The Phoenix Deep Survey

A. Hopkins¹, A. Georgakakis², J. Afonso³, B. Chan¹, L. Cram¹, B. Mobasher⁴, M. Sullivan⁵

University of Sydney
Imperial College, London
Observatorio Astronomico de Lisboa
Space Telescope Science Institute
University of Toronto

The Phoenix Deep Survey is a multiwavelength survey of a region a little over 2 degrees diameter in the southern constellation Phoenix. Observations have been made with many instruments, including:

1.4 GHz observations with the Australia Telescope Compact Array,
optical (R-band, V-band) and spectroscopic observations (2dF) with the Anglo-Australian Telescope,
deeper optical imaging with the WFI on the Anglo-Australian Telescope
NIR (K-band) imaging with the SofI instrument on the ESO NTT.
NIR (J and K-band) imaging with the OSIRIS instrument at CTIO.

The project is ongoing, and as additional data products and results are made public they will appear on this page.

The publication list from the Phoenix Deep Survey observations is ever growing. Please cite the relevant PDS publication if you make use of our work.

Here are some clickable colour images of one WFI field (a 30'x30' area), in the most sensitive portion of the radio survey, with radio contours overlayed.

Data products

Radio Images

The final ATCA 1.4 GHz mosaic image is now in the public domain, and various fits files can be downloaded. Refer to Hopkins et al 2003 AJ, 125, 465 for details.

phoenix_mosaic_all.fits: (95MB) The full mosaic image.
phoenix_mosaic_sens.fits: (95MB) The theoretical rms sensitivity image from the output of LINMOS.
phoenix_mosaic.fits: (75MB) The mosaic after trimming at the theoretical 250 microJy rms contour.
phoenix_mosaic_rms.fits: (75MB) The measured rms sensitivity for the trimmed image, estimated using 100x100 pixel regions over the image.

Radio Catalogues

Several PDS 1.4 GHz catalogues are also available. Again refer to Hopkins et al 2003 AJ, 125, 465 for details. The columns of these files are as follows:
1-6: RA and Dec (J2000);
7-8: peak flux density (mJy) and its uncertainty;
9-10: integrated flux density (mJy) and its uncertainty;
11-13: major, minor axes (arcsec) and position angle (degrees);
14: rms noise level (mJy) at the location of the source.

PDS_atca_fdr10_full.cat: (167kB) The full, unedited, 10% FDR threshold catalogue for the trimmed mosaic image. This catalogue contains 2090 sources.
PDS_atca_fdr10_full_vis.cat: (165kB) The 10% FDR threshold catalogue for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources. This catalogue contains 2058 sources.
PDS_atca_fdr10_deep.cat: (39kB) The 10% FDR threshold catalogue for the 33'x33' region centered on the most sensitive portion of the mosaic. This catalogue contains 491 sources.
PDS_atca_fdr10_merge.cat: (172kB) The merged catalogue coming from PDS_atca_fdr10_full_vis.cat and PDS_atca_fdr10_deep.cat. This 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 catalogue.

NIR (OSIRIS/CTIO) Images

Seven fields have been observed in J and K with OSIRIS on the CTIO 1.5 m telescope. These are detailed in Georgakakis et al 2004, MNRAS, 354,127. The processed images (fits format) for each of these fields are available here. See the file README for zeropoints.

OSIRIS_J1.fits (1.3MB); OSIRIS_K1.fits (956kB)
OSIRIS_J2.fits (802kB); OSIRIS_K2.fits (1.3MB)
OSIRIS_J3.fits (1.0MB); OSIRIS_K3.fits (1.0MB)
OSIRIS_J4.fits (1.4MB); OSIRIS_K4.fits (1.0MB)
OSIRIS_J5.fits (1.1MB); OSIRIS_K5.fits (1.4MB)
OSIRIS_J6.fits (1.0MB); OSIRIS_K6.fits (1.1MB)
OSIRIS_J7.fits (1.1MB); OSIRIS_K7.fits (1.1MB)

Published Tables

Tables 1 and 2 from Georgakakis et al 2004, MNRAS, 354,127 are available here in ascii format. The XMM-NEWTON area curve for 6-sigma detections in the 2-8keV band is given in the file area_curve_2080_6.dat.

table1.dat (5.9kB)
table2.dat (4.6kB)

The image below shows the ATCA mosaic at 1.4 GHz. This image has been normalised by subtracting a mean background value and dividing by local image rms noise values. This removes the effect of the varying sensitivity of the mosaic allowing most sources to be visible at once in this image. The image is trimmed at the 250 microJy theoretical noise level, with the black contours indicating the 90, 30 and 10 microJy theoretical rms noise levels. The outer white contour indicates the extent of the original 2 degree diameter 1.4 GHz survey of Hopkins et al. 1998, MNRAS, 296, 839. The inner white circle indicates the extent of the survey results described in Hopkins et al. 1999, ApJ, 519, L59. Please acknowledge one of the Phoenix Deep Survey publications in any work which makes use of the Phoenix survey data.

This page last updated on 2006/08/04.