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dc.contributor.authorAnderson, L.D.
dc.contributor.authorLuisi, M.
dc.contributor.authorLiu, B.
dc.contributor.authorLinville, D.J.
dc.contributor.authorBenjamin, R.A.
dc.contributor.authorHurley-Walker, Natasha
dc.contributor.authorMcClure-Griffiths, N.M.
dc.contributor.authorZucker, C.
dc.date.accessioned2024-11-06T09:50:23Z
dc.date.available2024-11-06T09:50:23Z
dc.date.issued2024
dc.identifier.citationAnderson, L.D. and Luisi, M. and Liu, B. and Linville, D.J. and Benjamin, R.A. and Hurley-Walker, N. and McClure-Griffiths, N.M. et al. 2024. The Galactic Center Lobe as an H ii Region. Astrophysical Journal. 969 (1).
dc.identifier.urihttp://hdl.handle.net/20.500.11937/96299
dc.identifier.doi10.3847/1538-4357/ad4d93
dc.description.abstract

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.

dc.titleThe Galactic Center Lobe as an H ii Region
dc.typeJournal Article
dcterms.source.volume969
dcterms.source.number1
dcterms.source.issn0004-637X
dcterms.source.titleAstrophysical Journal
dc.date.updated2024-11-06T09:50:23Z
curtin.departmentSchool of Elec Eng, Comp and Math Sci (EECMS)
curtin.accessStatusIn process
curtin.facultyFaculty of Science and Engineering
curtin.contributor.orcidHurley-Walker, Natasha [0000-0002-5119-4808]
curtin.contributor.researcheridHurley-Walker, Natasha [B-9520-2013] [P-6494-2019]
dcterms.source.eissn1538-4357
curtin.contributor.scopusauthoridHurley-Walker, Natasha [23972734500]
curtin.repositoryagreementV3


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