1 / 14

NOTES ON THE 15 FIELDS

SPECTRA OF GALACTIC COMPONENTS OBSERVED BY WMAP R.D.Davies, R.J.Davis Jodrell Bank Observatory C.Dickinson California Institute of Technology A.J.Banday, T.R.Jaffe MPI fur Astrophysik K.M.Gorski Caltech and JPL.

leoma
Download Presentation

NOTES ON THE 15 FIELDS

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. SPECTRA OF GALACTIC COMPONENTS OBSERVED BY WMAPR.D.Davies, R.J.Davis Jodrell Bank ObservatoryC.Dickinson California Institute of TechnologyA.J.Banday, T.R.Jaffe MPI fur AstrophysikK.M.Gorski Caltech and JPL Five regions in each of the foregrounds (free-free, synchrotron and anomalous dust) were selected for study which were minimally contaminated by the others. The standard templates (H-alpha, 408 MHz and 100-micron dust) were used in both a T-T and a cross-correlation analysis. The emissivity of each component in the WMAP frequency range was determined. The implications for determining the correction for CMB foreground emission, both in total power and polarization, are discussed.

  2. Polarisation 2005

  3. THE POSITIONS OF THE 15 REGIONS CHOSEN FOR STUDYFields 1-5 are free-free; fields 6-10 are dust; fields 11-15 are synchrotron. Polarisation 2005

  4. NOTES ON THE 15 FIELDS Polarisation 2005

  5. FIELD 4 – FREE-FREE DOMINATEDl = 250 to 260 b = -25 to -35 Polarisation 2005

  6. FIELD 6 – DUST DOMINATEDl = 118 to 135 b = +20 to =37 Polarisation 2005

  7. FIELD 11 – SYNCHROTRON DOMINATEDl = 33 to 45 b = +50 to +70 Polarisation 2005

  8. T-T PLOTS FOR FIELD 6 (DUST DOMINATED)The dust correlation for the K, Ka and Q bands Polarisation 2005

  9. THE FREE-FREE EMISSION AT K AND Ka BANDSComparison for Te = 8000K Polarisation 2005

  10. DUST AND SYNCHROTRON EMISSION IN WMAP BANDS Polarisation 2005

  11. CROSS-CORRLATION RESULTS FOR THE THREE FOREGROUNDSFor each foreground the average value is given in each band.There is agreement with the T-T analysis. Polarisation 2005

  12. DUST EMISSIVITIES IN 10 INDIVIDUAL CLOUDS Polarisation 2005

  13. AVERAGE DUST EMISSIVITY (10 CLOUDS) SPARATED INTO VIBRATIONAL AND ANOMALOUS COMPONENTSIndex of +1.67 is assumed for vibrational component. Polarisation 2005

  14. CONCLUSIONS The spectra of the free-free and synchrotron components were essentially as expected. For free-free the electron temperature is in the range 7000 – 8000K, with a spectral index of -2.13. The synchrotron spectral index at WMAP frequencies is -3.0 to -3.1. However the anomalous dust emissivity varies by a factor of 2 from cloud to cloud. The construction of an anomalous dust template for Planck will need to account for this varying emissivity. The predicted polarized emission from dust may be similarly affected. Polarisation 2005

More Related