ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells

Y. Yamane, H. Sano, J. Th Van Loon, M. D. Filipović, K. Fujii, K. Tokuda, K. Tsuge, T. Nagaya, S. Yoshiike, K. Grieve, F. Voisin, G. Rowell, R. Indebetouw, M. Lakićević, T. Temim, L. Staveley-Smith, J. Rho, K. S. Long, S. Park, J. Seok & 7 others N. Mizuno, A. Kawamura, T. Onishi, T. Inoue, S. Inutsuka, K. Tachihara, Y. Fukui

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Abstract

N49 (LHA 120-N49) is a bright X-ray supernova remnant (SNR) in the Large Magellanic Cloud. We present new 12CO (J = 1-0, 3-2), H i, and 1.4 GHz radio continuum observations of the SNR N49 using Mopra, ASTE, ALMA, and ATCA. We have newly identified three H i clouds using ATCA with an angular resolution of ∼20″: one associated with the SNR and the others located in front of the SNR. Both the CO and H i clouds in the velocity range from 281 to 291 km s-1 are spatially correlated with both the soft X-rays (0.2-1.2 keV) and the hard X-rays (2.0-7.0 keV) of N49 on a ∼10 pc scale. CO 3-2/1-0 intensity ratios indicate higher values of the CO cloud toward the SNR shell with an angular resolution of ∼45″, and thus a strong interaction was suggested. Using the ALMA, we have spatially resolved CO clumps embedded within or along the southeastern rim of N49 with an angular resolution of ∼3″. Three of the CO clumps are rim brightened on a 0.7-2 pc scale in both hard X-rays and the radio continuum: this provides further evidence for dynamical interactions between the CO clumps and the SNR shock wave. The enhancement of the radio synchrotron radiation can be understood in terms of magnetic field amplification around the CO clumps via a shock-cloud interaction. We also present a possible scenario in which the recombining plasma that dominates the hard X-rays from N49 was formed via thermal conduction between the SNR shock waves and the cold/dense molecular clumps.

Original languageEnglish
Article number55
JournalAstrophysical Journal
Volume863
Issue number1
DOIs
Publication statusPublished - 10 Aug 2018

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clumps
supernova remnants
shell
radio
continuums
angular resolution
shock wave
x rays
rims
shock waves
amplification
Magellanic clouds
magnetic field
plasma
synchrotron radiation
shock
interactions
conduction
augmentation
magnetic fields

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Yamane, Y. ; Sano, H. ; Van Loon, J. Th ; Filipović, M. D. ; Fujii, K. ; Tokuda, K. ; Tsuge, K. ; Nagaya, T. ; Yoshiike, S. ; Grieve, K. ; Voisin, F. ; Rowell, G. ; Indebetouw, R. ; Lakićević, M. ; Temim, T. ; Staveley-Smith, L. ; Rho, J. ; Long, K. S. ; Park, S. ; Seok, J. ; Mizuno, N. ; Kawamura, A. ; Onishi, T. ; Inoue, T. ; Inutsuka, S. ; Tachihara, K. ; Fukui, Y. / ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells. In: Astrophysical Journal. 2018 ; Vol. 863, No. 1.
@article{cd494148041046eb892a80822b1515c4,
title = "ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells",
abstract = "N49 (LHA 120-N49) is a bright X-ray supernova remnant (SNR) in the Large Magellanic Cloud. We present new 12CO (J = 1-0, 3-2), H i, and 1.4 GHz radio continuum observations of the SNR N49 using Mopra, ASTE, ALMA, and ATCA. We have newly identified three H i clouds using ATCA with an angular resolution of ∼20″: one associated with the SNR and the others located in front of the SNR. Both the CO and H i clouds in the velocity range from 281 to 291 km s-1 are spatially correlated with both the soft X-rays (0.2-1.2 keV) and the hard X-rays (2.0-7.0 keV) of N49 on a ∼10 pc scale. CO 3-2/1-0 intensity ratios indicate higher values of the CO cloud toward the SNR shell with an angular resolution of ∼45″, and thus a strong interaction was suggested. Using the ALMA, we have spatially resolved CO clumps embedded within or along the southeastern rim of N49 with an angular resolution of ∼3″. Three of the CO clumps are rim brightened on a 0.7-2 pc scale in both hard X-rays and the radio continuum: this provides further evidence for dynamical interactions between the CO clumps and the SNR shock wave. The enhancement of the radio synchrotron radiation can be understood in terms of magnetic field amplification around the CO clumps via a shock-cloud interaction. We also present a possible scenario in which the recombining plasma that dominates the hard X-rays from N49 was formed via thermal conduction between the SNR shock waves and the cold/dense molecular clumps.",
keywords = "cosmic rays, ISM: clouds, ISM: molecules, ISM: supernova remnants, X-rays: individual (LHA 120-N49)",
author = "Y. Yamane and H. Sano and {Van Loon}, {J. Th} and Filipović, {M. D.} and K. Fujii and K. Tokuda and K. Tsuge and T. Nagaya and S. Yoshiike and K. Grieve and F. Voisin and G. Rowell and R. Indebetouw and M. Lakićević and T. Temim and L. Staveley-Smith and J. Rho and Long, {K. S.} and S. Park and J. Seok and N. Mizuno and A. Kawamura and T. Onishi and T. Inoue and S. Inutsuka and K. Tachihara and Y. Fukui",
year = "2018",
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doi = "10.3847/1538-4357/aacfff",
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Yamane, Y, Sano, H, Van Loon, JT, Filipović, MD, Fujii, K, Tokuda, K, Tsuge, K, Nagaya, T, Yoshiike, S, Grieve, K, Voisin, F, Rowell, G, Indebetouw, R, Lakićević, M, Temim, T, Staveley-Smith, L, Rho, J, Long, KS, Park, S, Seok, J, Mizuno, N, Kawamura, A, Onishi, T, Inoue, T, Inutsuka, S, Tachihara, K & Fukui, Y 2018, 'ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells' Astrophysical Journal, vol. 863, no. 1, 55. https://doi.org/10.3847/1538-4357/aacfff

ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells. / Yamane, Y.; Sano, H.; Van Loon, J. Th; Filipović, M. D.; Fujii, K.; Tokuda, K.; Tsuge, K.; Nagaya, T.; Yoshiike, S.; Grieve, K.; Voisin, F.; Rowell, G.; Indebetouw, R.; Lakićević, M.; Temim, T.; Staveley-Smith, L.; Rho, J.; Long, K. S.; Park, S.; Seok, J.; Mizuno, N.; Kawamura, A.; Onishi, T.; Inoue, T.; Inutsuka, S.; Tachihara, K.; Fukui, Y.

In: Astrophysical Journal, Vol. 863, No. 1, 55, 10.08.2018.

Research output: Contribution to journalArticle

TY - JOUR

T1 - ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells

AU - Yamane, Y.

AU - Sano, H.

AU - Van Loon, J. Th

AU - Filipović, M. D.

AU - Fujii, K.

AU - Tokuda, K.

AU - Tsuge, K.

AU - Nagaya, T.

AU - Yoshiike, S.

AU - Grieve, K.

AU - Voisin, F.

AU - Rowell, G.

AU - Indebetouw, R.

AU - Lakićević, M.

AU - Temim, T.

AU - Staveley-Smith, L.

AU - Rho, J.

AU - Long, K. S.

AU - Park, S.

AU - Seok, J.

AU - Mizuno, N.

AU - Kawamura, A.

AU - Onishi, T.

AU - Inoue, T.

AU - Inutsuka, S.

AU - Tachihara, K.

AU - Fukui, Y.

PY - 2018/8/10

Y1 - 2018/8/10

N2 - N49 (LHA 120-N49) is a bright X-ray supernova remnant (SNR) in the Large Magellanic Cloud. We present new 12CO (J = 1-0, 3-2), H i, and 1.4 GHz radio continuum observations of the SNR N49 using Mopra, ASTE, ALMA, and ATCA. We have newly identified three H i clouds using ATCA with an angular resolution of ∼20″: one associated with the SNR and the others located in front of the SNR. Both the CO and H i clouds in the velocity range from 281 to 291 km s-1 are spatially correlated with both the soft X-rays (0.2-1.2 keV) and the hard X-rays (2.0-7.0 keV) of N49 on a ∼10 pc scale. CO 3-2/1-0 intensity ratios indicate higher values of the CO cloud toward the SNR shell with an angular resolution of ∼45″, and thus a strong interaction was suggested. Using the ALMA, we have spatially resolved CO clumps embedded within or along the southeastern rim of N49 with an angular resolution of ∼3″. Three of the CO clumps are rim brightened on a 0.7-2 pc scale in both hard X-rays and the radio continuum: this provides further evidence for dynamical interactions between the CO clumps and the SNR shock wave. The enhancement of the radio synchrotron radiation can be understood in terms of magnetic field amplification around the CO clumps via a shock-cloud interaction. We also present a possible scenario in which the recombining plasma that dominates the hard X-rays from N49 was formed via thermal conduction between the SNR shock waves and the cold/dense molecular clumps.

AB - N49 (LHA 120-N49) is a bright X-ray supernova remnant (SNR) in the Large Magellanic Cloud. We present new 12CO (J = 1-0, 3-2), H i, and 1.4 GHz radio continuum observations of the SNR N49 using Mopra, ASTE, ALMA, and ATCA. We have newly identified three H i clouds using ATCA with an angular resolution of ∼20″: one associated with the SNR and the others located in front of the SNR. Both the CO and H i clouds in the velocity range from 281 to 291 km s-1 are spatially correlated with both the soft X-rays (0.2-1.2 keV) and the hard X-rays (2.0-7.0 keV) of N49 on a ∼10 pc scale. CO 3-2/1-0 intensity ratios indicate higher values of the CO cloud toward the SNR shell with an angular resolution of ∼45″, and thus a strong interaction was suggested. Using the ALMA, we have spatially resolved CO clumps embedded within or along the southeastern rim of N49 with an angular resolution of ∼3″. Three of the CO clumps are rim brightened on a 0.7-2 pc scale in both hard X-rays and the radio continuum: this provides further evidence for dynamical interactions between the CO clumps and the SNR shock wave. The enhancement of the radio synchrotron radiation can be understood in terms of magnetic field amplification around the CO clumps via a shock-cloud interaction. We also present a possible scenario in which the recombining plasma that dominates the hard X-rays from N49 was formed via thermal conduction between the SNR shock waves and the cold/dense molecular clumps.

KW - cosmic rays

KW - ISM: clouds

KW - ISM: molecules

KW - ISM: supernova remnants

KW - X-rays: individual (LHA 120-N49)

UR - http://www.scopus.com/inward/record.url?scp=85051460860&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aacfff

DO - 10.3847/1538-4357/aacfff

M3 - Article

VL - 863

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 55

ER -