Extended Anomalous Foreground Emission in the WMAP Three-Year Data

By Gregory Dobler, Douglas P. Finkbeiner. 2007

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We study the spectral and morphological characteristics of the diffuse Galactic emission in the WMAP temperature data using a template-based multilinear regression, and obtain the following results. (1) We confirm previous observations of a bump in the dust-correlated spectrum, consistent with the Draine & Lazarian spinning dust model. (2) We also confirm the “haze” signal in the inner Galaxy, and argue that it does not follow a free-free spectrum as first thought, but instead is synchrotron emission from a hard electron cosmic-ray population. (3) In a departure from previous work, we allow the spectrum of Hα-correlated emission (which is used to trace the free-free component) to float in the fit, and find that it does not follow the expected free-free spectrum. Instead there is a bump near 50 GHz, modifying the spectrum at the 20% level, which we speculate is caused by spinning dust in the warm ionized medium. (4) The derived cross-correlation spectra are not sensitive to the map zero points, but are sensitive to the choice of CMB estimator. In cases where the CMB estimator is derived by minimizing variance of a linear combination of the WMAP bands, we show that a bias proportional to the cross-correlation of each template and the true CMB is always present. This bias can be larger than any of the foreground signals in some bands. (5) Lastly, we consider the frequency coverage and sensitivity of the Planck mission, and suggest linear combination coefficients for the CMB template that will reduce both the statistical and systematic uncertainty in the synchrotron and haze spectra by more than an order of magnitude.

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Citations in the corpus

THE FERMI BUBBLES. I. POSSIBLE EVIDENCE FOR RECENT AGN JET ACTIVITY IN THE GALAXY (2011, background): “…produces microwave synchrotron radiation, which was previously invoked to explain the microwave haze (at tens of GHz) discovered by the Wilkinson Microwave Anisotropy Probe (WMAP) - the ‘WMAP haze’, which is spatially associated with the Fermi bubbles (Finkbeiner 2004; Dobler & Finkbeiner 2008).”
Non-abelian dark sectors and their collider signatures (2009, unknown): “carrier. ATIC [2] detects an abundance of cosmic ray electrons between 300 − 800 GeV, while PAMELA [3] sees an excess of positrons (but not anti-protons [4]) at 10-100 GeV. Together with the CMB haze [5, 6, 7], these observations paint a consistent picture whereby DM annihilates primarily into muons”
GIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND? (2010, background): “30◦, these “Fermi bubbles” have a spatial morphology similar to the WMAP microwave haze (Finkbeiner 2004a; Dobler & Finkbeiner 2008).”
THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE (2009, methodology): “Here the 41 GHz synchrotron (haze plus Haslam-correlated emission, see Haslam et al. 1982; Dobler & Finkbeiner 2008) is shown side by side with the 5-10 GeV Fermi residual map with the mask used in the Dobler & Finkbeiner (2008) microwave analysis overlaid for visualization.”
Gamma Ray Signals from Dark Matter: Concepts, Status and Prospects (2012, background): “, they correspond to DM masses in the ∼MeV [209–211], ∼10 GeV [185, 212, 213], ∼100 GeV [214], ∼TeV [61, 215–217] (sometimes with possible counterparts at radio frequencies [218–220]) or even multi-TeV range [221–223].”
Background model systematics for the Fermi GeV excess (2014, background): “Moreover, the analysis of gamma-ray data has led to the discovery of the Fermi bubbles [23, 24], which are believed to be the inverse Compton scattering (ICS) counterpart [23] of the WMAP haze [25, 26], recently observed also with Planck [27].”
Abelian hidden sectors at a GeV (2009, background): “The positron and electron excesses seen by PAMELA [18], ATIC [19], and PPB-BETS [20], as well as the WMAP haze [21–23], can arise from dark matter annihilation, but seem to require an enhanced annihilation rate today relative to the value yielding the correct thermal relic density.”
Dark Matter Searches with Astroparticle Data (2011, background): “Further analysis of 3-year (Dobler & Finkbeiner, 2008; Bottino, Banday & Maino, 2008) and 5-year WMAP data (Bottino, Banday & Maino, 2010) also showed evidence of the excess emission, but analysis of the 7-year WMAP data (Gold et al., 2010) does not show evidence for a polarized signal, casting…”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “This excess appeared as a residual from the decomposition of WMAP K, Ka and Q maps using external templates (Finkbeiner 2004; Dobler & Finkbeiner 2008).”
Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization (2014, background): “…microwave emission (AME, Kogut et al. 1996; Leitch et al. 1997; de Oliveira-Costa et al. 1999; Banday et al. 2003; Lagache 2003; Davies et al. 2006; Dobler & Finkbeiner 2008; Miville-Deschênes et al. 2008; Ysard et al. 2010; Planck Collaboration XX 2011), and possibly dipolar magnetic emission of…”