Parsec-scale X-ray flows in high-mass star-forming regions

Townsley, Leisa K.; Feigelson, E.; Montmerle, T.; Broos, P. S.; Chu, Y-H; Garmire, G. P.; Getman, Konstantin V.

doi:10.1017/s1743921305004667

Cited by 9 publications

(11 citation statements)

References 40 publications

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“…Additionally, eight of the sources detected by Chandra (Townsley et al 2005) do not show JHK s characteristics similar to the previously mentioned groups but still present hints of youth, like considerable excess emission at λ > 3 μm not apparent at shorter wavelengths (#21, #33, #59, #87, #115, #126, #152 and #157). Three of them (#21, #87 and #115) are seen in the 3.6‐ and 4.5‐μm IRAC frames but are too faint to allow photometric measurements.…”

Section: Resultsmentioning

confidence: 72%

“…7 displays the K s versus H − K s diagram. Table 2 lists the 71 sources found to show excess emission at λ > 2 μm or X‐ray emission detected by Chandra (16 cases; Townsley et al 2005). The table gives positions, PANIC and IRAC magnitudes and individual remarks that describe their main properties.…”

Section: Resultsmentioning

confidence: 99%

“…Other seven sources showed 3.6 μm excess not evident at JHK . With one exception, all X‐ray sources in the list provided by Townsley et al (2005) were detected in the infrared. Of these 16 X‐ray and infrared sources, only four were found not to show a measurable infrared excess but in three cases, marginal IRAC detections suggested disc emission might be present.…”

Section: Resultsmentioning

confidence: 99%

“… Notes: xrs: Chandra X‐ray source (Townsley et al 2005); lexc: [3.6]‐band excess; I to V: near‐infrared properties group (); *: close pair of mid‐IR sources; **: within extended, nebulous emission in all IRAC bands; ***: very faint at 3.5 and 4.5 μm; †: IRAC [5.8]= 9.48::, [8]= 8.02:; ‡: IRAC [6.8]= 5.80, [8]= 4.94; ††: #106 and #110 IRAC magnitudes combined; ‡‡: #105 and #108 IRAC magnitudes combined. …”

Section: Resultsmentioning

confidence: 99%

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Imaging study of NGC 3372, the Carina nebula -- II. Evidence of activity in the complex Trumpler 14/Car I photodissociation region

Tapia¹,

Persi

Bohigas³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We present the results of an imaging survey, from the optical to the mid‐infrared, of the dark cloud associated with Car I, a dense cloud that is subject to an intense ultraviolet radiation field from the rich stellar cluster Trumpler 14. New ground‐based broad‐ and narrow‐band near‐infrared and narrow‐band optical images are analysed in combination with archived Spitzer/InfraRed Array Camera (IRAC) images to study this photodissociation region (PDR) and the triggering of a new generation of stars within the cloud, particularly close to its edges. Evidence is given of a clumpy morphology of the dense cloud. The ionization/dissociation front is delineated at the edges of these clumps. The existence of a number of embedded low‐ to intermediate‐mass pre‐main‐sequence objects is confirmed by their considerable infrared excesses arising from discs and/or detectable X‐ray emission. Most of the young stellar objects (YSOs) are located on or just behind ionization fronts, though a few are also outside the cloud. The infrared properties of the YSOs are discussed. Two Class I objects stand out, one of them is an FU Orionis system candidate that had an outburst of more than 3 mag in K between 1993 and 2003, with further evidence that it occurred in the 2000–02 period. Molecular hydrogen line filamentary emission behind the Balmer and Brackett lines along the ionization front is seen delineating the edges of the dense cloud. This emission is also seen in all IRAC images. The diffuse, filamentary emission is very similar in all four 3.6, 4.5, 5.8 and 8 μm bands, though there seem to be subtle differences. Across a bright section of the ionization/dissociation front, we found that, within the observational uncertainties, the maximum emission in all four IRAC channels coincides with that of H2 2.12 μm. The western, embedded, dissociation front close to the CO peak (Car I‐W) is seen delineated by a bright, long bar of emission in the 3–12 μm images, in the Midcourse Space Experiment bands A and C and also in radio continuum and hydrogen line emission. These occur in the vicinity of a region of previously reported strong [C i], [C ii] and [O i] emission, tracers of PDRs. A few bright, compact knots of H2 emission, some possibly associated with [S ii] emission, are found within the cloud. These may be shock‐excited.

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Section: Resultsmentioning

confidence: 72%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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Imaging study of NGC 3372, the Carina nebula -- II. Evidence of activity in the complex Trumpler 14/Car I photodissociation region

Tapia¹,

Persi

Bohigas³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…Early Chandra and XMM studies were summarized in Townsley et al (2003); more recent work is described in Feigelson et al (2006). Other MSFRs currently under study at Penn State include RCW 49 (Townsley et al 2004), NGC 7538 (Tsujimoto et al 2005), W51A (Townsley et al 2004, and the Rosette Nebula (Wang et al 2006, in preparation).…”

Section: Revealing the Life Cycle Of A Massive Stellar Clustermentioning

confidence: 99%

An x-ray tour of massive-star-forming regions with Chandra

Townsley¹

2009

Massive Stars

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The Chandra X-ray Observatory is providing fascinating new views of massive star-forming regions, revealing all stages in the life cycles of massive stars and their effects on their surroundings. I present a Chandra tour of some of the most famous of these regions: M17, NGC 3576, W3, Tr14 in Carina, and 30 Doradus. Chandra highlights the physical processes that characterize the lives of these clusters, from the ionizing sources of ultracompact HII regions (W3) to superbubbles so large that they shape our views of galaxies (30 Dor). X-ray observations usually reveal hundreds of pre-main sequence (lower-mass) stars accompanying the OB stars that power these great HII region complexes, although in one case (W3 North) this population is mysteriously absent. The most massive stars themselves are often anomalously hard X-ray emitters; this may be a new indicator of close binarity. These complexes are sometimes suffused by soft diffuse X-rays (M17, NGC 3576), signatures of multi-million-degree plasmas created by fast O-star winds. In older regions we see the X-ray remains of the deaths of massive stars that stayed close to their birthplaces (Tr14, 30 Dor), exploding as cavity supernovae within the superbubbles that these clusters created. Revealing the Life Cycle of a Massive Stellar ClusterHigh-resolution X-ray images from the Chandra X-ray Observatory and XMM-Newton elucidate all stages in the life cycles of massive stars -from ultracompact HII (UCHII) regions to supernova remnants -and the effects that those massive stars have on their surroundings. X-ray studies of massive star-forming regions (MSFRs) thus give insight into the massive stars themselves, the accompanying lower-mass cluster population, new generations of stars that may be triggered by the massive cluster, interactions of massive star winds with themselves and with the surrounding neutral medium, and the fate of massive stars that die as cavity supernovae inside the wind-blown bubbles they created.In the era of Spitzer and excellent ground-based near-infrared (IR) data, why are X-ray studies of MSFRs important? Chandra routinely penetrates A V > 100 mag of extinction with little confusion or contamination, revealing young stellar populations in a manner that is unbiased by the presence of inner disks around these stars. These vast pre-main sequence (pre-MS) populations are easily seen by Chandra and the 17 ′ ×17 ′ imaging array of its Advanced CCD Imaging Spectrometer (ACIS-I); a typical ACIS-I observation of a nearby (D < 3 kpc) MSFR, lasting 40-100 ksec, finds 500-1500 young stars, tracing the initial mass function (IMF) down to ∼ 1M ⊙ . These observations can increase the number of known cluster members by as much as a factor of 50 in poorly-studied regions (e.g. NGC 6357, J. .In the first 7 months of 2006, at least 18 refereed papers on X-ray observations of MSFRs (using Chandra or XMM) were published or submitted. These include studies of 30 Doradus (Townsley et al. 2006a,b), NGC 6334 (Ezoe et al.

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The Company Eta Carinae Keeps: Stellar and Interstellar Content of the Carina Nebula

Walborn

2012

Eta Carinae and the Supernova Impostors

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Parsec-scale X-ray flows in high-mass star-forming regions

Cited by 9 publications

References 40 publications

Imaging study of NGC 3372, the Carina nebula -- II. Evidence of activity in the complex Trumpler 14/Car I photodissociation region

Imaging study of NGC 3372, the Carina nebula -- II. Evidence of activity in the complex Trumpler 14/Car I photodissociation region

An x-ray tour of massive-star-forming regions with Chandra

The Company Eta Carinae Keeps: Stellar and Interstellar Content of the Carina Nebula

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