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NGC 3147
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NGC 3147 (also IRAS 10126+7339, MCG 12-10-25, UGC 5532 and PGC 30019) is a magnitude +10.6 face-on spiral galaxy located 129 million light-years away in the constellation Draco. 

The galaxy was discovered by German-British astronomer William Herschel using a 47.5 cm (18.7 inch) f/13 speculum reflector at Datchet, Berkshire, on the 3rd April 1785.

Right Ascension 10h 16m 53,2s, Declination +73° 24' 01"



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Title: The Suzaku X-ray spectrum of NGC 3147. Further insights on the best "true" Seyfert 2 galaxy candidate
Authors: G. Matt, S. Bianchi, M. Guainazzi, X. Barcons, F. Panessa

NGC 3147 is so far the most convincing case of a "true" Seyfert 2 galaxy, i.e. a source genuinely lacking the Broad Line Regions. We obtained a Suzaku observation with the double aim to study in more detail the iron line complex, and to check the Compton-thick hypothesis for the lack of observed optical broad lines.
The Suzaku XIS and HXD/PIN spectra of the source were analysed in detail. The line complex is composed of at least two unresolved lines, one at about 6.45 keV and the other one at about 7 keV, most likely identified with Fe XVII/XIX, the former, and Fe XXVI, the latter. The high-ionisation line can originate either in a photoionised matter or in an optically thin thermal plasma. In the latter case, an unusually high temperature is implied. In the photoionised model case, the large equivalent width can be explained either by an extreme iron overabundance or by assuming that the source is Compton-thick. In the Compton-thick hypothesis, however, the emission above 2 keV is mostly due to a highly ionised reflector, contrary to what is usually found in Compton-thick Seyfert 2s, where reflection from low ionized matter dominates. Moreover, the source flux varied between the XMM-Newton and the Suzaku observations, taken 3.5 years apart, confirming previous findings and indicating that the size of the emitting region must be smaller than a parsec.
The hard X-ray spectrum is also inconclusive on the Compton-thick hypothesis. Weighting the various arguments, a "true" Seyfert 2 nature of NGC 3147 seems to be still the most likely explanation, even if the "highly ionised reflector" Compton-thick hypothesis cannot at present be formally rejected.

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