J/A+A/561/A140 Low-luminosity type-1 QSO sample (Busch+, 2014)
A low-luminosity type-1 QSO sample.
I. Overluminous host spheroidals or undermassive black holes?
Busch G., Zuther J., Valencia-S. M., Moser L., Fischer S., Eckart A.,
Scharwachter J., Gadotti D.A., Wisotzki L.
<Astron. Astrophys. 561, A140 (2014)>
=2014A&A...561A.140B 2014A&A...561A.140B
ADC_Keywords: QSOs ; Active gal. nuclei ; Galaxies, Seyfert ;
Photometry, infrared
Keywords: galaxies: active - quasars: general - galaxies: Seyfert
Abstract:
Recognizing the properties of the host galaxies of quasi-stellar
objects (QSOs) is essential to understand the suspected coevolution of
central supermassive black holes (BHs) and their host galaxies. We
selected a subsample of the Hamburg/ESO survey for bright UV-excess
QSOs, containing only the 99 nearest QSOs with redshift z≤0.06, that
are close enough to allow detailed structural analysis. From this
"low-luminosity type-1 QSO sample", we observed 20 galaxies and
performed aperture photometry and bulge-disk-bar-AGN-decomposition
with BUDDA on near-infrared J, H, K band images. From the photometric
decomposition of these 20 objects and visual inspection of images of
another 26, we find that ∼50% of the hosts are disk galaxies and most
of them (86%) are barred. Stellar masses, calculated from parametric
models based on inactive galaxy colors, range from 2x109M☉ to
2x1011M☉. Black hole masses measured from single epoch
spectroscopy range from 1x106M☉ to 5x108M☉. In
comparison to higher luminosity QSO samples, LLQSOs tend to have lower
stellar and BH masses. Also, in the effective radius vs. mean
surface-brightness projection of the fundamental plane, they lie in
the transition area between luminous QSOs and "normal" galaxies. This
can be seen as further evidence that they can be pictured as a
"bridge" between the local Seyfert population and luminous QSOs at
higher redshift. Eleven low-luminosity QSOs for which we have reliable
morphological decompositions and BH mass estimations lie below the
published BH mass vs. bulge luminosity relations for inactive
galaxies. This could be partially explained by bulges of active
galaxies containing much younger stellar populations than bulges of
inactive galaxies. Also, one could suspect that their BHs are
undermassive. This might hint at the growth of the host spheroid to
precede that of the BH.
Description:
The results of the structural decomposition with BUDDA are presented
here. The galaxies have been observed in the near-infrared J, H, and K
band. For each band, there is one table. For all 20 galaxies the
following parameters are presented: central surface brightness and
scale length of the disk, effective surface brightness, effective
radius and Sersic index of the bulge component, the luminosity
fractions of bulge, disk, bar, and AGN component.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 104 20 Object information for the observed galaxies
paramj.dat 61 20 BUDDA fit parameters for J band
paramh.dat 61 20 BUDDA fit parameters for H band
paramk.dat 61 20 BUDDA fit parameters for K band
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [5/89] ID number in LLQSO sample
4- 14 A11 --- Name Hamburg/ESO survey name (HEHHMM+DDMM)
16- 17 I2 h RAh Right ascension (J2000)
19- 20 I2 min RAm Right ascension (J2000)
22- 26 F5.2 s RAs Right ascension (J2000)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination (J2000)
32- 33 I2 arcmin DEm Declination (J2000)
35- 39 F5.2 arcsec DEs Declination (J2000)
41- 46 F6.4 --- z Redshift
48- 52 F5.2 mag Bmag BJ nuclear magnitude
53 A1 --- n_Bmag [a] a: magnitude from NED
55- 60 F6.2 mag BMAG Absolute BJ nuclear magnitude
61 A1 --- n_BMAG [a] a: magnitude from NED
63- 66 A4 --- Inst Instrument
68- 70 F3.1 arcsec Jsee Seeing in the J band
72 A1 --- --- [-]
74- 76 F3.1 arcsec Hsee Seeing in the H band
78 A1 --- --- [-]
80- 82 F3.1 arcsec Ksee Seeing in the K band
84- 88 F5.2 mag/arcsec2 Jsky Sky deviation in the J band
90 A1 --- --- [-]
92- 96 F5.2 mag/arcsec2 Hsky Sky deviation in the H band
98 A1 --- --- [-]
100-104 F5.2 mag/arcsec2 Ksky Sky deviation in the K band
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Byte-by-byte Description of file: paramj.dat paramh.dat paramk.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [5/89] ID number in LLQSO sample
4- 14 A11 --- Name Hamburg/ESO survey name (HEHHMM+DDMM)
16- 19 F4.1 mag/arcsec2 mu0 ?=- Central surface brightness of disk
21- 24 F4.1 arcsec h ?=- Scale length of disk
26- 29 F4.1 mag/arcsec2 mue ?=- Effective surface brightness of bulge
31- 33 F3.1 arcsec re ?=- Effective radius of bulge
35- 37 F3.1 --- n ?=- Sersic index of bulge
39- 43 F5.3 --- B/T ?=- Bulge-to-total fraction
45- 49 F5.3 --- D/T ?=- Disk-to-total fraction
51- 55 F5.3 --- Bar/T ?=- Bar-to-total fraction
57- 61 F5.3 --- A/T ?=- AGN-to-total fraction
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Acknowledgements:
Gerold Busch, busch(at)ph1.uni-koeln.de
(End) Patricia Vannier [CDS] 23-Jan-2014