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• W3100250767 abstract "Fukui et al. (2006, Science, 314, 106) discovered two huge molecular loops in the galactic center located at (⁠|$l, b$|⁠) |$simeq$| (355|$^circ$|–359|$^circ$|⁠, 0|$^circ$|–2|$^circ$|⁠) in a large velocity range of |$-$|180—40 km s|$^{-1}$|⁠. Following the discovery, we present detailed observational properties of the two loops based on NANTEN |$^{12}$|CO (⁠|$J =$| 1–0) and |$^{13}$|CO (⁠|$J =$| 1–0) datasets at 10 pc resolution, including a complete set of velocity channel distributions and comparisons with HI and dust emissions as well as with the other broad molecular features. We have found new features on smaller scales in the loops, including helical distributions in the loop tops and vertical spurs. The loops have counterparts of the HI gas, indicating that the loops include atomic gas. The IRAS far-infrared emission is also associated with the loops, and was used to derive an X-factor of 0.7 (⁠|$pm$| 0.1) |$times$| 10|$^{20} $|cm|$^{-2}$| (K km s|$^{-1}$|⁠)|$^{-1}$| to convert the |$^{12}$|CO intensity into the total molecular hydrogen column density. From the |$^{12}$|CO, |$^{13}$|CO, HI, and dust datasets we estimated the total mass of loops 1 and 2 to be |$sim $|1.4 |$times$| 10|$^6$||$M_odot$| and |$sim $|1.9 |$times$| 10|$^6$||$M_odot$|⁠, respectively, where the HI mass corresponds to |$sim $|10%–20% of the total mass and the total kinetic energy of the two loops is |$sim $|10|$^{52} $|erg. An analysis of the kinematics of the loops yields that the loops are rotating at |$sim $|47 km s|$^{-1}$| and expanding at |$sim $|141 km s|$^{-1}$| at a radius of |$sim $|670 pc from the center. Fukui et al. (2006) presented a model that the loops are created by magnetic flotation due to the Parker instability with an estimated magnetic field strength of |$sim $|150|$ mu$|G. We present comparisons with the recent numerical simulations of the magnetized nuclear disk by Machida et al. (2009, PASJ, 61, 411) and Takahashi et al. (2009, PASJ, 61, 957), and show that the theoretical results are in good agreement with the observations. The helical distributions also suggest that some magnetic instability plays a role similarly to the solar helical features." @default.
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• W3100250767 date "2010-10-25" @default.
• W3100250767 modified "2023-10-18" @default.
• W3100250767 title "A Detailed Observational Study of Molecular Loops 1 and 2 in the Galactic Center" @default.
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• W3100250767 doi "https://doi.org/10.1093/pasj/62.5.1307" @default.
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