Microwave Interstellar Medium Emission Observed by the Wilkinson Microwave Anisotropy Probe

By Douglas P. Finkbeiner. 2004

258 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ef74ee9ab2d15d29b44e77565015664382dfc8b3

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Citations in the corpus

Dark Matter Searches with Astroparticle Data (2011, methodology): “At GHz frequencies, analysis of the Wilkinson Microwave Anisotropy Probe (WMAP) data showed evidence for excess diffuse emission within a 20◦ radial region about the center of the Milky Way, which was called the WMAP haze (Finkbeiner, 2004).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “The first claim of a haze (Finkbeiner 2004) suggested an excess of free-free emission compared to the expectation from Hα, and was dubbed a “free-free haze”.”
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).”
POLARIZED FAR-INFRARED AND SUBMILLIMETER EMISSION FROM INTERSTELLAR DUST (2008, unknown): “75 GHz) (Draine & Lazarian 1998; Finkbeiner 2004).”
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 ].”
THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE (2009, methodology): “…which roughly matches the microwave haze (i.e., centered on the GC, roughly spherical, and about 20-40◦ in radius), we now attempt to remove the π0 emission from the maps shown in Figure 1, using the same template fitting technique used in Finkbeiner (2004a) and Dobler & Finkbeiner (2008).”
GIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND? (2010, background): “Other hypotheses such as free-free, spinning dust, or thermal dust have failed to explain its morphology, spectrum, or both (Finkbeiner 2004b; Dobler & Finkbeiner 2008).”
THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES (2014, background): “…(Dobler et al. 2010; Su et al. 2010; Su & Finkbeiner 2012) in a search for a gamma-ray counterpart to the Wilkinson Microwave Anisotropy Probe (WMAP) haze (Finkbeiner 2004), which is residual microwave emission around the Galactic center that remains after subtracting synchrotron, free-free,…”
Extended Anomalous Foreground Emission in the WMAP Three-Year Data (2007, methodology): ““Anomalous” ISM emission mechanisms Given their dual approach, an important question to address is: why have the foreground analyses of the WMAP team not positively identified the spinning dust emission in DF07 and the haze emission in Finkbeiner (2004)?”
The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST (2008, methodology): “The set of models we have considered includes a model similar to the one recently proposed by Hooper et al. (2007) to explain the excess microwave emission around the Galactic center measured by WMAP (so-called “WMAP haze”, Finkbeiner 2004).”
Three Year Wilkinson Microwave Anistropy Probe (WMAP) Observations: Polarization Analysis (2006, methodology): “Finkbeiner (2004) and de Oliveira-Costa et al. (2004) argue that the Tenerife and Green Bank data show evidence for a rising spectrum between 10 and 15 GHz, suggesting the presence of spinning dust.”