Chandra and Magellan /FIRE follow-up observations of PSO167-13: An X-ray weak QSO at z = 6.515

Journal
Date Issued
2021
Author(s)
•
Brandt, W. N.
•
Ricci, F.
•
Congiu, E.
•
Connor, T.
•
Bañados, E.
•
Bauer, F. E.
•
•
Luo, B.
•
Mazzucchelli, C.
•
•
Shemmer, O.
•
Vignali, C.
•
•
•
•
Gallerani, S.
•
Nanni, R.
•
Brusa, M.
•
Cappelluti, N.
•
Civano, F.
•
Zamorani, G.
DOI
Abstract
Context. The discovery of hundreds of quasi-stellar objects (QSOs) in the first gigayear of the Universe powered by already grown supermassive black holes (SMBHs) challenges our knowledge of SMBH formation. In particular, investigations of z  >  6 QSOs that present notable properties can provide unique information on the physics of fast SMBH growth in the early Universe. Aims. We present the results of follow-up observations of the z  =  6.515 radio-quiet QSO PSO167-13, which is interacting with a close companion galaxy. The PSO167-13 system has recently been proposed to host the first heavily obscured X-ray source at high redshift. The goals of these new observations are to confirm the existence of the X-ray source and to investigate the rest-frame UV properties of the QSO. Methods. We observed the PSO167-13 system with Chandra/ACIS-S (177 ks) and obtained new spectroscopic observations (7.2 h) with Magellan/FIRE. Results. No significant X-ray emission is detected from the PSO167-13 system, suggesting that the obscured X-ray source previously tentatively detected was either due to a strong background fluctuation or is highly variable. The upper limit (90% confidence level) on the X-ray emission of PSO167-13 (L2-10  keV  <  8.3 × 1043  erg  s-1) is the lowest available for a z  >  6 QSO. The ratio between the X-ray and UV luminosity of αox  <  -1.95 makes PSO167-13 a strong outlier from the αox - LUV and LX - Lbol relations. In particular, its X-ray emission is more than six times weaker than the expectation based on its UV luminosity. The new Magellan/FIRE spectrum of PSO167-13 is strongly affected by unfavorable sky conditions, but the tentatively detected C IV and Mg II emission lines appear strongly blueshifted. Conclusions. The most plausible explanations for the X-ray weakness of PSO167-13 are intrinsic weakness or small-scale absorption by Compton-thick material. The possible strong blueshift of its emission lines hints at the presence of nuclear winds, which could be related to its X-ray weakness.
Volume
649
Start page
A133
Uri
Url
Issn Identifier
0004-6361
Rights
open.access
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