spinning dust

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µK at 30 GHz (d) Thermal dust

10 100 1000

µK at 545 GHz (e) Synchrotron polarization

10 20 30

µK at 30 GHz (f) CMB

−200 −100 100 200

µKCMB (g) CO J=2→1

0.2 0.4 0.6 0.8 1.0

K km s−1 (h) Thermal dust polarization

5 10 15 20

µK at 353 GHz

30 Dor

Clean CMB map Good agreement with ground- based surveys Up to 30% pol. Dominates SED

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SMC/LMC

Mike Peel, NAM, Llandudno, July 2015

101 102 103 104 105 106 0.1 1 10 100 1000 Flux density (Jy) Wavelength (mm) Model Archival data WMAP Planck 100 101 102 103 104 105 0.1 1 10 100 1000 Flux density (Jy) Frequency (GHz) Model Archival data WMAP Planck

(plots to be redone to fill in empty x-axes!)

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Mike Peel, NAM, Llandudno, July 2015

AME polarization

<1.6% <12.8%

See Paddy Leahy’s talk about Planck polarization!

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  • 1. Commander has done a relatively clean separation of Planck & WMAP

data into synchrotron, free-free, AME & thermal dust emission (+CO, HCN)

  • 2. New diffuse AME regions identified, λ Orionis particularly interesting.
  • 3. Upper limit on pol. AME of 1.6%: need better pol. synchrotron maps!
  • 4. Need better data at 2-15GHz, e.g. S-PASS, C-BASS & QUIJOTE

  • 5. For Commander results, see arXiv:1502.01588
  • 6. For the results presented here, see arXiv:1506.06660
  • 7. For more polarization results, see Paddy Leahy’s talk

Mike Peel, NAM, Llandudno, July 2015

Conclusions

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Planck is a project

  • f the European

Space Agency, with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark.

X name "The talk"

The scientific results that we present today are a product of the Planck Collaboration, including individuals from more than 100 scientific institutes in Europe, the USA and Canada.

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Thank you

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C-Band All-Sky Survey: A First Look at the Galaxy

Irfan et al. (2015), MNRAS, 448, 3572; arXiv:1501.06069