The results are provided as hdf5 files. See here for information about the file format and here for the python interface.

Alternative fits files containing the same information are also provided.

All results provided make use of the 'polar caps' data split described in the paper.

In this hdf5 file, you find the reconstruction of the Galactic Faraday depth, stored in HEALPix format. The structure of the file is the following:

'angspec': The reconstructed angular power spectrum of the dimensionless auxiliary field as shown in Fig. 10 of the paper. The values correspond to multipoles from *l*=0 to *l*=383.

'profile': The Galactic variance profile that relates the dimensionless auxiliary field and the Galactic Faraday depth, as shown in Fig. 11, in units of rad/m^{2}.

'maps/s': The reconstructed dimensionless auxiliary field, i.e., the Galactic Faraday depth divided by the Galactic variance profile.

'maps/phi': The reconstructed Galactic Faraday depth in units of rad/m^{2}.

'uncertainty/s': The pixel-wise uncertainty of the reconstructed dimensionless auxiliary field.

'uncertainty/phi': The pixel-wise uncertainty of the reconstructed Galactic Faraday depth in units of rad/m^{2}.

The last five results are stored as RING-ordered HEALPix maps at a resolution of *N*_{side}=128. The last four results correspond to the top four panels of Fig. 15.

Alternatively, you may use this fits file, which contains six binary table extensions corresponding to the six data sets described above. The names of the extensions are the same as the names of the data sets in the hdf5 file (i.e. ANGSPEC, PROFILE, MAPS/S, MAPS/PHI, UNCERTAINTY/S, UNCERTAINTY/PHI).

Here we provide samples drawn from the approximate posterior
probability distribution for the extragalactic contributions
to each data point. Each sample consists of 41632 numbers, the
extragalactic contributions to each of the data points, in
rad/m^{2}. We provide 1000 such samples in total. Each
one of these samples represents a possible configuration of
extragalactic Faraday rotation contributions that is not ruled
out by the data.

A range of values that is less likely
appears less often in the samples and vice versa. Thus, the frequency with
which the sample values lie within a certain interval gives
the posterior probability for the true extragalactic
contribution to lie within that interval.

When calculating a quantity as a function of the extragalactic
Faraday contribution for one or several sources, this function
should be evaluated for each of the samples. This will yield
1000 different answers. The distribution of these answers corresponds
roughly to the posterior distribution for the quantity of
interest, given the data and assumptions used in our
paper.

Obviously, using a smaller number of samples is possible, but
the more samples are used, the more accurate the resulting
distribution.

See Appendix D of the paper for a more detailed description of
the suggested usage of these samples.

We provide one file containing all 1000 samples and one
containing a subset consisting of the first 100 samples. The
latter is provided to limit the data volume to be downloaded
for testing purposes or if a smaller number of samples is to
be used.

The structue of the hdf5 files is the following. The file
contains three groups, 'sourceinfo/', 'samples/', and 'summary/'. The contents of 'sourceinfo/' are:

'sourceinfo/catalog': The name of the catalogs from which the data points are taken, using the nomenclature of Table 1 of Oppermann et al. (2012) and "Mao 2012" for the newly added data points.

'sourceinfo/Gal_lon': Galactic longitude of the data points in degrees.

'sourceinfo/Gal_lat': Galactic latitude of the data
points in degrees.

'sourceinfo/observed': The observed Faraday rotation
value, for cases for which this is public, in rad/m^{2}.

'sourceinfo/sigma_observed': The error bar of the
observed value, for cases for which this is public, in
rad/m^{2}. For the data points of the `Taylor'
catalog, the published error bars are multiplied by a
factor 1.22.

'sourceinfo/foreground': The reconstructed posterior
mean for the Galactic Faraday depth at the source's
location, in rad/m^{2}.

'sourceinfo/sigma_foreground': The estimated posterior
uncertainty for the Galatctic Faraday depth at the source's
location, in rad/m^{2}.

The group 'samples/' contains the samples, named 'samples/sample000' to 'samples/sample999'. Each of these data sets also has an attribute 'randomseed' that coincides with the sample number (000 to 999).

The group 'summary/' summarizes the distribution of the
sample values by providing the mean in a data set
'summary/mean' and the standard deviation in a data set
'summary/standarddev', both in rad/m^{2}.

For easier identification, the data points of each individual catalog are used in the same order as they appear in the original catalogs, with the exception of the observations that appear in several catalogs. For these, both catalogs are mentioned in the 'sourceinfo/catalog' dataset; e.g., "Tabara / Broten".

samples.hdf5 (1000 samples; 162 MB)samples_subset.hdf5 (100 samples; 19 MB)

We again provide fits files as an alternative. The file with the complete set of samples has four binary table extensions, the file containing the subset of samples has three binary table extension.

The first extension contains 41632 rows for the 41632 sources and seven columns for the catalog identifier, Galactic longitude in degrees, Galactic latitude in degrees, observed Faraday rotation value in rad/m

The second and third (in the case of the large file) extension tables have 41632 rows for the 41632 sources and 500 columns each for the different samples (or 100 columns in the case of the smaller file). The values in this table are in rad/m

The last extension contains 41632 rows for the 41632 sources and two columns for the summary of the distributions, given by their mean in rad/m

samples.fits (1000 samples; 162 MB)

samples_subset.fits (100 samples; 19 MB)

The following table gives an overview over the information stored in the files. These first ten rows correspond to the first ten sources in the catalog. The large number of digits for the sky position is due to a coordinate conversion.

Canadian Institute for Theoretical Astrophysics

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Toronto, ON, M5S 3H8

Canada

e-mail: niels@cita.utoronto.ca

Page last updated on 2015-02-16.