25 Citations (Scopus)

Abstract

We report on two XMM-Newton observations of the bright narrow-line Seyfert 1 galaxy Ark 564 taken 1 yr apart (2000 June and 2001 June). The 0.6-10 keV continuum is well described by a soft blackbody component (kT ≈ 140-150 eV) plus a steep power law (Γ ≈ 2.50-2.55). No significant spectral changes are observed between the two observations, although the X-ray flux in the second observation is ≈40-50 per cent lower. In both observations, we detect a significant absorption edge at a rest-frame energy of ≈0.73 keV, corresponding to O VII. The presence of the absorption feature is confirmed by a simultaneous Chandra grating observation in 2000 June, although the best-fitting edge threshold is at a slightly lower energy in the Chandra data, possibly because of a different parametrization of the underlying X-ray continuum. We find tentative evidence for a broad iron emission line in the 2000 June observation. The results from an analysis of the power spectral density (PSD) function are also presented. The present XMM-Newton data support the idea that the PSD shows two breaks, although the location of the high-frequency break requires further constraints.

Original languageEnglish (US)
Pages (from-to)854-860
Number of pages7
JournalMonthly Notices of the Royal Astronomical Society
Volume347
Issue number3
DOIs
StatePublished - Jan 21 2004

Fingerprint

XMM-Newton telescope
newton
energy
power law
iron
continuums
x rays
gratings
galaxies
thresholds
analysis

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Vignali, Cristian ; Brandt, W. N. ; Boller, Th ; Fabian, A. C. ; Vaughan, Simon. / Arakelian 564 : An XMM-Newton view. In: Monthly Notices of the Royal Astronomical Society. 2004 ; Vol. 347, No. 3. pp. 854-860.
@article{8c06386ce4124b2693cbcc8cc76cbbec,
title = "Arakelian 564: An XMM-Newton view",
abstract = "We report on two XMM-Newton observations of the bright narrow-line Seyfert 1 galaxy Ark 564 taken 1 yr apart (2000 June and 2001 June). The 0.6-10 keV continuum is well described by a soft blackbody component (kT ≈ 140-150 eV) plus a steep power law (Γ ≈ 2.50-2.55). No significant spectral changes are observed between the two observations, although the X-ray flux in the second observation is ≈40-50 per cent lower. In both observations, we detect a significant absorption edge at a rest-frame energy of ≈0.73 keV, corresponding to O VII. The presence of the absorption feature is confirmed by a simultaneous Chandra grating observation in 2000 June, although the best-fitting edge threshold is at a slightly lower energy in the Chandra data, possibly because of a different parametrization of the underlying X-ray continuum. We find tentative evidence for a broad iron emission line in the 2000 June observation. The results from an analysis of the power spectral density (PSD) function are also presented. The present XMM-Newton data support the idea that the PSD shows two breaks, although the location of the high-frequency break requires further constraints.",
author = "Cristian Vignali and Brandt, {W. N.} and Th Boller and Fabian, {A. C.} and Simon Vaughan",
year = "2004",
month = "1",
day = "21",
doi = "10.1111/j.1365-2966.2004.07269.x",
language = "English (US)",
volume = "347",
pages = "854--860",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",

}

Arakelian 564 : An XMM-Newton view. / Vignali, Cristian; Brandt, W. N.; Boller, Th; Fabian, A. C.; Vaughan, Simon.

In: Monthly Notices of the Royal Astronomical Society, Vol. 347, No. 3, 21.01.2004, p. 854-860.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Arakelian 564

T2 - An XMM-Newton view

AU - Vignali, Cristian

AU - Brandt, W. N.

AU - Boller, Th

AU - Fabian, A. C.

AU - Vaughan, Simon

PY - 2004/1/21

Y1 - 2004/1/21

N2 - We report on two XMM-Newton observations of the bright narrow-line Seyfert 1 galaxy Ark 564 taken 1 yr apart (2000 June and 2001 June). The 0.6-10 keV continuum is well described by a soft blackbody component (kT ≈ 140-150 eV) plus a steep power law (Γ ≈ 2.50-2.55). No significant spectral changes are observed between the two observations, although the X-ray flux in the second observation is ≈40-50 per cent lower. In both observations, we detect a significant absorption edge at a rest-frame energy of ≈0.73 keV, corresponding to O VII. The presence of the absorption feature is confirmed by a simultaneous Chandra grating observation in 2000 June, although the best-fitting edge threshold is at a slightly lower energy in the Chandra data, possibly because of a different parametrization of the underlying X-ray continuum. We find tentative evidence for a broad iron emission line in the 2000 June observation. The results from an analysis of the power spectral density (PSD) function are also presented. The present XMM-Newton data support the idea that the PSD shows two breaks, although the location of the high-frequency break requires further constraints.

AB - We report on two XMM-Newton observations of the bright narrow-line Seyfert 1 galaxy Ark 564 taken 1 yr apart (2000 June and 2001 June). The 0.6-10 keV continuum is well described by a soft blackbody component (kT ≈ 140-150 eV) plus a steep power law (Γ ≈ 2.50-2.55). No significant spectral changes are observed between the two observations, although the X-ray flux in the second observation is ≈40-50 per cent lower. In both observations, we detect a significant absorption edge at a rest-frame energy of ≈0.73 keV, corresponding to O VII. The presence of the absorption feature is confirmed by a simultaneous Chandra grating observation in 2000 June, although the best-fitting edge threshold is at a slightly lower energy in the Chandra data, possibly because of a different parametrization of the underlying X-ray continuum. We find tentative evidence for a broad iron emission line in the 2000 June observation. The results from an analysis of the power spectral density (PSD) function are also presented. The present XMM-Newton data support the idea that the PSD shows two breaks, although the location of the high-frequency break requires further constraints.

UR - http://www.scopus.com/inward/record.url?scp=1642559259&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=1642559259&partnerID=8YFLogxK

U2 - 10.1111/j.1365-2966.2004.07269.x

DO - 10.1111/j.1365-2966.2004.07269.x

M3 - Article

AN - SCOPUS:1642559259

VL - 347

SP - 854

EP - 860

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -