skip to main content
Idioma:
Primo Search
Clear Search Box
Search in: Busca Geral
Busca Avançada
Busca por Índices

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.

Astronomy and astrophysics (Berlin), 2018-06, Vol.614, p.A121 [Periódico revisado por pares]

Heidelberg: EDP Sciences

Texto completo disponível

Citações Citado por
  • Título:
    The 500 ks Chandra observation of the z = 6.31 QSO SDSS J1030 + 0524
  • Autor: 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.
  • Assuntos: Accretion ; Computer simulation ; Deposition ; Emission ; Fluctuations ; Flux ; Galactic clusters ; Galaxies ; galaxies: active ; galaxies: high-redshift ; Luminosity ; quasars: general ; Radio galaxies ; X-ray emissions ; X-rays: general ; XMM (spacecraft)
  • É parte de: Astronomy and astrophysics (Berlin), 2018-06, Vol.614, p.A121
  • Notas: bibcode:2018A%26A...614A.121N
    istex:8C9C61E587C5C52B76C0CB9C57223206495B8488
    publisher-ID:aa32694-18
    dkey:10.1051/0004-6361/201832694
    ark:/67375/80W-HD59S0DB-6
    email: riccardo.nanni7@unibo.it
    href:https://www.aanda.org/articles/aa/abs/2018/06/aa32694-18/aa32694-18.html
  • Descrição: We present the results from a ~ 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 ~ 6 QSO. The QSO is detected with a total of 125 net counts in the full (0.500A0–7 keV) band and its spectrum can be modeled by a single power-law model with photon index of Γ = 1.81 ± 0.18 and full band flux of f = 3.95 × 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 (ΔΓ ≈ −0.6) spectrum and a 2.5 times fainter flux. Such a variation, in a timespan of ~ 2 yr rest-frame, is unexpected for such a luminous QSO powered by a > 109M⨀ 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 diffuse X-ray emission that extends for 30″ × 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 HR = 0.03 - 0.25 + 0.20 $\text{HR} = {0.03}_{-0.25}^{+0.20}$ , and soft band flux of f0.5– keV = 1.1+0.3−0.3 × 10−15 erg s−1 cm−2 f 0.5 - 2   keV = 1.1 - 0.3 + 0.3   ×   10 - 15   erg   s - 1   cm - 2 $ f_{0.5-2\,\text{keV}}={1.1}_{-0.3}^{+0.3}\enspace \times \enspace 1{0}^{-15\enspace }\mathrm{erg}\enspace {\mathrm{s}}^{-1}\;\rm{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 ≈ 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.
  • Editor: Heidelberg: EDP Sciences
  • Idioma: Inglês
Voltar para lista de resultados
Ir para página anteriorAnterior Resultado  8 AvançarIr para próxima página

  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

Buscando em bases de dados remotas. Favor aguardar.