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PDS1P4GHZ - Phoenix Deep Survey 1.4-GHz Catalog

 HEASARC
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Overview

The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg2 referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 < z < 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest.

The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01h 14m 12.16s, Dec = -45o 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01h 11m 13.0s, Dec = -45o 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg2 and reaches to a measured level of 12 microJy rms noise in the most sensitive regions.

The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.

Catalog Bibcode

2003AJ....125..465H

References

The Phoenix Deep Survey: The 1.4 GHz microJansky catalog.
    Hopkins A.M., Afonso J., Chan B., Cram L.E., Georgakakis A., Mobasher B.
   <Astron. J., 125, 465-477 (2003)>
   =2003AJ....125..465H

Provenance

This table was created by the HEASARC in November 2012 based on the file PDS_atca_fdr10_merge.cat, the merged PDS catalog (derived from the individual catalogs PDS_atca_fdr10_full_vis.cat and PDS_atca_fdr10_deep.cat as discussed in the Overview above), which was obtained from the first author's web site http://www.physics.usyd.edu.au/~ahopkins/phoenix/.

Parameters

Name
The radio source designation, using the designation registered by the authors with the Dictionary of Nomenclature of Celestial Objects, viz., 'PDF JHHMMSS.S+DDMMSS', where the prefix stands for 'Phoenix Deep Field'.

RA
The Right Ascension of the radio source in the selected equinox. This was given in J2000.0 equatorial coordinates to a precision of 0.001 seconds of time in the original table.

Dec
The Declination of the radio source in the selected equinox. This was given in J2000.0 equatorial coordinates to a precision of 0.01 arcseconds in the original table.

LII
The Galactic Longitude of the radio source.

BII
The Galactic Latitude of the radio source.

Flux_1p4_GHz
The 1.4-GHz peak flux density of the radio source, in mJy/beam.

Flux_1p4_GHz_Error
The 1-sigma error in the 1.4-GHz peak flux density of the radio source, in mJy/beam.

Int_Flux_1p4_GHz
The 1.4-GHz integrated flux density of the radio source, in mJy.

Int_Flux_1p4_GHz_Error
The error in the 1.4-GHz integrated flux density of the radio source, in mJy (see Section 3 of the reference paper for full details of how this quantity was calculated).

Major_Axis
The measured major (FWHM) axis of the best-fit Gaussian model of the source, in arcseconds. The source sizes have not been deconvolved from the synthesized beam size, so sources of 12" by 6" major and minor axes are point sources.

Minor_Axis
The measured minor (FWHM) axis of the best-fit Gaussian model of the source, in arcseconds. The source sizes have not been deconvolved from the synthesized beam size, so sources of 12" by 6" major and minor axes are point sources.

Position_Angle
The measured position angle, in degrees, of the best-fit Gaussian model of the source, and measured eastwards from North.

RMS_1p4_GHz
The rms noise level, in mJy/beam, in the image at the location of the source.

Contact Person

Questions regarding the PDS1P4GHZ database table can be addressed to the HEASARC User Hotline.

A service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysics Observatory (SAO)

Page Author: Browse Software Development Team
Last Modified: 13-Nov-2012