The VMC survey: VII. Reddening map of the 30 Doradus field and the structure of the cold interstellar medium

B. L. Tatton, J. Th. van Loon, M. -R. Cioni, G. Clementini, J. P. Emerson, L. Girardi, R. de Grijs, M. A. T. Groenewegen, M. Gullieuszik, V. D. Ivanov, M. I. Moretti, V. Ripepi, S. Rubele

Research output: Contribution to journalReview articleResearchpeer-review

Abstract

Context. The details of how galaxies have evolved over cosmological times are imprinted in their star formation history, chemical enrichment and morpho-kinematic structure. Parameters behind these, such as effective temperature and metallicity, can be measured by combining photometric techniques with modelling. However, there are uncertainties with this indirect approach from the ambiguity of colour and magnitude and the effects of interstellar reddening. 

Aims. In this paper we present a detailed reddening map of the central 30 Doradus region of the Large Magellanic Cloud; for both community use and as a test of the methods used for future use on a wider area. The reddening, a measurement of dust extinction, acts as a tracer of the interstellar medium (ISM). 

Methods. Near-infrared (NIR) photometry of the red clump stars is used to measure reddening as their fixed luminosity and intermediate age make extinction the dominant cause of colour and magnitude variance. The star formation history derived previously from these data is used to produce an intrinsic colour to act as a zero point in converting colour to reddening values E(J - Ks) which are subsequently converted to visual extinction AV. Results. Presented is a dust map for the 30 Doradus field in both AV and E(J - Ks). This map samples a region of 1° × 1.°5, containing ∼ 1.5 × 105 red clump stars which probe reddening up to AV ≃ 6 mag. We compare our map with maps from the literature, including optical extinction maps and radio, mid- and far-infrared maps of atomic hydrogen and dust emission. Through estimation of column density we locate molecular clouds. 

Conclusions. This new reddening map shows correlation with equivalent maps in the literature, validating the method of red clump star selection. We make our reddening map available for community use. In terms of ISM the red clump stars appear to be more affected by the cooler dust measured by 70 μm emission because there is stronger correlation between increasing emission and extinction due to red clump stars not being located near hot stars that would heat the dust. The transition from atomic hydrogen to molecular hydrogen occurs between densities of NH ≃ 4 × 1021 cm and NH ≃ 6 × 1021 cm.

LanguageEnglish
Article numberA33
Pages1-26
Number of pages26
JournalAstronomy and Astrophysics
Volume554
DOIs
Publication statusPublished - 2013
Externally publishedYes

Fingerprint

clumps
extinction
dust
stars
color
hydrogen
star formation
cold
histories
interstellar extinction
infrared photometry
hot stars
Magellanic clouds
history
molecular clouds
coolers
ambiguity
metallicity
tracers
near infrared

Keywords

  • Magellanic Clouds
  • Hertzsprung-Russell and C-M diagrams
  • galaxies: structure
  • dust, extinction
  • ISM: structure
  • stars: horizontal-branch

Cite this

Tatton, B. L., van Loon, J. T., Cioni, M. -R., Clementini, G., Emerson, J. P., Girardi, L., ... Rubele, S. (2013). The VMC survey: VII. Reddening map of the 30 Doradus field and the structure of the cold interstellar medium. Astronomy and Astrophysics, 554, 1-26. [A33]. https://doi.org/10.1051/0004-6361/201321209
Tatton, B. L. ; van Loon, J. Th. ; Cioni, M. -R. ; Clementini, G. ; Emerson, J. P. ; Girardi, L. ; de Grijs, R. ; Groenewegen, M. A. T. ; Gullieuszik, M. ; Ivanov, V. D. ; Moretti, M. I. ; Ripepi, V. ; Rubele, S. / The VMC survey : VII. Reddening map of the 30 Doradus field and the structure of the cold interstellar medium. In: Astronomy and Astrophysics. 2013 ; Vol. 554. pp. 1-26.
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abstract = "Context. The details of how galaxies have evolved over cosmological times are imprinted in their star formation history, chemical enrichment and morpho-kinematic structure. Parameters behind these, such as effective temperature and metallicity, can be measured by combining photometric techniques with modelling. However, there are uncertainties with this indirect approach from the ambiguity of colour and magnitude and the effects of interstellar reddening. Aims. In this paper we present a detailed reddening map of the central 30 Doradus region of the Large Magellanic Cloud; for both community use and as a test of the methods used for future use on a wider area. The reddening, a measurement of dust extinction, acts as a tracer of the interstellar medium (ISM). Methods. Near-infrared (NIR) photometry of the red clump stars is used to measure reddening as their fixed luminosity and intermediate age make extinction the dominant cause of colour and magnitude variance. The star formation history derived previously from these data is used to produce an intrinsic colour to act as a zero point in converting colour to reddening values E(J - Ks) which are subsequently converted to visual extinction AV. Results. Presented is a dust map for the 30 Doradus field in both AV and E(J - Ks). This map samples a region of 1° × 1.°5, containing ∼ 1.5 × 105 red clump stars which probe reddening up to AV ≃ 6 mag. We compare our map with maps from the literature, including optical extinction maps and radio, mid- and far-infrared maps of atomic hydrogen and dust emission. Through estimation of column density we locate molecular clouds. Conclusions. This new reddening map shows correlation with equivalent maps in the literature, validating the method of red clump star selection. We make our reddening map available for community use. In terms of ISM the red clump stars appear to be more affected by the cooler dust measured by 70 μm emission because there is stronger correlation between increasing emission and extinction due to red clump stars not being located near hot stars that would heat the dust. The transition from atomic hydrogen to molecular hydrogen occurs between densities of NH ≃ 4 × 1021 cm and NH ≃ 6 × 1021 cm.",
keywords = "Magellanic Clouds, Hertzsprung-Russell and C-M diagrams, galaxies: structure, dust, extinction, ISM: structure, stars: horizontal-branch",
author = "Tatton, {B. L.} and {van Loon}, {J. Th.} and Cioni, {M. -R.} and G. Clementini and Emerson, {J. P.} and L. Girardi and {de Grijs}, R. and Groenewegen, {M. A. T.} and M. Gullieuszik and Ivanov, {V. D.} and Moretti, {M. I.} and V. Ripepi and S. Rubele",
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Tatton, BL, van Loon, JT, Cioni, M-R, Clementini, G, Emerson, JP, Girardi, L, de Grijs, R, Groenewegen, MAT, Gullieuszik, M, Ivanov, VD, Moretti, MI, Ripepi, V & Rubele, S 2013, 'The VMC survey: VII. Reddening map of the 30 Doradus field and the structure of the cold interstellar medium', Astronomy and Astrophysics, vol. 554, A33, pp. 1-26. https://doi.org/10.1051/0004-6361/201321209

The VMC survey : VII. Reddening map of the 30 Doradus field and the structure of the cold interstellar medium. / Tatton, B. L.; van Loon, J. Th.; Cioni, M. -R.; Clementini, G.; Emerson, J. P.; Girardi, L.; de Grijs, R.; Groenewegen, M. A. T.; Gullieuszik, M.; Ivanov, V. D.; Moretti, M. I.; Ripepi, V.; Rubele, S.

In: Astronomy and Astrophysics, Vol. 554, A33, 2013, p. 1-26.

Research output: Contribution to journalReview articleResearchpeer-review

TY - JOUR

T1 - The VMC survey

T2 - Astronomy and Astrophysics

AU - Tatton, B. L.

AU - van Loon, J. Th.

AU - Cioni, M. -R.

AU - Clementini, G.

AU - Emerson, J. P.

AU - Girardi, L.

AU - de Grijs, R.

AU - Groenewegen, M. A. T.

AU - Gullieuszik, M.

AU - Ivanov, V. D.

AU - Moretti, M. I.

AU - Ripepi, V.

AU - Rubele, S.

PY - 2013

Y1 - 2013

N2 - Context. The details of how galaxies have evolved over cosmological times are imprinted in their star formation history, chemical enrichment and morpho-kinematic structure. Parameters behind these, such as effective temperature and metallicity, can be measured by combining photometric techniques with modelling. However, there are uncertainties with this indirect approach from the ambiguity of colour and magnitude and the effects of interstellar reddening. Aims. In this paper we present a detailed reddening map of the central 30 Doradus region of the Large Magellanic Cloud; for both community use and as a test of the methods used for future use on a wider area. The reddening, a measurement of dust extinction, acts as a tracer of the interstellar medium (ISM). Methods. Near-infrared (NIR) photometry of the red clump stars is used to measure reddening as their fixed luminosity and intermediate age make extinction the dominant cause of colour and magnitude variance. The star formation history derived previously from these data is used to produce an intrinsic colour to act as a zero point in converting colour to reddening values E(J - Ks) which are subsequently converted to visual extinction AV. Results. Presented is a dust map for the 30 Doradus field in both AV and E(J - Ks). This map samples a region of 1° × 1.°5, containing ∼ 1.5 × 105 red clump stars which probe reddening up to AV ≃ 6 mag. We compare our map with maps from the literature, including optical extinction maps and radio, mid- and far-infrared maps of atomic hydrogen and dust emission. Through estimation of column density we locate molecular clouds. Conclusions. This new reddening map shows correlation with equivalent maps in the literature, validating the method of red clump star selection. We make our reddening map available for community use. In terms of ISM the red clump stars appear to be more affected by the cooler dust measured by 70 μm emission because there is stronger correlation between increasing emission and extinction due to red clump stars not being located near hot stars that would heat the dust. The transition from atomic hydrogen to molecular hydrogen occurs between densities of NH ≃ 4 × 1021 cm and NH ≃ 6 × 1021 cm.

AB - Context. The details of how galaxies have evolved over cosmological times are imprinted in their star formation history, chemical enrichment and morpho-kinematic structure. Parameters behind these, such as effective temperature and metallicity, can be measured by combining photometric techniques with modelling. However, there are uncertainties with this indirect approach from the ambiguity of colour and magnitude and the effects of interstellar reddening. Aims. In this paper we present a detailed reddening map of the central 30 Doradus region of the Large Magellanic Cloud; for both community use and as a test of the methods used for future use on a wider area. The reddening, a measurement of dust extinction, acts as a tracer of the interstellar medium (ISM). Methods. Near-infrared (NIR) photometry of the red clump stars is used to measure reddening as their fixed luminosity and intermediate age make extinction the dominant cause of colour and magnitude variance. The star formation history derived previously from these data is used to produce an intrinsic colour to act as a zero point in converting colour to reddening values E(J - Ks) which are subsequently converted to visual extinction AV. Results. Presented is a dust map for the 30 Doradus field in both AV and E(J - Ks). This map samples a region of 1° × 1.°5, containing ∼ 1.5 × 105 red clump stars which probe reddening up to AV ≃ 6 mag. We compare our map with maps from the literature, including optical extinction maps and radio, mid- and far-infrared maps of atomic hydrogen and dust emission. Through estimation of column density we locate molecular clouds. Conclusions. This new reddening map shows correlation with equivalent maps in the literature, validating the method of red clump star selection. We make our reddening map available for community use. In terms of ISM the red clump stars appear to be more affected by the cooler dust measured by 70 μm emission because there is stronger correlation between increasing emission and extinction due to red clump stars not being located near hot stars that would heat the dust. The transition from atomic hydrogen to molecular hydrogen occurs between densities of NH ≃ 4 × 1021 cm and NH ≃ 6 × 1021 cm.

KW - Magellanic Clouds

KW - Hertzsprung-Russell and C-M diagrams

KW - galaxies: structure

KW - dust, extinction

KW - ISM: structure

KW - stars: horizontal-branch

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U2 - 10.1051/0004-6361/201321209

DO - 10.1051/0004-6361/201321209

M3 - Review article

VL - 554

SP - 1

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JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

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