X-ray properties of the z ~ 4.5 Lyman-alpha Emitters in the Chandra Deep Field South Region

Details X-ray properties of the z ~ 4.5 Lyman-alpha Emitters in the Chandra Deep Field South Region X-ray properties of the z ~ 4.5 Lyman-alpha Emitters in the Chandra Deep Field South Region

2010-05-20

arxiv.org/abs/1005.3829v2

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

12 pages, 5 figures, ApJ accepted

Scientific paper

We report the first X-ray detection of 113 Lyman-alpha emitters at redshift z ~ 4.5. Only one source (J033127.2-274247) is detected in the Extended Chandra Deep Field South (ECDF-S) X-ray data, and has been spectroscopically confirmed as a z = 4.48 quasar with $L_X = 4.2\times 10^{44}$ erg/s. The single detection gives a Lyman-alpha quasar density consistent with the X-ray luminosity function of quasars. The coadded counts of 22 Lyman-alpha emitters (LAEs) in the central Chandra Deep Field South (CDF-S) region yields a S/N=2.4 (p=99.83%) detection at soft band, with an effective exposure time of ~36 Ms. Further analysis of the equivalent width (EW) distribution shows that all the signal comes from 12 LAE candidates with EW_rest < 400 \AA, and 2 of them contribute about half of the signal. Following-up spectroscopic observations show that the two are a low-redshift emission line galaxy and a Lyman break galaxy at z = 4.4. Excluding these two and combined with ECDF-S data, we derive a 3-sigma upper limit on the average luminosity of $L_{0.5-2 keV}$ $<$ 2.4 $\times 10^{42}$ ergs/s for z ~ 4.5 LAEs. If the average X-ray emission is due to star formation, it corresponds to a star-formation rate (SFR) of < 180--530 M$_\sun$ per yr. We use this SFR_X as an upper limit of the unobscured SFR to constrain the escape fraction of Lyman-alpha photons, and find a lower limit of f_esc > 3-10%. However, our upper limit on the SFR_X is ~7 times larger than the upper limit on SFR_X on z ~ 3.1 LAEs in the same field, and at least 30 times higher than the SFR estimated from Lyman-alpha emission. From the average X-ray to Lyman-alpha line ratio, we estimate that fewer than 3.2% (6.3%) of our LAEs could be high redshift type 1 (type 2) AGNs, and those hidden AGNs likely show low rest frame EWs.

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