Emission lines properties of the radio-loud quasar LAMOST J1131+3114

Free Access

Table 1

Average parameters of emission lines components derived from multi-Gaussian fit.


Comp.^a	Flux	V _offset	FWHM	Src.^b
	(10^-17erg s^-1 cm^-2)	(km s^-1)	(km s^-1)


	Hβ


BASE	242 ± 22	−80 ± 10	720 ± 40	(1)
BC	2304 ± 68	−70 ± 20	3540 ± 60	(1)
VBC	2263 ± 143	1960 ± 150	13 350 ± 320	(1)


	[O III] λ5007


NC	176 ± 26	10 ± 10	270 ± 10	(2)
BASE	675 ± 43	−30 ± 10	750 ± 20	(2)


	[O III] λ4959


NC	66 ± 19	10 ± 10	300 ± 60	(2)
BASE	182 ± 31	−60 ± 30	710 ± 70	(2)


	Hγ


BASE	61 ± 13	40 ± 40	710 ± 130	(3)
BC	638 ± 44	50 ± 80	3110 ± 200	(3)
VBC	853 ± 83	630 ± 180	9700 ± 650	(3)


	[O III] λ4363


BASE	115 ± 16	50 ± 20	720 ± 80	(3)

Notes.

^(a)

NC: narrow component, BASE: a broader line base underlying NC in [O III], BC: broad component, VBC: very broad component.

^(b)

Weighted averages from spectra: (1) LAMOST, APO, Marziani et al. (2003), Grupe et al. (2004); (2): the same plus Eracleous & Halpern (1994); (3) LAMOST and SDSS.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.