Late Epoch Infrared Spectroscopy and Two-Component 3D Photoionization Modeling of Classical Nova V5668 Sgr

Abstract

V5668 Sgr is an Fe II classical nova (CN) that exploded on 15 March 2015. We present near-infrared (NIR) spectroscopy of the ejecta from the Mt. Abu observatory which exhibits emission lines of species H, He, N, S, Ti, and Si. We also present SOFIA (+FORCAST) spectroscopy which shows two forbidden emission lines, [Ne II] at 12.8 μm and [O IV] at 25.9 μm, as well as two emission features attributed to polycyclic aromatic hydrocarbons (PAH) at 6.2 μm and 11.3 μm. 1D Cloudy photoionization simulations require two components to model the system, which suggests a multifaceted, morphologically complex ejecta. The 1D simulations also reveal He, N, Ne, S, Ti, Si, and O chemical abundances elevated above fiducial solar levels. 3D pyCloudy photoionization emission profiles visualize the ejecta and elucidate the system's complex composition.

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BibTeX RIS

BibTeX

@misc{taft2026late,
  title = {{Late Epoch Infrared Spectroscopy and Two-Component 3D Photoionization Modeling of Classical Nova V5668 Sgr}},
  author = {Sarah H. Taft and Charles E. Woodward and Bruno C. Santos and D. P. K. Banerjee and R. D. Gehrz},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.33376},
  eprint = {2610.33376},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.33376},
  note = {CC BY 4.0},
}

RIS

TY  - UNPB
TI  - Late Epoch Infrared Spectroscopy and Two-Component 3D Photoionization Modeling of Classical Nova V5668 Sgr
AU  - Sarah H. Taft
AU  - Charles E. Woodward
AU  - Bruno C. Santos
AU  - D. P. K. Banerjee
AU  - R. D. Gehrz
PY  - 2026
DA  - 2026/10/24
PB  - arXiv
DO  - 10.48550/arxiv.2610.33376
UR  - https://arxiv.org/abs/2610.33376
AB  - V5668 Sgr is an Fe II classical nova (CN) that exploded on 15 March 2015. We present near-infrared (NIR) spectroscopy of the ejecta from the Mt. Abu observatory which exhibits emission lines of species H, He, N, S, Ti, and Si. We also present SOFIA (+FORCAST) spectroscopy which shows two forbidden emission lines, [Ne II] at 12.8 μm and [O IV] at 25.9 μm, as well as two emission features attributed to polycyclic aromatic hydrocarbons (PAH) at 6.2 μm and 11.3 μm. 1D Cloudy photoionization simulations require two components to model the system, which suggests a multifaceted, morphologically complex ejecta. The 1D simulations also reveal He, N, Ne, S, Ti, Si, and O chemical abundances elevated above fiducial solar levels. 3D pyCloudy photoionization emission profiles visualize the ejecta and elucidate the system's complex composition.
ER  -

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