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X-ray properties of Lyman Break Galaxies in the Hubble Deep Field North region | | K. Nandra
; R.F. Mushotzky
; K.A. Arnaud
; C.C. Steidel
; K.A. Adelberger
; J.P. Gardner
; H.I. Teplitz
; R.A. Windhorst
; | | Date: |
15 May 2002 | | Journal: | Astrophys.J. 576 (2002) 625-639 | | Subject: | astro-ph | | Affiliation: | USRA/GSFC), R.F. Mushotzky (GSFC), K.A. Arnaud (UMCP/GSFC), C.C. Steidel (Caltech), K.A. Adelberger (Harvard), J.P. Gardner (GSFC), H.I. Teplitz (CUA/GSFC), R.A. Windhorst (ASU | | Abstract: | We describe the X-ray properties of a large sample of $zsim3$ Lyman Break Galaxies (LBGs) in the region of the Hubble Deep Field North, derived from the 1 Ms public Chandra observation. Of our sample of 148 LBGs, four are detected individually. This immediately gives a measure of the bright AGN fraction in these galaxies of $sim 3$~per cent, which is in agreement with that derived from the UV spectra. The X-ray color of the detected sources indicates that they are probably moderately obscured. Stacking of the remainder shows a significant detection ($6sigma$) with an average luminosity of $3.5 imes 10^{41}$~erg s$^{-1}$ per galaxy in the rest frame 2-10 keV band. We have also studied a comparison sample of 95 z$sim 1$ ``Balmer Break’’ galaxies. Eight of these are detected directly, with at least two clear AGN based on their high X-ray luminosity and very hard X-ray spectra respectively. The remainder are of relatively low luminosity ($<10^{42}$~erg s$^{-1}$), and the X-rays could arise from either AGN or rapid star-formation. The X-ray colors and evidence from other wavebands favor the latter interpretation. Excluding the clear AGN, we deduce a mean X-ray luminosity of $6.6 imes 10^{40}$~erg s$^{-1}$, a factor $sim 5$ lower than the LBGs. The average ratio of the UV and X-ray luminosities of these starforming galaxies $L_{
m UV}/L_{
m X}$, however, is approximately the same at $z = 1$ as it is at $z = 3$. This scaling implies that the X-ray emission follows the current star formation rate, as measured by the UV luminosity. We use our results to constrain the star formation rate at $zsim 3$ from an X-ray perspective (truncated). | | Source: | arXiv, astro-ph/0205215 | | Services: | Forum | Review | PDF | Favorites | |
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