高能天体物理研究组知识库

We present the results of X-ray spectroscopic observations with XMM-We present the results of X-ray spectroscopic observations with XMM-Newton for four high-redshift radio-loud quasars at z > 4. Among these, three objects, namely GB B1508 + 5714, PMN J0324 - 2918 and PKS B1251 - 407, do not show soft X-ray spectral flattening; the derived upper limits on assumed intrinsic absorption are (3.3-17.3) x 10(21) cm(-2), the least of which is among the most stringent limits for z > 4 quasars. There is a tentative indication for soft X-ray spectral flattening in PMN J1451 - 1512 at z = 4.76, though the significance is not high. These observations more than double the number of z > 4 radio-loud quasars that have X-ray spectroscopic data to seven, which compose a significant subset of a flux-limited sample of z > 4 radio-loud quasars. Based on this subset, we show, in the second part of this paper, some preliminary results on the overall X-ray spectral properties of the sample. Soft X-ray spectral flattening, which is thought to arise from intrinsic X-ray absorption, was found in about half of the sample (3/7 or 4/7). We give a preliminary distribution of the absorption column density N-H. For those with detected X-ray absorption, the derived N-H values fall into a very narrow range ( around a few times 10(22) cm(-2) for 'cold' absorption), suggesting a possible common origin of the absorber. This N-H distribution is consistent with that in the redshift range of 2-4, though the data are sparse. Those that do not show X-ray absorption are constrained to have upper limits on the N-H broadly consistent in general with the lower end of the distribution of the detected N-H. Compared to lower redshift samples at z < 2, there is an extension, or a systematic shift, towards higher values in the intrinsic N-H distribution at z > 4, and an increase of the fraction of radio-loud quasars showing X-ray absorption towards high redshifts. These results indicate a cosmic evolution effect, which seems to be the strongest at redshifts around 2. There is a tentative tendency that objects showing X-ray absorption have X-ray fluxes systematically higher than those showing apparently no absorption. After the spectral flattening is accounted for, the rest frame 1-50 keV continua have photon indices with a mean of 1.64 and a standard deviation of 0.11 (or a mean of 1.67 and a standard deviation of 0.14 for a Gaussian fit). Variability appears to be common on time-scales from a few months to years in the quasar rest frame, sometimes in both fluxes and spectral slopes.