Probing Accretion and Outflow in V1180 Cas through High-Resolution Optical Spectroscopy

Abstract

We present an analysis of a high-resolution optical spectrum of V1180 Cas obtained with HIRES at the W. M. Keck Observatory during a bright photometric state of the source. The spectrum is dominated by strong emission lines, including Hα, the Ca II infrared triplet, He I, and O I, along with numerous Fe I and Fe II transitions and several forbidden lines such as [O I] and [S II], indicating ongoing accretion and mass-loss activity. A weak Li I λ6708 absorption feature confirms the youth of the source. Using the Li I absorption and selected Fe I emission lines, we report for the first time a radial velocity of −16 ± 3 km s⁻¹ for V1180 Cas. The Hα and Hβ profiles exhibit asymmetric structures with blueshifted absorption components, suggesting outflowing material along the line of sight. The He I λ5876 line displays a narrow component likely associated with post-shock accretion regions and a broad, slightly blueshifted component probably arising from magnetospheric flows and/or inner disk winds. The [O I] λ6300 profile is decomposed into low- and high-velocity components, tracing a slow disk wind and a fast jet. Using the forbidden [O I] line, we estimate for the first time a disk inclination angle of ≈50^∘. The derived mass accretion and jet mass-loss rates imply Ṁ_jet/Ṁ_acc ∼ 0.01--$0.03$, at the lower end of, but consistent with, the range observed for Class II YSOs. Forbidden-line diagnostics indicate densities ∼10³ and 10⁶ cm⁻³ with temperatures of ∼10⁴ K, supporting a multi-component outflow scenario. Overall, the results support a picture in which V1180 Cas is an actively accreting, moderately inclined system hosting a multi-component outflow.

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BibTeX RIS

BibTeX

@misc{chand2026probing,
  title = {{Probing Accretion and Outflow in V1180 Cas through High-Resolution Optical Spectroscopy}},
  author = {Tarak Chand and Saurabh Sharma and Koshvendra Singh and Joe P. Ninan and Arpan Ghosh and Devendra K. Ojha and Jyotirmoy Dey and Manojit Chakraborty and Kartik Gokhe and Aayushi Verma and Mamta and Ajay Kumar Singh},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.01226},
  eprint = {2610.01226},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.01226},
}

RIS

TY  - UNPB
TI  - Probing Accretion and Outflow in V1180 Cas through High-Resolution Optical Spectroscopy
AU  - Tarak Chand
AU  - Saurabh Sharma
AU  - Koshvendra Singh
AU  - Joe P. Ninan
AU  - Arpan Ghosh
AU  - Devendra K. Ojha
AU  - Jyotirmoy Dey
AU  - Manojit Chakraborty
AU  - Kartik Gokhe
AU  - Aayushi Verma
AU  - Mamta
AU  - Ajay Kumar Singh
PY  - 2026
DA  - 2026/10/01
PB  - arXiv
DO  - 10.48550/arxiv.2610.01226
UR  - https://arxiv.org/abs/2610.01226
AB  - We present an analysis of a high-resolution optical spectrum of V1180 Cas obtained with HIRES at the W. M. Keck Observatory during a bright photometric state of the source. The spectrum is dominated by strong emission lines, including Hα, the Ca II infrared triplet, He I, and O I, along with numerous Fe I and Fe II transitions and several forbidden lines such as [O I] and [S II], indicating ongoing accretion and mass-loss activity. A weak Li I λ6708 absorption feature confirms the youth of the source. Using the Li I absorption and selected Fe I emission lines, we report for the first time a radial velocity of −16 ± 3 km s^−1 for V1180 Cas. The Hα and Hβ profiles exhibit asymmetric structures with blueshifted absorption components, suggesting outflowing material along the line of sight. The He I λ5876 line displays a narrow component likely associated with post-shock accretion regions and a broad, slightly blueshifted component probably arising from magnetospheric flows and/or inner disk winds. The [O I] λ6300 profile is decomposed into low- and high-velocity components, tracing a slow disk wind and a fast jet. Using the forbidden [O I] line, we estimate for the first time a disk inclination angle of ≈50^∘. The derived mass accretion and jet mass-loss rates imply Ṁ_jet/Ṁ_acc ∼ 0.01--$0.03$, at the lower end of, but consistent with, the range observed for Class II YSOs. Forbidden-line diagnostics indicate densities ∼10^3 and 10^6 cm^−3 with temperatures of ∼10^4 K, supporting a multi-component outflow scenario. Overall, the results support a picture in which V1180 Cas is an actively accreting, moderately inclined system hosting a multi-component outflow.
ER  -

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