Nobeyama 45 m 对附近分子云 Orion A、Aquila Rift 和 M17 的映射观测：项目概述,Publications of the Astronomical Society of Japan

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Nobeyama 45 m 对附近分子云 Orion A、Aquila Rift 和 M17 的映射观测：项目概述
Publications of the Astronomical Society of Japan ( IF 2.2 ) Pub Date : 2019-09-06 , DOI: 10.1093/pasj/psz057
Fumitaka Nakamura _{1,

2,

3} , Shun Ishii _{1,

4} , Kazuhito Dobashi ₅ , Tomomi Shimoikura _{5,

6} , Yoshito Shimajiri _{1,

7,

8} , Ryohei Kawabe _{1,

2,

3} , Yoshihiro Tanabe ₉ , Asha Hirose ₅ , Shuri Oyamada _{1,

10} , Yumiko Urasawa ₁₁ , Hideaki Takemura _{1,

2} , Takashi Tsukagoshi ₁ , Munetake Momose ₉ , Koji Sugitani ₁₂ , Ryoichi Nishi ₁₁ , Sachiko Okumura ₁₀ , Patricio Sanhueza ₁ , Quang Nygen-Luong _{1,

13} , Takayoshi Kusune ₁

Affiliation

National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Joint ALMA Observatory, Alonso de Coŕdova 3107 Vitacura, Santiago, Chile
Department of Astronomy and Earth Sciences, Tokyo Gakugei University, 4-1-1 Nukuikitamachi, Koganei, Tokyo 184-8501, Japan
Faculty of Social Information Studies, Otsuma Women's University, 12 Sanban-cho, Chiyoda-ku, Tokyo 102-8357, Japan
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d'Astrophysique, CEA Saclay, F-91191 Gif-sur-Yvette, France
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan
College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
Faculty of Science, Department of Mathematical and Physical Sciences, Japan Women’s University, 2-8-1 Mejirodai, Bunkyo-ku, Tokyo 112-8681, Japan
Department of Physics, Niigata University, 8050 Ikarashi-2, Niigata 950-2181, Japan
Graduate School of Natural Sciences, Nagoya City University, Mizuho-ku, Nagoya, Aichi 467-8601, Japan
IBM Canada, 120 Bloor Street East, Toronto, ON, M4Y 1B7, Canada

我们使用 Nobeyama 45 米望远镜上的新型 100 GHz 接收器 FOREST，对附近的三个分子云 Orion A、Aquila Rift 和 M17 进行了测绘观测。在本文中，我们描述了所获得数据的细节，例如强度校准、数据灵敏度、角分辨率和速度分辨率。每个目标包含至少一个大质量恒星形成区域。目标分子线为 $^{12}$CO ($J = 1 - 0$), $^{13}$CO ($J = 1 - 0$), C$^{18}$O ($J = 1 - 0$)、N$_2$H$^+$ ($J=1-0$) 和 CCS ($J_N=8_7-7_6$)，我们覆盖了 10$^2 的密度范围$ cm$^{-3}$ 到 10$^6$ cm$^{-3}$，角分辨率为 $\sim 20\arcsec$，速度分辨率为 $\sim$ 0.1 km s$^{ -1}$。假设代表距离分别为 414 pc、436 pc 和 2.1 kpc，Orion A、Aquila Rift、M17 覆盖了大部分最密集的部分，面积分别约为 7 pc $\times$ 15 pc、7 pc $\times$ 7 pc 和 36 pc $\times$ 18 pc。根据 $^{13}$CO 柱密度分布，推导出总分子质量为 $3.86 \times 10^4 M_\odot$、$2.67 \times 10^4 M_\odot$ 和 $8.1\times Orion A、Aquila Rift 和 M17 分别为 10^5 M_\odot$。对于所有云，H$_2$柱密度超过了大质量恒星形成的理论阈值$\gtrsim$ 1 g cm$^{-2}$，仅朝着包含当前大质量恒星的区域-形成场所。对于其他区域，未来的大质量恒星形成需要进一步的质量吸积或动力压缩。这与目前的恒星形成活动一致。使用 $^{12}$CO 数据，我们证明我们的数据有足够的能力来识别分子流出，对于 Aquila Rift，我们确定了 4 个新的流出候选者。科学结果将在单独的论文中详细讨论。

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Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

We carried out mapping observations toward three nearby molecular clouds, Orion A, Aquila Rift, and M17, using a new 100 GHz receiver, FOREST, on the Nobeyama 45-m telescope. In the present paper, we describe the details of the data obtained such as intensity calibration, data sensitivity, angular resolution, and velocity resolution. Each target contains at least one high-mass star-forming region. The target molecular lines were $^{12}$CO ($J = 1 - 0$), $^{13}$CO ($J = 1 - 0$), C$^{18}$O ($J = 1 - 0$), N$_2$H$^+$ ($J=1-0$), and CCS ($J_N=8_7-7_6$), with which we covered the density range of 10$^2$ cm$^{-3}$ to 10$^6$ cm$^{-3}$ with an angular resolution of $\sim 20\arcsec$ and a velocity resolution of $\sim$ 0.1 km s$^{-1}$. Assuming the representative distances of 414 pc, 436 pc, and 2.1 kpc, the maps of Orion A, Aquila Rift, and M17 cover most of the densest parts with areas of about 7 pc $\times$ 15 pc, 7 pc $\times$ 7 pc, and 36 pc $\times$ 18 pc, respectively. On the basis of the $^{13}$CO column density distribution, the total molecular masses are derived to be $3.86 \times 10^4 M_\odot$, $2.67 \times 10^4 M_\odot$, and $8.1\times 10^5 M_\odot$ for Orion A, Aquila Rift, and M17, respectively. For all the clouds, the H$_2$ column density exceeds the theoretical threshold for high-mass star formation of $\gtrsim$ 1 g cm$^{-2}$, only toward the regions which contain current high-mass star-forming sites. For other areas, further mass accretion or dynamical compression would be necessary for future high-mass star formation. This is consistent with the current star formation activity. Using the $^{12}$CO data, we demonstrate that our data have enough capability to identify molecular outflows, and for Aquila Rift, we identify 4 new outflow candidates. The scientific results will be discussed in details in separate papers.

更新日期：2019-09-06

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