The first broad-band X-ray images and spectra of the 30 Doradus region in the LMC

Dennerl, K.; Haberl, F.; Aschenbach, B.; Briel, U. G.; Balasini, M.; Bräuninger, H.; Burkert, Wolfgang; Hartmann, R.; Hartner, Gisela; Hasinger, G.; Kemmer, J.; Kendziorra, E.; Kirsch, Marcus; Krause, Norbert; Kuster, M.; Lumb, D.; Massa, Piero; Meidinger, Norbert; Pfeffermann, E.; Pietsch, W.; Reppin, C.; Soltau, H.; Staubert, R.; Strüder, L.; Trümper, J.; Turner, Martin; Villa, G.; Zavlin, V. E.

doi:10.1051/0004-6361:20000049

Cited by 35 publications

(32 citation statements)

References 16 publications

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“…The excess in 0.7-1.5 keV of Region B spectrum is particularly clear at the energies of the K-shell emission lines of Ne IX, Ne X, and Mg XI, and Fe L-shell blends. These features are likely to originate from thermal emissions from the Honeycomb nebula (SNR 0536-69.3: Dennerl et al 2001), which is partially included in the Region B area, although no clear structure is found in figure 1.…”

Section: Background Selection and Analysis Proceduresmentioning

confidence: 99%

Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

Yamaguchi

Bamba

Koyama

2009

Publications of the Astronomical Society of Japan

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This paper reports on the Suzaku results of thermal and non-thermal features of 30 Dor C, a supernova remnant (SNR) in a superbubble of the Large Magellanic Cloud (LMC). The west rim exhibits a nonthermal X-ray spectrum with no thermal component. A single power-law model is rejected but a powerlaw model with spectral cutoff is accepted. The cutoff frequency of (3 − 7) × 10 17 Hz is the highest among the shell type SNRs like SN 1006 (∼ 6 × 10 16 Hz), and hence 30 Dor C would be the site of the highest energy accelerator of the SNR shock. The southeast (SE) and northeast (NE) rims have both the thermal and non-thermal components. The thin-thermal plasmas in the both rims are in collisional ionization equilibrium state. The electron temperature of the plasma in the SE rim (kT e ∼ 0.7 keV) is found to be higher than the previously reported value. The power-law index from SE is nearly the same as, while that from the NE is larger than that of the West rim. The SNR age would be in the range of (4 − 20) × 10 3 yr. Thus, 30 Dor C is likely to be the oldest shell-like SNR with non-thermal emission.

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Section: Background Selection and Analysis Proceduresmentioning

confidence: 99%

Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

Yamaguchi

Bamba

Koyama

2009

Publications of the Astronomical Society of Japan

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“…Much of the evidence comes from the spectral decomposition of the overall emission from the SNR. The thermal emission arises over a region more extended than the PWN, but only very limited spatial analysis has been previously presented ( WG98; Dennerl et al 2001;Townsley et al 2006). It is thus of great interest to examine the physical, chemical, and morphological properties of the thermal emission and to determine how they are related to the PWN and to the OB association and superbubble environment.…”

Section: à2mentioning

confidence: 99%

ChandraACIS Spectroscopy of N157B: A Young Composite Supernova Remnant in a Superbubble

Chen

Wang

Gotthelf

et al. 2006

ApJ

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We present a Chandra ACIS observations of N157B, a young supernova remnant (SNR) located in the 30 Doradus star formation region of the Large Magellanic Cloud. This remnant contains the most energetic pulsar known (PSR J053747.39À691020.2;Ė ¼ 4:8 ; 10 38 ergs s À1 ), which is surrounded by a X-ray-bright nonthermal nebula that likely represents a toroidal pulsar wind terminal shock observed edge-on. Two of the eight pointlike X-ray sources detected in the observation are shown to have near-IR and optical counterparts (within 0B5 offsets), which are identified as massive stellar systems in the Cloud. We confirm the nonthermal nature of the comet-shaped X-ray emission feature and show that the spectral steepening of this feature away from the pulsar is quantitatively consistent with synchrotron cooling of shocked pulsar wind particles flowing downstream at a bulk velocity close to the speed of light. Around the cometary nebula we unambiguously detect a spatially resolved thermal component, which accounts for about 1/3 of the total 0.5-10 keV flux from the remnant. This thermal component is distributed among various clumps of metal-enriched plasma embedded in the low surface brightness X-ray-emitting diffuse gas. The relative metal enrichment pattern suggests that the mass of the supernova progenitor is k20 M . A comparison of the X-ray data with Hubble Space Telescope optical images now suggests that the explosion site is close to a dense cloud, against which a reflection shock is launched. The interaction between the reflected material and the nebula has likely produced both its cometary shape and the surrounding thermal emission enhancement. SNR N157B is apparently expanding into the hot low-density interior of the surrounding superbubble formed by the young OB association LH 99, as revealed by Spitzer mid-infrared images. This scenario naturally explains the exceptionally large sizes of both the thermal and nonthermal components, as well as the lack of an outer shell of the SNR. However, the real situation in the region is likely to be more complicated. We find that a partially round soft X-ray-emitting clump with distinct spectral properties may result from a separate oxygen-rich remnant. These results provide a rare glimpse into the SNR structure and evolution in a region of recent star formation.

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“…In these images, there is evidence for spectral variations in the X-ray emission across the face of the bubble. While the western part of the bubble is easily seen in the medium-and hard-band images, it is almost invisible in the soft-band image, clearly because of the X-ray absorption by foreground cool gas (see also Dennerl et al 2001 andDunne et al 2001). There is a region of localized CO emission projected onto the western part of 30 Dor C (Johansson et al 1998).…”

Section: Morphologg Ical Propertiesmentioning

confidence: 99%

Confronting the Superbubble Model with X‐Ray Observations of 30 Doradus C

Smith

Wang

2004

ApJ

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We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the results with the predictions from the standard wind-blown bubble model. We find that the observed X-ray spectra cannot be fitted satisfactorily with the model alone and that there is evidence for nonthermal X-ray emission, which is particularly important at k4 keV. The combination of the bubble model and a power law gives a reasonable fit to the observed spectra. The thermal pressure and central temperature of the bubble are 3:3 ; 10 À11 dynes cm À2 and 7:4 ; 10 6 K, respectively, and we infer that for a bubble age of t $ 4 ; 10 6 yr the ambient density is n 0 ' 38 cm À3 , the mechanical luminosity is L mech $ 10 37 ergs s À1 , and the coefficient of thermal conductivity is $0.05 of the Spitzer value. The total unabsorbed 0.1-10 keV luminosities of the eastern and western parts of the bubble are '3 ; 10 36 and '5 ; 10 36 ergs s À1 , respectively. The unabsorbed 0.1-10 keV luminosity of the bubble model is $4 ; 10 36 ergs s À1 , and so the power-law component contributes between 1 3 and 1 2 of the total unabsorbed luminosity in this energy band. The nature of the hard nonthermal emission is not clear, although recent supernovae in the bubble may be responsible. We expect that about one or two core-collapse supernovae could have occurred and are required to explain the enrichment of the hot gas, as evidenced by the overabundance of -elements by a factor of k3, compared to the mean value of $0.5 solar for the interstellar medium in the Large Magellanic Cloud. As in previous studies of various superbubbles, the amount of energy currently present in 30 Dor C is significantly less than the expected energy input from the enclosed massive stars over their lifetime. We speculate that a substantial fraction of the input energy may be radiated in the far-infrared by dust grains, which are mixed with the hot gas because of the thermal conduction and/or dynamic mixing.

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The first broad-band X-ray images and spectra of the 30 Doradus region in the LMC

Cited by 35 publications

References 16 publications

Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

ChandraACIS Spectroscopy of N157B: A Young Composite Supernova Remnant in a Superbubble

Confronting the Superbubble Model with X‐Ray Observations of 30 Doradus C

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