J/MNRAS/521/1556 HII-CHI-Mistry-UV for AGN. Abundances (Perez-Montero+, 2023)
Assessing model-based carbon and oxygen abundance derivation from
ultraviolet emission lines in AGNs.
Perez-Montero E., Amorin R., Perez-Diaz B., Garcia-Benito R.
<Mon. Not. R. Astron. Soc. 521, 1556 (2023)>
=2023MNRAS.521.1556P 2023MNRAS.521.1556P (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Abundances ; Ultraviolet
Keywords: galaxies: active - galaxies: abundances - galaxies: evolution -
galaxies: ISM - galaxies: nuclei - galaxies: Seyfert
Abstract:
We present an adapted version of the code HII-CHI-mistry-UV
(Perez-Montero & Amorin, 2017MNRAS.467.1287P 2017MNRAS.467.1287P) to derive chemical
abundances from emission lines in the ultraviolet, for use in narrow
line regions (NLR) of Active Galactic Nuclei (AGN). We evaluate
different ultraviolet emission line ratios and how different
assumptions about the models, including the presence of dust grains,
the shape of the incident spectral energy distribution, or the
thickness of the gas envelope around the central source, may affect
the final estimates as a function of the set of emission lines used.
We compare our results with other published recipes for deriving
abundances using the same emission lines and show that deriving the
carbon-to-oxygen abundance ratio using CIII] λ1909Å and
OIII] λ1665Å emission lines is a robust indicator of the
metal content in AGN that is nearly independent of model assumptions,
similar to the case of star-forming regions. Moreover, we show that a
prior determination of C/O allows for a much more precise
determination of the total oxygen abundance using carbon UV lines, as
op- posed to assuming an arbitrary relationship between O/H and C/O,
which can lead to non-negligible discrepancies.
Description:
Table 2: List of UV fluxes for the sample of AGN and references.
Table 3: Chemical abundances estimated from HCm-UV, using the grid of
AGN models for alpha(OX)=-1.2 and the stopping criteria of 98% of
free electrons. Dust-free or grain-included models are selected based
on their C3C4 value.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 257 234 UV emission lines for the sample of AGN and
references
table3.dat 59 234 Chemical abundances estimated from UV emission
lines
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- ID Names or identificators of the objects
21- 25 F5.3 --- z [0.0/6.13] Redshifts
27- 30 A4 --- Type Spectral type of the objects (1)
32- 42 F11.6 10-17W/m2 Lya1216 [0.0/713.0]? Ly-alpha 1216Å line flux
44- 49 E6.1 10-17W/m2 e_Lya1216 [0.0/100.0]? Ly-alpha 1216Å flux
uncertainty
51- 58 E8.2 10-17W/m2 NV1239 [0.0/224.0]? [NV] 1239Å line flux
60- 67 E8.2 10-17W/m2 e_NV1239 [0.0/41.0]? [NV] 1239Å flux uncertainty
69- 78 F10.5 10-17W/m2 CIV1549 [0.0/520.0]? CIV 1549Å line flux
80- 84 E5.1 10-17W/m2 e_CIV1549 [0.0/80.0]? CIV 1549Å flux uncertainty
86- 96 F11.6 10-17W/m2 HeII1640 [0.0/187.0]? HeII 1640Å line flux
98-104 E7.2 10-17W/m2 e_HeII1640 [0.0/29.0]? HeII 1640Å flux uncertainty
106-111 E6.1 10-17W/m2 OIII1665 [0.0/22.0]? [OIII] 1665Å line flux
113-118 E6.1 10-17W/m2 e_OIII1665 [0.0/8.0]? [OIII] 1665Å flux uncertainty
120-130 F11.6 10-17W/m2 CIII1909 [0.0/240.0]? CIII] 1909Å line flux
132-139 E8.2 10-17W/m2 e_CIII1909 [0.0/35.0]? CIII] 1909Å flux uncertainty
141-157 A17 --- Ref References for emission lines (2)
159-257 A99 --- Notes Notes on units or upper limits (3)
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Note (1): Abbreviations for spectral types as follows:
S2 = Seyferts Type-2
Q2 = Type II Quasars
zRG = High-z Radio Galaxies
QRG = Quiet Radio Galaxies
zAGN = High-z AGN
QSO = Quasars
ERQ = Extremely Red Quasars
Note (2): References for line fluxes as follows:
AS88 = Allington-Smith et al., 1988MNRAS.234.1091A 1988MNRAS.234.1091A
BER81 = Bergeron et al., 1981A&A....97...94B 1981A&A....97...94B
BES99 = Best et al., 1999MNRAS.310..223B 1999MNRAS.310..223B
BES00 = Best et al., 2000MNRAS.311....1B 2000MNRAS.311....1B
BOR07 = Bornancini et al., 2007MNRAS.378..551B 2007MNRAS.378..551B
BRE00 = De Breuck et al., 2000A&A...362..519D 2000A&A...362..519D, Cat. J/A+A/362/519
BRE01 = De Breuck et al., 2001AJ....121.1241D 2001AJ....121.1241D
CIM98 = Cimatii et al., 1998ApJ...499L..21C 1998ApJ...499L..21C
DO19 = Dors et al., 2019MNRAS.486.5853D 2019MNRAS.486.5853D
GK95 = Gopal-Krishna et al., 1995&6A...303..705G
KI93 = Kinnet et al., 1993ApJS...86....5K 1993ApJS...86....5K, Cat. III/167
KRA94 = Kraemer et al., 1994ApJ...435..171K 1994ApJ...435..171K
LAC94 = Lacy et al., 1994MNRAS.271..504L 1994MNRAS.271..504L
LAC99 = Lacy et al., 1999MNRAS.308.1096L 1999MNRAS.308.1096L
LIL88 = Lilly, 1988ApJ...333..161L 1988ApJ...333..161L
LIL07 = Lilly et al., 2007ApJS..172...70L 2007ApJS..172...70L, Cat. J/ApJS/172/70
LIN22 = Lin et al., 2022MNRAS.509..489L 2022MNRAS.509..489L
MAL83 = Malkan & Oke, 1983ApJ...265...92M 1983ApJ...265...92M
MAT09 = Matsuoka et al., 2009A&A...503..721M 2009A&A...503..721M
MAT18 = Matsuoka et al., 2018A&A...616L...4M 2018A&A...616L...4M
MCC90 = McCarthy et al., 1990AJ....100.1014M 1990AJ....100.1014M
MCC90b = McCarthy et al., 1990ApJ...365..487M 1990ApJ...365..487M
MCC91 = McCarthy, 1991AJ....102..518M 1991AJ....102..518M
MCC91b = MCCarthy et al., 1991AJ....102..522M 1991AJ....102..522M
NA06 = Nagao et al., 2006A&A...447..863N 2006A&A...447..863N
RAW96 = Rawlings et al., 1996Natur.383..502R 1996Natur.383..502R
ROB88 = De Robertis et al., 1988AJ.....95.1371D 1988AJ.....95.1371D
ROT97 = Roettgering et al., 1997A&A...326..505R 1997A&A...326..505R
ONO21 = Onoue et al., 2021ApJ...919...61O 2021ApJ...919...61O
SIM99 = Simpson et al., 1999ApJ...525..659S 1999ApJ...525..659S
SKO04 = Szokoly et al., 2004ApJS..155..271S 2004ApJS..155..271S, Cat. J/ApJS/155/271
SNI86 = Snijders et al., 1986MNRAS.222..549S 1986MNRAS.222..549S
SPI95 = Spinrad et al., 1995ApJ...438L..51S 1995ApJ...438L..51S
STE99 = Stern et al., 1999AJ....117.1122S 1999AJ....117.1122S
STE01 = Stern et al., 2002ApJ...568...71S 2002ApJ...568...71S
TAN22 = Tang et al., 2022MNRAS.509.3102T 2022MNRAS.509.3102T
THU84 = Thuan, 1984ApJ...281..126T 1984ApJ...281..126T
VM99 = Villar-Martin et al., 1999A&A...351...47V 1999A&A...351...47V
VM20 = Villar Martin et al., 2020A&A...634A.116V 2020A&A...634A.116V
WAD99 = Waddington et al., 1999ApJ...526L..77W 1999ApJ...526L..77W
Note (3): Comments on the measurements:
- Some of the emission line fluxes are upper limits
- Units for QSO S82-20 are: 1043erg/s (luminosity)
- Emission line ratios for the sample of ERQ are referred to CIV1549 = 1
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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- 19 A19 --- ID Names or identificators of the objects
21- 25 F5.2 --- OH [7.53/9.09]? UV-based oxygen abundance
12+log(O/H)
27- 31 F5.2 --- e_OH [0.01/0.68]? UV-based oxygen abundance
12+log(O/H) error
33- 37 F5.2 --- CO [-0.87/0.24]? UV-based carbon-to-oxygen
abundance ratio log(C/O)
39- 43 F5.2 --- e_CO [0.18/0.52]? UV-based carbon-to-oxygen
abundance ratio log(C/O) error
45- 49 F5.2 --- logU [-2.64/-0.56]? UV-based ionization parameter
log(U)
51- 55 F5.2 --- e_logU [0.01/0.65]? UV-based ionization parameter
log(U) error
57- 59 A3 --- Grains [Yes No] The models include grains ("Yes")
or are dust- free ("No")
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Acknowledgements:
Borja Perez Diaz, bperez(at)iaa.es or borjapd96(at)gmail.com
(End) Patricia Vannier [CDS] 07-Mar-2023