Is MgIIλ2800 a reliable virial broadening estimator for quasars?

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Table 3

Derived quantities from the Hβ and Mgiiλ2800 profiles composite spectra multicomponent analysis.

Sp. type

Hβ

Mgiiλ2800

BC^a

Shift^b

FWHM ^b

VBC^a

Shift^b

FWHM ^b

BC^a

Shift^b

FWHM ^b

VBC^a

Shift^b

FWHM ^b

Pop. B Full Sample

20^c

5720 ± 100

1740 ± 150

15 600 ± 150

−165 ± 50

4620 ± 100

2160^c

11 500 ± 300

B1⁺

5^c

7750 ± 200

1920 ± 190

15 700 ± 260

−60 ± 80

6330 ± 100

1520^c

14 500 ± 1230

B1⁺⁺

–165^c

10 100 ± 420

915 ± 70

15 830 ± 860

–105^c

8870 ± 420

1305^c

13 000^c

−120 ± 60

4410 ± 100

1950 ± 280

13400 ± 600

−240 ± 40

3220 ± 240

1420 ± 540

10 000^c

PG 1201+436

42^d

–5^c

7500^c

179^d

2125 ±370

11 800 ± 770

118^d

0^c

7220 ± 590

94^d

1790 ± 330

9780 ± 740

Radio Loud

B1 CD

80^c

5330 ± 200

1935 ± 190

13 160 ± 260

45 ± 60

4680 ± 120

1630^c

11 000^c

B1 FRII

235 ± 55

5370 ± 130

1645 ± 170

15 450 ± 530

−55 ± 70

4790 ± 200

1630^c

11 000^c

Notes.

^(a)

Line intensity normalized to the continuum at 5080 Å. The value roughly corresponds to the rest-frame equivalent width in Å for Hβ. Intensity ratios within each spectral type can be computed from the reported values.

^(b)

In units of km s^-1.

^(c)

Kept fixed or allowed to vary within a narrow interval in SPECFIT analysis.

^(d)

In units of 10^-15 erg s^-1 cm^-2 Å^-1.

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