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Emission-line Data Cubes of the HH 32 Stellar Jet
The Astronomical Journal ( IF 5.3 ) Pub Date : 2020-09-11 , DOI: 10.3847/1538-3881/abadfa
Patrick Hartigan 1 , Lynne A. Hillenbrand 2 , Matuesz Matuszewski 3 , Arlindo Chan Borges 2 , James D. Neill 3 , D. Christopher Martin 3 , Patrick Morrissey 3 , Anna M. Moore 4
Affiliation  

We analyze data cubes of over 60 emission lines in the HH 32 stellar jet acquired with the Keck Cosmic Web Imager (KCWI). The data cover the less explored blue portion of the spectrum between 3586 and 6351 A and have both high spectral (R ~ 10,000) and spatial (≾ 1") resolution. The study includes all three major ionization states of oxygen, three Balmer lines, multiple lines of Fe ii and Fe iii, and the first data cubes ever acquired for important unblended diagnostic lines such as He ii λ4686, Ca i λ3933, and Mg i] λ4571. The data cubes generally sort according to excitation and have a relatively continuous progression from the highest-excitation ions (He ii, O iii) through the intermediate-excitation ions (O i and H i) to the lowest-excitation ions (Ca ii and Mg i). Merging the KCWI cubes with Hubble Space Telescope images leads to several new insights about the flow, including evidence for bow shocks, partial bow shocks, spur shocks, Mach disks, jet deflection shocks, a wiggling jet, and potential shock precursors. The most surprising result is that one of the velocity components of Fe ii in the Mach disk suddenly increases in flux relative to other lines by a factor of two, implying that the Mach disk vaporizes dust in the jet. Hence, jets must accelerate or entrain dust to speeds of over 300 km s⁻¹ without destroying the grains.

中文翻译:

HH 32 Stellar Jet 的发射线数据立方体

我们分析了使用 Keck Cosmic Web Imager (KCWI) 获得的 HH 32 恒星喷流中超过 60 条发射线的数据立方体。数据涵盖了 3586 和 6351 A 之间光谱中较少探索的蓝色部分,并且具有高光谱 (R ~ 10,000) 和空间 (≾ 1") 分辨率。该研究包括氧气的所有三种主要电离态、三个巴尔默线、 Fe ii 和 Fe iii 的多条线,以及为重要的非混合诊断线获得的第一个数据立方体,例如 He ii λ4686、Ca i λ3933 和 Mg i] λ4571。数据立方体通常根据激发进行排序并且具有相对连续的从最高激发离子(He ii、O iii)到中间激发离子(O i 和H i)再到最低激发离子(Ca ii 和Mg i)的过程。将 KCWI 立方体与哈勃太空望远镜图像合并,可以得出关于流动的几个新见解,包括弓形激波、部分弓形激波、刺激波、马赫盘、射流偏转激波、摆动射流和潜在激波前兆的证据。最令人惊讶的结果是马赫盘中 Fe ii 的速度分量之一相对于其他线的通量突然增加了两倍,这意味着马赫盘蒸发了射流中的灰尘。因此,喷流必须在不破坏颗粒的情况下将灰尘加速或夹带至超过 300 公里 s⁻¹ 的速度。最令人惊讶的结果是马赫盘中 Fe ii 的速度分量之一相对于其他线的通量突然增加了两倍,这意味着马赫盘蒸发了射流中的灰尘。因此,喷流必须在不破坏颗粒的情况下将灰尘加速或夹带至超过 300 公里 s⁻¹ 的速度。最令人惊讶的结果是马赫盘中 Fe ii 的速度分量之一相对于其他线的通量突然增加了两倍,这意味着马赫盘蒸发了射流中的灰尘。因此,喷流必须在不破坏颗粒的情况下将灰尘加速或夹带至超过 300 公里 s⁻¹ 的速度。
更新日期:2020-09-11
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