J/A+A/666/A115 HII-CHI-Mistry-IR for AGN. Abundances (Perez-Diaz+, 2022)
Measuring chemical abundances in AGN from infrared nebular lines:
HII-CHI-Mistry-IR for AGN.
Perez-Diaz B., Perez-Montero E., Fernandez-Ontiveros J.A., Vilchez J.M.
<Astron. Astrophys. 666, A115 (2022)>
=2022A&A...666A.115P 2022A&A...666A.115P (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Abundances ; Infrared sources ; Optical
Keywords: galaxies: abundances - galaxies: active - galaxies: ISM -
galaxies: nuclei - infrared: ISM
Abstract:
Future and on-going infrared and radio observatories such as JWST,
METIS or ALMA will increase the amount of rest-frame IR spectroscopic
data for galaxies by several orders of magnitude. While studies of the
chemical composition of the ISM based on optical observations have
been widely spread over decades for SFG and, more recently, for AGN,
similar studies need to be performed using IR data. This regime can be
especially useful in the case of AGN given that it is less affected by
temperature and dust extinction, traces higher ionic species and can
also provide robust estimations of the chemical abundance ratio N/O.
We present a new tool based on a bayesian-like methodology
(HII-CHI-Mistry-IR) to estimate chemical abundances from IR emission
lines in AGN. We use a sample of 58 AGN with IR spectroscopic data
retrieved from the literature, composed by 43 Seyferts, 8 ULIRGs, 4
LIRGs and 3 LINERs, to probe the validity of our method. The
estimations of the chemical abundances based on IR lines in our sample
are later compared with the corresponding abundances derived from the
optical emission lines in the same objects. HII-CHI-Mistry-IR takes
advantage of photoionization models, characterized by the chemical
abundance ratios O/H and N/O and the ionization parameter U, to
compare their predicted emission- line fluxes with a set of observed
values. Instead of matching single emission lines, the code uses some
specific emission-line ratios sensitive to the above free parameters.
We report mainly solar and also subsolar abundances for O/H in the
nuclear region for our sample of AGN, whereas N/O clusters around
solar values. We find a discrepancy between the chemical abundances
derived from IR and optical emission lines, being the latter higher
than the former. This discrepancy, also reported by previous studies
of the composition of the ISM in AGN from IR observations, is
independent from the gas density or the incident radiation field to
the gas, and it is likely associated with dust obscuration and/or
temperature stratification within the gas nebula.
Description:
The final sample thus consists of 17 Seyfert 1 nuclei (Sy1), 14
Seyfert nuclei with hidden broad lines in the polarized spectrum
(Sy1h), 12 Seyfert 2 nuclei (Sy2), three LINERs, four LIRGs and eight
ULIRGs.
Table A1: List of IR fluxes for our sample of AGN.
Table A2: Chemical abundances estimated from HCm-IR, using the grid of
AGN models for alpha(OX)=-0.8 and the stopping criteria of 2% of
free electrons.
Table A3: List of optical fluxes for our sample of AGN.
Table A4: Chemical abundances estimated from optical emission lines.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 330 58 IR emission line fluxes for the sample of
AGN and their references
tablea2.dat 50 58 Chemical abundances estimated from IR
emission lines
tablea3.dat 206 58 Optical emission line fluxes for the sample of
AGN and their references
tablea4.dat 71 58 Chemical abundances estimated from optical
emission lines
refs.dat 73 76 References
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Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- ID Name or identificator of the object
16- 17 I2 h RAh Right ascension (J2000.0)
19- 20 I2 min RAm Right ascension (J2000.0)
22- 28 F7.4 s RAs Right ascension (J2000.0)
30 A1 --- DE- Declination sign (J2000.0)
31- 32 I2 deg DEd Declination (J2000.0)
34- 35 I2 arcmin DEm Declination (J2000.0)
37- 43 F7.4 arcsec DEs Declination (J2000.0)
45- 53 F9.6 --- z Redshift
55- 59 A5 --- Type Spectral type (G1)
61- 66 F6.2 10-17W/m2 HI4m [-1.68/21.8]? Brackett alpha line flux
(in 10-14erg/s/cm2)
68- 72 F5.2 10-17W/m2 e_HI4m [0.11/5.0]? Brackett alpha flux uncertainty
(in 10-14erg/s/cm2)
74- 77 I4 10-17W/m2 HI7m ? Pfund alpha line flux
(in 10-14erg/s/cm2)
79- 82 I4 10-17W/m2 e_HI7m ? Pfund alpha flux uncertainty
(in 10-14erg/s/cm2)
84- 90 F7.2 10-17W/m2 SIV10m [-2.83/536.1]? [SIV] at 10.5 microns line
flux (in 10-14erg/s/cm2)
92- 97 F6.2 10-17W/m2 e_SIV10m [0.11/53.2]? [SIV] at 10.5 microns flux
uncertainty (in 10-14erg/s/cm2)
99-103 F5.2 10-17W/m2 HI12m [-0.66/6.81]? Humphreys alpha line flux
(in 10-14erg/s/cm2)
105-109 F5.2 10-17W/m2 e_HI12m [0.06/1.53]? Humphreys alpha flux
uncertainty (in 10-14erg/s/cm2)
111-117 F7.2 10-17W/m2 NeII12m [1.35/698.4]? [NeII] at 12.8 microns line
flux (in 10-14erg/s/cm2)
119-124 F6.2 10-17W/m2 e_NeII12m [0.09/67.5]? [NeII] at 12.8 microns flux
uncertainty (in 10-14erg/s/cm2)
126-132 F7.2 10-17W/m2 NeV14m [-3.0/899.0]? [NeV] at 14.3 microns line
flux (in 10-14erg/s/cm2)
134-139 F6.2 10-17W/m2 e_NeV14m [0.05/22.9]? [NeV] at 14.3 microns flux
uncertainty (in 10-14erg/s/cm2)
141-148 F8.2 10-17W/m2 NeIII15m [1.27/1371.0]? [NeIII] at 15.6 microns line
flux (in 10-14erg/s/cm2)
150-155 F6.2 10-17W/m2 e_NeIII15m [0.04/29.9]? [NeIII] at 15.6 microns flux
uncertainty (in 10-14erg/s/cm2)
157-163 F7.2 10-17W/m2 SIII18m [-15.0/240.6]? [SIII] at 18 microns line
flux (in 10-14erg/s/cm2)
165-170 F6.2 10-17W/m2 e_SIII18m [0.03/26.2]? [SIII] at 18 microns flux
uncertainty (in 10-14erg/s/cm2)
172-178 F7.2 10-17W/m2 NeV24m [-50.9/816.0]? [NeV] at 24 microns line
flux (in 10-14erg/s/cm2)
180-185 F6.2 10-17W/m2 e_NeV24m [0.08/58.8]? [NeV] at 24 microns flux
uncertainty (in 10-14erg/s/cm2)
187-194 F8.2 10-17W/m2 OIV26m [-9.5/2030.0]? [OIV] at 26 microns line
flux (in 10-14erg/s/cm2)
196-203 F8.2 10-17W/m2 e_OIV26m [-9.5/2030.0]? [OIV] at 26 microns flux
uncertainty (in 10-14erg/s/cm2)
205-211 F7.2 10-17W/m2 SIII33m [-13.0/848.02]? [SIII] at 33 microns line
flux (in 10-14erg/s/cm2)
213-219 F7.2 10-17W/m2 e_SIII33m [0.08/102.0]? [SIII] at 33 microns flux
uncertainty (in 10-14erg/s/cm2)
221-228 F8.2 10-17W/m2 OIII52m [-461.77/1514.0]? [OIII] at 52 microns line
flux (in 10-14erg/s/cm2)
230-236 F7.2 10-17W/m2 e_OIII52m [1.21/201.0]? [OIII] at 52 microns flux
uncertainty (in 10-14erg/s/cm2)
238-244 F7.2 10-17W/m2 NIII57m [-25.99/637.37]? [NIII] at 57 microns line
flux (in 10-14erg/s/cm2)
246-251 F6.2 10-17W/m2 e_NIII57m [0.37/59.0]? [NIII] at 57 microns flux
uncertainty (in 10-14erg/s/cm2)
253-260 F8.2 10-17W/m2 OIII88m [-2.04/1577.0]? [OIII] at 88 microns line
flux (in 10-14erg/s/cm2)
262-267 F6.2 10-17W/m2 e_OIII88m [0.26/65.0]? [OIII] at 88 microns flux
uncertainty (in 10-14erg/s/cm2)
269-275 F7.2 10-17W/m2 NII122m [-19.0/459.34]? [NII] at 122 microns line
flux (in 10-14erg/s/cm2)
277-282 F6.2 10-17W/m2 e_NII122m [0.1/17.37]? [NII] at 122 microns flux
uncertainty (in 10-14erg/s/cm2)
284-290 F7.2 10-17W/m2 NII205m [0.49/186.65]? [NII] at 205 microns line
flux (in 10-14erg/s/cm2)
292-296 F5.2 10-17W/m2 e_NII205m [0.1/6.83]? [NII] at 205 microns flux
uncertainty (in 10-14erg/s/cm2)
298-330 A33 --- Refs References for IR emission lines,
in refs.dat file
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- ID Name or identificator of the object
16- 20 F5.2 --- 12+log(O/H)ir [7.66/8.52]? IR-based oxygen abundance
12+log(O/H)
22- 26 F5.2 --- e_12+log(O/H)ir [0.22/0.43]? IR-based oxygen abundance
12+log(O/H) error
28- 32 F5.2 --- 12+log(N/O)ir [-1.11/-0.22]? IR-based nitrogen-to-oxygen
abundance ratio log(N/O)
34- 38 F5.2 --- e_12+log(N/O)ir [0.11/0.35]? IR-based nitrogen-to-oxygen
abundance ratio log(N/O) error
40- 44 F5.2 --- logUir [-3.6/-1.0]? IR-based ionization parameter
log(U)
46- 50 F5.2 --- e_logUir [0.07/0.49]? IR-based ionization parameter
log(U) error
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- ID Name or identificator of the object
16- 17 I2 h RAh Right ascension (J2000.0)
19- 20 I2 min RAm Right ascension (J2000.0)
22- 28 F7.4 s RAs Right ascension (J2000.0)
30 A1 --- DE- Declination sign (J2000.0)
31- 32 I2 deg DEd Declination (J2000.0)
34- 35 I2 arcmin DEm Declination (J2000.0)
37- 43 F7.4 arcsec DEs Declination (J2000.0)
45- 53 F9.6 --- z Redshift
55- 59 A5 --- Type Spectral type (G1)
61- 67 F7.3 --- OII3727 [0.09/45.9]? Sum of the relative fluxes
of emission lines [OII] at 3726Å and
[OII] at 3729Å referred to Hbeta flux
69- 75 F7.3 --- e_OII3727 [0.02/12.48]? Sum of the relative flux
errors of emission lines [OII] at
3726Å and [OII] at 3729Å referred
to Hbeta flux
77- 82 F6.3 --- NeIII3868 [0.05/5.77]? Relative flux of emission
lines [NeIII] at 3868Å referred to
Hbeta flux
84- 89 F6.3 --- e_NeIII3868 [0.01/6.13]? Relative flux error of
emission lines [NeIII] at 3868Å
referred to Hbeta flux
91- 96 F6.3 --- OIII4363 [0.05/0.69]? Relative flux of emission
lines [OIII] at 4363Å referred to
Hbeta flux
98-103 F6.3 --- e_OIII4363 [0.01/0.16]? Relative flux error of
emission lines [OIII] at 4363Å
referred to Hbeta flux
105-110 F6.3 --- OIII4959 [0.08/9.9]? Relative flux of emission
lines [OIII] at 4959Å referred to
Hbeta flux
112-117 F6.3 --- e_OIII4959 [0.0/3.17]? Relative flux error of
emission lines [OIII] at 4959Å
referred to Hbeta flux
119-125 F7.3 --- OIII5007 [0.08/29.62]? Relative flux of emission
lines [OIII] at 5007Å referred to
Hbeta flux
127-132 F6.3 --- e_OIII5007 [0.0/8.27]? Relative flux error of
emission lines [OIII] at 5007Å
referred to Hbeta flux
134-139 F6.3 --- NII6584 [0.11/9.8]? Relative flux of emission
lines [NII] at 6584Å referred to
Hbeta flux
141-146 F6.3 --- e_NII6584 [0.01/3.86]? Relative flux error of
emission lines [NII] at 6584Å
referred to Hbeta flux
148-153 F6.3 --- SII6725 [0.02/4.5]? Sum of the relative fluxes of
emission lines [SII] at 6717Å and
[SII] at 6731Å referred to Hbeta flux
155-160 F6.3 --- e_SII6725 [0.0/1.1]? Sum of the relative flux
errors of emission lines [SII] at
6717Å and [SII] at 6731Å
referred to Hbeta flux
162-174 F13.7 10-17W/m2 FHbeta [0.08/16767.73] Balmer line Hbeta flux
(in 10-14erg/s/cm2)
176-188 F13.7 10-147W/m2 e_FHbeta [0.06/1678.98]? Balmer line Hbeta flux
error (in 10-14erg/s/cm2)
190-206 A17 --- Refs References for optical emission lines,
in refs.dat files
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Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- ID Name or identificator of the object
16- 19 F4.2 --- 12+log(O/H)opt [7.58/8.84] Opt-based oxygen abundance
12+log(O/H)
21- 24 F4.2 --- e_12+log(O/H)opt [0.07/0.53] Opt-based oxygen abundance
12+log(O/H) error
26- 30 F5.2 --- 12+log(N/O)opt [-1.28/-0.17]? Opt-based
nitrogen-to-oxygen abundance ratio
log(N/O)
32- 36 F5.2 --- e_12+log(N/O)opt [0.09/0.42]? Opt-based
nitrogen-to-oxygen abundance ratio
log(N/O) error
38- 42 F5.2 --- logUopt [-3.89/-0.81] Opt-based ionization
parameter log(U)
44- 47 F4.2 --- e_logUopt [0.01/0.73] Opt-based ionization
parameter log(U) error
49- 53 F5.2 --- 12+log(O/H)FM20 [7.57/8.73]? Oxygen abundance
12+log(O/H) obtained after applying the
calibration from Flury & Morgan
(2020MNRAS.496.2191F 2020MNRAS.496.2191F)
55- 59 F5.2 --- e_12+log(O/H)FM20 ? Oxygen abundance 12+log(O/H) error
obtained after applying the calibration
from Flury & Morgan
(2020MNRAS.496.2191F 2020MNRAS.496.2191F)
61- 65 F5.2 --- 12+log(O/H)Ca20 [8.27/8.98]? Oxygen abundance
12+log(O/H) obtained after applying the
calibration from Carvalho et al.
(2020MNRAS.492.5675C 2020MNRAS.492.5675C)
67- 71 F5.2 --- e_12+log(O/H)Ca20 [0.01/0.5]? Oxygen abundance 12+log(O/H)
error obtained after applying the
calibration from Carvalho et al.
(2020MNRAS.492.5675C 2020MNRAS.492.5675C)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Ref Reference code
7- 25 A19 --- BibCode BibCode
27- 52 A26 --- Aut Author's name
54- 73 A20 --- Com Comments
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Global notes:
Note (G1): Spectral types as follows:
S1h = Seyfert type 2 with detected polarized optical broad lines
S1.5 = Seyfert type 1.5
S1.8 = Seyfert type 1.8
S1.9 = Seyfert type 1.9
S2 = Seyfert type 2
LIN = Low-ionization nuclear emission-line region (LINER)
LIRG = Luminous infrared Galaxy
ULIRG = Ultraluminous infrared galaxy
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Acknowledgements:
Borja Perez Diaz, bperez(at)iaa.es or borjapd96(at)gmail.com
(End) Patricia Vannier [CDS] 19-Jul-2022