The Discovery of Diffuse X-Ray Emission in NGC 2024, One of the Nearest Massive Star-forming Regions

Ezoe, Yuichiro; Kokubun, M.; Makishima, Kazuo; Sekímoto, Yutaro; Matsuzaki, Keiichi

doi:10.1086/508163

Cited by 9 publications

(6 citation statements)

References 23 publications

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“…Diffuse X-ray emission with a radius of 0.5 pc from the centre of NGC 2024 was reported by Ezoe et al (2006b). The emission has a very hard continuum (kT > 8 keV) and shows a He-like Fe Kα line.…”

Section: A12 Ngc 2024 (The Flame Nebula)mentioning

confidence: 81%

“…Early studies indicated that the detection of diffuse Xray emission in stellar clusters required the presence of stars earlier than O6 (Townsley et al 2003), although an exception, the O7-powered Hourglass nebula (Rauw et al 2002), was known. Ezoe et al (2006b) have since discovered diffuse X-ray emission from NGC 2024 (the Flame nebula), which contains only late O-to early B-type stars. On the other hand, it is curious that diffuse X-ray emission has yet to be detected from some very massive stellar clusters where very early O-type stars are present, such as Trumpler 16 (Wolk et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Many works on MSFRs simply compare the observed X-ray luminosity against the mechanical wind power of the stars, or the thermal energy of the plasma against an estimate of the time-integrated energy input of the winds (e.g. Townsley et al 2003;Ezoe et al 2006b;Güdel et al 2008). The efficiency of the conversion of mechanical energy to radiation is then found to range from 10 −4 to 0.1.…”

Section: Introductionmentioning

confidence: 99%

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Feedback from winds and supernovae in massive stellar clusters – II. X-ray emission

Rogers

Pittard

2014

Monthly Notices of the Royal Astronomical Society

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The X-ray emission from a simulated massive stellar cluster is investigated. The emission is calculated from a 3D hydrodynamical model which incorporates the mechanical feedback from the stellar winds of 3 O-stars embedded in a giant molecular cloud (GMC) clump containing 3240 M ⊙ of molecular material within a 4 pc radius. A simple prescription for the evolution of the stars is used, with the first supernova explosion at t = 4.4 Myrs. We find that the presence of the GMC clump causes shortlived attenuation effects on the X-ray emission of the cluster. However, once most of the material has been ablated away by the winds the remaining dense clumps do not have a noticable effect on the attenuation compared with the assumed interstellar medium (ISM) column. We determine the evolution of the cluster X-ray luminosity, L X , and spectra, and generate synthetic images. The intrinsic X-ray luminosity drops from nearly 10 34 ergs s −1 while the winds are 'bottled up', to a near constant value of 1.7×10 32 ergs s −1 between t = 1-4 Myrs. L X reduces slightly during each star's red supergiant (RSG) stage due to the depressurization of the hot gas. However, L X increases to ≈ 10 34 ergs s −1 during each star's Wolf-Rayet (WR) stage. The X-ray luminosity is enhanced by 2-3 orders of magnitude to ∼ 10 37 ergs s −1 for at least 4600 yrs after each supernova (SN) explosion, at which time the blast wave leaves the grid and the X-ray luminosity drops. The X-ray luminosity of our simulation is generally considerably fainter than predicted from spherically-symmetric bubble models, due to the leakage of hot gas material through gaps in the outer shell. This process reduces the pressure within our simulation and thus the X-ray emission. However, the X-ray luminosities and temperatures which we obtain are comparable to similarly powerful massive young clusters.

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Section: A12 Ngc 2024 (The Flame Nebula)mentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Feedback from winds and supernovae in massive stellar clusters – II. X-ray emission

Rogers

Pittard

2014

Monthly Notices of the Royal Astronomical Society

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“…With significant advances in X-ray observing techniques, diffuse X-ray emission has been detected from many massive star forming regions. Nearby ( < ∼ 2 kpc) samples include RCW 38 (Wolk et al 2002), the Rosette nebula (Townsely et al 2003), M17 (Townsely et al 2003;Hyodo et al 2008), NGC 6334 (Ezoe et al 2006a), NGC 2024 (Ezoe et al 2006b), the Carina nebula (Hamaguchi et al 2007;Ezoe et al 2009;Townsely et al 2011a), the Orion nebula (Güdel et al 2008) and the Cyg OB2 association (Albacete Colombo et al 2018). Their spectra are characterized by multiple-temperature thermal plasma emission with typical plasma temperatures below 1 keV and luminosities of 10 32−35 erg s −1 and some of them (e.g., RCW38, NGC 6334, NGC 2024) also show a hint of a power-law spectrum.…”

Section: Introductionmentioning

confidence: 99%

Suzaku observation of diffuse X-ray emission from a southwest region of the Carina Nebula

Ezoe

Hamaguchi

Fukushima

et al. 2019

Publications of the Astronomical Society of Japan

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A southwest region of the Carina nebula was observed with the Suzaku observatory for 47 ks in 2010 December. This region shows distinctively soft X-ray emission in the Chandra campaign observations. Suzaku clearly detects the diffuse emission above known foreground and background components between 0.4−5 keV at the surface brightness of 3.3×10 −14 erg s −1 arcmin −2 . The spectrum requires two plasma emission components with kT ∼0.2 and 0.5 keV, which suffer interstellar absorption of N H ∼1.9×10 21 cm −2 . Multiple absorption models assuming two temperature plasmas at ionization equilibrium or non-equilibrium are tested but there is no significant difference in terms of χ 2 /d.o.f.. These plasma temperatures are similar to those of the central and eastern parts of the Carina nebula measured in earlier Suzaku observations, but the surface brightness of the hot component is significantly lower than those of the other regions. This means that these two plasma components are physically separated and have different origins. The elemental abundances of O, Ne and Mg with respect to Fe favor that the diffuse plasma originates from core-collapsed supernovae or massive stellar winds.

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“…Such hard diffuse X-ray emission has been observed from a over a dozen massive star formation regions (e.g. M42 [10], Cyg OB2 [13], Westerlund 1 and 2 [16,17]; see also [19] for a comprehensive list), most of which are also seen at GeV and/or TeV gamma-ray energies.…”

Section: Introductionmentioning

confidence: 99%

Chandra X-ray observations of the HII region G5.89-0.39 and TeV Source HESSJ1800-240B

Rowell¹,

Horns²,

Uchiyama³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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The TeV gamma-ray sources in the field of the old age (> 10 4 yr) supernova remnant (SNR) W28 [2] present a unique opportunity to probe for a new type of multi-TeV particle accelerator, namely, HII regions. One such example is the TeV source HESS J1800−240B which is found towards the highly unusual HII region complex G5.89−0.39. In this context X-rays studies are highly valuable in probing the particle acceleration potential of such HII regions and their subsequent contribution to the gamma-ray emission. Previous high resolution XMM-Newton X-ray observations despite being affected by stray light from a nearby X-ray binary, revealed several sources co-located with the two star forming components of G5.89−0.39, namely G5.89-0.39A, a HII region, as well as G5.89-0.39B, an ultracompact or UCHII region. Here we describe preliminary analysis and results from our Chandra observations towards G5.89−0.39 and HESS J1800−240B (∼80 ks) which are not affected by stray light. With Chandra, we reveal over 200 X-ray sources which appear to cluster somewhat towards G5.89−0.39A and B respectively. This includes possibly extended emission towards a massive O5 or earlier spectral type star (known as Feldt's star) thought to provide much of the ionisation and energetics in G5.89−0.39B. Some of the X-ray sources exhibit energetics typical of young moderate to high mass stars. Our Chandra observations reveal for the first time the extent of star formation in the two HII components. Ongoing work centres on detailed spectral studies, cross-correlation with stellar catalogues, and the search for extended X-ray emission.

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The Discovery of Diffuse X-Ray Emission in NGC 2024, One of the Nearest Massive Star-forming Regions

Cited by 9 publications

References 23 publications

Feedback from winds and supernovae in massive stellar clusters – II. X-ray emission

Feedback from winds and supernovae in massive stellar clusters – II. X-ray emission

Suzaku observation of diffuse X-ray emission from a southwest region of the Carina Nebula

Chandra X-ray observations of the HII region G5.89-0.39 and TeV Source HESSJ1800-240B

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