J/MNRAS/469/3125 Abundance ratio in gamma-ray burst (Contini, 2017)
N/O abundance ratios in gamma-ray burst and supernova host galaxies at z < 4.
Comparison with AGN, starburst and H II regions.
Contini M.
<Mon. Not. R. Astron. Soc., 469, 3125-3140 (2017)>
=2017MNRAS.469.3125C 2017MNRAS.469.3125C (SIMBAD/NED BibCode)
ADC_Keywords: GRB ; Supernovae ; Abundances
Keywords: radiation mechanisms: general - shock waves - ISM: abundances -
galaxies: high redshift
Abstract:
The distribution of the N/O element abundance ratios calculated by the
detailed modelling of different galaxy spectra at z<4 is investigated.
Supernova (SN) and long gamma-ray-burst (LGRB) host galaxies cover
different redshift domains. N/O ratios in SN hosts increase due to
secondary N production towards low z (0.01) accompanying the growing
trend of active galaxies [active galactic nucleus (AGN),
low-ionization nuclear emission-line region (LINER)]. N/O ratios in
LGRB hosts decrease rapidly between z>1 and z∼0.1 following the N/H
trend and reach the characteristic N/O ratios calculated for the H II
regions in local and nearby galaxies. The few short-period
gamma-ray-burst (SGRB) hosts included in the galaxy sample show
N/H≤0.04 solar and O/H solar. They seem to continue the low bound N/H
trend of SN hosts at z<0.3. The distribution of N/O as a function of
metallicity for SN and LGRB hosts is compared with star chemical
evolution models. The results show that several LGRB hosts can be
explained by star multibursting models when 12+log(O/H)<8.5, while
some objects follow the trend of continuous star formation models. N/O
in SN hosts at log(O/H)+12<8.5 are not well explained by stellar
chemical evolution models calculated for starburst galaxies. At
12+log(O/H)>8.5 many different objects are nested close to O/H solar
with N/O ranging between the maximum corresponding to starburst
galaxies and AGN and the minimum corresponding to HII regions and
SGRB.
Description:
The distribution of the N/O abundance ratios over the full redshift
range is calculated by the detailed modelling of line spectra in order
to compare the characteristic metallicities in various galaxy types,
in particular SN and LGRB hosts at z≤3.5 (age≥1.823Gyr).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 56 32 Modelling line ratios to Hβ=1 from the CALIFA
HII regions (Marino et al., 2013,
Cat. J/A+A/559/A114)
table2.dat 51 16 Models used to reproduce the spectra presented
in Table 1
table3.dat 93 102 Modelling line ratios to Hβ=1 from the
HII regions sample of
Berg et al. (2012ApJ...754...98B 2012ApJ...754...98B)
table4.dat 57 51 Models used to reproduce the spectra presented
in Table 3
table5.dat 51 56 Modelling line ratios to Hβ=1 of AGN
spectra at z≤0.1
(Dors et al. 2017MNRAS.468L.113D 2017MNRAS.468L.113D)
table6.dat 50 28 Models used to reproduce the spectra presented
in Table 5
table7.dat 63 54 Modelling line ratios to Hβ=1 of Type I SN
host spectra at z≤0.03 (Gallagher et al.,
2005ApJ...634..210G 2005ApJ...634..210G)
table8.dat 52 27 Models used to reproduce the spectra presented
in Table 7
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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- 17 A17 --- Name HII region or model name
20- 26 F7.5 --- z ? Redshift
28- 31 F4.2 --- [OII]3727+ Line ratio [OII]3727/Hβ
33- 37 F5.3 --- [OIII]4363 Line ratio [OII]4363/Hβ
39- 43 F5.3 --- [OIII]5007 Line ratio [OII]5007/Hβ
44- 48 F5.3 --- [NII]6583 Line ratio [NII]6583/Hβ
50- 56 F7.2 10-19W/m2 FHb ? Hβ flux (in 10-16erg/cm2/s)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Model Model name
5 A1 --- n_Model [2] 2: calculated by inflow
7- 9 I3 km/s Vs Shock velocity
11- 13 I3 cm-3 n0 Atomic pre-shock density
15- 19 F5.3 10+18cm D Geometrical thickness
22- 25 F4.2 10-4 N/H N/H relative abundance
28- 31 F4.2 10-4 O/H O/H relative abundance
32- 35 F4.1 10+4K T* Effective temperature
38- 43 F6.4 --- U Ionisation parameter
46- 51 F6.4 mW/m2 FHb Hβ flux, calculated at the nebula
(in erg/cm2/s)
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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- 13 A13 --- Name HII region or model name
15- 22 F8.6 --- z ? Redshift
24- 27 F4.2 --- [OII]3727+ Line ratio[OII]3727/Hβ
30- 33 F4.2 --- [NeIII]3869+ ? Line ratio [NeIII]3869/Hβ
36- 39 F4.2 --- Hg Line ratio Hγ(4340)/Hβ
42- 46 F5.3 --- [OIII]4363 ? Line ratio [OIII]4363/Hβ
49- 52 F4.2 --- [OIII]5007+ Line ratio [OIII]5007/Hβ
55- 59 F5.3 --- HeI ? Line ratio HeI5876/Hβ
61- 65 F5.3 --- [SIII]6312 ? Line ratio [SIII]6312/Hβ
67- 71 F5.3 --- [OI]6300+ ? Line ratio [OI]6300/Hβ
73- 77 F5.3 --- [NII]6548+ ? Line ratio [NII]6548/Hβ
79- 82 F4.2 --- Ha Line ratio Hα(6563)/Hβ
85- 88 F4.2 --- [SII]6717 ? Line ratio [SII]6717/Hβ
90- 93 F4.2 --- [SII]6731 ? Line ratio [SII]6731/Hβ
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- Model Model name
7- 9 I3 km/s Vs Shock velocity
11- 13 I3 cm-3 n0 Atomic pre-shock density
15- 19 F5.3 10+18cm D Geometrical thickness
21- 24 F4.2 10-4 N/H N/H relative abundance
26- 28 F3.1 10-4 O/H O/H relative abundance
30- 32 F3.1 10-4 Ne/H Ne/H relative abundance
34- 38 F5.3 10-4 S/H S/H relative abundance
40- 42 F3.1 10+3K T* Effective temperature
44- 49 F6.4 --- U Ionisation parameter
52- 57 F6.4 mW/m2 FHb Hβ flux, calculated at the nebula
(in erg/cm2/s)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name AGN or model name
11- 17 F7.5 --- z ? Redshift
19- 22 F4.2 --- [OII]3727+ Line ratio [OII]3727/Hβ
27- 31 F5.2 --- [OIII]5007+ Line ratio [OIII]5007/Hβ
35- 38 F4.2 --- [NII]6583+ Line ratio [NII]6583/Hβ
43- 46 F4.2 --- [SII]6719+ Line ratio [SII]6719/Hβ
51 I1 --- Ref [1/4]? References (1)
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Note (1): References as follows:
1 = Kraemer et al. (1994ApJ...435..171K 1994ApJ...435..171K)
2 = Koski (1978ApJ...223...56K 1978ApJ...223...56K)
3 = Cohen (1983ApJ...273..489C 1983ApJ...273..489C)
4 = Dopita et al. (2015, Cat. J/ApJS/217/12)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Model Model name
7- 9 I3 km/s Vs Shock velocity
11- 13 I3 cm-3 n0 Atomic pre-shock density
15- 19 F5.2 10+10ph/cm2/s/eV F Flux at the Lyman limit
21- 24 F4.1 10+17cm D Geometrical thickness
27- 30 F4.2 10-4 N/H N/H relative abundance
33- 35 F3.1 10-4 O/H O/H relative abundance
38- 42 F5.3 10-4 S/H S/H relative abundance
45- 50 F6.4 mW/m2 FHb Bβ flux, calculated at the nebula
(in erg/cm2/s)
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Host galaxy or model name
10- 15 A6 --- SN Supernova name
18- 23 F6.4 --- z ? Redshift
25- 29 F5.2 --- [OII]3727+ Line ratio [OII]3727/Hβ
32- 35 F4.2 --- [OIII]5007+ Line ratio [OII]5007/Hβ
38- 42 F5.3 --- [OI]6300 Line ratio [OI]6300/Hβ
44- 47 F4.2 --- [NII]6548+ Line ratio [NII]6548/Hβ
49- 51 F3.1 --- Ha Line ratio Hα(6563)/Hβ
54- 57 F4.2 --- [SII]6717 Line ratio [SII]6717/Hβ
60- 63 F4.2 --- [SII]6731 Line ratio [SII]6731/Hβ
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- Model Model name
6- 8 I3 km/s Vs Shock velocity
10- 12 I3 cm-3 n0 Atomic pre-shock density
15- 17 F3.1 10+18cm D Geometrical thickness
20- 23 F4.2 10-4 N/H N/H relative abundance
26- 28 F3.1 10-4 O/H O/H relative abundance
31- 35 F5.3 10-4 S/H S/H relative abundance
38- 41 F4.1 10+4K T* Effective temperature
44- 46 F3.1 10-3 U Ionisation parameter
48- 52 F5.2 10-6W/m2 FHb Hβ flux, calculated at the nebula
(in 10-3erg/cm2/s)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Apr-2020