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Peer-reviewedCC BY 4.0The Astrophysical Journal

JWST View of the Supernebula in NGC 5253. I. Overview and Continuum Features

  • Jean L. Turner1
  • Sara C. Beck2
  • Elm Zweig1
  • L. Barcos-Muñoz3,4
  • John H. Black5
  • Daniel P. Cohen1
  • S. Michelle Consiglio1
  • Nicholas G. Ferraro1
  • Paul T. P. Ho6
  • David S. Meier7
7 affiliations
  1. 1University of California, Los Angeles
  2. 2Tel Aviv University
  3. 3National Radio Astronomy Observatory
  4. 4University of Virginia
  5. 5Chalmers Institute of Technology
  6. 6Academia Sinica Astronomy and Astrophysics
  7. 7New Mexico Institute of Mining and Technology
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Abstract

We present 5–28 μ m imaging spectroscopy of the “supernebula” in the dwarf galaxy NGC 5253 made with the JWST/MIRI/Medium Resolution Spectrometer integral field spectrometer. NGC 5253 hosts a luminous ( L ∼ 10 ⁹ L ⊙ ) H II region, powered by a giant young star cluster, a possible local analog to super star cluster formation at Cosmic Dawn and Noon. In this paper, the first in a series about the mid-infrared (MIR) line and continuum emission in the center of NGC 5253, we present an overview and continuum spectra. The MIR images reveal four continuum sources that we identify as hot dust emission from luminous H II regions. The dominant source is the parsec-scale supernebula core seen at radio wavelengths. We find that the MIR-to-radio continuum flux ratio is identical to that of Galactic H II regions. The 9.7 μ m silicate feature is present and strongest in absorption toward the supernebula. Polycyclic aromatic hydrocarbon (PAH) features at 6.2, 6.8, 7.7, 8.6, and 11.2 μ m are detected across the region, although weakly, particularly in the supernebula. Unusual PAH line profiles are seen, including a broad 6 μ m feature, likely in part aliphatic, from the extended starburst region and strong 11.0 μ m emission from the supernebula. These observations suggest dust processing by intense radiation fields and possible dust production and dispersal by Wolf–Rayet stars within the region.

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Cite

BibTeXRIS
BibTeX
@article{turner2026jwst,
  title = {{JWST View of the Supernebula in NGC 5253. I. Overview and Continuum Features}},
  author = {Jean L. Turner and Sara C. Beck and Elm Zweig and L. Barcos-Muñoz and John H. Black and Daniel P. Cohen and S. Michelle Consiglio and Nicholas G. Ferraro and Paul T. P. Ho and David S. Meier},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = nov,
  doi = {10.3847/1538-4357/aeac2a},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeac2a},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - JWST View of the Supernebula in NGC 5253. I. Overview and Continuum Features
AU  - Jean L. Turner
AU  - Sara C. Beck
AU  - Elm Zweig
AU  - L. Barcos-Muñoz
AU  - John H. Black
AU  - Daniel P. Cohen
AU  - S. Michelle Consiglio
AU  - Nicholas G. Ferraro
AU  - Paul T. P. Ho
AU  - David S. Meier
PY  - 2026
DA  - 2026/11/04
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aeac2a
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aeac2a
AB  - We present 5–28 μ m imaging spectroscopy of the “supernebula” in the dwarf galaxy NGC 5253 made with the JWST/MIRI/Medium Resolution Spectrometer integral field spectrometer. NGC 5253 hosts a luminous ( L ∼ 10 ⁹ L ⊙ ) H II region, powered by a giant young star cluster, a possible local analog to super star cluster formation at Cosmic Dawn and Noon. In this paper, the first in a series about the mid-infrared (MIR) line and continuum emission in the center of NGC 5253, we present an overview and continuum spectra. The MIR images reveal four continuum sources that we identify as hot dust emission from luminous H II regions. The dominant source is the parsec-scale supernebula core seen at radio wavelengths. We find that the MIR-to-radio continuum flux ratio is identical to that of Galactic H II regions. The 9.7 μ m silicate feature is present and strongest in absorption toward the supernebula. Polycyclic aromatic hydrocarbon (PAH) features at 6.2, 6.8, 7.7, 8.6, and 11.2 μ m are detected across the region, although weakly, particularly in the supernebula. Unusual PAH line profiles are seen, including a broad 6 μ m feature, likely in part aliphatic, from the extended starburst region and strong 11.0 μ m emission from the supernebula. These observations suggest dust processing by intense radiation fields and possible dust production and dispersal by Wolf–Rayet stars within the region.
SN  - 1538-4357
SN  - 0004-637X
ER  -