Post on 29-Sep-2020
Chemical abundances in H II regions of the Magellanic Clouds
Gisela Domínguez-Guzmán Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE)
Tonantzintla, Puebla, Mexico gisedogu@inaoep.mx
Mónica Rodríguez (INAOE) César Esteban (IAC) Jorge García-Rojas (IAC)
October 23-27, 2017, Puebla, Mexico.
The cosmic feast of the elements. A conference to celebrate the work of Grażyna Stasińska.
Jonnathan Reyes-Pérez (INAOE)
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
Introduction
The Magellanic Clouds (MCs) are ideal laboratories to study H II regions, some of them with lower metallicities than those in the Milky Way. They are relatively close and it is possible to obtain high quality spectra.
Large Magellanic Cloud (LMC)
Small Magellanic Cloud (SMC)
Image credit: Aladin Sky Atlas
Image credit: John P. Gleason
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
Observations
The observations were taken with the UVES/VTL in Chile:
LMC: IC 2111 and NGC 1714 LMC: N11B, N44C SMC: N66A, N81, N88A and N90
• Spectral range: 3100 – 10400 Å • Resolution: Δλ ~ λ/11600 • The atmospheric dispersion corrector was used • Airmass range: 1.35 – 1.88 • Exposure time: 900 – 8000 s
2003 March 2013 November
Standard settings:
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
The best and the worst spectra for SMC-N81 and SMC-N90, respectively.
5753 5754 5755 5756 5757
⁄ (A)≠2
0
2
4
6
8
10
12
F ⁄(◊
10≠
15er
gs≠
1cm
≠2
A≠1 )
[N II] ⁄5755
SMC-N81SMC-N90
4361 4362 4363 4364 4365
⁄ (A)
0
1
2
3
4
5
F ⁄(◊
10≠
13er
gs≠
1cm
≠2
A≠1 )
[O III] ⁄4363
SMC-N81SMC-N90 ◊ 10
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
Physical conditions
Temperature diagnostics:
Density diagnostics:
The calculations were obtained using Pyneb (Luridiana et al. 2015). The uncertainties were obtained through Monte Carlo simulations.
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 5
O+
O2+
N+ S+
S2+ Cl+
Cl2+
Cl3+
Ne2+
Ar2+
Ar3+
Fe2+
Fe3+ (1 object)
He+
He2+ (1 object)
T [N II]
T [O III]
O++
H+
Ne++
O+
H+
N+
e
e
Ionic abundances
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 6
Nitrogen
Iron
Oxygen, sulfur, chlorine, argon, neon
N
O=
N+
O+as suggested by Delgado-Inglada et al. (2015)
ICFs by Rodríguez & Rubin (2005)
ICFs by Delgado-Inglada et al. (2014)
Total abundances
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 7
Delgado-Inglada et al. (2011)
The study of the iron depletion factor in H II regions and PNe.
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 7
Delgado-Inglada et al. (2011)
The study of the iron depletion factor in H II regions and PNe.
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 8
Results
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠3.7
≠3.5
≠3.3
≠3.1
≠2.9
≠2.7
≠2.5
≠2.3
≠2.1
≠1.9
≠1.7lo
g(Fe
/O)
≠2.25
≠2.00
≠1.75
≠1.50
≠1.25
≠1.00
≠0.75
≠0.50
log(
Fe/O
)-lo
g(Fe
/O) §
LMC SMC MW EG
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠1.8
≠1.6
≠1.4
≠1.2
≠1.0
≠0.8
≠0.6lo
g(N/
O)
9
LMC SMC MW EG
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠4.0
≠3.8
≠3.6
≠3.4
≠3.2
≠3.0lo
g(Cl
/O)
Te([O III]) for [Cl III]
LMC SMC MW EG
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
O N Cl S
Ne
O+
N+ Cl+ S+
Ne+
O++
N++ Cl++
S++ Ne++
eV 10 20 30 40 50 60
Ionization potential
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Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠4.0
≠3.8
≠3.6
≠3.4
≠3.2
≠3.0
log(
Cl/O
)
Te([N II]) for [Cl III]
12
LMC SMC MW EG
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠4.0
≠3.8
≠3.6
≠3.4
≠3.2
≠3.0
log(
Cl/O
)
Te([O III]) for [Cl III]
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠2.2
≠2.0
≠1.8
≠1.6
≠1.4
≠1.2
log(
S/O
)
Mean of Te([O III]) and Te([N II]) for [S III]
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠0.9
≠0.7
≠0.5
≠0.3
≠0.1
0.1
log(
Ne/O
)
Mean of Te([O III]) and Te([N II]) for [Ne III]
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠0.9
≠0.7
≠0.5
≠0.3
≠0.1
0.1
log(
Ne/O
)
Te([O III]) for [Ne III]
≠1.5 ≠1.0 ≠0.5 0.0 0.5 1.0log(O+/O++)
≠2.2
≠2.0
≠1.8
≠1.6
≠1.4
≠1.2lo
g(S/
O)
Te([O III]) for [S III]
13
LMC SMC MW EG
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠4.0
≠3.8
≠3.6
≠3.4
≠3.2
≠3.0
log(
Cl/O
)
Te([N II]) for [Cl III]
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠4.0
≠3.8
≠3.6
≠3.4
≠3.2
≠3.0
log(
Cl/O
)
Te([O III]) for [Cl III]
14
LMC SMC MW EG
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠0.9
≠0.7
≠0.5
≠0.3
≠0.1
0.1
log(
Ne/O
)
Te([O III]) for [Ne III]
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠0.9
≠0.7
≠0.5
≠0.3
≠0.1
0.1
log(
Ne/O
)
Mean of Te([O III]) and Te([N II]) for [Ne III]
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠2.2
≠2.0
≠1.8
≠1.6
≠1.4
≠1.2
log(
S/O
)
Mean of Te([O III]) and Te([N II]) for [S III]
7.8 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.712 + log(O/H)
≠2.2
≠2.0
≠1.8
≠1.6
≠1.4
≠1.2lo
g(S/
O)
Te([O III]) for [S III]
15
LMC SMC MW EG
Gisela Domínguez-Guzmán October 23-27, 2017, Puebla, Mexico. The cosmic feast of the elements 15
Conclusions
Ø The amounts of iron depletion into dust grains in H II regions of the MCs are similar to those found in Galactic ones.
Ø When we consider the structure of temperature the Cl/O, S/O and Ne/O abundance ratios are constant with metallicity.
We present new determinations of chemical abundances of 8 H II regions in the MCs, 4 in the LMC and 4 in the SMC, using deep echelle spectra taken at the VLT. The main conclusions are: