The Galactic Center Lobe as an H ii Region
The Galactic center lobe (GCL) is an object ∼1° across that is located north of the Galactic center. In the mid-infrared (MIR) the GCL appears as two 8.0 μm filaments between which there is strong 24 μm and radio continuum emission. Due to its morphology and location in the sky, previous authors hav...
| Main Authors: | , , , , , , , |
|---|---|
| Format: | Journal Article |
| Published: |
2024
|
| Online Access: | http://purl.org/au-research/grants/arc/FT190100231 http://hdl.handle.net/20.500.11937/96299 |
| _version_ | 1848766131351846912 |
|---|---|
| author | Anderson, Loren Luisi, M. Liu, B. Linville, D.J. Benjamin, R.A. Hurley-Walker, Natasha McClure-Griffiths, N.M. Zucker, C. |
| author_facet | Anderson, Loren Luisi, M. Liu, B. Linville, D.J. Benjamin, R.A. Hurley-Walker, Natasha McClure-Griffiths, N.M. Zucker, C. |
| author_sort | Anderson, Loren |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | The Galactic center lobe (GCL) is an object ∼1° across that is located north of the Galactic center. In the mid-infrared (MIR) the GCL appears as two 8.0 μm filaments between which there is strong 24 μm and radio continuum emission. Due to its morphology and location in the sky, previous authors have argued that the GCL is located in the Galactic center region, created by outflows from star formation or by activity of the central black hole Sagittarius A*. In an associated paper, low-frequency radio emission indicates that the GCL must instead lie foreground to the Galactic center. If the GCL is foreground to the Galactic center, it is likely to be a type of object common throughout the Galactic disk; we here investigate whether its properties are similar to those of Galactic H ii regions. We find that the GCL’s MIR morphology, MIR flux densities, dust temperatures, and radio recombination line properties as traced by the Green Bank Telescope Diffuse Ionized Gas Survey are consistent with those of known Galactic H ii regions, although the derived electron temperature is low. We search for the ionizing source(s) of the possible H ii region and identify a stellar cluster candidate (Camargo #1092/Ryu & Lee #532) and a cluster of young stellar objects (the SPICY cluster G359.3+0.3) whose members have Gaia parallaxes distances of 1.7 ± 0.4 kpc. Taken together, the results of our companion paper and those shown here suggest that the GCL has properties consistent with those of an H ii region located ∼2 kpc from the Sun. |
| first_indexed | 2025-11-14T11:46:16Z |
| format | Journal Article |
| id | curtin-20.500.11937-96299 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T11:46:16Z |
| publishDate | 2024 |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-962992024-12-17T01:36:43Z The Galactic Center Lobe as an H ii Region Anderson, Loren Luisi, M. Liu, B. Linville, D.J. Benjamin, R.A. Hurley-Walker, Natasha McClure-Griffiths, N.M. Zucker, C. The Galactic center lobe (GCL) is an object ∼1° across that is located north of the Galactic center. In the mid-infrared (MIR) the GCL appears as two 8.0 μm filaments between which there is strong 24 μm and radio continuum emission. Due to its morphology and location in the sky, previous authors have argued that the GCL is located in the Galactic center region, created by outflows from star formation or by activity of the central black hole Sagittarius A*. In an associated paper, low-frequency radio emission indicates that the GCL must instead lie foreground to the Galactic center. If the GCL is foreground to the Galactic center, it is likely to be a type of object common throughout the Galactic disk; we here investigate whether its properties are similar to those of Galactic H ii regions. We find that the GCL’s MIR morphology, MIR flux densities, dust temperatures, and radio recombination line properties as traced by the Green Bank Telescope Diffuse Ionized Gas Survey are consistent with those of known Galactic H ii regions, although the derived electron temperature is low. We search for the ionizing source(s) of the possible H ii region and identify a stellar cluster candidate (Camargo #1092/Ryu & Lee #532) and a cluster of young stellar objects (the SPICY cluster G359.3+0.3) whose members have Gaia parallaxes distances of 1.7 ± 0.4 kpc. Taken together, the results of our companion paper and those shown here suggest that the GCL has properties consistent with those of an H ii region located ∼2 kpc from the Sun. 2024 Journal Article http://hdl.handle.net/20.500.11937/96299 10.3847/1538-4357/ad4d93 http://purl.org/au-research/grants/arc/FT190100231 http://creativecommons.org/licenses/by/4.0/ fulltext |
| spellingShingle | Anderson, Loren Luisi, M. Liu, B. Linville, D.J. Benjamin, R.A. Hurley-Walker, Natasha McClure-Griffiths, N.M. Zucker, C. The Galactic Center Lobe as an H ii Region |
| title | The Galactic Center Lobe as an H ii Region |
| title_full | The Galactic Center Lobe as an H ii Region |
| title_fullStr | The Galactic Center Lobe as an H ii Region |
| title_full_unstemmed | The Galactic Center Lobe as an H ii Region |
| title_short | The Galactic Center Lobe as an H ii Region |
| title_sort | galactic center lobe as an h ii region |
| url | http://purl.org/au-research/grants/arc/FT190100231 http://hdl.handle.net/20.500.11937/96299 |