J/ApJ/702/441 Obscured active galaxies (Greene+, 2009)
The growth of black holes: insights from obscured active galaxies.
Greene J.E., Zakamska N.L., Liu X., Barth A.J., Ho L.C.
<Astrophys. J., 702, 441-459 (2009)>
=2009ApJ...702..441G 2009ApJ...702..441G
ADC_Keywords: Active gal. nuclei ; Galaxies, nearby ; Spectroscopy ;
Magnitudes, absolute
Keywords: galaxies: active - galaxies: nuclei - galaxies: Seyfert
Abstract:
Obscured or narrow-line active galaxies offer an unobstructed view of
the quasar environment in the presence of a luminous and vigorously
accreting black hole (BH). We exploit the large new sample of
optically selected luminous narrow-line active galaxies from the Sloan
Digital Sky Survey at redshifts 0.1<z<0.45, in conjunction with
follow-up observations with the Low Dispersion Survey Spectrograph
(LDSS3) at Magellan, to study the distributions of BH mass and host
galaxy properties in these extreme objects.
Description:
All of the data discussed in this paper were collected over two
observing runs using the Low Dispersion Survey Spectrograph (LDSS3) at
the Clay-Magellan telescope on Las Campanas in 2007 Mar 18-19 and Aug
14-15. For each target we obtained 2-5 minute acquisition images in g
and r, and sometimes i. The final spectra have a considerably higher
signal-to-noise ratio (S/N) than the SDSS spectra.
In order to increase our sample size, we have also considered all of
the targets in the Reyes et al. (2008, Cat. J/AJ/136/2373) sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 70 15 Sample and observations
table2.dat 80 15 Galaxy properties
table3.dat 83 111 Additional SDSS sample (version corrected by the
author)
table4.dat 79 15 Line emission and blue light
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See also:
J/MNRAS/399/1206 : SWIRE/SDSS quasars. II. Type 2 AGN (Hatziminaoglou+, 2009)
J/AJ/136/2373 : Type 2 quasars from SDSS (Reyes+, 2008)
J/AJ/131/84 : AGNs and host galaxies information (Vanden Berk+, 2006)
J/AJ/128/1002 : SDSS candidate type II quasars. II (Zakamska+, 2004)
J/ApJS/111/377 : Hγ + Hδ absorption features (Worthey+ 1997)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SDSS]
6- 24 A19 --- SDSS SDSS identification (JHHMMSS.ss+DDMMSS.s)
26- 30 F5.3 --- z Redshift
32- 36 F5.2 [10-7W] LOIII L[OIII] (in erg/s) (1)
38- 47 A10 "YYYY/MM/DD" Date Date of LDSS-3 observation
49- 52 I4 s Ts Total duration of spectroscopic exposure
54 I1 --- N Number of slit positions
56- 58 I3 s Ti ? Total integrated time
60- 62 I3 deg PA1 Position angle of slit 1 position (2)
64- 66 I3 deg PA2 ? Position angle of slit 2 position (2)
68- 70 I3 deg PA3 ? Position angle of slit 3 position (2)
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Note (1): L[OIII] as measured from the SDSS spectrum of Reyes et al.
2008, Cat. J/AJ/136/2373; used in the object selection.
Note (2): measured E from N.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SDSS]
6- 24 A19 --- SDSS SDSS identification (JHHMMSS.ss+DDMMSS.s)
26 A1 --- F Filter used for structural measurements
28 I1 --- n ? best-fit Sersic index for the bulge-like
component from the GALFIT model
30- 35 F6.2 mag rMAG Absolute magnitude of the bulge component (3)
37- 40 F4.2 mag e_rMAG rMAG uncertainty
42- 45 F4.2 mag k k-correction used to correct the absolute
magnitudes in F
47- 50 F4.2 mag Af Galactic reddening correction in F (4)
52- 55 F4.1 mag OIIIm Magnitude of the [OIII] line (5)
57- 59 F3.1 arcsec re ? Effective radius of the bulge-like
component of our best-fit model
61- 63 F3.1 arcsec e_re ? re uncertainty
65- 67 F3.1 kpc/arcsec S Scale-factor to convert re to a physical size
69- 73 F5.3 --- B/T ? Bulge-to-Total ratio for objects with
sensible GALFIT decompositions (6)
75- 77 I3 km/s Sig ? Stellar velocity dispersion within 2.25"
79- 80 I2 km/s e_Sig ? Sig uncertainty
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Note (3): Absolute magnitude as derived from our best-fit GALFIT model,
with an [OIII] correction (Column OIIIm), correction for Galactic
reddening (Column Af) and a k-correction (Column k) derived using the
code of Blanton & Roweis 2007AJ....133..734B 2007AJ....133..734B. Cases without sensible
multi-component models list total Petrosian magnitudes and are not
assigned a Sersic index, effective radius, or B/T.
Note (4): Galactic reddening correction in the filter shown in Column F.
Derived from the dust maps of Schlegel et al. 1998 and extinction law
of Cardelli et al. 1989.
Note (5): Magnitude of the [OIII] line used to correct the total r-band
(z≲0.38) or i-band magnitude.
Note (6): The B/T for SDSS J125334.49-034158.1 is very low because there is
also a bar component. If included as bulge light, the B/T increases to
0.05.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- SDSS Official SDSS name (HHMMSS.ss+DDMMSS.s; J2000)
21- 30 F10.6 deg RAdeg Right ascension in decimal degrees (J2000)
34- 42 F9.6 deg DEdeg Declination in decimal degrees (J2000)
46- 48 I3 --- Plate SDSS plate
51- 54 I4 --- Fiber SDSS fiber
56- 60 I5 --- MJD SDSS Modified Julian Date
62- 67 F6.4 --- z Redshift as measured by the SDSS pipeline
69- 73 F5.2 [10-7W] LOIII Log [OIII] luminosity in erg/s
76- 78 I3 km/s Sig Stellar velocity dispersion measured from
the SDSS spectra
81- 83 I3 km/s e_Sig Uncertainty in Sig
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SDSS]
6- 24 A19 --- SDSS SDSS identification (JHHMMSS.ss+DDMMSS.s)
26- 30 F5.2 [10-7W] logLOIII Luminosity in erg/s in the [OIII] line (7)
32- 35 I4 km/s FWHM The [OIII] line FWHM, corrected for
instrumental resolution (7)
37- 41 F5.2 --- OIII/Hb Ratio of [OIII] to Hβ emission (7)
43- 47 F5.3 --- OII/OIII Ratio of [OII] to [OIII] emission from the
SDSS spectra
49- 53 F5.2 [10-7W] logL5100d ? L5100Å (in erg/s) when detected in our
three-component continuum model
55- 59 F5.2 [10-7W] logL5100H ? L5100Å (erg/s) inferred from broad
Hβ when detected
61- 64 F4.1 [10-7W] logL5100l Final adopted upper limit on contribution to
L5100Å (erg/s) from scattered light (8)
65 A1 --- n_logL5100l [*] Possible star forming populations (9)
67- 69 F3.1 [-] logDn ? The Dn(4000) index (10)
71- 74 F4.1 --- HdA ? The HδA index (11)
76- 79 F4.1 [-] logM300 ? The fraction of total galaxy mass formed in
the last 300Myr, based on stellar population
synthesis
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Note (7): Within the 2.25" aperture.
Note (8): Final adopted upper limit on contribution to L5100Å from
scattered light, as derived from limits on a scattered broad Hβ
component.
Note (9): * indicates systems where the blue light is substantially more
than can be accounted for with scattered light. These systems may have
a substantial star-forming population.
Note (10): The Dn(4000) index, measured from our best-fit continuum model
to the SDSS spectra following Balogh et al. (1999ApJ...527...54B 1999ApJ...527...54B).
Note (11): The HδA index, measured from our best-fit continuum model
to the SDSS spectra following Worthey & Ottaviani (1997, Cat.
J/ApJS/111/377). Positive values of HδA indicate absorption.
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History:
* 28-Sep-2011: From electronic version of the journal
* 02-Feb-2012: In table3, the SDSS names seem to be screwed up.
* 14-May-2012: Table3 version corrected by the author.
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 28-Sep-2011