J/MNRAS/454/766 Mid-infrared-X-ray correlation for local AGNs (Asmus+, 2015)
The subarcsecond mid-infrared view of local active galactic nuclei -
II. The mid-infrared-X-ray correlation.
Asmus D., Gandhi P., Honig S.F., Smette A., Duschl W.J.
<Mon. Not. R. Astron. Soc., 454, 766-803 (2015)>
=2015MNRAS.454..766A 2015MNRAS.454..766A (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies, Seyfert ; Galaxies, IR ;
X-ray sources ; Galaxies, nearby
Keywords: galaxies: active - galaxies: Seyfert - infrared: galaxies -
X-rays: galaxies - stars: AGB and post-AGB - circumstellar matter -
stars: variables: Cepheids - infrared: stars
Abstract:
We present an updated mid-infrared (MIR) versus X-ray correlation for
the local active galactic nuclei (AGN) population based on the high
angular resolution 12 and 18µm continuum fluxes from the AGN
subarcsecond MIR atlas and 2-10 keV and 14-195 keV data collected from
the literature. We isolate a sample of 152 objects with reliable AGN
nature and multi-epoch X-ray data and minimal MIR contribution from
star formation. Although the sample is not homogeneous or complete, we
show that our results are unlikely to be affected by significant
biases. The MIR-X-ray correlation is nearly linear and within a factor
of 2 independent of the AGN type and the wavebands used. The observed
scatter is <0.4 dex. A possible flattening of the correlation slope at
the highest luminosities probed (∼1045 erg/s) towards low MIR
luminosities for a given X-ray luminosity is indicated but not significant.
Unobscured objects have, on average, an MIR-X-ray ratio that is only
≤0.15 dex higher than that of obscured objects. Objects with
intermediate X-ray column densities (22<logNH<23) actually show the
highest MIR-X-ray ratio on average. Radio-loud objects show a higher
mean MIR-X-ray ratio at low luminosities while the ratio is lower than
average at high luminosities. This may be explained by synchrotron
emission from the jet contributing to the MIR at low luminosities and
additional X-ray emission at high luminosities. True Seyfert 2 candidates
do not show any deviation from the general behaviour suggesting that
they possess a dusty obscurer as in other AGN. Double AGN also do not
deviate. Finally, we show that the MIR-X-ray correlation can be used
to investigate the AGN nature of uncertain objects. Specifically, we
give equations that allow us to determine the intrinsic 2-10 keV
luminosities and column densities for objects with complex X-ray
properties to within 0.34 dex. These techniques are applied to the
uncertain objects of the remaining AGN MIR atlas, demonstrating the
usefulness of the MIR-X-ray correlation as an empirical tool.
Description:
We start with the total sample from the AGN MIR atlas of 253 objects
(Asmus et al. 2014, J/MNRAS/439/1648). Note that sample is a combination
of a hard X-ray (14-195 keV) selected and a quasi-MIR selected sample
as explained in Asmus et al. (2014, J/MNRAS/439/1648). The MIR continuum
fluxes are the unresolved nuclear fluxes extracted from ground-based
multifilter photometry obtained with the instruments VISIR (Lagage et al.
2004Msngr.117...12L 2004Msngr.117...12L), T-ReCS (Telesco et al. 1998SPIE.3354..534T 1998SPIE.3354..534T),
Michelle (Glasse, Atad-Ettedgui & Harris 1997SPIE.2871.1197G 1997SPIE.2871.1197G), and COMICS;
(Kataza et al. 2000SPIE.4008.1144K 2000SPIE.4008.1144K). We collect observed 14-195 keV fluxes,
Fobs(14-195 keV), measured with Swift/BAT (Burst Alert Telescope) by
combining the data of the 54 and 70 month source catalogues with preference
for the latter (Cusumano et al. 2010, J/A+A/524/A64; Baumgartner et al.
2013, J/ApJS/207/19).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 122 151 Reliable sample
refs.dat 83 209 References
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See also:
J/A+A/418/465 : Mid-infrared and hard X-ray emission in AGN (Lutz+, 2004)
J/ApJ/610/128 : NIR colors of hard X-ray-selected AGN (Watanabe+, 2004)
J/ApJ/705/14 : Seyfert galaxies in the mid-IR (Deo+, 2009)
J/A+A/524/A64 : The 54-month Palermo BAT-survey catalogue (Cusumano+, 2010)
J/ApJ/725/2270 : Mid-IR emission lines in AGNs (Pereira-Santaella+, 2010)
J/ApJ/754/45 : IR properties of Swift/BAT X-ray AGNs (Ichikawa+, 2012)
J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 2004-2010
(Baumgartner+, 2013)
J/MNRAS/439/1648 : Subarcsecond mid-infrared atlas of local AGN (Asmus+, 2014)
J/ApJ/807/129 : X-ray to MIR luminosities relation of AGNs (Stern, 2015)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Short object name
17- 22 F6.1 Mpc Dist Distance
24- 30 A7 --- OClass Optical class (1)
32- 33 A2 --- l_logL12 [≤ ] Limit flag on logL12
34- 38 F5.2 [10-7W] logL12 Nuclear 12µm luminosity from Asmus et al.
(2014, J/MNRAS/439/1648) (in erg/s)
40- 43 F4.2 [10-7W] e_logL12 ? Uncertainty in logL12
45- 46 A2 --- l_logL18 [≤ ] Limit flag on logL18
47- 51 F5.2 [10-7W] logL18 ? Nuclear 18µm luminosity from Asmus et al.
(2014, J/MNRAS/439/1648) (in erg/s)
53- 56 F4.2 [10-7W] e_logL18 ? Uncertainty in logL18
58- 59 A2 --- Nep Number of 2-10 keV epochs used
61- 65 F5.2 [10-7W] logLobs Average observed 2-10 keV luminosity
(in erg/s)
67- 70 F4.2 [10-7W] e_logLobs Uncertainty in logLobs
72- 73 A2 --- l_logNH [<≥ ] Limit flag on logNH
74- 77 F4.1 [cm-2] logNH Average X-ray column density
79- 82 F4.2 [cm-2] e_logNH ? Uncertainty in logNH
84- 88 F5.2 [10-7W] logLint Average absorption-corrected 2-10 keV
luminosity
90- 93 F4.2 [10-7W] e_logLint ? Uncertainty in logLint
95- 96 A2 --- l_logL [≤ ] Limit flag on logL
97-101 F5.2 [10-7W] logL Average observed 14-195 keV luminosity from
Swift/BAT (2)
103-106 F4.2 [10-7W] e_logL ? Uncertainty in logL
108 A1 --- Flag [01?] Radio-loudness flag (see Section 4.6
for explanation) (3)
110-122 A13 --- Ref Reference(s) for the 2-10 keV luminosities and
column densities (see refs.dat file)
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Note (1): Optical class as follows:
1; 1.2; 1.5; 1/1.5 and 1.5/L = Seyferts with broad unpolarized emission lines;
1n = Narrow-line Seyferts 1;
1.8; 1.9 and 1.5/2 = Intermediate type Seyferts;
1.8/2; 1.9/2 and 2 = Seyferts without broad emission lines
(in unpolarized light);
L and L: = Low-ionization nuclear emission line regions.
Note (2): Obtained by combining the data of the 54 and 70 month source
catalogues (Cusumano et al. 2010, J/A+A/524/A64; Baumgartner et al.
2013, J/ApJS/207/19).
Note (3): Flag as follows:
0 = Radio-quiet object;
1 = Radio-loud object;
? = Unknown classification.
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Ref [1/209] Reference number
7- 44 A38 --- Aut Author's name(s)
48- 66 A19 --- Bibcode Bibcode
70- 83 A14 --- Com Comment on reference
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History:
From electronic version of the journal
References:
Asmus et al. Paper I. 2014MNRAS.439.1648A 2014MNRAS.439.1648A Cat. J/MNRAS/439/1648
Asmus et al. Paper III. 2016ApJ...822..109A 2016ApJ...822..109A Cat. J/ApJ/822/109
Isbell et al. Paper IV. 2021ApJ...910..104I 2021ApJ...910..104I Cat. J/ApJ/910/104
(End) Tiphaine Pouvreau [CDS] 02-Jan-2018