XMM–Newton observations of two hyperluminous IRAS galaxies: Compton‐thick quasars with obscuring starbursts
Identifieur interne : 000364 ( Main/Exploration ); précédent : 000363; suivant : 000365XMM–Newton observations of two hyperluminous IRAS galaxies: Compton‐thick quasars with obscuring starbursts
Auteurs : R. J. Wilman [Pays-Bas] ; A. C. Fabian ; C. S. Crawford ; R. M. Cutri [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2003-01.
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Abstract
We present XMM–Newton observations of two hyperluminous IRAS galaxies (LBol > 1013h−250 L⊙), neither of which were previously detected by ROSAT. Published models of the infrared spectral energy distributions imply that a starburst and obscured quasar contribute equally to the power of each source. IRAS F12514+1027 (z= 0.30) is detected in 18.6 ks with 130 EPIC‐pn counts over 0.2–12 keV. The soft X‐ray spectrum exhibits thermal emission from the starburst, with T≃ 0.3 keV and L (0.5–2.0 keV) =2.1 × 1042 erg s−1. With its Fe K‐edge, the flat continuum above 2 keV is interpreted as cold reflection from a hidden AGN of intrinsic L (2–10 keV) ≳ 1.8 × 1044 erg s−1. Comparison with the infrared power requires that the X‐ray reflector subtend ∼2π/5 sr at the central engine. IRAS F00235+1024 (z= 0.575) is not detected by the EPIC‐pn in 15.9 ks; the limits imply that the starburst is X‐ray weak, and (for the AGN) that any hard X‐ray reflector subtend <2π/5 sr. The direct lines of sight to the AGN in both objects are Compton‐thick (NH > 1.5 × 1024 cm−2), and the presence of a reflection component in F12514+1027, but not in F00235+1024, suggests that the AGN in the latter object is more completely obscured. This is consistent with their Seyfert‐2 and starburst optical spectra, respectively.
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DOI: 10.1046/j.1365-8711.2003.06113.x
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Published models of the infrared spectral energy distributions imply that a starburst and obscured quasar contribute equally to the power of each source. IRAS F12514+1027 (z= 0.30) is detected in 18.6 ks with 130 EPIC‐pn counts over 0.2–12 keV. The soft X‐ray spectrum exhibits thermal emission from the starburst, with T≃ 0.3 keV and L (0.5–2.0 keV) =2.1 × 1042 erg s−1. With its Fe K‐edge, the flat continuum above 2 keV is interpreted as cold reflection from a hidden AGN of intrinsic L (2–10 keV) ≳ 1.8 × 1044 erg s−1. Comparison with the infrared power requires that the X‐ray reflector subtend ∼2π/5 sr at the central engine. IRAS F00235+1024 (z= 0.575) is not detected by the EPIC‐pn in 15.9 ks; the limits imply that the starburst is X‐ray weak, and (for the AGN) that any hard X‐ray reflector subtend <2π/5 sr. The direct lines of sight to the AGN in both objects are Compton‐thick (NH > 1.5 × 1024 cm−2), and the presence of a reflection component in F12514+1027, but not in F00235+1024, suggests that the AGN in the latter object is more completely obscured. This is consistent with their Seyfert‐2 and starburst optical spectra, respectively.</div></front></TEI><affiliations><list><country><li>Pays-Bas</li><li>États-Unis</li></country></list><tree><noCountry><name sortKey="Crawford, C S" sort="Crawford, C S" uniqKey="Crawford C" first="C. S." last="Crawford">C. S. Crawford</name><name sortKey="Fabian, A C" sort="Fabian, A C" uniqKey="Fabian A" first="A. C." last="Fabian">A. C. Fabian</name></noCountry><country name="Pays-Bas"><noRegion><name sortKey="Wilman, R J" sort="Wilman, R J" uniqKey="Wilman R" first="R. J." last="Wilman">R. J. Wilman</name></noRegion></country><country name="États-Unis"><noRegion><name sortKey="Cutri, R M" sort="Cutri, R M" uniqKey="Cutri R" first="R. M." last="Cutri">R. M. Cutri</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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