The Chandra Deep Field North Survey. XII. The Link Between Faint X-ray and Radio Source Populations

Details The Chandra Deep Field North Survey. XII. The Link Between Faint X-ray and Radio Source Populations The Chandra Deep Field North Survey. XII. The Link Between Faint X-ray and Radio Source Populations

2002-07-19

arxiv.org/abs/astro-ph/0207433v1

Astronomy and Astrophysics

Astrophysics

12 pages, 5 figures (1 color), LaTeX emulateapj5.sty, accepted for publication by the Astronomical Journal

Scientific paper

10.1086/343778

We investigate the relationship between faint X-ray and 1.4 GHz radio source populations detected within 3' of the Hubble Deep Field North using the 1 Ms Chandra and 40 uJy VLA surveys. Within this region, we find that ~42% of the 62 X-ray sources have radio counterparts and ~71% of the 28 radio sources have X-ray counterparts; thus a 40 uJy VLA survey at 1.4 GHz appears to be well-matched to a 1 Ms Chandra observation. Among the different source populations sampled, we find that the majority of the 18 X-ray detected emission-line galaxies (ELGs) have radio and mid-infrared ISOCAM counterparts and appear to be luminous star-forming galaxies at z=0.3-1.3. Importantly, the radio-detected ELGs make up ~35% of the X-ray source population at 0.5-8.0 keV X-ray fluxes between ~(1-5)x10e-16 erg/cm2/s and signal the emergence of the luminous, high-z starburst galaxy population in the X-ray band. We find that the locally-determined correlation between X-ray luminosities and 1.4 GHz radio luminosity densities of the late-type galaxies can easily be extended to include the luminous intermediate-redshift ELGs, suggesting that the X-ray and radio emission processes are generally associated in star-forming galaxies. This result implies that the X-ray emission can be used as an indicator of star formation rate for star-forming galaxies. Finally, we show that there appear to be two statistically distinct types of ISOCAM-detected star-forming galaxies: those with detectable radio and X-ray emission and those without. The latter type may have stronger mid-infrared emission-line features that increase their detectability at mid-infrared wavelengths.

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