A Full-Sky Hα Template for Microwave Foreground Prediction

By Douglas P. Finkbeiner. 2003

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A full-sky Hα map with 6′ (FWHM) resolution is presented. This map is a composite of the Virginia Tech Spectral line Survey (VTSS) in the north and the Southern H-Alpha Sky Survey Atlas (SHASSA) in the south. The Wisconsin H-Alpha Mapper (WHAM) survey provides a stable zero point over 3/4 of the sky on a 1° scale. This composite map can be used to provide limits on thermal bremsstrahlung (free-free emission) from ionized gas known to contaminate microwave-background data. The map is available on the World Wide Web for public use.

Subfields: Atmospheric Science, Global and Planetary Change, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/55376612673032aa782b112b7ce6e4bf1c1dc6af

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Citations in the corpus

A full sky, low foreground, high resolution CMB map from WMAP (2008, methodology): “An additional free-free template is obtained from Hα emission (Finkbeiner 2003) corrected for dust extinction (Bennett et al. 2003).”
Non-Gaussian signatures in the temperature fluctuation observed by the Wilkinson Microwave Anisotropy Probe (2003, methodology): “Therefore, we use the 100-µm dust (Schlegel, Finkbeiner & Davis 1998; Finkbeiner, Davis & Schlegel 1999), Hα (Finkbeiner 2003) and synchrotron (Haslam et al. 1981, 1982) emission maps multiplied with coefficients given in table 3 of Bennett et al. (2003b) to reduce the foreground emission in each…”
The Outer Scale of Turbulence in the Magnetoionized Galactic Interstellar Medium (2008, methodology): “Therefore, we have used the total intensity 1.4 GHz radio data from the ATCA combinedwith Parkes singledish data, as well as H maps (Finkbeiner 2003), to discard 27 extragalactic sources with a sight line passing through a visible supernova remnant or H ii region.”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: ANGULAR POWER SPECTRA (2008, methodology): “For the temperature map, three templates are used: a synchrotron template (the WMAP K − Ka difference map), an Hα template as a proxy for free-free (Finkbeiner 2003), and a thermal dust template (Finkbeiner et al. 1999).”
First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission (2003, neutral): “Finkbeiner (2003) assembled a full sky Hα map using data from several surveys: the Wisconsin H-Alpha Mapper (WHAM), the Virginia Tech Spectral-Line Survey (VTSS), and the Southern H-Alpha Sky Survey Atlas (SHASSA).”
Radio observational constraints on Galactic 3D-emission models (2007, methodology): “Hinshaw et al. (2007) used the Hα template by Finkbeiner (2003) as a prior estimate in the maximum entropy method analysis of the 3-year WMAP data to construct the free-free emission template.”
The non‐Gaussian cold spot in Wilkinson Microwave Anisotropy Probe: significance, morphology and foreground contribution (2006, methodology): “For the free–free emission we consider the Hα map of Finkbeiner (2003), with magnitudes c© 0000 RAS, MNRAS 000, 000–000 corrected by the Galactic reddening E(B–”
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)).”
A NEW ELECTRON-DENSITY MODEL FOR ESTIMATION OF PULSAR AND FRB DISTANCES (2016, methodology): “On the basis of an image from the Southern Hα Sky Survey Atlas (Finkbeiner 2003), Purcell et al. (2015) modeled the GN with a spherical shell of outer angular radius ~ 23 as seen from the Sun (corresponding to a physical radius of about 170 pc) and thickness about 20 pc. Based on the DMs of pulsars…”
Microwave Interstellar Medium Emission Observed by the Wilkinson Microwave Anisotropy Probe (2004, methodology): “The WMAP strategy, using data at the WMAP frequencies and priors based on the Haslam et al. (1982) 408 MHz map, the Finkbeiner (2003) H map, and the Finkbeiner et al. (1999; hereafter FDS99) dust prediction, produces a ‘‘synchrotron’’ template highly correlated with thermal dust emission (see Fig.”
Detection of Non-Gaussianity in the Wilkinson Microwave Anisotropy Probe First-Year Data Using Spherical Wavelets (2003, methodology): “The 94 GHz dust map of Finkbeiner et al. (1999) is used as the thermal dust template; the H map of Finkbeiner (2003) corrected for extinction through the EB V map of Schlegel et al. (1998) is used as 3 During the refereeing process new works have appeared in astro-ph, such as Eriksen et al. (2004b).”
The AAO/UKST SuperCOSMOS Hα survey (2005, methodology): “Finkbeiner (2003) also showed there is no significant offset between WHAM and SHASSA data.”
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.”
Hemispherical Power Asymmetry in the Third-Year Wilkinson Microwave Anisotropy Probe Sky Maps (2007, methodology): “For the Q-band data, we marginalize over a synchrotron (Haslam et al. 1982), a free-free (Finkbeiner 2003), and a dust (Finkbeiner et al. 1999) template individually.”