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J/other/RMxAA/45.261 Diffuse ionized gas database DIGEDA (Flores-Fajardo+ 2009)
The following files can be converted to FITS (extension .fit or fit.gz)
digeda.dat refsid.dat galaxies.dat refs.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/other/RMxAA/45.261
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Beginning of ReadMe :J/other/RMxAA/45.261 Diffuse ionized gas database DIGEDA (Flores-Fajardo+ 2009)
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Analysis of the diffuse ionized gas database: DIGEDA.
Flores-Fajardo N., Morisset C., Binette L.
<Rev. Mex. Astron. Astrofis., 45, 261-272 (2009)>
=2009RMxAA..45..261F
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ADC_Keywords: Galaxies, spectra ; H II regions ; Interstellar medium ;
Spectroscopy
Keywords: astronomical data bases: miscellaneous - galaxies: general -
ISM: HII regions - ISM: lines and bands - line: formation
Abstract:
Studies of the Diffuse Ionized Gas (DIG) have progressed without
providing so far any strict criterion to distinguish DIGs from HII
regions. In this work, we compile the emission line measurements of 29
galaxies that are available in the scientific literature, thereby
setting up the first DIG database DIGEDA. Making use of this database,
we proceeded to analyze global properties of the DIG using the
[NII]6583/Halpha, [OI]6300/Halpha, [OIII]5007/Hbeta and
[SII]6716/Halpha lines ratios, including the Halpha emission measure.
This analysis leads us to conclude that the [NII]/Halpha ratio
provides an objective criterion for distinguishing whether an emission
region is DIG or an HII region, while the EM(Halpha) is a useful
quantity only when the galaxies are considered individually. Finally,
we find that the emission regions of Irr galaxies classified as DIG in
the literature appear in fact to be much more similar to HII regions
than to the DIGs of spiral galaxies.
Description:
DIGEDA is a comprehensive database comprising 1061 DIG and HII region
spectroscopic observations of 29 different galaxies (25 spiral
galaxies and 4 irregulars) from 18 bibliographic references. This
survey contains galaxies with significant spread in star formation
rates, Halpha luminosities, distances, disk inclinations, slit
positions and slit orientations. The 1061 observations obtained from
these references were extracted by digitalization of published figures
or tables. The data were subsequently normalized and incorporated in
DIGEDA. This resulted in a table of 26 columns containing 1061 data
lines or records (DIGEDA.dat file). We have not performed any
reddening by dust correction or for the presence of underlying
absorption lines, although we did use the reddening corrected ratios
when made available by the authors. Missing entries are represented by
(-1) in the corresponding data field. In DIGEDA the observed areas are
classificated in three possible emission region types: HII region,
transition zones or DIG. When this classification was not reported (no
matter the criterion) for the authors, we introduce our own
classification taking into account the value of |z| as described in
the paper.