A new sample of X-ray selected narrow emission-line galaxies - I. The nature of optically elusive AGN

E. Pons; M. G. Watson

doi:10.1051/0004-6361/201423866

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Volume 568 (August 2014)

A&A, 568 (2014) A108

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Table 3

True Sy2: observed and predicted parameters for Hα.


SRCID	Narrow Hα¹		Broad Hα²		Predicted broad Hα³
SRCID	flux^a	FWHM ^b	flux^a	FWHM ^b,∗	flux^a	FWHM ^b

1780	357 ± 6	188 ± 3	139 ± 26	1181 ± 430	2338 ± 295	5638 ± 375
47793	631 ± 8	275 ± 3	<190	4940	2741 ± 264	4940 ± 286
93640	398 ± 5	212 ± 2	238 ± 14	1071 ± 278	1642 ± 190	2454 ± 279
266125	216 ± 4	242 ± 4	<117	4428	1210 ± 238	4428 ± 1769
275370	843 ± 9	266 ± 2	<107	4047	2130 ± 221	4047 ± 246
303293	243 ± 43	237 ± 16	<296	5638	2887 ± 209	5638 ± 303
305003	887 ± 9	327 ± 3	644 ± 23	1265 ± 268	4099 ± 318	4579 ± 177
339379	691 ± 7	280 ± 2	<119	3915	3934 ± 222	3915 ± 155

Notes.

⁽¹⁾

Parameters from the optical spectrum, obtained by the SDSS line fitting pipeline (SDSS SpecLine table) (Fig. 12 red curve).

⁽²⁾

Fitted weak line (SRCIDs 1780, 93640, 305003) or the upper limit of the broad component (Fig. 12 dashed blue line).

⁽³⁾

Predicted broad Hα component computed using equations of Sect. 4.4 (Fig. 12 green curve).

^(a)

Line flux in units of 10^-17 erg/cm²/ s.

^(b)

Full Width at Half Maximum in units of km s^-1.

^(∗)

The FWHM of the broad component is the fitted value when a weak broad line is present, otherwise it is fixed at the predicted value (Col. 7 of the table).

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