[N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star
In this study, we performed high-resolution near-infrared (NIR) spectroscopy ( R = 28,000; λ = 0.90–1.35 μ m) with a high signal-to-noise ratio on HD 200775, a very young (∼0.1 Myr old) and massive intermediate-mass star (a binary star with a mass of about 10 M _⊙ each) with a protoplanetary disk. T...
| Main Authors: | , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad2842 |
| _version_ | 1797218188968067072 |
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| author | Haruki Katoh Chikako Yasui Yuji Ikeda Naoto Kobayashi Noriyuki Matsunaga Sohei Kondo Hiroaki Sameshima Satoshi Hamano Misaki Mizumoto Hideyo Kawakita Kei Fukue Shogo Otsubo Keiichi Takenaka |
| author_facet | Haruki Katoh Chikako Yasui Yuji Ikeda Naoto Kobayashi Noriyuki Matsunaga Sohei Kondo Hiroaki Sameshima Satoshi Hamano Misaki Mizumoto Hideyo Kawakita Kei Fukue Shogo Otsubo Keiichi Takenaka |
| author_sort | Haruki Katoh |
| collection | DOAJ |
| description | In this study, we performed high-resolution near-infrared (NIR) spectroscopy ( R = 28,000; λ = 0.90–1.35 μ m) with a high signal-to-noise ratio on HD 200775, a very young (∼0.1 Myr old) and massive intermediate-mass star (a binary star with a mass of about 10 M _⊙ each) with a protoplanetary disk. The obtained spectra show eight forbidden lines of three elements: two of [S ii ] (10289 and 10323 Å), two of [N i ] (10400 and 10410 Å), and four of [Fe ii ] (12570, 12946, 12981, and 13209 Å). This is the first time that the [N i ] lines are detected in a young stellar object with a doublet deblended. Gaussian fitting of the spectra indicates that all line profiles have low-velocity components and exhibit blueshifted features, suggesting that all lines originate from the disk winds (magnetohydrodynamic disk wind and/or photoevaporative wind). Based on the fit, the [N i ] and [Fe ii ] lines are categorized into narrow components, while the [S ii ] lines are at the boundary between broad and narrow components. These forbidden lines are suggested to be very promising disk wind tracers among the existing ones because they are in the NIR-wavelength range, which can be observed from early stages with high sensitivities. Among these lines, [N i ] lines would be a rather powerful probe for deriving the basic physical parameters of disk wind gases. However, the study of these lines herein is limited to one object; thus, further studies are needed to examine their properties. |
| first_indexed | 2024-04-24T12:13:47Z |
| format | Article |
| id | doaj.art-9c348c9941f840ffa696006f3d4e52e9 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T12:13:47Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-9c348c9941f840ffa696006f3d4e52e92024-04-08T09:27:03ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0196517010.3847/1538-4357/ad2842[N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass StarHaruki Katoh0Chikako Yasui1https://orcid.org/0000-0003-3579-7454Yuji Ikeda2https://orcid.org/0000-0003-2380-8582Naoto Kobayashi3https://orcid.org/0000-0003-4578-2619Noriyuki Matsunaga4Sohei Kondo5Hiroaki Sameshima6https://orcid.org/0000-0001-6401-723XSatoshi Hamano7https://orcid.org/0000-0002-6505-3395Misaki Mizumoto8https://orcid.org/0000-0003-2161-0361Hideyo Kawakita9https://orcid.org/0000-0003-2011-9159Kei Fukue10https://orcid.org/0000-0003-2516-9753Shogo Otsubo11Keiichi Takenaka12Department of Physics, Graduate School of Science, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-Ku, Kyoto, 603-8555, Japan; Laboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan ; ck.yasui@gmail.comLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Photocoding , 460-102 Iwakura-Nakamachi, Sakyo-ku, Kyoto 606-0025, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Kiso Observatory, The University of Tokyo , 10762-30 Mitake, Kiso-machi, Kiso-gun, Nagano 397-0101, Japan; Institute of Astronomy, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Department of Astronomy, Graduate School of Science, The University of Tokyo , Bunkyo-ku, Tokyo 113-0033, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Kiso Observatory, The University of Tokyo , 10762-30 Mitake, Kiso-machi, Kiso-gun, Nagano 397-0101, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Institute of Astronomy, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan ; ck.yasui@gmail.comHakubi Center, Kyoto University , Yoshida-honmachi, Sakyo-ku, Kyoto 606-8501, Japan; Department of Astronomy, Graduate School of Science, Kyoto University , Kitashirakawa-oiwakecho, Sakyo-ku, Kyoto 606-8502, JapanDepartment of Physics, Graduate School of Science, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-Ku, Kyoto, 603-8555, Japan; Laboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan; Education Center for Medicine and Nursing, Shiga University of Medical Science , Seta Tsukinowa-cho, Otsu, Shiga, 520-2192, JapanLaboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, JapanDepartment of Physics, Graduate School of Science, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-Ku, Kyoto, 603-8555, Japan; Laboratory of Infrared High-resolution spectroscopy (LIH), Koyama Astronomical Observatory, Kyoto Sangyo University , Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, JapanIn this study, we performed high-resolution near-infrared (NIR) spectroscopy ( R = 28,000; λ = 0.90–1.35 μ m) with a high signal-to-noise ratio on HD 200775, a very young (∼0.1 Myr old) and massive intermediate-mass star (a binary star with a mass of about 10 M _⊙ each) with a protoplanetary disk. The obtained spectra show eight forbidden lines of three elements: two of [S ii ] (10289 and 10323 Å), two of [N i ] (10400 and 10410 Å), and four of [Fe ii ] (12570, 12946, 12981, and 13209 Å). This is the first time that the [N i ] lines are detected in a young stellar object with a doublet deblended. Gaussian fitting of the spectra indicates that all line profiles have low-velocity components and exhibit blueshifted features, suggesting that all lines originate from the disk winds (magnetohydrodynamic disk wind and/or photoevaporative wind). Based on the fit, the [N i ] and [Fe ii ] lines are categorized into narrow components, while the [S ii ] lines are at the boundary between broad and narrow components. These forbidden lines are suggested to be very promising disk wind tracers among the existing ones because they are in the NIR-wavelength range, which can be observed from early stages with high sensitivities. Among these lines, [N i ] lines would be a rather powerful probe for deriving the basic physical parameters of disk wind gases. However, the study of these lines herein is limited to one object; thus, further studies are needed to examine their properties.https://doi.org/10.3847/1538-4357/ad2842Protoplanetary disksStellar windsStar formationHerbig Ae/Be starsT Tauri starsPre-main sequence stars |
| spellingShingle | Haruki Katoh Chikako Yasui Yuji Ikeda Naoto Kobayashi Noriyuki Matsunaga Sohei Kondo Hiroaki Sameshima Satoshi Hamano Misaki Mizumoto Hideyo Kawakita Kei Fukue Shogo Otsubo Keiichi Takenaka [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star The Astrophysical Journal Protoplanetary disks Stellar winds Star formation Herbig Ae/Be stars T Tauri stars Pre-main sequence stars |
| title | [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star |
| title_full | [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star |
| title_fullStr | [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star |
| title_full_unstemmed | [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star |
| title_short | [N i] 10400/10410 Å Lines as Possible Disk Wind Tracers in a Young Intermediate-mass Star |
| title_sort | n i 10400 10410 a lines as possible disk wind tracers in a young intermediate mass star |
| topic | Protoplanetary disks Stellar winds Star formation Herbig Ae/Be stars T Tauri stars Pre-main sequence stars |
| url | https://doi.org/10.3847/1538-4357/ad2842 |
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