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Date and Time of the Query: 2019-06-16 T06:50:11 PDT
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For refcode 2008ApJ...682...94M:
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2008ApJ...682...94M New Indicators for AGN Power: The Correlation between [O IV] 25.89 micron and Hard X-Ray Luminosity for Nearby Seyfert Galaxies Melendez, M.; Kraemer, S. B.; Armentrout, B. K.; Deo, R. P.; Crenshaw, D. M.; Schmitt, H. R.; Mushotzky, R. F.; Tueller, J.; Markwardt, C. B.; Winter, L. Abstract. We have studied the relationship between the [O IV] 25.89 micron emission-line luminosities, obtained from Spitzer spectra, the X-ray continua in the 2-10 keV band, primarily from ASCA, and the 14-195 keV band obtained with the SWIFT Burst Alert Telescope (BAT), for a sample of nearby (z<0.08) Seyfert galaxies. For comparison, we have examined the relationship between the [O III] {lambda}5007, the 2-10 keV, and the 14-195 keV luminosities for the same set of objects. We find that both the [O IV] and [O III] luminosities are well correlated with the BAT luminosities. When comparing [O IV] and [O III] luminosities for the different types of galaxies, we find that the Seyfert 2s have significantly lower [O III] to [O IV] ratios than the Seyfert 1s. We suggest that this is due to more reddening of the narrow-line region (NLR) of the Seyfert 2s, since the [O IV] 25.89 micron emission line is much less affected by extinction. The combined effects of reddening and the X-ray absorption is the probable reason why the [O III] versus 2-10 keV correlation is better than the [O IV] versus 2-10 kev correlation. Based on photoionization models, we find that the [O IV] comes from higher ionization states and lower density regions than previous studies had determined for [O III]. Overall, we find the [O IV] to be an accurate indicator of the power of the AGN. Key words: Galaxies: Seyfert, Infrared: Galaxies, X-Rays: Galaxies
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