An improved map of the Galactic Faraday sky

NOTE: This is a reupload of the data set originally hosted at http://www.mpa-garching.mpg.de/ift/faraday/ . Below follows the content of the corresponding webpage, with only slight changes concerning formatting and the removal of obsolete links and contact information. An improved map of the galactic Faraday sky Here you can download the results presented in the paper "An improved map of the galactic Faraday sky" (arXiv:1111.6186) by Niels Oppermann, Henrik Junklewitz, Georg Robbers, Mike R. Bell, Torsten A. Enßlin, Annalisa Bonafede, Robert Braun, Jo-Anne C. Brown, Tracy E. Clarke, Ilana J. Feain, Bryan M. Gaensler, Alison Hammond, Lisa Harvey-Smith, George Heald, Melanie Johnston-Hollitt, Uli Klein, Phil P. Kronberg, S. Ann Mao, Naomi M. McClure-Griffiths, Shane P. O'Sullivan, Luke Pratley, Tim Robishaw, Subhashis Roy, Dominic H.F.M. Schnitzeler, Carlos Sotomayor-Beltran, Jamie Stevens, Jeroen M. Stil, Caleb Sunstrum, Anant Tanna, A. Russell Taylor, and Cameron L. Van Eck. Note that there was an UPDATE to the map on 2012-03-05 due to an update in one of the data catalogs. In the faraday.fits file, you find the the results of the paper stored in HEALPIX format. The file contains six binary table extensions: The reconstructed signal map, i.e. the galactic Faraday depth divided by a galactic variance profile The corresponding uncertainty map. The reconstructed map of the galactic Faraday depth in rad/m2. The corresponding uncertainty map in rad/m2. The map of the galactic variance profile, i.e. the ratio between the Faraday depth and the signal field, in rad/m2. The reconstructed angular power spectrum of the signal field All maps are presented at a HEALPIX resolution of Nside=128 and are stored in RING ordering scheme. The power spectrum ranges from multipole scales of l=0 to l=383. Acknowledgment The authors would like to thank Steven R. Spangler for the valuable contributions he made to this paper as a referee. N.O. thanks Marco Selig and Maximilian Ullherr for fruitful discussions during the genesis of this work. Some of the results in this paper have been derived using the HEALPIX package (Gorski et al. (2005). The calculations were performed using the SAGE mathematics software. This research has made use of NASA's Astrophysics Data System. This research was performed in the framework of the DFG Forschergruppe 1254 "Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations. Basic research in radio astronomy at the Naval Research Laboratory is funded by 6.1 Base funding. B.M.G. and T.R. acknowledge the support of the Australian Research Council through grants FF0561298, FL100100114 and FS100100033. M.J.-H. and L.P. acknowledge support via Victoria University of Wellington Faculty of Science and Marsden Development Fund research grants awarded to M.J.-H. The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This paper includes archived data obtained through the Australia Telescope Online Archive. NOTE: below is the traceback of the Wayback Machine that was used to download data and original webpage: FILE ARCHIVED ON 02:18:00 Feb 25, 2022 AND RETRIEVED FROM THE INTERNET ARCHIVE ON 08:43:40 Dec 15, 2025. JAVASCRIPT APPENDED BY WAYBACK MACHINE, COPYRIGHT INTERNET ARCHIVE ALL OTHER CONTENT MAY ALSO BE PROTECTED BY COPYRIGHT (17 U.S.C. SECTION 108(a)(3)).