The Kinematic Map of the Ionized Gas of the Supergiant Shell LMC SGS 2

Ambrocio-Cruz, P.; Laval, A.; Rosado, M.; Georgelin, Y. P.; Marcelin, M.; Comerón, F.; Delmotte, N.; Viale, A.

doi:10.1086/382093

Cited by 8 publications

(7 citation statements)

References 5 publications

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“…They obtain a spectral index of α = −0.45 ± 0.03, which is confirmed by Gao et al (2011) (α = −0.47 ± 0.04). According to the X-ray and optical studies, the SNR is probably evolving in low-density environment (Leahy 1986;Ambrocio-Cruz et al 2014). Based on a large CO map in the direction of G206.9+2.3, Su et al (2017) detected a molecular gas cavity in the region where the remnant located.…”

Section: G2069+23 Pks 0646+06mentioning

confidence: 99%

Three-dimensional dust mapping of 12 supernovae remnants in the Galactic anticentre

Chen

Jiang

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present three dimensional (3D) dust mapping of 12 supernova remnants (SNRs) in the Galactic anti-center (Galactic longitude l between 150 • and 210 • ) based on a recent 3D interstellar extinction map. The dust distribution of the regions which cover the full extents in the radio continuum for the individual SNRs are discussed. Four SNRs show significant spatial coincidences between molecular clouds (MCs) revealed from the 3D extinction mapping and the corresponding radio features. The results confirm the interactions between these SNRs and their surrounding MCs. Based on these correlations, we provide new distance estimates of the four SNRs, G189.1+3.0 (IC443, d = 1729 +116 −94 pc), G190.9-2.2 (d = 1036 +17 −81 pc), G205.5+0.5 (d = 941 +96 −94 or 1257 +92 −101 pc) and G213.0-0.6 (d = 1146 +79 −80 pc). In addition, we find indirect evidences of potential interactions between SNRs and MCs for three other SNRs. New distance constraints are also given for these three SNRs.

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Section: G2069+23 Pks 0646+06mentioning

confidence: 99%

Three-dimensional dust mapping of 12 supernovae remnants in the Galactic anticentre

Chen

Jiang

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Given its age, ∼15 Myr (Cassatella et al 1996), Points et al (1999) has postulated that all of NGC 2100's O stars have exploded as supernovae, implying that it has played an important role in shaping the observed structure of LMC 2. Points et al (1999) and Ambrocio-Cruz et al (2004) observed complex Hα velocity components which vary across the extent of NGC 2100, suggesting the presence of a turbulent interstellar environment. The interstellar polarization near NGC 2100 is also known to differ from general behavior of the LMC (0.32 -0.57% at position angles of 28-45 • , Wisniewski 2005;Wisniewski et al 2007); Mathewson & Ford (1970b) observed a strong focusing of magnetic lines around 30 Doradus (30 Dor), which is located ∼16.…”

Section: Introductionmentioning

confidence: 99%

“…With a diameter of ∼ 900 pc, LMC 2 was initially identified as a supershell based upon its morphology (Meaburn 1980). The kinematics of the LMC 2 supershell has been a subject of some debate: Caulet et al (1982) suggested that LMC 2 was expanding as a cohesive structure; however, followup studies by Meaburn et al (1987), Points et al (1999) and Ambrocio-Cruz et al (2004) argue against a global expansion, asserting the structure is a conglomeration of localized expanding structures. Observed extended X-ray emission in the region led Wang & Helfand (1991) to suggest that LMC 2 was formed as a result of a superbubble breaking out from the plane of the Large Magellanic Cloud (LMC).…”

Section: Introductionmentioning

confidence: 99%

The Magnetic Field Structure of the LMC 2 Supershell: NGC 2100

Wisniewski¹,

Bjorkman²,

Magalhães³

et al. 2007

ApJ

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We present U,B,V,R,I imaging polarimetry of NGC 2100 and its surrounding environment, which comprise a part of the LMC 2 supershell. The morphology of the observed position angle distribution provides a tracer of the projected magnetic field in this environment. Our polarization maps detail regions exhibiting similarly aligned polarization position angles, as well as more complex position angle patterns. We observe regions of coherent fields on spatial scales of 42 x 24 pc to 104 x 83 pc, and infer projected field strengths of ∼14-30µG. We propose that the superposition of global outflows from the LMC 2 environment, as well as outflows created within NGC 2100, produce the unique field geometry in the region.

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“…Therefore, we were able to spatially study the different morphology of the velocity profiles from the central part of the galaxy (see Section 3.1.1). On the other hand, the morphology of the SNRs velocity profiles, which are fitted with three components, is related to the systemic velocity of the galaxy represented by the main velocity component, and to the shell expansion morphology represented by the secondary components (see Ambrocio-Cruz et al 2004, Figure 5). The VF shows that the Hα emitting gas does not seem to follow circular rotation, and that the gas motions are dis-ordered due to the presence of the superbubbles and SNRs hosted in this galaxy.…”

Section: Profile Fittingmentioning

confidence: 99%

A kinematical study of the dwarf irregular galaxy NGC 1569 and its supernova remnants

Sánchez-Cruces

Sardaneta

Fuentes-Carrera

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present Fabry-Pérot observations in the Hα and [S ii] lines to study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569, these observations allowed us to computed the Hα velocity field of this galaxy. Doing a detailed analysis of the velocity along the line-of-sight and Hα velocity profiles, we identified the origin of most of the motions in the innermost parts of the galaxy and discarded the possibility of deriving a rotation curve that traces the gravitational well of the galaxy. We analysed the kinematics of the ionised gas around 31 supernova remnants previously detected in NGC 1569 by other authors, in optical and radio emission. We found that the Hα velocity profiles of the supernova remnants are complex indicating the presence of shocks. Fitting these profiles with several Gaussian functions, we computed their expansion velocities which rank from 87 to 188 km s−1 confirming they are supernova remnants. Also, we determined the physical properties such as electron density, mechanical energy, and kinematic age for 30 of the 31 supernova remnants and found they are in the radiative phase with an energy range from 1 to 39 × 1050 erg s−1 and an age from 2.3 to 8.9 × 104 yr. Finally, we estimated the Surface Brightness - Diameter (Σ-D) Relation for NGC 1569 and obtained a slope β = 1.26 ± 0.2, comparable with the β value obtained for supernova remnants in galaxies M31 and M33.

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The Kinematic Map of the Ionized Gas of the Supergiant Shell LMC SGS 2

Cited by 8 publications

References 5 publications

Three-dimensional dust mapping of 12 supernovae remnants in the Galactic anticentre

Three-dimensional dust mapping of 12 supernovae remnants in the Galactic anticentre

The Magnetic Field Structure of the LMC 2 Supershell: NGC 2100

A kinematical study of the dwarf irregular galaxy NGC 1569 and its supernova remnants

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