SIMBAD references

2010A&A...519A..92G - Astronomy and Astrophysics, volume 519, A92-92 (2010/9-1)

The X-ray to [Ne V]3426 flux ratio: discovering heavily obscured AGN in the distant universe.


Abstract (from CDS):

We investigate the possibility of using the ratio between the 2-10keV flux and the [NeV]3426 emission line flux (X/NeV) as a diagnostic diagram to discover heavily obscured, possibly Compton-thick active galactic nuclei (AGN) in the distant Universe. While it is on average about one order of magnitude fainter than the more commonly used [OIII]5007 emission line, the [NeV]3426 line can be observed with optical spectroscopy up to z∼1.5, whereas the [OIII]5007 line is redshifted out of the optical bands already at z∼0.8. First, we calibrated a relation between X/NeV and the cold absorbing column density NH using a sample of 74 bright, nearby Seyferts with both X-ray and [NeV] data available in the literature and for which the column density is determined unambiguously. Similar to what is found for the X-ray to [OIII]5007 flux ratio (X/OIII), we found that the X/NeV ratio decreases towards high column densities, as expected if [Ne V]3426 emission is a good tracer of the AGN intrinsic power. Essentially all local Seyferts with X/NeV values below 15 are found to be Compton-thick objects. At X/NeV values below 100, the percentage of Compton-thick nuclei decreases to ∼50%, but ∼80% of the considered sample is still absorbed with NH>1023cm–2. Second, we applied this diagnostic diagram to different samples of distant obscured and unobscured QSOs in the Sloan Digital Sky Survey (SDSS). SDSS blue, unobscured, type-1 QSOs in the redshift range z=[0.1-1.5] indeed show X/NeV values typical of unobscured Seyfert 1s in the local Universe. Conversely, SDSS type-2 QSOs at z∼0.5 classified either as Compton-thick or Compton-thin on the basis of their X/OIII ratio, would have mostly been classified in the same way based on the X/NeV ratio. We applied the X/NeV diagnostic diagram to 9 SDSS obscured QSOs in the redshift range z=[0.85-1.31], selected by means of their prominent [NeV]3426 line (rest EW>4Å) and observed with Chandra ACIS-S for 10ks each (8 of them as part of our proprietary program). Based on the X/NeV ratio, complemented by X-ray spectral analysis, 2 objects appear good Compton-thick QSO candidates, 4 objects appear as Compton-thin QSOs, while 3 have an ambiguous classification. When excluding broad-lined QSOs with a red continuum from the sample and thus considering only genuine narrow-line objects, the efficiency in selecting Compton-thick QSOs through the [NeV] line is about 50% (with large errors, though), more similar to what is achieved with [OIII] selection. We discuss the possibility of applying the X/NeV diagnostic to deep X-ray surveys to search for Compton-thick Seyferts at z∼1, i.e., those objects that are thought to be responsible for the ``missing'' X-ray background. Finally, we compared the optical spectral properties of [NeV]-selected QSOs with those of other SDSS populations of obscured and unobscured QSOs. By restricting the analysis to objects in the same redshift (and luminosity) range z=[0.4-1.5], we found evidence that, at any given [NeV] luminosity, increasing obscuration is accompanied by increasing [OII]3727 emission. This correlation is interpreted as evidence of enhanced star formation in obscured QSOs, which is consistent with current popular scenarios of BH-galaxy coevolution.

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Journal keyword(s): galaxies: active - X-rays: general - X-rays: galaxies

Simbad objects: 88

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