High-resolution CO ( J = 1–0) and ( J = 3–2) Observations of Molecular Counterparts to the Double Helix Nebula in the Galactic Center
- 1National Astronomical Observatory of Japan
- 2University of Tsukuba
- 3Nagoya University
Abstract
The Double Helix Nebula (DHN) is a peculiar infrared nebula that exhibits two intertwined helical strands at b ∼ 0 . ° 7 . Since two candidates for its molecular counterparts at 0 and −35 km s ⁻¹ extend from the central ∼10 pc of the Galactic center, and magnetic field lines aligned with the infrared DHN have been measured, a scenario in which a magnetic tower anchored to the circumnuclear disk has been proposed. In this paper, we present results from new observations of CO( J = 1–0) and ¹² CO( J = 3–2) obtained with the Nobeyama Radio Observatory 45 m telescope and the Atacama Submillimeter Telescope Experiment. We find robust evidence that the 0 km s ⁻¹ component is associated with the DHN and is located in the Galactic center. In contrast, the −35 km s ⁻¹ component exhibits line intensity ratios typically seen in foreground molecular clouds. The favored molecular counterpart is resolved into 11 dense, elongated clumps whose typical sizes, line widths, and column densities are 1–2 pc, ∼2 km s ⁻¹ , and 10 ²¹ –10 ²² cm ⁻² , respectively. Within the framework of the magnetic tower model, we discuss how these clumps are formed through interactions between dense H I blobs and associated bow shocks.
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BibTeX
@article{enokiya2026highresolution,
title = {{High-resolution CO ( J = 1–0) and ( J = 3–2) Observations of Molecular Counterparts to the Double Helix Nebula in the Galactic Center}},
author = {Rei Enokiya and Yuta Asahina and Yasuo Fukui},
journal = {The Astrophysical Journal},
year = {2026},
month = oct,
doi = {10.3847/1538-4357/ae9f4e},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/ae9f4e},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - High-resolution CO ( J = 1–0) and ( J = 3–2) Observations of Molecular Counterparts to the Double Helix Nebula in the Galactic Center
AU - Rei Enokiya
AU - Yuta Asahina
AU - Yasuo Fukui
PY - 2026
DA - 2026/10/15
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/ae9f4e
UR - https://iopscience.iop.org/article/10.3847/1538-4357/ae9f4e
AB - The Double Helix Nebula (DHN) is a peculiar infrared nebula that exhibits two intertwined helical strands at b ∼ 0 . ° 7 . Since two candidates for its molecular counterparts at 0 and −35 km s ⁻¹ extend from the central ∼10 pc of the Galactic center, and magnetic field lines aligned with the infrared DHN have been measured, a scenario in which a magnetic tower anchored to the circumnuclear disk has been proposed. In this paper, we present results from new observations of CO( J = 1–0) and ¹² CO( J = 3–2) obtained with the Nobeyama Radio Observatory 45 m telescope and the Atacama Submillimeter Telescope Experiment. We find robust evidence that the 0 km s ⁻¹ component is associated with the DHN and is located in the Galactic center. In contrast, the −35 km s ⁻¹ component exhibits line intensity ratios typically seen in foreground molecular clouds. The favored molecular counterpart is resolved into 11 dense, elongated clumps whose typical sizes, line widths, and column densities are 1–2 pc, ∼2 km s ⁻¹ , and 10 ²¹ –10 ²² cm ⁻² , respectively. Within the framework of the magnetic tower model, we discuss how these clumps are formed through interactions between dense H I blobs and associated bow shocks.
SN - 0004-637X
SN - 1538-4357
ER -