Large expanding molecular arc in the Sagittarius Bl complex

Kunihiko Tanaka, Tomoharu Oka, Makoto Nagai, Kazuhisa Kamegai

Research output: Contribution to journalArticle

14 Citations (Scopus)

Abstract

Results of molecular line observations toward the Sagittarius B1 complex are reported. Maps of the HCN, HCO + and SiO J = 1-0 emissions were taken with the NRO 45-m telescope. With these data, combined with the ASTE CO J = 3-2 survey data, we have investigated the spatial structure, kinematics and physical conditions of two peculiar molecular features: CO0.55+0.07 and SiO0.56-0.01. The CO arc, CO0.55+0.07, shows clear expanding motion with sizes of 8.5 × 6.8 pc 2 and an expansion velocity of 40 km s -1. The SiO shell, SiO0.56-0.01, has a size of 3.0×3.4 pc 2, and surrounds an X-ray Fe line source, GO.570-0.018. The mass and the kinetic energy of CO0.55+0.07 are estimated to be 10 5.5M⊙ and 10 51.5erg, respectively. The kinetic energy of SiO0.56-0.01 is ∼ 10 50.4erg. An LVG analysis shows that the typical density and kinetic temperature are 10 3.8 cm -3 and 28 K, respectively. High-density clumps with a density of 10 4.0-4.5 cm -3 associated with CO0.55+0.07 and SiO0.56-0.01 have been found, supporting the idea that they consist of swept-up material. The huge kinetic energy of CO0.55+0.07 is considered to be injected by a series of supernova explosions that took place within ∼ 2× 10 5yr, which would suggest that it is a 'bubble' created by a massive stellar cluster, whose mass is estimated to be 10 3.5-4.5 M⊙. The origin of SiO0.56-0.01 is rather unclear, but we suggest that it could be related to the X-ray source G0.570-0.018.

Original languageEnglish
Pages (from-to)461-469
Number of pages9
JournalPublications of the Astronomical Society of Japan
Volume61
Issue number3
Publication statusPublished - 2009

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kinetic energy
arcs
clumps
supernovae
explosions
bubble
explosion
x rays
kinematics
bubbles
telescopes
shell
kinetics
expansion
temperature
line source
material
physical conditions
analysis

Keywords

  • Galaxy: center
  • ISM: bubbles
  • ISM: clouds

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Large expanding molecular arc in the Sagittarius Bl complex. / Tanaka, Kunihiko; Oka, Tomoharu; Nagai, Makoto; Kamegai, Kazuhisa.

In: Publications of the Astronomical Society of Japan, Vol. 61, No. 3, 2009, p. 461-469.

Research output: Contribution to journalArticle

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abstract = "Results of molecular line observations toward the Sagittarius B1 complex are reported. Maps of the HCN, HCO + and SiO J = 1-0 emissions were taken with the NRO 45-m telescope. With these data, combined with the ASTE CO J = 3-2 survey data, we have investigated the spatial structure, kinematics and physical conditions of two peculiar molecular features: CO0.55+0.07 and SiO0.56-0.01. The CO arc, CO0.55+0.07, shows clear expanding motion with sizes of 8.5 × 6.8 pc 2 and an expansion velocity of 40 km s -1. The SiO shell, SiO0.56-0.01, has a size of 3.0×3.4 pc 2, and surrounds an X-ray Fe line source, GO.570-0.018. The mass and the kinetic energy of CO0.55+0.07 are estimated to be 10 5.5M⊙ and 10 51.5erg, respectively. The kinetic energy of SiO0.56-0.01 is ∼ 10 50.4erg. An LVG analysis shows that the typical density and kinetic temperature are 10 3.8 cm -3 and 28 K, respectively. High-density clumps with a density of 10 4.0-4.5 cm -3 associated with CO0.55+0.07 and SiO0.56-0.01 have been found, supporting the idea that they consist of swept-up material. The huge kinetic energy of CO0.55+0.07 is considered to be injected by a series of supernova explosions that took place within ∼ 2× 10 5yr, which would suggest that it is a 'bubble' created by a massive stellar cluster, whose mass is estimated to be 10 3.5-4.5 M⊙. The origin of SiO0.56-0.01 is rather unclear, but we suggest that it could be related to the X-ray source G0.570-0.018.",
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AU - Tanaka, Kunihiko

AU - Oka, Tomoharu

AU - Nagai, Makoto

AU - Kamegai, Kazuhisa

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N2 - Results of molecular line observations toward the Sagittarius B1 complex are reported. Maps of the HCN, HCO + and SiO J = 1-0 emissions were taken with the NRO 45-m telescope. With these data, combined with the ASTE CO J = 3-2 survey data, we have investigated the spatial structure, kinematics and physical conditions of two peculiar molecular features: CO0.55+0.07 and SiO0.56-0.01. The CO arc, CO0.55+0.07, shows clear expanding motion with sizes of 8.5 × 6.8 pc 2 and an expansion velocity of 40 km s -1. The SiO shell, SiO0.56-0.01, has a size of 3.0×3.4 pc 2, and surrounds an X-ray Fe line source, GO.570-0.018. The mass and the kinetic energy of CO0.55+0.07 are estimated to be 10 5.5M⊙ and 10 51.5erg, respectively. The kinetic energy of SiO0.56-0.01 is ∼ 10 50.4erg. An LVG analysis shows that the typical density and kinetic temperature are 10 3.8 cm -3 and 28 K, respectively. High-density clumps with a density of 10 4.0-4.5 cm -3 associated with CO0.55+0.07 and SiO0.56-0.01 have been found, supporting the idea that they consist of swept-up material. The huge kinetic energy of CO0.55+0.07 is considered to be injected by a series of supernova explosions that took place within ∼ 2× 10 5yr, which would suggest that it is a 'bubble' created by a massive stellar cluster, whose mass is estimated to be 10 3.5-4.5 M⊙. The origin of SiO0.56-0.01 is rather unclear, but we suggest that it could be related to the X-ray source G0.570-0.018.

AB - Results of molecular line observations toward the Sagittarius B1 complex are reported. Maps of the HCN, HCO + and SiO J = 1-0 emissions were taken with the NRO 45-m telescope. With these data, combined with the ASTE CO J = 3-2 survey data, we have investigated the spatial structure, kinematics and physical conditions of two peculiar molecular features: CO0.55+0.07 and SiO0.56-0.01. The CO arc, CO0.55+0.07, shows clear expanding motion with sizes of 8.5 × 6.8 pc 2 and an expansion velocity of 40 km s -1. The SiO shell, SiO0.56-0.01, has a size of 3.0×3.4 pc 2, and surrounds an X-ray Fe line source, GO.570-0.018. The mass and the kinetic energy of CO0.55+0.07 are estimated to be 10 5.5M⊙ and 10 51.5erg, respectively. The kinetic energy of SiO0.56-0.01 is ∼ 10 50.4erg. An LVG analysis shows that the typical density and kinetic temperature are 10 3.8 cm -3 and 28 K, respectively. High-density clumps with a density of 10 4.0-4.5 cm -3 associated with CO0.55+0.07 and SiO0.56-0.01 have been found, supporting the idea that they consist of swept-up material. The huge kinetic energy of CO0.55+0.07 is considered to be injected by a series of supernova explosions that took place within ∼ 2× 10 5yr, which would suggest that it is a 'bubble' created by a massive stellar cluster, whose mass is estimated to be 10 3.5-4.5 M⊙. The origin of SiO0.56-0.01 is rather unclear, but we suggest that it could be related to the X-ray source G0.570-0.018.

KW - Galaxy: center

KW - ISM: bubbles

KW - ISM: clouds

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