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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
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:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 6- 24 A19 --- SDSS SDSS identification ( 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)
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.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 6- 24 A19 --- SDSS SDSS identification ( 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
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. 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.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 18 A18 --- SDSS Official SDSS name (; 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
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 6- 24 A19 --- SDSS SDSS identification ( 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
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). 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.
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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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