A Spectroastrometric Study of the Low-velocity Wind from DG Tau A
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| Autores principales: | , , , , , , , , , , , |
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| Formato: | Preprint |
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2025
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| author | Chou, Yu-Ru Takami, Michihiro Lai, Shin-Ping Whelan, Emma Otten, Noah B. Fang, Min Tajitsu, Akito Otsuka, Masaaki Shang, Hsien Liu, Chun-Fan Karr, Jennifer Murphy, Aisling |
| author_facet | Chou, Yu-Ru Takami, Michihiro Lai, Shin-Ping Whelan, Emma Otten, Noah B. Fang, Min Tajitsu, Akito Otsuka, Masaaki Shang, Hsien Liu, Chun-Fan Karr, Jennifer Murphy, Aisling |
| contents | We obtained high spectral resolution spectra ($Δv$ $\sim$ 2.5 km s$^{-1}$) for DG Tau A from 4800 Å to 7500 Å using Subaru High Dispersion Spectrograph (HDS) for the first time. The low-velocity components (LVCs, |$v$| < 100 km s$^{-1}$) were observed in the [O I] 5577, 6300, 6364 Å, [S II] 6716, 6731 Å lines. The offset position spectra observed in the LVCs show a "negative velocity gradient", supporting the presence of a wide-angled wind associated with the LVC emission. The offset position spectra observed in a component within the LVC velocity range between -16 km s$^{-1}$ to -41 km s$^{-1}$, namely, LVC-M, show a "negative velocity gradient'', supporting the presence of a wide-angled wind. With 12-70 au wind lengths measured using spectroastrometry, we estimate a lower limit to the wind mass-loss rate of $\sim$10$^{-8}$ M$_\odot$ yr$^{-1}$. In addition to the LVCs, we identify two high-velocity components (HVCs, |$v$| > 100 km s$^{-1}$) associated with the collimated jet in 26 lines ([N I], [N II], [O I], [O II], [O III], [S II], [Ca II], [Fe II], H$α$, H$β$, He I). The one with a clear spatial offset from the star ($n_e$ $\sim$10$^4$ cm$^{-3}$, HVC1) is associated with an internal shock surface of the jet, while the other at the base ($n_e$ $\sim$10$^6$ cm$^{-3}$, HVC2) may be a stationary shock component. We find that the observed line profiles and the spatial scales of the LVC emission do not agree with the existing predictions for photoevaporative or magnetohydrodynamical (MHD) disk winds. These could be explained by the X-wind model, but synthetic observations are required for detailed comparisons. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_02433 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A Spectroastrometric Study of the Low-velocity Wind from DG Tau A Chou, Yu-Ru Takami, Michihiro Lai, Shin-Ping Whelan, Emma Otten, Noah B. Fang, Min Tajitsu, Akito Otsuka, Masaaki Shang, Hsien Liu, Chun-Fan Karr, Jennifer Murphy, Aisling Solar and Stellar Astrophysics Astrophysics of Galaxies We obtained high spectral resolution spectra ($Δv$ $\sim$ 2.5 km s$^{-1}$) for DG Tau A from 4800 Å to 7500 Å using Subaru High Dispersion Spectrograph (HDS) for the first time. The low-velocity components (LVCs, |$v$| < 100 km s$^{-1}$) were observed in the [O I] 5577, 6300, 6364 Å, [S II] 6716, 6731 Å lines. The offset position spectra observed in the LVCs show a "negative velocity gradient", supporting the presence of a wide-angled wind associated with the LVC emission. The offset position spectra observed in a component within the LVC velocity range between -16 km s$^{-1}$ to -41 km s$^{-1}$, namely, LVC-M, show a "negative velocity gradient'', supporting the presence of a wide-angled wind. With 12-70 au wind lengths measured using spectroastrometry, we estimate a lower limit to the wind mass-loss rate of $\sim$10$^{-8}$ M$_\odot$ yr$^{-1}$. In addition to the LVCs, we identify two high-velocity components (HVCs, |$v$| > 100 km s$^{-1}$) associated with the collimated jet in 26 lines ([N I], [N II], [O I], [O II], [O III], [S II], [Ca II], [Fe II], H$α$, H$β$, He I). The one with a clear spatial offset from the star ($n_e$ $\sim$10$^4$ cm$^{-3}$, HVC1) is associated with an internal shock surface of the jet, while the other at the base ($n_e$ $\sim$10$^6$ cm$^{-3}$, HVC2) may be a stationary shock component. We find that the observed line profiles and the spatial scales of the LVC emission do not agree with the existing predictions for photoevaporative or magnetohydrodynamical (MHD) disk winds. These could be explained by the X-wind model, but synthetic observations are required for detailed comparisons. |
| title | A Spectroastrometric Study of the Low-velocity Wind from DG Tau A |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.02433 |