10 MK gas in M17 and the Rosette Nebula: X-ray flows in galactic H II regions

Leisa K. Townsley, Eric D. Feigelson, Thierry Montmerle, Patrick S. Broos, You Hua Chu, Gordon P. Garmire

Research output: Contribution to journalArticle

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Abstract

We present the first high spatial resolution X-ray images of two high-mass star forming regions, the Omega Nebula (M17) and the Rosette Nebula (NGC 2237-2246), obtained with the Chandra X-Ray Observatory Advanced CCD Imaging Spectrometer instrument. The massive clusters powering these H II regions are resolved at the arcsecond level into more than 900 (M17) and 300 (Rosette) stellar sources similar to those seen in closer young stellar clusters. However, we also detect soft diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point-source population. The diffuse emission has luminosity LX ≃ 3.4 × 1033 ergs s -1 in M17 with plasma energy components at kT ≃ 0.13 and ≃0.6 keV (1.5 and 7 MK), while in Rosette it has LX ≃ 6 × 1032 ergs s-1 with plasma energy components at kT ≃ 0.06 and ≃0.8 keV (0.7 and 9 MK). This extended emission most likely arises from the fast O star winds thermalized either by wind-wind collisions or by a termination shock against the surrounding media. We establish that only a small portion of the wind energy and mass appears in the observed diffuse X-ray plasma; in these blister H II regions, we suspect that most of it flows without cooling into the low-density interstellar medium. These data provide compelling observational evidence that strong wind shocks are present in H II regions.

Original languageEnglish (US)
Pages (from-to)874-905
Number of pages32
JournalAstrophysical Journal
Volume593
Issue number2 I
DOIs
StatePublished - Aug 20 2003

Fingerprint

H II regions
nebulae
gases
gas
x rays
plasma
erg
shock
blisters
windpower utilization
O stars
imaging spectrometers
energy
point sources
charge coupled devices
observatories
spatial resolution
luminosity
point source
stars

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Townsley, Leisa K. ; Feigelson, Eric D. ; Montmerle, Thierry ; Broos, Patrick S. ; Chu, You Hua ; Garmire, Gordon P. / 10 MK gas in M17 and the Rosette Nebula : X-ray flows in galactic H II regions. In: Astrophysical Journal. 2003 ; Vol. 593, No. 2 I. pp. 874-905.
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10 MK gas in M17 and the Rosette Nebula : X-ray flows in galactic H II regions. / Townsley, Leisa K.; Feigelson, Eric D.; Montmerle, Thierry; Broos, Patrick S.; Chu, You Hua; Garmire, Gordon P.

In: Astrophysical Journal, Vol. 593, No. 2 I, 20.08.2003, p. 874-905.

Research output: Contribution to journalArticle

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T1 - 10 MK gas in M17 and the Rosette Nebula

T2 - X-ray flows in galactic H II regions

AU - Townsley, Leisa K.

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AU - Broos, Patrick S.

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N2 - We present the first high spatial resolution X-ray images of two high-mass star forming regions, the Omega Nebula (M17) and the Rosette Nebula (NGC 2237-2246), obtained with the Chandra X-Ray Observatory Advanced CCD Imaging Spectrometer instrument. The massive clusters powering these H II regions are resolved at the arcsecond level into more than 900 (M17) and 300 (Rosette) stellar sources similar to those seen in closer young stellar clusters. However, we also detect soft diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point-source population. The diffuse emission has luminosity LX ≃ 3.4 × 1033 ergs s -1 in M17 with plasma energy components at kT ≃ 0.13 and ≃0.6 keV (1.5 and 7 MK), while in Rosette it has LX ≃ 6 × 1032 ergs s-1 with plasma energy components at kT ≃ 0.06 and ≃0.8 keV (0.7 and 9 MK). This extended emission most likely arises from the fast O star winds thermalized either by wind-wind collisions or by a termination shock against the surrounding media. We establish that only a small portion of the wind energy and mass appears in the observed diffuse X-ray plasma; in these blister H II regions, we suspect that most of it flows without cooling into the low-density interstellar medium. These data provide compelling observational evidence that strong wind shocks are present in H II regions.

AB - We present the first high spatial resolution X-ray images of two high-mass star forming regions, the Omega Nebula (M17) and the Rosette Nebula (NGC 2237-2246), obtained with the Chandra X-Ray Observatory Advanced CCD Imaging Spectrometer instrument. The massive clusters powering these H II regions are resolved at the arcsecond level into more than 900 (M17) and 300 (Rosette) stellar sources similar to those seen in closer young stellar clusters. However, we also detect soft diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point-source population. The diffuse emission has luminosity LX ≃ 3.4 × 1033 ergs s -1 in M17 with plasma energy components at kT ≃ 0.13 and ≃0.6 keV (1.5 and 7 MK), while in Rosette it has LX ≃ 6 × 1032 ergs s-1 with plasma energy components at kT ≃ 0.06 and ≃0.8 keV (0.7 and 9 MK). This extended emission most likely arises from the fast O star winds thermalized either by wind-wind collisions or by a termination shock against the surrounding media. We establish that only a small portion of the wind energy and mass appears in the observed diffuse X-ray plasma; in these blister H II regions, we suspect that most of it flows without cooling into the low-density interstellar medium. These data provide compelling observational evidence that strong wind shocks are present in H II regions.

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