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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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)
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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 2001ApJ...546..681T). Following Jensen et
al. (2003ApJ...583..712J 2003ApJ...583..712J), we have corrected the distance modulus
reported by Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T) by subtracting 0.16mag.
Note (3): Distances obtained using the PNLF method; see Herrmann et al.
(2008ApJ...683..630H 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 2002A&A...389..812K) (the distance
to NGC 3031 obtained by the Cepheid method by Freedman et al.,
1994ApJ...427..628F 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 1999MNRAS.304..595G);
* NGC 4438, NGC 4457, and NGC 4579 using the Tully-Fisher method (see
Gavazzi et al., 1999MNRAS.304..595G 1999MNRAS.304..595G);
* NGC 3031, NGC 4548, and NGC 7331 using the Cepheid variable method
(Freedman et al., 2001ApJ...553...47F 2001ApJ...553...47F, 1994ApJ...427..628F 1994ApJ...427..628F).
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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- 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)
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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 1994ApJ...429..582C), while the maximum correction corresponds to
the Milky Way law of Seaton (1979MNRAS.187p..73S 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.
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [NGC]
5- 8 I4 --- NGC NGC number
10- 80 A71 --- Note Text of note from section 3.3
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode Bibcode
24- 46 A23 --- Aut First author name
47- 69 A23 --- Comm Comments
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-Apr-2010