J/A+A/692/A209 A CIGALE module for low-luminosity AGN (Lopez+, 2024)
A CIGALE module tailored (not only) for low-luminosity active galactic nuclei.
Lopez I.E., Yang G., Mountrichas G., Brusa M., Alexander D.M., Baldi R.D.,
Bertola E., Bonoli S., Comastri A., Shankar F., Acharya N.,
Alonso Tetilla A.V., Lapi A., Laloux B., Lopez Lopez X., Munoz Rodriguez I.,
Musiimenta B., Osorio Clavijo N., Sala L., Sengupta D.
<Astron. Astrophys. 692, A209 (2024)>
=2024A&A...692A.209L 2024A&A...692A.209L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; X-ray sources ; Radio sources
Keywords: techniques: photometric - galaxies: active - galaxies: nuclei -
galaxies: Seyfert
Abstract:
The spectral energy distribution (SED) of low-luminosity active
galactic nuclei (LLAGN) presents unique challenges as the emission
from these objects is comparable to the radiation from their host
galaxy and the accretion physics involved is particularly complex.
This study introduces a novel CIGALE module specifically designed to
address these challenges. The module combines the empirical
LX-L12um relationship with physically motivated accretion models,
such as advection-dominated accretion flows (ADAFs) and truncated
accretion disks, providing a more accurate depiction of LLAGN central
engine emission. A mock analysis of the module revealed good recovery
of true parameters, with only a slight bias toward higher input
values, further validating its reliability.
We tested the module on a sample of 50 X-ray-detected local galaxies,
including low-ionization nuclear emission-line regions (LINERs) and
Seyferts, and demonstrated its capacity to accurately estimate
bolometric luminosities, even in the presence of significant galaxy
contamination. Notably, the previous X-ray module failed to provide
AGN solutions for this sample, stressing the need for a novel
approach. Comparisons with mid-luminosity AGN datasets confirm the
module's robustness and applicability up to L_X<1045erg/s. We also
expanded the X-ray-to-bolometric correction formula, making it
applicable to AGN spanning ten orders of magnitude in luminosity, and
revealing lower kX values for LLAGN than typically assumed.
Additionally, our analysis of the alphaox index, which represents
the slope between UV and X-ray emissions, uncovered trends that differ
from those observed in high-luminosity AGN. Unlike quasars, where
alphaox correlates with lambdaEdd, LLAGN exhibit nearly constant
or weakly correlated alphaox values, suggesting a shift in accretion
physics and photon production mechanisms in low-luminosity regimes.
These results underscore the importance of a multiwavelength approach
in AGN studies and reveal distinct behaviors in LLAGN compared to
quasars. Our findings significantly advance our understanding of LLAGN
and offer a comprehensive framework for future research to complete
the AGN population census.
Description:
This work introduces a novel CIGALE module specifically designed
for the analysis of low-luminosity AGN (LLAGN). By integrating
empirical relationships and physics-based accretion models, this
module improves our understanding of LLAGN through SED fitting,
without relying on standard QSO extrapolation.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 50 49 Key properties of galaxies in the LLAGN sample
table3.dat 91 46 Properties obtained from the SED fitting of
the LLAGN sample
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Galaxy name
9- 15 F7.3 deg RAdeg Right ascension (J2000)
17- 25 F9.5 deg DEdeg Declination (J2000)
27- 34 F8.5 --- z Redshift
36- 40 F5.2 Mpc Dist Distance
42- 48 F7.4 [10-7W] logLum2-10 log X-ray luminosity between 2-10keV
50 I1 --- RefCAT [1/7] Reference (1)
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Note (1): References as follows:
1 = Williams et al. (2022MNRAS.510.4909W 2022MNRAS.510.4909W)
2 = Gonzalez-Martin et al. (2009A&A...506.1107G 2009A&A...506.1107G)
3 = Osorio-Clavijo et al. (2023MNRAS.522.5788O 2023MNRAS.522.5788O)
4 = Yun et al. (2022ApJ...935...12Y 2022ApJ...935...12Y)
5 = Kammoun et al. (2020ApJ...901..161K 2020ApJ...901..161K)
6 = Cappi et al. (2006A&A...446..459C 2006A&A...446..459C)
7 = Masini et al. (2022A&A...663A..87M 2022A&A...663A..87M)
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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- 7 A7 --- Name Galaxy Name
9- 14 F6.3 [10-7W] logLACR log Intrinsic AGN accretion luminosity
16- 20 F5.3 [10-7W] e_logLACR Error on log Intrinsic AGN accretion
luminosity
22- 26 F5.3 --- lambdaEdd Eddington rate
28- 33 F6.3 [10-7W] logLBol log Bolometric AGN luminosity
35- 39 F5.3 [10-7W] e_logLBol Error log Bolometric AGN luminosity
41- 46 F6.3 [10-7W] LXcigale modelled X-ray AGN Luminosity
between 2-10keV
48- 52 F5.3 [10-7W] e_LXcigale Error on modelled X-ray AGN Luminosity
between 2-10keV
54- 59 F6.3 [10-7W/Hz] logL2500 Monocromatic AGN luminosity measure
at 2500Å
61- 65 F5.3 [10-7W/Hz] e_logL2500 Error on Monocromatic AGN luminosity
measure at 2500Å
67- 72 F6.3 [10-7W/Hz] logL2kev Monocromatic AGN luminosity measure
at 2keV
74- 78 F5.3 [10-7W/Hz] e_logL2kev Error on Monocromatic AGN luminosity
measure at 2keV
80- 85 F6.3 --- alphaox Slope between the X-ray emission and UV
87- 91 F5.3 --- e_alphaox Error on slope between the X-ray emission
and UV
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Acknowledgements:
Ivan Lopez, ivan.lopez(at)inaf.it
(End) Patricia Vannier [CDS] 08-Dec-2024