2011ApJ...742...93A


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.24CEST06:03:44

2011ApJ...742...93A - Astrophys. J., 742, 93 (2011/December-1)

Black hole mass estimates based on C IV are consistent with those based on the Balmer lines.

ASSEF R.J., DENNEY K.D., KOCHANEK C.S., PETERSON B.M., KOZLOWSKI S., AGEORGES N., BARROWS R.S., BUSCHKAMP P., DIETRICH M., FALCO E., FEIZ C., GEMPERLEIN H., GERMEROTH A., GRIER C.J., HOFMANN R., JUETTE M., KHAN R., KILIC M., KNIERIM V., LAUN W., LEDERER R., LEHMITZ M., LENZEN R., MALL U., MADSEN K.K., MANDEL H., MARTINI P., MATHUR S., MOGREN K., MUELLER P., NARANJO V., PASQUALI A., POLSTERER K., POGGE R.W., QUIRRENBACH A., SEIFERT W., STERN D., SHAPPEE B., STORZ C., VAN SADERS J., WEISER P. and ZHANG D.

Abstract (from CDS):

Using a sample of high-redshift lensed quasars from the CASTLES project with observed-frame ultraviolet or optical and near-infrared spectra, we have searched for possible biases between supermassive black hole (BH) mass estimates based on the C IV, Hα, and Hβ broad emission lines. Our sample is based upon that of Greene, Peng, & Ludwig, expanded with new near-IR spectroscopic observations, consistently analyzed high signal-to-noise ratio (S/N) optical spectra, and consistent continuum luminosity estimates at 5100 Å. We find that BH mass estimates based on the full width at half-maximum (FWHM) of C IV show a systematic offset with respect to those obtained from the line dispersion, σl, of the same emission line, but not with those obtained from the FWHM of Hα and Hβ. The magnitude of the offset depends on the treatment of the He II and Fe II emission blended with C IV, but there is little scatter for any fixed measurement prescription. While we otherwise find no systematic offsets between C IV and Balmer line mass estimates, we do find that the residuals between them are strongly correlated with the ratio of the UV and optical continuum luminosities. This means that much of the dispersion in previous comparisons of C IV and Hβ BH mass estimates are due to the continuum luminosities rather than to any properties of the lines. Removing this dependency reduces the scatter between the UV- and optical-based BH mass estimates by a factor of approximately two, from roughly 0.35 to 0.18 dex. The dispersion is smallest when comparing the C IV σl mass estimate, after removing the offset from the FWHM estimates, and either Balmer line mass estimate. The correlation with the continuum slope is likely due to a combination of reddening, host contamination, and object-dependent SED shapes. When we add additional heterogeneous measurements from the literature, the results are unchanged. Moreover, in a trial observation of a remaining outlier, the origin of the deviation is clearly due to unrecognized absorption in a low S/N spectrum. This not only highlights the importance of the quality of the observations, but also raises the question whether cases like this one are common in the literature, further biasing comparisons between C IV and other broad emission lines.

Abstract Copyright:

Journal keyword(s): galaxies: active - gravitational lensing: strong - quasars: emission lines

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 Mrk 1502 Sy1 00 53 34.9326560879 +12 41 35.927159668   14.41 14.03     ~ 1065 1
2 QSO B0142-100 QSO 01 45 16.5955770048 -09 45 17.269954127   17.23 16.95     ~ 230 1
3 [VV2006] J024634.1-082536 QSO 02 46 34.1072517858 -08 25 36.201597772   18.42 18.20 17.94   ~ 47 1
4 HD 50951 * 06 56 11.7753685444 +18 48 00.645714954   8.04 8.08     B9 8 0
5 QSO B0810+2554 QSO 08 13 31.2926 +25 45 03.061   16.58 16.18     ~ 86 1
6 QSO B0909+5312 QSO 09 13 01.031 +52 59 28.90   17.29 16.71     ~ 135 1
7 8C 0958+561 QSO 10 01 20.6915852239 +55 53 55.595776916   17.16 16.95     ~ 706 3
8 QSO J1004+1229 QSO 10 04 24.8871 +12 29 22.245   24.83 23.23 20.80   ~ 48 1
9 QSO B1001+4127 QSO 10 04 34.9236085542 +41 12 42.771226567   19.14 19.03     ~ 171 1
10 Feige 34 HS* 10 39 36.7377085527 +43 06 09.209752646 9.613 10.91 11.14 11.319 11.464 sdOp 621 0
11 QSO B1104-181 QSO 11 06 33.39 -18 21 23.8   15.8 15.9 15.7   ~ 308 1
12 QSO B1115+080A QSO 11 18 16.951 +07 45 58.23   16.61 16.44     ~ 640 2
13 QSO J1138+0314 QSO 11 38 03.7479119406 +03 14 57.836414453   19.42 19.17     ~ 51 1
14 [VV2006] J115111.2+034048 QSO 11 51 11.2030741555 +03 40 48.346648913   21.03 20.78     ~ 24 0
15 QSO J1415+1129 QSO 14 15 46.25 +11 29 43.4   17.63 17.23     ~ 608 0
16 QSO B1422+2309 BLL 14 24 38.09400 +22 56 00.5900   16.77 15.84 14.79   ~ 425 1
17 [PBW92] 1422+231 gLS 14 24 38.09400 +22 56 00.5900   16.77 15.84 14.79   ~ 355 0
18 Feige 98 HS* 14 38 15.7540771045 +27 29 32.913319195   11.7 11.7     sdB9IIIHe1 35 0
19 [VV2000] J163348.9+313411 QSO 16 33 48.9842 +31 34 11.871   17.1 17.41 17.0   ~ 47 1
20 QSO J2240+0321 QSO 22 40 30.234 +03 21 30.63           ~ 650 1
21 Z 378-15 G 22 40 30.23447 +03 21 30.6290           ~ 629 0

    Equat.    Gal    SGal    Ecl

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2021.06.24-06:03:44

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