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

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 intensity Polarization 30 44 70 100 143 217 353 30 44 70 100 143 217 353 545 857 Sum fg Thermal dust Synchrotron Rms brightness temperature ( µ K RJ ) Rms brightness temperature ( µ K) 2 2 10 10 CMB Thermal dust 1 1 10 10 Sum fg Free-free 0 0 10 10 S CMB p CO 1-0 i n Synchrotron n i n g d -1 -1 u 10 10 s t 10 30 100 300 1000 10 30 100 300 1000 Frequency (GHz) Frequency (GHz) Dominated by Galactic emission at nearly every frequency Need to understand them well to subtract them. Also interesting in their own right! Mike Peel, NAM, Llandudno, July 2015

Overview (a) (b) 30GHz foregrounds Synchrotron (c) (d) Thermal Dust H ɑ Mike Peel, NAM, Llandudno, July 2015

Motivation 1. Many previous attempts at component separation 2. Spinning dust predicted 1957 … 3. By-product of CMB maps Mike Peel, NAM, Llandudno, July 2015

Free-free emission RRLs (Alves et al.) Commander free-free 15.0 15.0 4 4 b [degree] b [degree] 2 2 7.0 7.0 0 0 -2 -2 -4 -4 -1.0 -1.0 50 40 30 20 10 0 50 40 30 20 10 0 l [degree] l [degree] 15.0 15.0 4 4 b [degree] b [degree] 2 2 7.0 7.0 0 0 -2 -2 -4 -4 -1.0 -1.0 350 340 330 320 310 350 340 330 320 310 l [degree] l [degree] 15.0 15.0 4 4 b [degree] b [degree] 2 2 7.0 7.0 0 0 -2 -2 -4 -4 -1.0 -1.0 300 290 280 270 260 300 290 280 270 260 l [degree] l [degree] 10.0 10.0 4 4 b [degree] b [degree] 2 2 4.5 4.5 0 0 -2 -2 -4 -4 -1.0 -1.0 240 230 220 210 200 240 230 220 210 200 l [degree] l [degree] Mike Peel, NAM, Llandudno, July 2015

Free-free emission Mike Peel, NAM, Llandudno, July 2015

H ɑ scattering Residual Ha after subtracting mean correlation 28+-12% Traces scattered light? 36+-12% (after dust absorption correction) Mike Peel, NAM, Llandudno, July 2015

Anomalous Microwave Emission Commander AME solution Mike Peel, NAM, Llandudno, July 2015

AME correlations Mike Peel, NAM, Llandudno, July 2015

New AME regions AME Thermal dust Planck 28.4GHz - CMB 2 3 5 6 7 Mike Peel, NAM, Llandudno, July 2015

Emissivities Emissivities against 545/t353 Region . . . . . . . . AME / 545 GHz AME / 100 µ m AME / τ 353 [ µ K (MJy sr � 1 ) � 1 ] [ µ K (MJy sr � 1 ) � 1 ] [ µ K 10 � 6 ] vary by factor of 2 R1: Perseus . . . . . 24 ± 7 12 . 3 ± 1 . 9 1 . 5 ± 0 . 9 R2: Plume . . . . . 47 ± 6 18 ± 2 7 . 7 ± 1 . 0 v. high emissivity in λ Orionis 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 . . . . . . Mike Peel, NAM, Llandudno, July 2015

Synchrotron emission A s 10 30 100 300 K RJ @ 408 MHz Synchrotron spectrum Amplitude based on based on Galprop Haslam 408MHz (Orlando & Strong 2013) Mike Peel, NAM, Llandudno, July 2015

Comparison with WMAP 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 Synchrotron is not Free-free about the same 1:1 - two populations Synchrotron lower, however: due to spectral indices Mike Peel, NAM, Llandudno, July 2015

LMC/SMC Dominates 30 Dor SED (b) Free-free (a) Synchrotron (c) Spinning dust (d) Thermal dust 0 10 100 1000 10 20 30 40 50 10 30 100 300 10 100 1000 cm − 6 pc µ K at 30 GHz µ K at 30 GHz µ K at 545 GHz (e) Synchrotron polarization (f) CMB (g) CO J =2 → 1 (h) Thermal dust polarization 0 10 20 30 − 200 − 100 0 100 200 0 0.2 0.4 0.6 0.8 1.0 0 5 10 15 20 µ K CMB K km s − 1 µ K at 30 GHz µ K at 353 GHz Up to Clean Good agreement 30% pol. CMB map with ground- based surveys Mike Peel, NAM, Llandudno, July 2015

SMC/LMC Wavelength (mm) 1000 100 10 1 0.1 10 5 10 6 Model Model Archival data 10 4 Archival data WMAP 10 5 WMAP Flux density (Jy) Planck 10 3 Flux density (Jy) Planck 10 4 10 2 10 3 10 1 10 2 10 0 10 1 0.1 1 10 100 1000 Frequency (GHz) (plots to be redone to fill in empty x-axes!) Mike Peel, NAM, Llandudno, July 2015

AME polarization <1.6% <12.8% See Paddy Leahy’s talk about Planck polarization! Mike Peel, NAM, Llandudno, July 2015

Conclusions 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

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. Planck is a project of 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"

Thank you

C-Band All-Sky Survey: A First Look at the Galaxy Irfan et al. (2015), MNRAS, 448, 3572; arXiv:1501.06069