We present the results from a similar to 500 ks Chandra observation of the z = 6 : 31 QSO SDSS J1030 + 0524. This is the deepest X-ray observation to date of a z similar to 6 QSO. The QSO is detected with a total of 125 net counts in the full (0 : 5 7 keV) band and its spectrum can be modeled by a single power-law model with photon index of Gamma= 1 : 81 +/- 0 : 18 and full band flux of f = 3 : 95 x 10(-15) erg s(-1) cm(-2). When compared with the data obtained by XMM-Newton in 2003, our Chandra observation in 2017 shows a harder (Delta Gamma approximate to -0.6) spectrum and a 2.5 times fainter flux. Such a variation, in a timespan of similar to 2 yr rest-frame, is unexpected for such a luminous QSO powered by a > 10(9) M-circle dot black hole. The observed source hardening and weakening could be related to an intrinsic variation in the accretion rate. However, the limited photon statistics does not allow us to discriminate between an intrinsic luminosity and spectral change, and an absorption event produced by an intervening gas cloud along the line of sight. We also report the discovery of di ff use X-ray emission that extends for 30 `' x 20 `' southward of the QSO with a signal-to-noise ratio (S/N) of approximately six, hardness ratio of HR = 0 .03 +0.20-0.25, and soft band flux of f 0.5-2 keV = 1.1+0.3-0.3 x 10(-15) erg s(-1) cm(-2), that is not associated to a group or cluster of galaxies. We discuss two possible explanations for the extended emission, which may be either associated with the radio lobe of a nearby, foreground radio galaxy (at z approximate to 1-2), or ascribed to the feedback from the QSO itself acting on its surrounding environment, as proposed by simulations of early black hole formation.
The 500 ks Chandra observation of the z=6.31 QSO SDSS J1030+0524 / Nanni R., Gilli R., Vignali C., Mignoli M., Comastri A., Vanzella E., Zamorani G., Calura F., Lanzuisi G., Brusa M., Tozzi P., Iwasawa K., Cappi M., Vito F., Balmaverde B., Costa T., Risaliti G., Paolillo M., Prandoni I., Liuzzo E., Rosati P., Chiaberge M., Caminha G. B., Sani E., Cappelluti N., Norman C.. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 1432-0746. - STAMPA. - 614:(2018), pp. 121.1-121.13. [10.1051/0004-6361/201832694]
The 500 ks Chandra observation of the z=6.31 QSO SDSS J1030+0524
NANNI, RICCARDOWriting – Original Draft Preparation
;Vignali C.Supervision
;LANZUISI, GIORGIOMembro del Collaboration Group
;Brusa M.Membro del Collaboration Group
;
2018
Abstract
We present the results from a similar to 500 ks Chandra observation of the z = 6 : 31 QSO SDSS J1030 + 0524. This is the deepest X-ray observation to date of a z similar to 6 QSO. The QSO is detected with a total of 125 net counts in the full (0 : 5 7 keV) band and its spectrum can be modeled by a single power-law model with photon index of Gamma= 1 : 81 +/- 0 : 18 and full band flux of f = 3 : 95 x 10(-15) erg s(-1) cm(-2). When compared with the data obtained by XMM-Newton in 2003, our Chandra observation in 2017 shows a harder (Delta Gamma approximate to -0.6) spectrum and a 2.5 times fainter flux. Such a variation, in a timespan of similar to 2 yr rest-frame, is unexpected for such a luminous QSO powered by a > 10(9) M-circle dot black hole. The observed source hardening and weakening could be related to an intrinsic variation in the accretion rate. However, the limited photon statistics does not allow us to discriminate between an intrinsic luminosity and spectral change, and an absorption event produced by an intervening gas cloud along the line of sight. We also report the discovery of di ff use X-ray emission that extends for 30 `' x 20 `' southward of the QSO with a signal-to-noise ratio (S/N) of approximately six, hardness ratio of HR = 0 .03 +0.20-0.25, and soft band flux of f 0.5-2 keV = 1.1+0.3-0.3 x 10(-15) erg s(-1) cm(-2), that is not associated to a group or cluster of galaxies. We discuss two possible explanations for the extended emission, which may be either associated with the radio lobe of a nearby, foreground radio galaxy (at z approximate to 1-2), or ascribed to the feedback from the QSO itself acting on its surrounding environment, as proposed by simulations of early black hole formation.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
