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## ATPMNCAT - Australia Telescope-PMN Catalog of Southern Radio Sources |
HEASARC Archive |

This Australia Telescope PMN (ATPMN) catalog lists the source measurements of flux density, position and structure of a selection of sources from the PMN catalog. Each catalog entry corresponds to a discrete source observed by the ATCA. In many cases, a single PMN source yields several ATPMN sources. Apart from the name of the parent PMN source, there is no indication of physical association: multiple sources in the one field may be aligned by chance, or may be components of the one object.

This catalog contains the following information for each source: position; the flux density at 4.8 and 8.6 GHz; uncertainties in each flux density; the source size modelled as an ellipse (major axes, minor axes, position angle) of the best fit for a Gaussian brightness distribution; the spectral index computed between 4.8 and 8.6 GHz; the uncertainty in the spectral index; a code denoting the epoch of the observation. In the table as given in the original reference, the positions were given with varying degrees of precision, from 0.001 to 1 second of time in RA and from 0.01 to 1 arcsecond in Declination. The authors state in Section 4 of the reference paper that the error in a position coordinate is less than 10 times the final digit given in the coordinate. The positions as displayed in this table do not reflect this system: e.g., a Dec value displayed as '-79 58 34.00' may have been given in the original table as '-79 58 34.00' or '-79 58 34.0' or '-79 58 34'. To recover this information about positional precision the HEASARC has created two additional parameters ra_accuracy and dec_accuracy which list the number of digits after the decimal point given in the original table for the RA and Dec, respectively. Thus, if ra_accuracy = 3, the RA was given to a precision of 0.001 s in the original table, implying that the actual error in RA was less than 10 * 0.001 = 0.01 s.

ATPMN: accurate positions and flux densities at 5 and 8 GHz for 8,385 PMN sources. McConnell D., Sadler E.M., Murphy T., Ekers R.D. <Mon. Not. R. Astron. Soc. 422, 1527 (2012)> =2012MNRAS.422.1527M

**Name**

The ATPMN source designation, using the designation registered by the
authors with the Dictionary of Nomenclature of Celestial Objects, viz.,
'ATPMN JHHMMSS.S+DDMMSS'.

**Pmn_Name**

The PMN source designation of the parent field,
using the designation registered with the Dictionary of Nomenclature of
Celestial Objects, viz., 'PMN JHHMM+DDMMa'.

**RA**

The Right Ascension of the ATCA source in the selected equinox. This
was given in J2000.0 equatorial coordinates with varying degrees of
precision, from 0.001 to 1 second of time, in the original reference. The
authors state in Section 4 of the reference paper that the error in a
position coordinate is less than 10 times the final digit given in the
coordinate. The positions as displayed in this table do not reflect this
system: e.g., a Dec value displayed as '-79 58 34.00' may have been given in
the original table as '-79 58 34.00' or '-79 58 34.0' or '-79 58 34'. To
recover this information about positional precision the HEASARC has created
two additional parameters ra_accuracy and dec_accuracy which list the number
of digits after the decimal point given in the original table for the RA and
Dec, respectively. Thus, if ra_accuracy = 3, the RA was given to a precision
of 0.001 s in the original table, implying that the actual error in RA was
less than 10 * 0.001 or 0.01 s.

**Dec**

The Declination of the ATCA source in the selected equinox. This was
given in J2000.0 equatorial coordinates with varying degrees of precision,
from 0.01 to 1 arcsecond, in the original reference. The authors state in
Section 4 of the reference paper that the error in a position coordinate is
less than 10 times the final digit given in the coordinate. The positions as
displayed in this table do not reflect this system: e.g., a Dec value
displayed as '-79 58 34.00' may have been given in the original table as
'-79 58 34.00' or '-79 58 34.0' or '-79 58 34'. To recover this information
about positional precision the HEASARC has created two additional parameters
ra_accuracy and dec_accuracy which list the number of digits after the
decimal point given in the original table for the RA and Dec, respectively.
Thus, if ra_accuracy = 3, the RA was given to a precision of 0.001 s in the
original table, implying that the actual error in RA was less than 10 *
0.001 or 0.01 s.

**LII**

The Galactic Longitude of the ATCA source.

**BII**

The Galactic Latitude of the ATCA source.

**RA_Accuracy**

The number of digits after the decimal point given in the
original table for the RA of the source. Thus, if ra_accuracy = 3, the RA was
given to a precision of 0.001 s in the original table, implying that the
actual error in RA was less than 10 * 0.001 = 0.01 s.

**Dec_Accuracy**

The number of digits after the decimal point given in the
original table for the Declination of the source. Thus, if dec_accuracy = 2,
the Declination was given to a precision of 0.01" in the original table,
implying that the actual error in Dec was less than 10 * 0.01" = 0.1".

**Flux_6_cm**

The flux density of the ATCA source at 4.8 GHz, in mJy.

**Flux_6_cm_Error**

The uncertainty in the flux density of the ATCA source at
4.8 GHz, in mJy.

**Flux_3p5_cm**

The flux density of the ATCA source at 8.6 GHz, in mJy.

**Flux_3p5_cm_Error**

The uncertainty in the flux density of the ATCA source at
8.6 GHz, in mJy.

**Major_Axis_6_cm**

The major axis of the elliptical Gaussian best-fit
model to the ATCA source at 4.8 GHz, in arcseconds.

**Minor_Axis_6_cm**

The minor axis of the elliptical Gaussian best-fit
model to the ATCA source at 4.8 GHz, in arcseconds.

**Position_Angle_6_cm**

The position angle of the major axis of the elliptical
Gaussian best-fit model to the ATCA source at 4.8 GHz, in degrees.

**Major_Axis_3p5_cm**

The major axis of the elliptical Gaussian best-fit
model to the ATCA source at 8.6 GHz, in arcseconds.

**Minor_Axis_3p5_cm**

The minor axis of the elliptical Gaussian best-fit
model to the ATCA source at 8.6 GHz, in arcseconds.

**Position_Angle_3p5_cm**

The position angle of the major axis of the
elliptical Gaussian best-fit model to the ATCA source at 8.6 GHz, in degrees.

**Spectral_Index**

The spectral index Alpha of the ATCA source between 4.8 and
8.6Ghz, defined as Alpha = log(S_{6}/S_{3} )/log(f_{6}/f_{3}), where the
subscripts denote the observing bands at 6 cm (4.8 GHz) and 3.5 cm (8.6 GHz),
S is the measured flux density, and f_{6} = 4.8 GHz and f_{3} = 8.6 GHz.

**Spectral_Index_Error**

The calculated uncertainty e_{Alpha} in the spectral
index Alpha between 4.8 and 8.6 GHz, defined as
e_Alpha = sqrt[(e_{6}/S_{6})^{2} + (e_{3}/S_{3})^{2}]/(log(f_{6}/f_{3}),
where the
subscripts denote the observing bands at 6 cm (4.8 GHz) and 3.5 cm (8.6 GHz),
S is the measured flux density, e is the error in the corresponding flux
density, and f_{6} = 4.8 GHz and f_{3} = 8.6 GHz.

**Obs_Epochs**

The epochs of the ATCA observation of the source, coded as
follows:

Epoch Dates Array Shortest baseline (m) 1 1992 Nov 09-15 6A 337 2 1993 Mar 03-07 6D 76 3 1993 Jun 11-15 6A 337 4 1993 Sep 23-26 6D 76 5 1994 Mar 11-14 6C 153

**Fit_Flag**

This parameter contains a flag indicating the quality of the
model fit to the source, where 0 means OK, i.e., the amplitude of the residual
noise after the fitted source components were subtracted from the data is
below the threshold indicated in Figure 3 of the reference paper, whereas 1
means that the amplitude of the residual noise is above this threshold.

**Hour_Angle_Flag**

This parameter contains a flag indicating the hour angle
coverage for the radio source. Normally, fields were observed with 3 scans at
different hour angles to give 45 visibility measurements. A few fields (166)
had less than 20 visibility measurements: these were not included in the
processing. A value of 0 for this flag means OK, i.e., there were at least 30
and usually 45 visibility measurements for the source, whereas 1 means that
there were only 20 to 30 visibility measurements, i.e., only 2 different hour
angles were observed.