TY - JOUR
T1 - A VLA View of the Flared, Asymmetric Disk around the Class 0 Protostar L1527 IRS
AU - Sheehan, Patrick D.
AU - Tobin, John J.
AU - Li, Zhi Yun
AU - van ’t Hoff, Merel L.R.
AU - Jørgensen, Jes K.
AU - Kwon, Woojin
AU - Looney, Leslie W.
AU - Ohashi, Nagayoshi
AU - Takakuwa, Shigehisa
AU - Williams, Jonathan P.
AU - Aso, Yusuke
AU - Gavino, Sacha
AU - Gregorio-Monsalvo, Itziar de
AU - Han, Ilseung
AU - Lee, Chang Won
AU - Plunkett, Adele
AU - Sharma, Rajeeb
AU - Aikawa, Yuri
AU - Lai, Shih Ping
AU - Lee, Jeong Eun
AU - Lin, Zhe Yu Daniel
AU - Saigo, Kazuya
AU - Tomida, Kengo
AU - Yen, Hsi Wei
N1 - Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/8/1
Y1 - 2022/8/1
N2 - We present high-resolution Karl G. Jansky Very Large Array (VLA) observations of the protostar L1527 IRS at 7 mm, 1.3 cm, and 2 cm wavelengths. We detect the edge-on dust disk at all three wavelengths and find that it is asymmetric, with the southern side of the disk brighter than the northern side. We confirm this asymmetry through analytic modeling and also find that the disk is flared at 7 mm. We test the data against models including gap features in the intensity profile, and though we cannot rule such models out, they do not provide a statistically significant improvement in the quality of fit to the data. From these fits, we can, however, place constraints on allowed properties of any gaps that could be present in the true, underlying intensity profile. The physical nature of the asymmetry is difficult to associate with physical features owing to the edge-on nature of the disk, but it could be related to spiral arms or asymmetries seen in other imaging of more face-on disks.
AB - We present high-resolution Karl G. Jansky Very Large Array (VLA) observations of the protostar L1527 IRS at 7 mm, 1.3 cm, and 2 cm wavelengths. We detect the edge-on dust disk at all three wavelengths and find that it is asymmetric, with the southern side of the disk brighter than the northern side. We confirm this asymmetry through analytic modeling and also find that the disk is flared at 7 mm. We test the data against models including gap features in the intensity profile, and though we cannot rule such models out, they do not provide a statistically significant improvement in the quality of fit to the data. From these fits, we can, however, place constraints on allowed properties of any gaps that could be present in the true, underlying intensity profile. The physical nature of the asymmetry is difficult to associate with physical features owing to the edge-on nature of the disk, but it could be related to spiral arms or asymmetries seen in other imaging of more face-on disks.
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U2 - 10.3847/1538-4357/ac7a3b
DO - 10.3847/1538-4357/ac7a3b
M3 - Article
AN - SCOPUS:85135451430
SN - 0004-637X
VL - 934
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 95
ER -