Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements

M. H. Vuong, T. Montmerle, N. Grosso, Eric Feigelson, L. Verstraete, H. Ozawa

Research output: Contribution to journalArticle

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Abstract

We present a comparison of the gas and dust properties of the dense interstellar matter in six nearby star-forming regions (d < 500 pc): ρ Oph, Cha I, R CrA, IC 348, NGC 1333, and Orion. We measure from Chandra and XMM-Newton observations the X-ray absorption toward pre-main sequence stars (PMS) without accretion disks (i.e., Class III sources) to obtain the total hydrogen column density NH,X. For these sources we take from the literature the corresponding dust extinction in the near-infrared, A J, or when unavailable we derive it from SED fitting using the available DENIS, 2MASS, ISOCAM and other data. We then compare NH,X and AJ for each object, up to unprecedently high extinction. For the ρ Oph dark cloud with a relatively large sample of 20 bona-fide Class III sources, we probe the extinction up to AJ ≲ 14 (AV ≲ 45), and find a best-fit linear relation NH,X/AJ = 5.6 (± 0.4) × 1021 cm-2 mag-1, adopting standard ISM abundances. The other regions reveal a large dispersion in the NH,X/AJ ratio for each source but for lack of adequate IR data these studies remain limited to moderate extinctions (A J ≲ 1.5 or AV ≲ 5). For σ Oph, the N H,X/AJ ratio is significantly lower (≳2σ) than the galactic value, derived using the standard extinction curve (RV = 3.1). This result is consistent with the recent downwards revision of the metallicity of the Sun and stars in the solar vicinity. We find that the ρ Oph dense cloud has the same metallicity than the local ISM when assuming that the galactic gas-to-dust ratio remains unchanged. The difference between galactic and local values of the gas-to-dust ratio can thus be attributed entirely to a difference in metallicity.

Original languageEnglish (US)
Pages (from-to)581-599
Number of pages19
JournalAstronomy and Astrophysics
Volume408
Issue number2
DOIs
StatePublished - Jan 1 2003

Fingerprint

extinction
dust
metallicity
gases
gas
x rays
interstellar matter
stars
pre-main sequence stars
XMM-Newton telescope
accretion disks
newton
near infrared
sun
accretion
probe
hydrogen
probes
curves

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Vuong, M. H. ; Montmerle, T. ; Grosso, N. ; Feigelson, Eric ; Verstraete, L. ; Ozawa, H. / Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements. In: Astronomy and Astrophysics. 2003 ; Vol. 408, No. 2. pp. 581-599.
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abstract = "We present a comparison of the gas and dust properties of the dense interstellar matter in six nearby star-forming regions (d < 500 pc): ρ Oph, Cha I, R CrA, IC 348, NGC 1333, and Orion. We measure from Chandra and XMM-Newton observations the X-ray absorption toward pre-main sequence stars (PMS) without accretion disks (i.e., Class III sources) to obtain the total hydrogen column density NH,X. For these sources we take from the literature the corresponding dust extinction in the near-infrared, A J, or when unavailable we derive it from SED fitting using the available DENIS, 2MASS, ISOCAM and other data. We then compare NH,X and AJ for each object, up to unprecedently high extinction. For the ρ Oph dark cloud with a relatively large sample of 20 bona-fide Class III sources, we probe the extinction up to AJ ≲ 14 (AV ≲ 45), and find a best-fit linear relation NH,X/AJ = 5.6 (± 0.4) × 1021 cm-2 mag-1, adopting standard ISM abundances. The other regions reveal a large dispersion in the NH,X/AJ ratio for each source but for lack of adequate IR data these studies remain limited to moderate extinctions (A J ≲ 1.5 or AV ≲ 5). For σ Oph, the N H,X/AJ ratio is significantly lower (≳2σ) than the galactic value, derived using the standard extinction curve (RV = 3.1). This result is consistent with the recent downwards revision of the metallicity of the Sun and stars in the solar vicinity. We find that the ρ Oph dense cloud has the same metallicity than the local ISM when assuming that the galactic gas-to-dust ratio remains unchanged. The difference between galactic and local values of the gas-to-dust ratio can thus be attributed entirely to a difference in metallicity.",
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Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements. / Vuong, M. H.; Montmerle, T.; Grosso, N.; Feigelson, Eric; Verstraete, L.; Ozawa, H.

In: Astronomy and Astrophysics, Vol. 408, No. 2, 01.01.2003, p. 581-599.

Research output: Contribution to journalArticle

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T1 - Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements

AU - Vuong, M. H.

AU - Montmerle, T.

AU - Grosso, N.

AU - Feigelson, Eric

AU - Verstraete, L.

AU - Ozawa, H.

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N2 - We present a comparison of the gas and dust properties of the dense interstellar matter in six nearby star-forming regions (d < 500 pc): ρ Oph, Cha I, R CrA, IC 348, NGC 1333, and Orion. We measure from Chandra and XMM-Newton observations the X-ray absorption toward pre-main sequence stars (PMS) without accretion disks (i.e., Class III sources) to obtain the total hydrogen column density NH,X. For these sources we take from the literature the corresponding dust extinction in the near-infrared, A J, or when unavailable we derive it from SED fitting using the available DENIS, 2MASS, ISOCAM and other data. We then compare NH,X and AJ for each object, up to unprecedently high extinction. For the ρ Oph dark cloud with a relatively large sample of 20 bona-fide Class III sources, we probe the extinction up to AJ ≲ 14 (AV ≲ 45), and find a best-fit linear relation NH,X/AJ = 5.6 (± 0.4) × 1021 cm-2 mag-1, adopting standard ISM abundances. The other regions reveal a large dispersion in the NH,X/AJ ratio for each source but for lack of adequate IR data these studies remain limited to moderate extinctions (A J ≲ 1.5 or AV ≲ 5). For σ Oph, the N H,X/AJ ratio is significantly lower (≳2σ) than the galactic value, derived using the standard extinction curve (RV = 3.1). This result is consistent with the recent downwards revision of the metallicity of the Sun and stars in the solar vicinity. We find that the ρ Oph dense cloud has the same metallicity than the local ISM when assuming that the galactic gas-to-dust ratio remains unchanged. The difference between galactic and local values of the gas-to-dust ratio can thus be attributed entirely to a difference in metallicity.

AB - We present a comparison of the gas and dust properties of the dense interstellar matter in six nearby star-forming regions (d < 500 pc): ρ Oph, Cha I, R CrA, IC 348, NGC 1333, and Orion. We measure from Chandra and XMM-Newton observations the X-ray absorption toward pre-main sequence stars (PMS) without accretion disks (i.e., Class III sources) to obtain the total hydrogen column density NH,X. For these sources we take from the literature the corresponding dust extinction in the near-infrared, A J, or when unavailable we derive it from SED fitting using the available DENIS, 2MASS, ISOCAM and other data. We then compare NH,X and AJ for each object, up to unprecedently high extinction. For the ρ Oph dark cloud with a relatively large sample of 20 bona-fide Class III sources, we probe the extinction up to AJ ≲ 14 (AV ≲ 45), and find a best-fit linear relation NH,X/AJ = 5.6 (± 0.4) × 1021 cm-2 mag-1, adopting standard ISM abundances. The other regions reveal a large dispersion in the NH,X/AJ ratio for each source but for lack of adequate IR data these studies remain limited to moderate extinctions (A J ≲ 1.5 or AV ≲ 5). For σ Oph, the N H,X/AJ ratio is significantly lower (≳2σ) than the galactic value, derived using the standard extinction curve (RV = 3.1). This result is consistent with the recent downwards revision of the metallicity of the Sun and stars in the solar vicinity. We find that the ρ Oph dense cloud has the same metallicity than the local ISM when assuming that the galactic gas-to-dust ratio remains unchanged. The difference between galactic and local values of the gas-to-dust ratio can thus be attributed entirely to a difference in metallicity.

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