Multiwavelength continuum, emission line and BAL variability with prominent P V absorption in the X-ray-weakest quasar PG 0043+039

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Table 9.

UV absorption trough equivalent widths, outflow velocities (max/min), FWHM, and their depths.

	1991				2013				2022

Absorption	W_λ	v_outfl.	FWHM	Depth	W_λ	v_outfl.	FWHM	Depth	W_λ	v_outfl.	FWHM	Depth
	[Å]	[km s⁻¹]	[km s⁻¹]		[Å]	[km s⁻¹]	[km s⁻¹]		[Å]	[km s⁻¹]	[km s⁻¹]
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)
O VI λ 1038					4.6:	−9620/−1150	4710	0.43	12.9	−13450/−4750	4130	0.64
S IV λ 1074					5.5	−8320/−1300	2420	0.35	6.8	−11910/−2110	3120	0.41
P V λ 1128					10.6	−10950/−50	4360	0.47	7.0	−12200/−4540	2300	0.35
C III λ 1176					3.3	−5880/−890	2930:	0.29	5.4	−9010/−3380	4030	0.34
Lyα λ1216		/−3670		0.65:		−16340:/−6130	3430:	0.32:		/−7240		0.19:
Si IV λ 1403	25.3	−18710/−1220	11980	0.56	18.9	−17230/0	12110	0.43	15.2	−11940/−420	4290	0.58
C IV λ 1550	21.9	−19660/−1030	9210	0.51					24.6	−16120/−50	4920	0.64
He II λ 1640									9.9	−10260/−4430	3720	0.45
Al III λ 1863	6.7	−8750/3000	4640	0.22

Notes. Given are the modified full widths at half minimum after subtracting the doublet separations. Errors for the equivalent widths reach up to 20%, and 5 to 10% for the FWHM and line depths. The outflow velocities have an error of 5%. The errors are larger in some cases due to unclear continuum intensities as well as superpositions of absorption troughs. They are marked by the symbol:.

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