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J/ApJS/187/135    SEDs of weak AGNs associated with LINERs    (Eracleous+, 2010)

Spectral energy distributions of weak active galactic nuclei associated with low-ionization nuclear emission regions. Eracleous M., Hwang J.A., Flohic H.M.L.G. <Astrophys. J. Suppl. Ser., 187, 135-148 (2010)> =2010ApJS..187..135E
ADC_Keywords: Active gal. nuclei ; Energy distributions ; X-ray sources Keywords: galaxies: active - galaxies: nuclei - X-rays: galaxies Abstract: We present a compilation of spectral energy distributions (SEDs) of 35 weak active galactic nuclei (AGNs) in low-ionization nuclear emission regions (LINERs) using recent data from the published literature. We make use of previously published compilations of data, after complementing and extending them with more recent data. The main improvement in the recent data is afforded by high-spatial-resolution observations with the Chandra X-Ray Observatory and high spatial resolution radio observations utilizing a number of facilities. In addition, a considerable number of objects have been observed with the Hubble Space Telescope in the near-IR through near-UV bands since the earlier compilations were published. The data include upper limits resulting from either non-detections or observations at low spatial resolution that do not isolate the AGN. For the sake of completeness, we also compute and present a number of quantities from the data, such as optical-to-X-ray spectral indices (αox), bolometric corrections, bolometric luminosities, Eddington ratios, and the average SED. We anticipate that these data will be useful for a number of applications. In a companion paper, we use a subset of these data ourselves to assess the energy budgets of LINERs. Description: We constructed a sample of objects classified as LINERs or transition objects by Ho et al. (1997, cat. J/ApJS/112/315). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 54 35 Sample of galaxies and their basic properties table3.dat 57 350 Spectral Energy Distributions of individual LINERs refs.dat 69 25 References from table 3 notes.dat 80 104 Notes on individual objects
See also: VII/145 : Nearby Galaxies Catalogue (NBG) (Tully 1988) VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998) VIII/71 : The FIRST Survey Catalog, Version 03Apr11 (Becker+ 2003) J/ApJS/107/215 : UV Images of Nearby Galaxies (Maoz+, 1996) J/ApJS/112/315 : Spectroscopic parameters of Seyfert nuclei (Ho+ 1997) J/ApJ/577/31 : PNe in six galaxies (Ciardullo+, 2002) J/A+A/414/825 : Mid-infrared spectroscopy of LINERs (Satyapal+, 2004) J/A+A/435/521 : Radio Sources in Low-Luminosity AGNs. IV (Nagar+, 2005) J/ApJ/663/81 : SED of hard X-ray selected AGN in XMDS (Polletta+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [NGC] 5- 8 I4 --- NGC NGC number 9 A1 --- n_NGC [*] indicates a note in notes.dat file 11- 23 A13 --- OName Other name(s) 25- 34 A10 --- TType Hubble morphological type (1) 36- 39 F4.1 Mpc DistT Distance from Tully (1988, Cat. VII/145) 41- 44 F4.1 Mpc DistS ? SBF distance (2) 46- 49 F4.1 Mpc DistP ? PNLF distance (3) 51- 54 F4.1 Mpc DistO ? Distance from other source (4)
Note (1): Host galaxy Hubble types were taken from the catalog of Tully, Cat. VII/145. Note (2): Distances obtained using the surface brightness fluctuation method; see Tonry et al. (2001ApJ...546..681T). Following Jensen et al. (2003ApJ...583..712J), we have corrected the distance modulus reported by Tonry et al. (2001ApJ...546..681T) by subtracting 0.16mag. Note (3): Distances obtained using the PNLF method; see Herrmann et al. (2008ApJ...683..630H) for NGC 4736 and compilation of Ciardullo et al. (2002, J/ApJ/577/31) and references therein for other galaxies. Note (4): Distances obtained using a variety of different methods: * NGC 404, NGC 3031, and NGC 4736 using the tip of the red giant branch (TRGB) method (Karachetsev et al., 2002A&A...389..812K) (the distance to NGC 3031 obtained by the Cepheid method by Freedman et al., 1994ApJ...427..628F, agrees exactly with the TRGB distance); * NGC 4261, NGC 4552, and NGC 4636 using the fundamental plane relation (see Gavazzi et al., 1999MNRAS.304..595G); * NGC 4438, NGC 4457, and NGC 4579 using the Tully-Fisher method (see Gavazzi et al., 1999MNRAS.304..595G); * NGC 3031, NGC 4548, and NGC 7331 using the Cepheid variable method (Freedman et al., 2001ApJ...553...47F, 1994ApJ...427..628F).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [NGC] 5- 8 I4 --- NGC Galaxy name 10- 17 E8.3 Hz nu Frequency 19 A1 --- l_Lobs Limit flag on Lobs 20- 27 E8.3 10-7W Lobs ? Observed monochromatic luminosity 28 A1 --- l_L(C) Limit flag on L(C) 29- 36 E8.3 10-7W L(C) ? Calzetti corrected monochromatic luminosity (1) 37 A1 --- l_L(S) Limit flag on L(S) 38- 45 E8.3 10-7W L(S) ? Seaton corrected monochromatic luminosity (1) 46- 48 I3 % Frac ? Fractional dispersion (2) 50- 53 A4 --- Ref Reference(s) in refs.dat file 55- 57 A3 --- Note Note flag (3)
Note (1): In erg/s from 0.1 to 1µm after correction for extinction. The minimum correction employs the starburst extinction law of Calzetti et al. (1994ApJ...429..582C), while the maximum correction corresponds to the Milky Way law of Seaton (1979MNRAS.187p..73S). Details are given in Section 3.1 of the text. The "observed" X-ray luminosities already have this correction built in. The distances used are those of Tully (Cat. VII/145); see Table 1 and the discussion in Section 2.1. Note (2): In the monochromatic luminosity in cases where a number of measurements were averaged together. See Section 3.1 of the text for details. Note (3): Flags as follows: d = See detailed notes on this object in notes.dat file. e = Upper limit to νLν(2500Å) derived by assuming αox=1.5. See Section 4.1 of the text for details. f = This limit is a result of a non-detection. g = This limit is a result of contamination of the source by other, neighboring sources; the observations were taken through a large aperture. h = The observed UV flux most likely originates in hot stars in the immediate vicinity of the nucleus, not in the AGN. See the discussion in Section 3.3 of the text. The values of αox implied by the UV flux is extremely high for such a low-luminosity AGN thus, the UV flux listed here can be taken as a generous upper limit to the UV flux of the AGN.
Byte-by-byte Description of file: notes.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [NGC] 5- 8 I4 --- NGC NGC number 10- 80 A71 --- Note Text of note from section 3.3
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode Bibcode 24- 46 A23 --- Aut First author name 47- 69 A23 --- Comm Comments
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-Apr-2010
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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