J/ApJ/788/159 17 Seyfert 1 galaxies light curves (Koshida+, 2014)
Reverberation measurements of the inner radius of the dust torus in 17 Seyfert galaxies. Koshida S., Minezaki T., Yoshii Y., Kobayashi Y., Sakata Y., Sugawara S., Enya K., Suganuma M., Tomita H., Aoki T., Peterson B.A. <Astrophys. J., 788, 159 (2014)> =2014ApJ...788..159K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, Seyfert ; Redshifts ; Photometry, VRI ; Photometry, infrared Keywords: dust, extinction - galaxies: active - galaxies: Seyfert - infrared: galaxies Abstract: We present the results of a dust reverberation survey for 17 nearby Seyfert 1 galaxies, which provides the largest homogeneous data collection for the radius of the innermost dust torus. A delayed response of the K-band light curve after the V-band light curve was found for all targets, and 49 measurements of lag times between the flux variation of the dust emission in the K band and that of the optical continuum emission in the V band were obtained by the cross-correlation function analysis and also by an alternative method for estimating the maximum likelihood lag. The lag times strongly correlated with the optical luminosity in the luminosity range of MV=-16 to -22 mag, and the regression analysis was performed to obtain the correlation log Δt (days)=-2.11 -0.2 MV assuming Δt∝L0.5, which was theoretically expected. We discuss the possible origins of the intrinsic scatter of the dust lag-luminosity correlation, which was estimated to be approximately 0.13 dex, and we find that the difference of internal extinction and delayed response of changes in lag times to the flux variations could have partly contributed to intrinsic scatter. However, we could not detect any systematic change of the correlation with the subclass of the Seyfert type or the Eddington ratio. Finally, we compare the dust reverberation radius with the near-infrared interferometric radius of the dust torus and the reverberation radius of broad Balmer emission lines. The interferometric radius in the K band was found to be systematically larger than the dust reverberation radius in the same band by the about a factor of two, which could be interpreted by the difference between the flux-weighted radius and response-weighted radius of the innermost dust torus. The reverberation radius of the broad Balmer emission lines was found to be systematically smaller than the dust reverberation radius by about a factor of four to five, which strongly supports the unified scheme of the Seyfert type of active galactic nuclei (AGNs). Moreover, we examined the radius-luminosity correlations for the hard X-ray (14-195 keV) and the [O IV] λ25.89 µm emission-line luminosities, which would be applicable for obscured AGNs. Description: Monitoring observations were conducted by using the multicolor imaging photometer (MIP) mounted on the MAGNUM telescope (Kobayashi et al. 1998SPIE.3352..120K, 1998SPIE.3354..769K). The MIP has a field of view of 1.5x1.5 arcmin2; it is capable of simultaneously obtaining images in optical (U, B, V, R, and I) and near-infrared (J, H, and K) bands by splitting the incident beam into two different detectors including an SITe CCD (1024x1024 pixels, 0.277 arcsec/pixel) and an SBRC InSb array (256x256 pixels, 0.346 arcsec/pixel). Monitoring observations with the MAGNUM telescope began in 2001-2003, although that for NGC 3516 and NGC 4593 began in 2005. We present the data obtained through 2006-2007 to include monitoring spans of three to seven yr. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 81 17 List of Target Active Galactic Nuclei table4.dat 40 3925 Light curve data
See also: VII/224 : Quasars and Active Galactic Nuclei (10th Ed.) (Veron+ 2001) VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) (Veron+ 2010) J/ApJS/141/31 : JHK' imaging photometry of Seyfert 1. II. (Enya+, 2002) J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+, 2004) J/AJ/143/83 : Properties of a sample of Seyfert 1 galaxies (Xu+, 2012) J/ApJ/755/60 : Reverberation mapping for five Seyfert 1 galaxies (Grier+, 2012) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Target AGN name 17- 18 I2 h RAh Hour of Right Ascension (J2000) 20- 21 I2 min RAm Minute of Right Ascension (J2000) 23- 26 F4.1 s RAs Second of Right Ascension (J2000) 28 A1 --- DE- Sign of the Declination (J2000) 29- 30 I2 deg DEd Degree of Declination (J2000) 32- 33 I2 arcmin DEm Arcminute of Declination (J2000) 35- 38 F4.1 arcsec DEs Arcsecond of Declination (J2000) 40- 43 F4.2 arcmin MajDiam Major diameter taken from the NED 45- 48 F4.2 arcmin MinDiam Minor diameter taken from the NED 50- 55 F6.4 --- z Redshift 57- 62 F6.2 mag VMag V-band absolute magnitude (1) 64- 66 F3.1 --- Type [1/1.8] Seyfert type of AGN 68 I1 --- Ref ? [1/2] Type reference (2) 70- 73 A4 [Msun] logM Log of mass accretion rate: log(MBH/M☉) 75- 78 F4.2 [Msun] e_logM ? Uncertainty in logM 81 I1 --- Ref1 ? [3/7] logM reference (3)
Note (1): Reported by Veron-Cetty & Veron (2001A&A...374...92V, Cat. VII/224). Note (2): Reference as follows: 1 = Osterbrock & Martel 1993ApJ...414..552O; 2 = Veron-Cetty & Veron 2010A&A...518A..10V, Cat. VII/258. Note (3): Reference as follows: 3 = Grier et al. 2012ApJ...755...60G; 4 = Peterson et al. 2004, J/ApJ/613/682; 5 = Denney et al. 2010ApJ...721..715D; 6 = Bentz et al. 2006ApJ...651..775B; 7 = Bentz et al. 2007ApJ...662..205B.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Target AGN name 17 A1 --- Band [VK] Observing band 19- 26 F8.2 d MJD Observation date 28- 33 F6.2 mJy Flux Flux in Band (1) 35- 40 F6.2 mJy e_Flux Error in Flux
Note (1): Correction for the Galactic extinction has not been applied to the light curves, and the fluxes from the host galaxy and narrow emission lines have not been subtracted.
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 18-Jul-2017
|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|