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The Ophiuchus DIsc Survey Employing ALMA (ODISEA) – II. The effect of stellar multiplicity on disc properties
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2020-07-02 , DOI: 10.1093/mnras/staa1886
Alice Zurlo 1, 2 , Lucas A Cieza 1 , Sebastián Pérez 3 , Valentin Christiaens 4 , Jonathan P Williams 5 , Greta Guidi 6 , Hector Cánovas 7 , Simon Casassus 8 , Antonio Hales 9 , David A Principe 10 , Dary Ruíz-Rodríguez 11 , Antonia Fernandez-Figueroa 8
Affiliation  

We present Adaptive Optics (AO) near infrared (NIR) observations using VLT/NACO and Keck/NIRC2 of ODISEA targets. ODISEA is an ALMA survey of the entire population of circumstellar discs in the Ophiuchus molecular cloud. From the whole sample of ODISEA we select all the discs that are not already observed in the NIR with AO and that are observable with NACO or NIRC2. The NIR-ODISEA survey consists of 147 stars observed in NIR AO imaging for the first time, as well as revisiting almost all the binary systems of Ophiuchus present in the literature (20 out of 21). In total, we detect 20 new binary systems and one triple system. For each of them we calculate the projected separation and position angle of the companion, as well as their NIR and millimeter flux ratios. From the NIR contrast we derived the masses of the secondaries, finding that 9 of them are in the sub-stellar regime (30-50 \MJup). Discs in multiple systems reach a maximum total dust mass of $\sim$ 50 M$_{\oplus}$, while discs in single stars can reach a dust mass of 200 M$_{\oplus}$. Discs with masses above 10 M$_{\oplus}$ are found only around binaries with projected separations larger than $\sim$ 110 au. The maximum disc size is also larger around single star than binaries. However, since most discs in Ophiuchus are very small and low-mass, the effect of visual binaries is relatively weak in the general disc population.

中文翻译:

使用 ALMA (ODISEA) 的 Ophiuchus DISc 调查 – II。恒星多样性对圆盘特性的影响

我们使用 ODISEA 目标的 VLT/NACO 和 Keck/NIRC2 呈现自适应光学 (AO) 近红外 (NIR) 观测。ODISEA 是 ALMA 对蛇夫座分子云中整个星周盘群的调查。从 ODISEA 的整个样本中,我们选择了在 NIR 中尚未通过 AO 观察到的所有圆盘,以及通过 NACO 或 NIRC2 可观测到的圆盘。NIR-ODISEA 巡天由首次在 NIR AO 成像中观察到的 147 颗恒星组成,并重新审视了文献中几乎所有的蛇夫座双星系统(21 个中的 20 个)。我们总共检测到 20 个新的二元系统和一个三元系统。对于它们中的每一个,我们计算同伴的投影分离和位置角,以及它们的 NIR 和毫米通量比。从 NIR 对比中,我们推导出次级的质量,发现其中 9 个处于亚恒星区域 (30-50 \MJup)。多个系统中的圆盘达到的最大总尘埃质量为 $\sim$ 50 M$_{\oplus}$,而单星中的盘可以达到 200 M$_{\oplus}$ 的尘埃质量。质量大于 10 M$_{\oplus}$ 的圆盘仅在投影间距大于 $\sim$ 110 au 的双星周围发现。单星周围的最大圆盘尺寸也比双星大。然而,由于蛇夫座中的大多数圆盘都非常小且质量低,因此视觉双星的影响在一般圆盘群中相对较弱。质量大于 10 M$_{\oplus}$ 的圆盘仅在投影间距大于 $\sim$ 110 au 的双星周围发现。单星周围的最大圆盘尺寸也比双星大。然而,由于蛇夫座中的大多数圆盘都非常小且质量低,因此视觉双星的影响在一般圆盘群中相对较弱。质量大于 10 M$_{\oplus}$ 的圆盘仅在投影间距大于 $\sim$ 110 au 的双星周围发现。单星周围的最大圆盘尺寸也比双星大。然而,由于蛇夫座中的大多数圆盘都非常小且质量低,因此视觉双星的影响在一般圆盘群中相对较弱。
更新日期:2020-07-02
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