Microwave ISM Emission Observed by WMAP

By Douglas P. Finkbeiner. 2003

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We investigate the nature of the diffuse Galactic emission in the Wilkinson Microwave Anisotropy Probe (WMAP) temperature anisotropy data. Substantial dust-correlated emission is observed at all WMAP frequencies, far exceeding the expected thermal dust emission in the lowest frequency channels (23, 33, 41 GHz). The WMAP team (Bennett et al.) interpret this emission as dust-correlated synchrotron radiation, attributing the correlation to the natural association of relativistic electrons produced by SNae with massive star formation in dusty clouds, and deriving an upper limit of 5% on the contribution of Draine & Lazarian spinning dust at K-band (23 GHz). We pursue an alternative interpretation that much, perhaps most, of the dust-correlated emission at these frequencies is indeed spinning dust, and explore the spectral dependence on environment by considering a few specific objects as well as the full sky average. Models similar to Draine & Lazarian spinning dust provide a good fit to the full-sky data. The full-sky fit also requires a significant component with free-free spectrum uncorrelated with \Halpha, possibly hot (~million K) gas within 30 degrees of the Galactic center.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/bd2defb15142586ccc73a2ef2fd0cef10605c09f

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Citations in the corpus

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].”
WIMP dark matter candidates and searches—current status and future prospects (2017, background): “Interesting features were identified in the spectrum of γ-rays originating from regions around the GC in the WMAP data [342] (so-called WMAP haze), Fermi-LAT data [343, 344] (Fermi bubbles) and Planck data [345] (Planck haze), with a possible common origin.”
Non-abelian dark sectors and their collider signatures (2009, unknown): “Together with the CMB haze [5, 6, 7], these observations paint a consistent picture whereby DM annihilates primarily into muons and/or electrons [8].”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “The templates most often used for this purpose are the Haslam 408 MHz map, a de-extincted form of the Finkbeiner (2003) Hα all-sky mosaic and the Finkbeiner et al. (1999) thermal dust models.”
Probing dark forces and light hidden sectors at low-energy e+e- colliders (2009, background): “If their source is dark matter annihilation or decay, synchrotron radiation from these electrons and positrons could also explain the WMAP haze near the galactic center [25].”
Extended Anomalous Foreground Emission in the WMAP Three-Year Data (2007, methodology): “Our template for this foreground is the Hα map, assembled from the VTSS (Dennison et al. 1998), SHASSA (Gaustad et al. 2001), and WHAM (Haffner et al. 2003) surveys by Finkbeiner (2003).”
Separation of anomalous and synchrotron emissions using WMAP polarization data (2008, methodology): “Hα, corrected for dust extinction, is often used as a proxy for free-free as they both depend linearly on the emission measure, EM= ∫ n2e dl (see Dickinson et al. (2003) and Finkbeiner (2003)).”