Multiwavelength analysis of the X-ray spur and southeast of the Large Magellanic Cloud

Knies, Jonathan; Sasaki, M.; Fukui, Y.; Tsuge, Kisetsu; Haberl, F.; Points, Sean; Kavanagh, Patrick; Filipović, Miroslav

doi:10.1051/0004-6361/202038488

Cited by 9 publications

(8 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We thus obtain a mean temperature of kT 1 = 0.22 keV with a standard deviation of σ kT 1 = 0.02 keV for the lower-temperature component and kT 2 = 0.74 keV and σ kT 2 = 0.10 keV for the higher-temperature component. These temperature values are consistent with the results of the analysis of XMM-Newton observations of southeastern parts of the LMC (regions around 30 Dor, in the X-ray spur, and west of them) by Knies et al (2021). As can be seen in Fig.…”

Section: Thermal Componentsupporting

confidence: 91%

“…The same stars, which have created the giant H ii region 30 Dor and the other H ii structures in its surroundings, are the likely sources of the hot interstellar plasma. This result corroborates nicely the scenario of the collision of large HI structures in the LMC for the origin of 30 Dor and the star-forming regions south of 30 Dor presented by Fukui et al (2017) and recently confirmed by Knies et al (2021) based on multi-wavelength study of the southeastern part of the LMC, in particular the X-ray spur. A large HI component, called the Lcomponent has encountered the HI component in the disk of the LMC (D-component) in the past, starting roughly at the position where 30 Dor is observed now.…”

Section: Foreground Absorption In the Lmcsupporting

confidence: 90%

“…The X-ray spur is located south of 30 Dor and the supergiant shell LMC 2 (LMC-SGS 2) and seems to coincide with the regions in which the L-and D-components of H i collide with each other. The analysis of X-ray data taken with XMM-Newton has shown that the X-ray spur was most likely caused by the H i collision (Knies et al 2021). While in 30 Dor and in regions around it, the interstellar medium (ISM) was heated by the stellar winds and supernovae of massive stars, there are no indication of stellar heating in the X-ray spur.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

Sasaki,

Knies,

Haberl

et al. 2021

Preprint

View full text Add to dashboard Cite

Context. In the first months after the launch in July 2019, eROSITA (extended Roentgen Survey with an Imaging Telescope Array) onboard Spektrum-Roentgen-Gamma (Spektr-RG, SRG) performed long-exposure observations in the regions around supernova (SN) 1987A and supernova remnant (SNR) N132D in the Large Magellanic Cloud (LMC). Aims. We analyse the distribution and the spectrum of the diffuse X-ray emission in the observed fields to determine the physical properties of the hot phase of the interstellar medium (ISM). Methods. Spectral extraction regions were defined using the Voronoi tessellation method. The spectra are fitted with a combination of thermal and non-thermal emission models. The eROSITA data are complemented by newly derived column density maps for the Milky Way and the LMC, 888 MHz radio continuum map from the Australian Square Kilometer Array Pathfinder (ASKAP), and optical images of the Magellanic Cloud Emission Line Survey (MCELS). Results. We detect significant emission from thermal plasma with kT = 0.2 keV in all the regions. There is also an additional highertemperature emission component from a plasma with kT ≈ 0.7 keV. The surface brightness of the latter component is one order of magnitude lower than that of the lower-temperature component. In addition, non-thermal X-ray emission is significantly detected in the superbubble 30 Dor C. The absorbing column density N H in the LMC derived from the analysis of the X-ray spectra taken with eROSITA is consistent with the N H obtained from the emission of the cold medium over the entire area. Neon abundance is enhanced in the regions in and around 30 Dor and SN 1987A, indicating that the ISM has been chemically enriched by the young stellar population. In the centre of 30 Dor, there are two bright extended X-ray sources, which coincide with the stellar cluster RMC 136 and the Wolf-Rayet stars RMC 139 and RMC 140. For both regions, the emission is best modelled with a high-temperature (kT > 1 keV) non-equilibrium ionisation plasma emission and a non-thermal component with a photon index of Γ = 1.3. In addition, we detect an extended X-ray source at the position of the optical SNR candidate J0529-7004 with thermal emission and thus confirm its classification as an SNR. Conclusions. Using data from the early observations of the regions around SN 1987A and SNR N132D with eROSITA we confirm that there is thermal interstellar plasma in the entire observed field. eROSITA with its large field of view and high sensitivity at lower X-ray energies allows us for the first time to carry out a detailed study of the ISM at high energies consistently over a large region in the LMC. We thus measure the properties of the interstellar plasma and the distribution of non-thermal particles and derive the column density of the cold matter on the line of sight.

show abstract

Section: Thermal Componentsupporting

confidence: 91%

Section: Foreground Absorption In the Lmcsupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

Sasaki,

Knies,

Haberl

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…It seems to emit higher energy X-rays than what is typically expected from interstellar plasma in galaxies. XMM-Newton studies of the X-ray spur have shown that the interstellar plasma has a higher temperature than in most other parts of the LMC, being as high as in the region around the Tarantula nebula in 30 Doradus and the super-star cluster RMC 136 inside it, which are heated by a large number of very massive stars and is located north of the X-ray spur [65]. In the X-ray spur, however, as the complementary multiwavelength analysis shows, there are no indications for the past and present existence of massive stars which might have caused the heating of the plasma at the position.…”

Section: X-ray Spur In the Lmcmentioning

confidence: 99%

Diffuse Hot Plasma in the Interstellar Medium and Galactic Outflows

Sasaki¹,

Ponti²,

Mackey³

2022

Preprint

View full text Add to dashboard Cite

We summarise observations and our current understanding of the interstellar medium (ISM) in galaxies, which mainly consists of three phases: cold atomic or molecular gas and clouds, warm neutral or ionised gas, and hot ionised gas. These three gas phases form thermally stable states, while disturbances are caused by gravitation and stellar feedback in form of photons and shocks in stellar winds and supernovae. Hot plasma is mainly found in stellar bubbles, superbubbles, and Galactic outflows/fountains and is often dynamically unstable and is over-pressurised. In addition, in galactic nuclear regions, accretion onto the supermassive black hole causes enhanced star formation, outflows, additional heating, and acceleration of cosmic rays.

show abstract

“…We have recently analyzed the properties of the hot interstellar plasma in the entire interaction region using Xray data. The spectral analysis has shown that the plasma in the region around 30 Doradus and SGS LMC 2 has been heated by the young stars, while the region to the south must have been heated by the cloud collision (Knies et al 2021).…”

Section: Supergiant Shell Lmcmentioning

confidence: 99%

Tracking down the origin of superbubbles and supergiant shells in the Magellanic Clouds with Minkowski tensor analysis

Collischon

Sasaki

Mecke

et al. 2021

A&A

View full text Add to dashboard Cite

Aims. We develop an automatic bubble-recognition routine based on Minkowski functionals (MF) and tensors (MT) to detect bubble-like interstellar structures in optical emission line images. Methods. Minkowski functionals and MT are powerful mathematical tools for parameterizing the shapes of bodies. Using the papaya2-library, we created maps of the desired MF or MT of structures at a given window size. We used maps of the irreducible MT ψ2, which is sensitive to elongation, to find filamentary regions in Hα, [S II], and [O III] images of the Magellanic Cloud Emission Line Survey. Using the phase of ψ2, we were able to draw lines perpendicular to each filament and thus obtain line-density maps. This allowed us to find the center of a bubble-like structure and to detect structures at different window sizes. Results. The detected bubbles in all bands are spatially correlated to the distribution of massive stars, showing that we indeed detect interstellar bubbles without large spatial bias. Eighteen out of 59 supernova remnants in the Large Magellanic Cloud (LMC) and 13 out of 20 superbubbles are detected in at least one wavelength. The lack of detection is mostly due to surrounding emission that disturbs the detection, a too small size, or the lack of a (circular) counterpart in our emission line images. In line-density maps at larger scales, maxima can be found in regions with high star formation in the past, often inside supergiant shells (SGS). In SGS LMC 2, there is a maximum west of the shell where a collision of large gas clouds is thought to have occurred. In the Small Magellanic Cloud (SMC), bubble detection is impaired by the more complex projected structure of the galaxy. Line maps at large scales show large filaments in the SMC in a north-south direction, especially in the [S II] image. The origin of these filaments is unknown.

show abstract

Multiwavelength analysis of the X-ray spur and southeast of the Large Magellanic Cloud

Cited by 9 publications

References 50 publications

First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

Diffuse Hot Plasma in the Interstellar Medium and Galactic Outflows

Tracking down the origin of superbubbles and supergiant shells in the Magellanic Clouds with Minkowski tensor analysis

Contact Info

Product

Resources

About