X‐Ray Observations of Markarian 231

Turner, T. J.

doi:10.1086/306674

Cited by 26 publications

(27 citation statements)

References 39 publications

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“…The measured luminosities are in agreement with the one estimated using ROSAT and ASCA data (Iwasawa 1999;Turner 1999), but about a factor 4−6 higher than that found by G02 using Chandra data (L (0.5−2) = 10 41.2 erg s −1 ).…”

Section: The Starburst Component In Mkn 231supporting

confidence: 88%

“…In the low-energy domain (E < 2 keV), the X-ray emission of MKN 231 appears to be extended 2 , with a roughly circular symmetry. The presence of extended soft X-ray emission was first noted using ROSAT observations (Turner 1999), and it has been confirmed by the recent Chandra observation (G02). The Chandra data show that the galaxy emission (0.35−2 keV range) extends over a radius of ∼25 arcsec.…”

Section: Xmm-newton Datamentioning

confidence: 53%

“…Previous X-ray observations by ROSAT, ASCA (Turner 1999;Iwasawa 1999;Maloney & Reynolds 2000, hereafter MR00) and more recently Chandra (Gallagher et al 2002b, hereafter G02;Ptak et al 2003), revealed the presence of: a) extended soft X-ray emission of thermal origin, likely associated with the circumnuclear starburst; b) a hard and flat (photon index Γ ∼ 0.7) non-thermal component having an observed X-ray luminosity L (2−10) ∼ 10 42 erg s −1 and c) a Fe K α emission line having an observed equivalent width of ∼300 eV (the line was measured by ASCA but is not detected by Chandra).…”

Section: Introductionmentioning

confidence: 99%

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The XMM-Newton and BeppoSAX view of the Ultra Luminous Infrared Galaxy MKN 231

Braito

Ceca

Piconcelli³

et al. 2004

A&A

105

100

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Abstract. We discuss XMM-Newton and BeppoSAX observations of MKN 231, the lowest-redshift Broad Absorption Line (BAL) QSO known so far and one of the best-studied Ultra Luminous Infrared Galaxies. By combining the XMM-Newton spectral resolution and the high-energy bandpass of BeppoSAX we have been able to study in more detail than previously possible its 0.2-50 keV spectral properties. The BeppoSAX PDS data unveiled, for the first time, a highly absorbed (N H ∼ 2 × 10 24 cm −2 ) power-law component. We find that: a) below 10 keV we are seeing only reprocessed radiation through reflection and/or scattering; b) the intrinsic 2-10 keV luminosity of MKN 231 is 1 +1.0 −0.5 × 10 44 erg s −1 , i.e. more than an order of magnitude greater than previous measurements; c) the starburst activity significantly contributes to the soft (E < 2 keV) X-ray emission.

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Section: The Starburst Component In Mkn 231supporting

confidence: 88%

Section: Xmm-newton Datamentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

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The XMM-Newton and BeppoSAX view of the Ultra Luminous Infrared Galaxy MKN 231

Braito

Ceca

Piconcelli³

et al. 2004

A&A

105

100

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show abstract

“…Using ASCA and ROSAT observations, Turner (1999) determined an absorbing column of to 22 N ∼ 2 # 10 H 10 23 cm Ϫ2 depending on whether the absorbing material is neutral or ionized. The ASCA data were analyzed in Maloney & Reynolds (2000), who deduced that the direct observation of the nuclear X-rays was blocked by an optically thick absorber, and we observe a strong reflected and scattered component through a neutral column density of .…”

Section: ϫ2mentioning

confidence: 99%

Diagnostics of Quasar Broad Absorption Line Geometry: X-Ray Observations and Two-dimensional Optical Spectroscopy

Punsly

Lípari

2005

ApJ

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A new generation of sensitive X-ray measurements are indicating that the existence of X-ray attenuation column densities, , is quite common among broad absorption line quasars (BALQSOs). This is significant 24 Ϫ2 N 1 10 cm H to the geometry of the broad absorption line (BAL) outflow. In particular, such an X-ray shield also shields equatorial accretion disk winds from the UV, thereby preventing high-velocity equatorial outflows from being launched. By contrast, bipolar winds initiated by continuum radiation pressure from the funnel of a slim accretion disk flare outward (like a trumpet) and offer vastly different absorbing columns to the X-ray and UV emission that are emitted from distinct regions of the disk, ∼6M and ∼10M-40M, respectively (where M is the radius of the black hole). Recent numerical work indicates that it is also possible to launch bipolar outflows from the inner regions of a thin disk. The recent discovery with VLBI that the Galactic analog of a BALQSO, the X-ray binary Circinus X-1 (with high-velocity P Cygni X-ray absorption lines), is viewed virtually along the radio jet axis (and therefore along the spin axis of the black hole and the normal to the accretion disk) has rekindled interest in the bipolar models of BALQSOs. We explore this possibility by studying the nearest BALQSO, Mrk 231. High-resolution two-dimensional optical spectroscopy and VLBI mappings of the radio jet axis indicate that the BAL outflow is parallel to the parsec-scale radio jet.

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“…The presence of absorption possibly associated with the BAL outflows combined with the strong starburst activity, makes the X-ray continuum of Mrk 231 particularly complex. ROSAT, ASCA and Chandra [6,8,11,15] observations have shown this complexity revealing both an extended soft X-ray emission (associated to the starburst activity) and a hard X-ray emission indicative of a heavily obscured AGN. The models proposed to explain the flat X-ray spectra of Mrk 231 accumulated so far (which were limited to E<10 keV), invoke reprocessed emission: thus the estimate of the intrinsic power of the AGN can be obtained only through indirect arguments.…”

Section: Introductionmentioning

confidence: 99%