论文标题
CO中的扫描磁盘环和风在0.01-10 AU：高分辨率$ m $频带光谱调查
Scanning disk rings and winds in CO at 0.01-10 au: a high-resolution $M$-band spectroscopy survey with IRTF-iSHELL
论文作者
论文摘要
我们提出了概述和首先是对与ISHELL在IRTF上进行的Planet形成磁盘的$ M $频带光谱调查，使用两个缝隙，可提供分辨力R $ $ \ $ $ \ $ 60,000-92,000（5-3.3 km/s）。 ISHELL一枪提供了几乎完整的覆盖范围，涵盖了$^{12} $ CO和$^{12} $ CO和$^{13} $ CO的$> 50 $ $> 50 $的行，并提供多个振动级别的$^{13} $ co，并提供了对多种发射和吸收和吸收组件激发的前所未有的信息。 Some of the most notable new findings of this survey are: 1) the detection of two CO Keplerian rings at $<2$ au (in HD 259431), 2) the detection of H${_2}$O ro-vibrational lines at 5 $μ$m (in AS 205 N), and 3) the common kinematic variability of CO lines over timescales of 1-14 years.通过同质分析这项调查，以及先前对冷却器恒星的VLT-Crires调查，我们讨论了CO光谱的统一视图，其中发射和吸收成分从灰尘过滤中的无尘区域扫描了Radii的磁盘表面，从灰尘过滤到$ \ $ \ \ \ \ \ of \ of。我们将两种基本类型的CO线形状分类为解释为从开普勒环（双峰线）和磁盘表面发射的发射，再加上风（三角线）的低速部分（三角线），其中CO激发反映了不同的发射区域（及其气体dust的比率），而不仅仅是受传递样品。三角形线的磁盘+风解释自然解释了在CO光谱中观察到的几种特性，包括线蓝移，线形在高倾斜下变成狭窄的吸收，以及磁盘风的频率随着恒星类型的函数。
We present an overview and first results from a $M$-band spectroscopic survey of planet-forming disks performed with iSHELL on IRTF, using two slits that provide resolving power R $\approx$ 60,000-92,000 (5-3.3 km/s). iSHELL provides a nearly complete coverage at 4.52-5.24 $μ$m in one shot, covering $>50$ lines from the R and P branches of $^{12}$CO and $^{13}$CO for each of multiple vibrational levels, and providing unprecedented information on the excitation of multiple emission and absorption components. Some of the most notable new findings of this survey are: 1) the detection of two CO Keplerian rings at $<2$ au (in HD 259431), 2) the detection of H${_2}$O ro-vibrational lines at 5 $μ$m (in AS 205 N), and 3) the common kinematic variability of CO lines over timescales of 1-14 years. By homogeneously analyzing this survey together with a previous VLT-CRIRES survey of cooler stars, we discuss a unified view of CO spectra where emission and absorption components scan the disk surface across radii from a dust-free region within dust sublimation out to $\approx10$ au. We classify two fundamental types of CO line shapes interpreted as emission from Keplerian rings (double-peak lines) and a disk surface plus a low-velocity part of a wind (triangular lines), where CO excitation reflects different emitting regions (and their gas-to-dust ratio) rather than just the irradiation spectrum. A disk+wind interpretation for the triangular lines naturally explains several properties observed in CO spectra, including the line blue-shifts, line shapes that turn into narrow absorption at high inclinations, and the frequency of disk winds as a function of stellar type.
