VLA AND CARMA OBSERVATIONS OF PROTOSTARS IN THE CEPHEUS CLOUDS: SUB-ARCSECOND PROTO-BINARIES FORMED VIA DISK FRAGMENTATION
VLA AND CARMA OBSERVATIONS OF PROTOSTARS IN THE CEPHEUS CLOUDS: SUB-ARCSECOND PROTO-BINARIES FORMED VIA DISK FRAGMENTATION
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仙王星云中原恒星的 VLA 和 CARMA 观测：通过盘碎片形成的亚弧秒原双星
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发表时间：
2013
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通讯作者：
W. Kwon
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作者：
J. Tobin;C. Chandler;D. Wilner;L. Looney;L. Loinard;Hsin;L. Hartmann;N. Calvet;P. D’Alessio;T. Bourke;W. Kwon
本文利用卡尔·杨斯基甚大阵列（VLA）观测了3颗0/I类原恒星（L1157-mm、CB230 IRS1和L1165-SMM1），并利用毫米波天文研究联合阵列（CARMA）观测了2颗0/I类原恒星（L1165-SMM1和CB230 IRS1）。VLA观测波长分别为λ = 7.3 mm、1.4 cm、3.3 cm、4.0 cm和6.5 cm，最佳分辨率为~ 0。″06 (18 AU), 7.3 mm。L1165-SMM1 CARMA观测在λ = 1.3 mm处进行，最佳分辨率为~ 0。″3 （100 AU）和CB230 IRS1在λ = 3.4 mm处进行观测，最佳分辨率为~ 3″（900 AU）。我们发现L1165-SMM1和CB230 IRS1在~ 0的距离上可能有双星伴星。″3 （100 AU）从多个波长的次峰探测得到。这些伴星的位置角度几乎与观测到的双极流出的方向正交，与预期的原恒星盘方向一致。我们认为这些伴星可能是由磁盘碎片形成的；湍流破碎不会优先安排二元伴体与流出方向正交。对于L1165-SMM1, 7.3 mm和1.3 mm的发射都显示了一个大的（rbbb100 AU）圆盘的证据。对于L1165-SMM1主原星和CB230 IRS1次原星，7.3 mm的发射被分解成与~ 20 AU半径盘一致的结构。对于其他的原恒星，包括l1157毫米，发射是无法确定的，表明圆盘的半径小于20天文单位。
We present observations of three Class 0/I protostars (L1157-mm, CB230 IRS1, and L1165-SMM1) using the Karl G. Jansky Very Large Array (VLA) and observations of two (L1165-SMM1 and CB230 IRS1) with the Combined Array for Research in Millimeter-wave Astronomy (CARMA). The VLA observations were taken at wavelengths of λ = 7.3 mm, 1.4 cm, 3.3 cm, 4.0 cm, and 6.5 cm with a best resolution of ∼0.″06 (18 AU) at 7.3 mm. The L1165-SMM1 CARMA observations were taken at λ = 1.3 mm with a best resolution of ∼0.″3 (100 AU) and the CB230 IRS1 observations were taken at λ = 3.4 mm with a best resolution of ∼3″ (900 AU). We find that L1165-SMM1 and CB230 IRS1 have probable binary companions at separations of ∼0.″3 (100 AU) from detections of secondary peaks at multiple wavelengths. The position angles of these companions are nearly orthogonal to the direction of the observed bipolar outflows, consistent with the expected protostellar disk orientations. We suggest that these companions may have formed from disk fragmentation; turbulent fragmentation would not preferentially arrange the binary companions to be orthogonal to the outflow direction. For L1165-SMM1, both the 7.3 mm and 1.3 mm emission show evidence of a large (R > 100 AU) disk. For the L1165-SMM1 primary protostar and the CB230 IRS1 secondary protostar, the 7.3 mm emission is resolved into structures consistent with ∼20 AU radius disks. For the other protostars, including L1157-mm, the emission is unresolved, suggesting disks with radii <20 AU.