Chemical abundances in H II regions of the Magellanic Clouds · Gisela Domínguez-Guzmán October...

Chemical abundances in H II regions of the Magellanic Clouds

Gisela Domínguez-Guzmán Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE)

Tonantzintla, Puebla, Mexico [email protected]

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

1


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:

2


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

3


Physical conditions

Temperature diagnostics:

Density diagnostics:

The calculations were obtained using Pyneb (Luridiana et al. 2015). The uncertainties were obtained through Monte Carlo simulations.

4

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


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


Delgado-Inglada et al. (2011)

The study of the iron depletion factor in H II regions and PNe.


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


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


≠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

10


O N Cl S

Ne

O+

N+ Cl+ S+

Ne+

O++

N++ Cl++

S++ Ne++

eV 10 20 30 40 50 60

Ionization potential

11


≠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

)



≠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


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

)


14

LMC SMC MW EG


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


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:

Chemical abundances in H II regions of the Magellanic Clouds · Gisela Domínguez-Guzmán October...

Documents

Transcript of Chemical abundances in H II regions of the Magellanic Clouds · Gisela Domínguez-Guzmán October...