J/ApJ/815/128 AGNs rest-frame UV and optical parameters (Karouzos+, 2015)
Rest-frame UV single-epoch black hole mass estimates of low-luminosity AGNs
at intermediate redshifts.
Karouzos M., Woo J.-H., Matsuoka K., Kochanek C.S., Onken C.A.,
Kollmeier J.A., Park D., Nagao T., Kim S.C.
<Astrophys. J., 815, 128 (2015)>
=2015ApJ...815..128K 2015ApJ...815..128K (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; QSOs ; Redshifts ; Magnitudes ;
Spectroscopy ; Ultraviolet
Keywords: galaxies: active - quasars: emission lines -
quasars: supermassive black holes
Abstract:
The ability to accurately derive black hole (BH) masses at
progressively higher redshifts and over a wide range of continuum
luminosities has become indispensable in the era of large-area
extragalactic spectroscopic surveys. In this paper, we present an
extension of existing comparisons between rest-frame UV and optical
virial BH mass estimators to intermediate redshifts and luminosities
comparable to the local Hβ reverberation-mapped active galactic
nuclei (AGNs). We focus on the Mg II, C IV, and C III] broad emission
lines and compare them to both Hα and Hβ. We use newly
acquired near-infrared spectra from the Fiber-fed Multi-object
Spectrograph instrument on the Subaru telescope for 89 broad-lined
AGNs at redshifts between 0.3 and 3.5, complemented by data from the
AGES survey. We employ two different prescriptions for measuring the
emission line widths and compare the results. We confirm that Mg II
shows a tight correlation with Hα and Hβ, with a scatter of
∼0.25 dex. The C IV and C III] estimators, while showing larger
scatter, are viable virial mass estimators after accounting for a
trend with the UV-to-optical luminosity ratio. We find an intrinsic
scatter of ∼0.37 dex between Balmer and carbon virial estimators by
combining our data set with previous high redshift measurements. This
updated comparison spans a total of three decades in BH mass. We
calculate a virial factor for C IV/C III] logf_C IV/C III]_=0.87 with
an estimated systematic uncertainty of ∼0.4 dex and find excellent
agreement between the local reverberation mapped AGN sample and our
high-z sample.
Description:
We used AGNs from the AGN and Galaxy Evolution Survey (AGES;
Kochanek et al. 2012, J/ApJS/200/8), which has a lower flux limit
(mI<22.5) than other wide-area surveys such as the Sloan Digital Sky
Survey (SDSS). We selected 89 broad-line AGNs at redshifts of
0.3<z<3.5 with at least one of the broad UV lines of interest (Mg II,
C IV, and C III]) detected in the optical spectra. We used the FMOS
(Kimura et al. 2010PASJ...62.1135K 2010PASJ...62.1135K) at the Subaru 8.2 m telescope to
obtain near-IR spectra (rest-frame optical) of 89 high redshift and
low luminosity Type 1 AGNs. The optical spectroscopy (Kochanek et al.
2012, J/ApJS/200/8) was acquired using the Hectospec instrument
(Fabricant et al. 1998SPIE.3355..285F 1998SPIE.3355..285F, 2005PASP..117.1411F 2005PASP..117.1411F; Roll et
al. 1998SPIE.3355..324R 1998SPIE.3355..324R) at the 6.5 m MMT telescope.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 82 89 The FMOS-AGES Sample of Type 1 Quasars
table4.dat 75 89 Continuum and Emission Line Luminosities
in the UV and Optical
table5.dat 75 82 Best-fit Profile Parameters for Rest-frame UV
Emission Lines
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See also:
J/ApJS/168/1 : Black hole mass estimates (Kelly+, 2007)
J/ApJ/680/169 : SDSS DR5 virial black hole masses (Shen+, 2008)
J/ApJS/194/42 : SDSS-DR3 MgII-based black hole masses (Rafiee+, 2011)
J/ApJS/200/8 : AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)
J/A+A/587/A138 : Low-luminosity type-1 QSO sample. V. (Busch+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [spec]
5- 9 I5 --- spec [00409/02277] FMOS ID (specNNNNN)
11- 12 I2 h RAh Hour of Right Ascension (J2000)
14- 15 I2 min RAm Minute of Right Ascension (J2000)
17- 21 F5.2 s RAs Second of Right Ascension (J2000)
23 A1 --- DE- Sign of the Declination (J2000)
24- 25 I2 deg DEd Degree of Declination (J2000)
27- 28 I2 arcmin DEm Arcminute of Declination (J2000)
30- 33 F4.1 arcsec DEs Arcsecond of Declination (J2000)
35- 38 F4.2 --- z Redshift derived from the AGES survey
(Kochanek et al. 2012, J/ApJS/200/8)
40- 44 F5.2 mag Imag I-band AB magnitude
46- 50 F5.2 [10-7W] logLI Log of monochromatic luminosity calculated at
the effective wavelength 7467Å
52- 57 I6 --- Code [16/782272] Selection code for the AGES survey
(see Kochanek et al. 2012, J/ApJS/200/8)
59- 60 I2 --- S/N [1/35] Mean signal-to-noise ratio for the AGES
spectrum
62- 66 F5.2 mag Ksmag Ks-band AB magnitude
68- 72 F5.2 [10-7W] logLKs Log of monochromatic luminosity calculated at
the effective wavelength 21900Å
74 A1 --- CIV [0/1] Information about the detection of emission
for the CIV broad emission line (1)
76 A1 --- CIII [0/1] Information about the detection of emission
for the CIII] broad emission line (1)
78 A1 --- MgII [0/1] Information about the detection of emission
for the MgII broad emission line (1)
80 A1 --- Hbeta [0/1] Information about the detection of emission
for the Hβ broad emission line (1)
82 A1 --- Halpha [0/1] Information about the detection of emission
for the Hα broad emission line (1)
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Note (1): Information as follows:
1 = Detection;
0 = Non-detection.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [spec]
5- 9 I5 --- spec [00409/02277] FMOS ID (specNNNNN)
11- 15 F5.2 [10-7W] logL1350 ? Log of monochromatic luminosity at 1350Å
17- 20 F4.2 [10-7W] e_logL1350 ? Uncertainty in logL1350
22- 26 F5.2 [10-7W] logL1800 ? Log of monochromatic luminosity at 1800Å
28- 31 F4.2 [10-7W] e_logL1800 ? Uncertainty in logL1800
33- 37 F5.2 [10-7W] logL3000 ? Log of monochromatic luminosity at 3000Å
39- 42 F4.2 [10-7W] e_logL3000 ? Uncertainty in logL3000
44- 48 F5.2 [10-7W] logL5100 ? Log of monochromatic luminosity at 5100Å
50- 53 F4.2 [10-7W] e_logL5100 ? Uncertainty in logL5100
55- 59 F5.2 [10-7W] logLHa ? Log of the integrated luminosity of
the Hα emission line
61- 64 F4.2 [10-7W] e_logLHa ? Uncertainty in logLHa
66- 70 F5.2 [10-7W] logLHb ? Log of the integrated luminosity of
the Hβ emission line
72- 75 F4.2 [10-7W] e_logLHb ? Uncertainty in logLHb
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [spec]
5- 9 I5 --- spec [00409/02277] FMOS ID (specNNNNN)
11- 14 F4.2 km/s sigCIII] ? Second moment of the CIII] emission line
16- 19 F4.2 km/s e_sigCIII] ? Uncertainty in sigCIII]
21- 24 F4.2 km/s FW(CIII]) ? FWHM of the CIII] emission line
26- 29 F4.2 km/s e_FW(CIII]) ? Uncertainty in FW(CIII])
31 A1 --- Flag1 [ABCF] Visual quality flag for CIII] (1)
33- 36 F4.2 km/s sigCIV ? Second moment of the CIV emission line
38- 41 F4.2 km/s e_sigCIV ? Uncertainty in sigCIV
43- 46 F4.2 km/s FW(CIV) ? FWHM of the CIV emission line
48- 51 F4.2 km/s e_FW(CIV) ? Uncertainty in FW(CIV)
53 A1 --- Flag2 [ABCF] Visual quality flag for CIV (1)
55- 58 F4.2 km/s sigMgII ? Second moment of the MgII emission line
60- 63 F4.2 km/s e_sigMgII ? Uncertainty in sigMgII
65- 68 F4.2 km/s FW(MgII) ? FWHM of the MgII emission line
70- 73 F4.2 km/s e_FW(MgII) ? Uncertainty in FW(MgII)
75 A1 --- Flag3 [ABCF] Visual quality flag for MgII (1)
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Note (1): Based on visual inspection, a quality flag is assigned to each fit,
that ranges from A for the best fits to C for the poorest fits. These
quality flags do not reflect the actual noise of the data but rather
correspond to how well the best-fit model describes the emission line
profile. A visual quality flag F is assigned to sources for which the
fit fails completely (usually due to extremely noisy data).
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History:
From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 19-Oct-2017