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 - - PowerPoint PPT Presentation

Apr 14, 2023 375 likes •669 views

Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds A&A (in publication), arXiv: 1506.06660 Corresponding authors: Clive Dickinson, Paddy Leahy Significant contributions by Mike Peel, Matias Vidal Mike Peel Jodrell Bank

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

A&A (in publication), arXiv: 1506.06660

Corresponding authors: Clive Dickinson, Paddy Leahy Significant contributions by Mike Peel, Matias Vidal

Mike Peel Jodrell Bank Centre for Astrophysics, The University of Manchester

  • n behalf of the Planck Collaboration
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Overview

Mike Peel, AME Workshop, Noordwijk, June 2016

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Overview

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!

(Figures from Planck 2015 results. X.)

Mike Peel, AME Workshop, Noordwijk, June 2016

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SLIDE 4

Overview

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

Synchrotron Hɑ Thermal Dust 30GHz foregrounds

Mike Peel, AME Workshop, Noordwijk, June 2016

(Figures from Planck 2015 results. XXV.)

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Planck early results

100 101 102 103 104 105 1 10 100 1000 Flux density [Jy] Frequency [GHz] Model Ancillary data WMAP Planck 10-2 10-1 100 101 102 103 104 105 106 1 10 100 1000 Flux density [Jy] Frequency [GHz] Model Ancillary data WMAP Planck

Perseus ρ Oph

102 103 104 105 106 1 10 100 1000 Flux density [Jy] Frequency [GHz] Model Ancillary data WMAP Planck

  • 100
  • 50

50 100 10 100 Residual flux density [Jy] Frequency [GHz]

M42

Mike Peel, AME Workshop, Noordwijk, June 2016

Planck early results. XX. New light on anomalous microwave emission from spinning dust grains A&A, 536, A20, arXiv: 1101.2031 Planck early results. XXI. Properties of the interstellar medium in the Galactic plane A&A, 536, A21, arXiv: 1101.2032

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PIP XV: Planck AME study

Mike Peel, AME Workshop, Noordwijk, June 2016

Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds A&A, 565, A103, arXiv: 1309.1357

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PIP XV: Planck AME study

Mike Peel, AME Workshop, Noordwijk, June 2016

Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds A&A, 565, A103, arXiv: 1309.1357

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PIP XXIII: Galactic Plane

Planck intermediate results. XXIII. Galactic plane emission components derived from Planck with ancillary data A&A, 580, A13, arXiv: 1406.5093

Mike Peel, AME Workshop, Noordwijk, June 2016

  • 30
  • 20
  • 10

10 20 30 100 200 300 Temperature [K] (a) 408 MHz

  • 30
  • 20
  • 10

10 20 30 2 4 6 8 10 Temperature [mK] (d) 353 GHz

408MHz 28.4GHz 353GHz

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PIP XXIII: Galactic Plane

60 40 20 340 320 300 Longitude [degrees] 0.0001 0.0010 0.0100 0.1000 1.0000 10.0000 Intensity [MJy sr-1] Thermal Dust Free-free AME Synchrotron

0.1 1.0 10.0 100 1000 10000 0.01 0.10 1.00 10.00 100.00 1000.00 10000.00 Intensity [MJy sr-1] (a) 0.1 1.0 10.0 100 1000 10000 0.01 0.10 1.00 10.00 100.00 1000.00 10000.00 Intensity [MJy sr-1] (b) 0.1 1.0 10.0 100 1000 10000 0.01 0.10 1.00 10.00 100.00 1000.00 10000.00 Intensity [MJy sr-1] (c) 0.1 1.0 10.0 100 1000 10000 Frequency [GHz] 0.01 0.10 1.00 10.00 100.00 1000.00 10000.00 Intensity [MJy sr-1] (d)

Planck intermediate results. XXIII. Galactic plane emission components derived from Planck with ancillary data A&A, 580, A13, arXiv: 1406.5093

Mike Peel, AME Workshop, Noordwijk, June 2016

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AME in nearby galaxies

0.1 1 10 100 1000 1 10 100 1000 Flux density (Jy) Frequency (GHz)

Messier 82

Model Archival data WMAP Planck 0.1 1 10 100 1000 1 10 100 1000 Flux density (Jy) Frequency (GHz)

NGC 4945

Model Archival data WMAP Planck

NGC 6946

(Murphy et al. 2010, Scaife et al. 2010, Hensley et al. 2015)

8 µm

Mike Peel, AME Workshop, Noordwijk, June 2016

0.1 1 10 100 1000 1 10 100 1000 Flux density (Jy) Frequency (GHz)

NGC 253

Model Archival data WMAP Planck

Radio to infrared spectra of late-type galaxies with Planck and WMAP data. MNRAS Letters, 416, 99, arXiv: 1105.6336

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PIP XXV: Andromeda Galaxy

Right Ascension (J2000) Declination (J2000) +40:00 +41:00 +42:00 +43:00 28.4 GHz (10.5 mm)

  • 3.75
  • 3.25

log(TRJ (K))

44.1 GHz (6.8 mm)

  • 4.0 -3.5

log(TRJ (K))

70.4 GHz (4.3 mm)

  • 4.0 -3.5

log(TRJ (K))

+40:00 +41:00 +42:00 +43:00 100 GHz (3.0 mm)

  • 4.25
  • 3.75

log(TRJ (K))

143 GHz (2.1 mm)

  • 4.25
  • 3.75

log(TRJ (K))

217 GHz (1.38 mm)

  • 4.0
  • 3.5

log(TRJ (K))

00:50 00:40 +40:00 +41:00 +42:00 +43:00 353 GHz (850 µm)

  • 4.0
  • 3.5

log(TRJ (K))

00:50 00:40 545 GHz (550 µm)

  • 4.0 -3.5 -3.0

log(TRJ (K))

00:50 00:40 857 GHz (350 µm)

  • 4.0 -3.5 -3.0

log(TRJ (K))

100 101 102 103 104 1 10 100 1000 0.1 1 10 100 1000 Flux density (Jy) Frequency (GHz) Wavelength (mm)

Synchrotron Free-free CMB Thermal dust AME

Model Archival data Planck WMAP Herschel

Parameter Value τ250 (1.2 ± 0.2) ⇥ 105 βdust 1.62 ± 0.11 Tdust [K] 18.2 ± 1.0 EM [cm6 pc] 1.8 ± 1.3 ∆TCMB [K] (1.7 ± 1.0) ⇥ 106 Asynch [Jy] 9.5 ± 1.1 αsynch 0.92 ± 0.16 AAME [Sr cm2] (7.7 ± 3.3) ⇥ 1016 χ2 15.4 Ndof 14

2.3σ

Planck intermediate results. XXV. The Andromeda Galaxy as seen by Planck A&A, 582, A28, arXiv: 1407.5452

Mike Peel, AME Workshop, Noordwijk, June 2016

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PIP XXV: Andromeda Galaxy

Mike Peel, AME Workshop, Noordwijk, June 2016

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  • Component separation mostly focuses on CMB maps, having e.g., a

single low-frequency component. (see Planck Col. 2015. IX.)

  • Commander: Bayesian technique, separate components using

frequency information (see Eriksen et al. 2008)

  • Thanks to many maps from Planck+WMAP+Haslam, we can separate:
  • Synchrotron (but fixed spectral index)
  • Free-free (EM & Te)
  • AME (two spinning dust components combined)
  • Thermal dust (only fitting up to 857GHz)
  • + CMB, CO, HCN, calibration factors, bandpass shifts;

described in Planck Col. 2015. X.

  • Also: high S/N synchrotron polarization map. Combined


Planck & WMAP data (weighted, mostly WMAP K & Planck 30).

Commander component maps

Mike Peel, AME Workshop, Noordwijk, June 2016

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Anomalous Microwave Emission

Commander AME solution

Perseus Pegasus plume ρ Ophiuchus Corona Australis Musca/Chameleon Orion λ Orionis

Mike Peel, AME Workshop, Noordwijk, June 2016

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New AME regions

AME Thermal dust Planck 28.4GHz - CMB

Pegasus plume Corona Australis Musca/ Chameleon Orion λ Orionis

Mike Peel, AME Workshop, Noordwijk, June 2016

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AME correlations

Mike Peel, AME Workshop, Noordwijk, June 2016

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Emissivities

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/τ353 appear to vary by factor of 2 Very high emissivity in λ Orionis (Also Chamaeleon) Good agreement with previous emissivities (e.g., Davies et al.)

Mike Peel, AME Workshop, Noordwijk, June 2016

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High-frequency peakers

Mike Peel, AME Workshop, Noordwijk, June 2016

(b)

Fig 3b from Planck 2016 XXV. ILC with CMB, free-free and thermal dust nulled.

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High-frequency peakers

Mike Peel, AME Workshop, Noordwijk, June 2016

Combined peak frequency from the two AME components fitted by Commander

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AME polarization

<1.6% <8.4% <12.8%

Spinning dust models predict low polarization fractions.

Mike Peel, AME Workshop, Noordwijk, June 2016

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Anomalous Microwave Emission

Commander AME solution

Perseus Pegasus plume ρ Ophiuchus Corona Australis Musca/Chameleon Orion λ Orionis

Mike Peel, AME Workshop, Noordwijk, June 2016

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Anomalous Microwave Emission

Planck+WMAP polarisation

Perseus Pegasus plume ρ Ophiuchus Corona Australis Musca/Chameleon Orion λ Orionis

Mike Peel, AME Workshop, Noordwijk, June 2016

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Comparison with WMAP

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

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

AME systematically higher Free-free about the same Synchrotron lower

|b| > 20°

Mike Peel, AME Workshop, Noordwijk, June 2016

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Large Magellanic Cloud

(a) Synchrotron

10 20 30 40 50

µK at 30 GHz (b) Free-free

10 100 1000

cm−6 pc (c) Spinning dust

10 30 100 300

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 Could be too steep? AME emissivities comparable to our Galaxy (except 100um)

Mike Peel, AME Workshop, Noordwijk, June 2016

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Large & Small Magellanic Clouds

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

Mike Peel, AME Workshop, Noordwijk, June 2016

AME <~0.2Jy c.f. 3-5Jy from Hensley

LMC SMC

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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. AME emission seems best correlated with thermal dust at 545GHz.
  • 3. New diffuse AME regions identified, λ Orionis particularly interesting.
  • 4. Upper limit on pol. AME of 1.6%: need better pol. synchrotron maps!
  • 5. Fixed synchrotron spectral index is a key limitation.
  • 6. Need better data at 2-15GHz, e.g. S-PASS, C-BASS & QUIJOTE



 For Commander analysis and maps, see arXiv:1502.01588
 For the results presented here, see arXiv:1506.06660

Conclusions

Mike Peel, AME Workshop, Noordwijk, June 2016

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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