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195 results on '"Takakuwa, Shigehisa"'

1. Early Planet Formation in Embedded Disks (eDisk):XVI. Asymmetric dust disk driving a multicomponent molecular outflow in the young Class 0 protostar GSS30 IRS3

Author: Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Ohashi, Nagayoshi, Tobin, John J., Sai, Jinshi, Jørgensen, Jes K., Aso, Yusuke, Daniel Lin, Zhe-yu, Flores, Christian, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Plunkett, Adele L., Takakuwa, Shigehisa, R Van’t Hoff, Merel L., Williams, Jonathan P., Yen, Hsi-wei, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Ohashi, Nagayoshi, Tobin, John J., Sai, Jinshi, Jørgensen, Jes K., Aso, Yusuke, Daniel Lin, Zhe-yu, Flores, Christian, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Plunkett, Adele L., Takakuwa, Shigehisa, R Van’t Hoff, Merel L., Williams, Jonathan P., and Yen, Hsi-wei
Published: 2024

2. Early Planet Formation in Embedded Disks. XI. A High-resolution View Toward the BHR 71 Class 0 Protostellar Wide Binary

Author: Gavino, Sacha, Jørgensen, Jes K., Sharma, Rajeeb, Yang, Yao-lun, Li, Zhi-yun, Tobin, John J., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Plunkett, Adele L., Kwon, Woojin, De Gregorio-monsalvo, Itziar, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, Aso, Yusuke, Sai, Jinshi, Aikawa, Yuri, Tomida, Kengo, Koch, Patrick M., Lee, Jeong-eun, Lee, Chang Won, Lai, Shih-ping, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Thieme, Travis J., Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yen, Hsi-wei, Gavino, Sacha, Jørgensen, Jes K., Sharma, Rajeeb, Yang, Yao-lun, Li, Zhi-yun, Tobin, John J., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Plunkett, Adele L., Kwon, Woojin, De Gregorio-monsalvo, Itziar, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, Aso, Yusuke, Sai, Jinshi, Aikawa, Yuri, Tomida, Kengo, Koch, Patrick M., Lee, Jeong-eun, Lee, Chang Won, Lai, Shih-ping, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Thieme, Travis J., Van ’t Hoff, Merel L. R., Williams, Jonathan P., and Yen, Hsi-wei
Published: 2024

3. Early Planet Formation in Embedded Disks (eDisk). XV. Influence of Magnetic Field Morphology in Dense Cores on Sizes of Protostellar Disks

Author: Yen, Hsi-wei, Williams, Jonathan P., Sai, Jinshi, Koch, Patrick M., Han, Ilseung, Jørgensen, Jes K., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Narang, Mayank, Ohashi, Nagayoshi, Takakuwa, Shigehisa, Tobin, John J., De Gregorio-monsalvo, Itziar, Lai, Shih-ping, Lee, Jeong-eun, Tomida, Kengo, Yen, Hsi-wei, Williams, Jonathan P., Sai, Jinshi, Koch, Patrick M., Han, Ilseung, Jørgensen, Jes K., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Narang, Mayank, Ohashi, Nagayoshi, Takakuwa, Shigehisa, Tobin, John J., De Gregorio-monsalvo, Itziar, Lai, Shih-ping, Lee, Jeong-eun, and Tomida, Kengo
Published: 2024

4. Early Planet Formation in Embedded Disks (eDisk):XVI. Asymmetric dust disk driving a multicomponent molecular outflow in the young Class 0 protostar GSS30 IRS3

Author: Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Ohashi, Nagayoshi, Tobin, John J., Sai, Jinshi, Jørgensen, Jes K., Aso, Yusuke, Daniel Lin, Zhe-yu, Flores, Christian, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Plunkett, Adele L., Takakuwa, Shigehisa, R Van’t Hoff, Merel L., Williams, Jonathan P., Yen, Hsi-wei, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Ohashi, Nagayoshi, Tobin, John J., Sai, Jinshi, Jørgensen, Jes K., Aso, Yusuke, Daniel Lin, Zhe-yu, Flores, Christian, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Plunkett, Adele L., Takakuwa, Shigehisa, R Van’t Hoff, Merel L., Williams, Jonathan P., and Yen, Hsi-wei
Published: 2024

5. Early Planet Formation in Embedded Disks. XI. A High-resolution View Toward the BHR 71 Class 0 Protostellar Wide Binary

Author: Gavino, Sacha, Jørgensen, Jes K., Sharma, Rajeeb, Yang, Yao-lun, Li, Zhi-yun, Tobin, John J., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Plunkett, Adele L., Kwon, Woojin, De Gregorio-monsalvo, Itziar, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, Aso, Yusuke, Sai, Jinshi, Aikawa, Yuri, Tomida, Kengo, Koch, Patrick M., Lee, Jeong-eun, Lee, Chang Won, Lai, Shih-ping, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Thieme, Travis J., Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yen, Hsi-wei, Gavino, Sacha, Jørgensen, Jes K., Sharma, Rajeeb, Yang, Yao-lun, Li, Zhi-yun, Tobin, John J., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Plunkett, Adele L., Kwon, Woojin, De Gregorio-monsalvo, Itziar, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, Aso, Yusuke, Sai, Jinshi, Aikawa, Yuri, Tomida, Kengo, Koch, Patrick M., Lee, Jeong-eun, Lee, Chang Won, Lai, Shih-ping, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Thieme, Travis J., Van ’t Hoff, Merel L. R., Williams, Jonathan P., and Yen, Hsi-wei
Published: 2024

6. Early Planet Formation in Embedded Disks (eDisk). XV. Influence of Magnetic Field Morphology in Dense Cores on Sizes of Protostellar Disks

Author: Yen, Hsi-wei, Williams, Jonathan P., Sai, Jinshi, Koch, Patrick M., Han, Ilseung, Jørgensen, Jes K., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Narang, Mayank, Ohashi, Nagayoshi, Takakuwa, Shigehisa, Tobin, John J., De Gregorio-monsalvo, Itziar, Lai, Shih-ping, Lee, Jeong-eun, Tomida, Kengo, Yen, Hsi-wei, Williams, Jonathan P., Sai, Jinshi, Koch, Patrick M., Han, Ilseung, Jørgensen, Jes K., Kwon, Woojin, Lee, Chang Won, Li, Zhi-yun, Looney, Leslie W., Narang, Mayank, Ohashi, Nagayoshi, Takakuwa, Shigehisa, Tobin, John J., De Gregorio-monsalvo, Itziar, Lai, Shih-ping, Lee, Jeong-eun, and Tomida, Kengo
Published: 2024

7. Early Planet Formation in Embedded Disks (eDisk) XIII: Aligned Disks with Non-Settled Dust Around the Newly Resolved Class 0 Protobinary R CrA IRAS 32

Author: Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-Yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lin, Zhe-Yu Daniel, Santamarıa-Miranda, Alejandro, de Gregorio-Monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai, Jinshi, Sharma, Rajeeb, Yen, Hsi-Wei, Han, Ilseung, Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-Yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lin, Zhe-Yu Daniel, Santamarıa-Miranda, Alejandro, de Gregorio-Monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai, Jinshi, Sharma, Rajeeb, Yen, Hsi-Wei, and Han, Ilseung
Abstract: Young protostellar binary systems, with expected ages less than $\sim$10$^5$ years, are little modified since birth, providing key clues to binary formation and evolution. We present a first look at the young, Class 0 binary protostellar system R CrA IRAS 32 from the Early Planet Formation in Embedded Disks (eDisk) ALMA large program, which observed the system in the 1.3 mm continuum emission, $^{12}$CO (2-1), $^{13}$CO (2-1), C$^{18}$O (2-1), SO (6$_5$-5$_4$), and nine other molecular lines that trace disk, envelope, shocks, and outflows. With a continuum resolution of $\sim$0.03$^{\prime\prime}$ ($\sim$5 au, at a distance of 150 pc), we characterize the newly discovered binary system with a separation of 207 au, their circumstellar disks, and a circumbinary disk-like structure. The circumstellar disk radii are 26.9$\pm$0.3 and 22.8$\pm$0.3 au for sources A and B, respectively, and their circumstellar disk dust masses are estimated as 22.5$\pm$1.1 and 12.4$\pm$0.6 M$_{\Earth}$. The circumstellar disks and the circumbinary structure have well aligned position angles and inclinations, indicating formation in a smooth, ordered process such as disk fragmentation. In addition, the circumstellar disks have a near/far-side asymmetry in the continuum emission suggesting that the dust has yet to settle into a thin layer near the midplane. Spectral analysis of CO isotopologues reveals outflows that originate from both of the sources and possibly from the circumbinary disk-like structure. Furthermore, we detect Keplerian rotation in the $^{13}$CO isotopologues toward both circumstellar disks and likely Keplerian rotation in the circumbinary structure; the latter suggests that it is probably a circumbinary disk., Comment: 33 pages, 29 figures, 6 tables
Published: 2024

8. Early Planet Formation in Embedded Disks (eDisk) XIV: Flared Dust Distribution and Viscous Accretion Heating of the Disk around R CrA IRS 7B-a

Author: Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Sai, Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-Wei, Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Sai, Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-Wei
Abstract: We performed radiative transfer calculations and observing simulations to reproduce the 1.3-mm dust-continuum and C$^{18}$O (2-1) images in the Class I protostar R CrA IRS7B-a, observed with the ALMA Large Program ``Early Planet Formation in Embedded Disks (eDisk)". We found that the dust disk model passively heated by the central protostar cannot reproduce the observed peak brightness temperature of the 1.3-mm continuum emission ($\sim$195 K), regardless of the assumptions about the dust opacity. Our calculation suggests that viscous accretion heating in the disk is required to reproduce the observed high brightness temperature. The observed intensity profile of the 1.3-mm dust-continuum emission along the disk minor axis is skewed toward the disk far side. Our modeling reveals that such an asymmetric intensity distribution requires flaring of the dust along the disk's vertical direction with the scale-height following $h/r \sim r^{0.3}$ as function of radius. These results are in sharp contrast to those of Class II disks, which show geometrically flat dust distributions and lower dust temperatures. From our modeling of the C$^{18}$O (2-1) emission, the outermost radius of the gas disk is estimated to be $\sim$80 au, larger than that of the dust disk ($\sim$62 au), to reproduce the observed distribution of the C$^{18}$O (2-1) emission in IRS 7B-a. Our modeling unveils a hot and thick dust disk plus a larger gas disk around one of the eDisk targets, which could be applicable to other protostellar sources in contrast to more evolved sources., Comment: 26 pages, 13 figures
Published: 2024

9. Formation of unipolar outflow and $\textit{protostellar rocket effect}$ in magnetized turbulent molecular cloud cores

Author: Takaishi, Daisuke, Tsukamoto, Yusuke, Kido, Miyu, Takakuwa, Shigehisa, Misugi, Yoshiaki, Kudoh, Yuki, Suto, Yasushi, Takaishi, Daisuke, Tsukamoto, Yusuke, Kido, Miyu, Takakuwa, Shigehisa, Misugi, Yoshiaki, Kudoh, Yuki, and Suto, Yasushi
Abstract: Observed protostellar outflows exhibit a variety of asymmetrical features, including remarkable unipolar outflows and bending outflows. Revealing the formation and early evolution of such asymmetrical protostellar outflows, especially the unipolar outflows, is essential for a better understanding of the star and planet formation because they can dramatically change the mass accretion and angular momentum transport to the protostars and protoplanetary disks. Here, we perform the three-dimensional non-ideal magnetohydrodynamics simulations to investigate the formation and early evolution of the asymmetrical protostellar outflows in magnetized turbulent isolated molecular cloud cores. We find, for the first time to our knowledge, that the unipolar outflow forms even in the single low-mass protostellar system. The results show that the unipolar outflow is driven in the weakly magnetized cloud cores with the dimensionless mass-to-flux ratios of $\mu=8$ and $16$. Furthermore, we find the $\textit{protostellar rocket effect}$ of the unipolar outflow, which is similar to the launch and propulsion of a rocket. The unipolar outflow ejects the protostellar system from the central dense region to the outer region of the parent cloud core, and the ram pressure caused by its ejection suppresses the driving of additional new outflows. In contrast, the bending bipolar outflow is driven in the moderately magnetized cloud core with $\mu=4$. The ratio of the magnetic to turbulent energies of a parent cloud core may play a key role in the formation of asymmetrical protostellar outflows., Comment: 24 pages, 6 figures, accepted for publication in ApJ
Published: 2024

10. Early Planet Formation in Embedded Disks (eDisk). XIII. Aligned Disks with Nonsettled Dust around the Newly Resolved Class 0 Protobinary R CrA IRAS 32

Author: Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai (insa Choi), Jinshi, Sharma, Rajeeb, Yen, Hsi-wei, Han, Ilseung, Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai (insa Choi), Jinshi, Sharma, Rajeeb, Yen, Hsi-wei, and Han, Ilseung
Published: 2024

11. Early Planet Formation in Embedded Disks (eDisk). XIV. Flared Dust Distribution and Viscous Accretion Heating of the Disk around R CrA IRS 7B-a

Author: Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, (insa Choi), Jinshi Sai, Sharma, Rajeeb, Sheehan, Patrick D., Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-wei, Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, (insa Choi), Jinshi Sai, Sharma, Rajeeb, Sheehan, Patrick D., Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-wei
Published: 2024

12. Early Planet Formation in Embedded Disks (eDisk). XIII. Aligned Disks with Nonsettled Dust around the Newly Resolved Class 0 Protobinary R CrA IRAS 32

Author: Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai (insa Choi), Jinshi, Sharma, Rajeeb, Yen, Hsi-wei, Han, Ilseung, Encalada, Frankie J., Looney, Leslie W., Takakuwa, Shigehisa, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes K., Li, Zhi-yun, Aikawa, Yuri, Aso, Yusuke, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lin, Zhe-yu Daniel, Santamaría-miranda, Alejandro, De Gregorio-monsalvo, Itziar, Phuong, Nguyen Thi, Plunkett, Adele, Sai (insa Choi), Jinshi, Sharma, Rajeeb, Yen, Hsi-wei, and Han, Ilseung
Published: 2024

13. Early Planet Formation in Embedded Disks (eDisk). XIV. Flared Dust Distribution and Viscous Accretion Heating of the Disk around R CrA IRS 7B-a

Author: Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, (insa Choi), Jinshi Sai, Sharma, Rajeeb, Sheehan, Patrick D., Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-wei, Takakuwa, Shigehisa, Saigo, Kazuya, Kido, Miyu, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, (insa Choi), Jinshi Sai, Sharma, Rajeeb, Sheehan, Patrick D., Tomida, Kengo, Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-wei
Published: 2024

14. Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359

Author: Thieme, Travis J., Lai, Shih-ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., (insa Choi), Jinshi Sai, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Yen, Hsi-wei, Thieme, Travis J., Lai, Shih-ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., (insa Choi), Jinshi Sai, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, and Yen, Hsi-wei
Published: 2023

15. Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63

Author: Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-yun, Lin, Zhe-yu Daniel, Van ’t Hoff, Merel L. R., Plunkett, Adele L., Yamato, Yoshihide, Sai (insa Choi), Jinshi, Koch, Patrick M., Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, De Gregorio-monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-eun, Lee, Chang Won, Looney, Leslie W., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, Lai, Shih-ping, Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-yun, Lin, Zhe-yu Daniel, Van ’t Hoff, Merel L. R., Plunkett, Adele L., Yamato, Yoshihide, Sai (insa Choi), Jinshi, Koch, Patrick M., Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, De Gregorio-monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-eun, Lee, Chang Won, Looney, Leslie W., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, and Lai, Shih-ping
Published: 2023

16. Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System

Author: Sai, Jinshi, Yen, Hsi-wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Sai, Jinshi, Yen, Hsi-wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, and Williams, Jonathan P.
Published: 2023

17. Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings

Author: Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-yu Daniel, Li, Zhi-yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai (insa Choi), Jinshi, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Santamaría-miranda, Alejandro, Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-ping, Lee, Jeong-eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., Williams, Jonathan P., Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-yu Daniel, Li, Zhi-yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai (insa Choi), Jinshi, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Santamaría-miranda, Alejandro, Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-ping, Lee, Jeong-eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., and Williams, Jonathan P.
Published: 2023

18. Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429

Author: Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jørgensen, Jes K., Tobin, John J., Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Saigo, Kazuya, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Yen, Hsi-wei, Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jørgensen, Jes K., Tobin, John J., Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Saigo, Kazuya, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., and Yen, Hsi-wei
Published: 2023

19. Early Planet Formation in Embedded Disks (eDisk). VII. Keplerian Disk, Disk Substructure, and Accretion Streamers in the Class 0 Protostar IRAS 16544–1604 in CB 68

Author: Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, De Gregorio-monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Thieme, Travis J., Tomida, Kengo, Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-wei, Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, De Gregorio-monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Thieme, Travis J., Tomida, Kengo, Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-wei
Published: 2023

20. Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247

Author: Lin, Zhe Yu Daniel, Li, Zhi Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, van’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Phuong, Nguyen Thi, Sai (Insa Choi), Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi Wei, Lin, Zhe Yu Daniel, Li, Zhi Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, van’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Phuong, Nguyen Thi, Sai (Insa Choi), Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi Wei
Abstract: While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the “Butterfly Star.” With a resolution of 0.″05 (8 au), the 1.3 mm continuum shows an asymmetry along the minor axis that is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.″1 (16 au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for 12CO J = 2-1, 13CO J = 2-1, C18O J = 2-1, H 2CO J = 30,3-20,2, and SO J = 65-54, and constrain the CO midplane snow line to ∼130 au. We find Keplerian rotation around a protostar of 1.6 ± 0.4 M ⊙ using C18O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is ∼6 au at a radius of 100 au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class I source has yet to vertically settle significantly.
Published: 2023

21. Early Planet Formation in Embedded Disks (eDisk). III. A First High-resolution View of Submillimeter Continuum and Molecular Line Emission toward the Class 0 Protostar L1527 IRS

Author: van ’t Hoff, Merel L.R., Tobin, John J., Li, Zhi Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Insa Choi, Jinshi Sai, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih Ping, Phuong, Nguyen Thi, Yen, Hsi Wei, van ’t Hoff, Merel L.R., Tobin, John J., Li, Zhi Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Insa Choi, Jinshi Sai, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih Ping, Phuong, Nguyen Thi, and Yen, Hsi Wei
Abstract: Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here we present Atacama Large Millimeter/submillimeter Array observations of dust continuum at ∼0.″06 (8 au) resolution and molecular line emission at ∼0.″17 (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of 12CO, 13CO, C18O, H2CO, c-C3H2, SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in 12CO. The 13CO brightness temperature and the H2CO line ratio confirm that the disk is too warm for CO freezeout, with the snowline located at ∼350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100″ or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.
Published: 2023

22. Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS

Author: Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Insa Choi, Jinshi Sai, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Li, Zhi Yun, Lin, Zhe Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, van ’t Hoff, Merel L.R., Yen, Hsi Wei, Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Insa Choi, Jinshi Sai, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Li, Zhi Yun, Lin, Zhe Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, van ’t Hoff, Merel L.R., and Yen, Hsi Wei
Abstract: Constraining the physical and chemical structure of young embedded disks is crucial for understanding the earliest stages of planet formation. As part of the Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Large Program, we present high spatial resolution (∼0.″1 or ∼15 au) observations of the 1.3 mm continuum and 13CO J = 2-1, C18O J = 2-1, and SO J N = 65-54 molecular lines toward the disk around the Class I protostar L1489 IRS. The continuum emission shows a ring-like structure at 56 au from the central protostar and tenuous, optically thin emission extending beyond ∼300 au. The 13CO emission traces the warm disk surface, while the C18O emission originates from near the disk midplane. The coincidence of the radial emission peak of C18O with the dust ring may indicate a gap-ring structure in the gaseous disk as well. The SO emission shows a highly complex distribution, including a compact, prominent component at ≲30 au, which is likely to originate from thermally sublimated SO molecules. The compact SO emission also shows a velocity gradient along a direction tilted slightly (∼15°) with respect to the major axis of the dust disk, which we interpret as an inner warped disk in addition to the warp around ∼200 au suggested by previous work. These warped structures may be formed by a planet or companion with an inclined orbit, or by a gradual change in the angular momentum axis during gas infall.
Published: 2023

23. Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results

Author: Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi Yun, Looney, Leslie W., Williams, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai (Insa Choi), Jinshi, Yamato, Yoshihide, Lee, Jeong Eun, Tomida, Kengo, Yen, Hsi Wei, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., van ’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, Mori, Shoji, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi Yun, Looney, Leslie W., Williams, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai (Insa Choi), Jinshi, Yamato, Yoshihide, Lee, Jeong Eun, Tomida, Kengo, Yen, Hsi Wei, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., van ’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, and Mori, Shoji
Abstract: We present an overview of the Large Program, “Early Planet Formation in Embedded Disks (eDisk),” conducted with the Atacama Large Millimeter/submillimeter Array (ALMA). The ubiquitous detections of substructures, particularly rings and gaps, in protoplanetary disks around T Tauri stars raise the possibility that at least some planet formation may have already started during the embedded stages of star formation. In order to address exactly how and when planet formation is initiated, the program focuses on searching for substructures in disks around 12 Class 0 and 7 Class I protostars in nearby (<200 pc) star-forming regions through 1.3 mm continuum observations at a resolution of ∼7 au (0.″04). The initial results show that the continuum emission, mostly arising from dust disks around the sample protostars, has relatively few distinctive substructures, such as rings and spirals, in marked contrast to Class II disks. The dramatic difference may suggest that substructures quickly develop in disks when the systems evolve from protostars to Class II sources, or alternatively that high optical depth of the continuum emission could obscure internal structures. Kinematic information obtained through CO isotopologue lines and other lines reveals the presence of Keplerian disks around protostars, providing us with crucial physical parameters, in particular, the dynamical mass of the central protostars. We describe the background of the eDisk program, the sample selection and their ALMA observations, and the data reduction, and we also highlight representative first-look results.
Published: 2023

24. Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low-Mass and Young Class 0 Protostar, IRAS 15398-3359

Author: Thieme, Travis J., Lai, Shih-Ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Sai, Jinshi, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Yen, Hsi-Wei, Thieme, Travis J., Lai, Shih-Ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Sai, Jinshi, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, and Yen, Hsi-Wei
Abstract: Protostellar disks are a ubiquitous part of the star formation process and the future sites of planet formation. As part of the Early Planet Formation in Embedded Disks (eDisk) large program, we present high-angular resolution dust continuum ($\sim40\,$mas) and molecular line ($\sim150\,$mas) observations of the Class 0 protostar, IRAS 15398-3359. The dust continuum is small, compact, and centrally peaked, while more extended dust structures are found in the outflow directions. We perform a 2D Gaussian fitting to find the deconvolved size and $2\sigma$ radius of the dust disk to be $4.5\times2.8\,\mathrm{au}$ and $3.8\,\mathrm{au}$, respectively. We estimate the gas+dust disk mass assuming optically thin continuum emission to be $0.6-1.8\,M_\mathrm{jup}$, indicating a very low-mass disk. The CO isotopologues trace components of the outflows and inner envelope, while SO traces a compact, rotating disk-like component. Using several rotation curve fittings on the PV diagram of the SO emission, the lower limits of the protostellar mass and gas disk radius are $0.022\,M_\odot$ and $31.2\,\mathrm{au}$ from our Modified 2 single power-law fitting. A conservative upper limit of the protostellar mass is inferred to be $0.1\,M_\odot$. The protostellar mass-accretion rate and the specific angular momentum at the protostellar disk edge are found to be between $1.3-6.1\times10^{-6}\,M_\odot\,\mathrm{yr^{-1}}$ and $1.2-3.8\times10^{-4}\,\mathrm{km\,s^{-1}\,pc}$, respectively, with an age estimated between $0.4-7.5\times10^{4}\,$yr. At this young age with no clear substructures in the disk, planet formation would likely not yet have started. This study highlights the importance of high-resolution observations and systematic fitting procedures when deriving dynamical properties of deeply embedded Class 0 protostars., Comment: 28 pages, 16 figures. Accepted for publication in ApJ as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023

25. Early Planet Formation in Embedded Disks (eDisk) VI: Kinematic Structures around the Very Low Mass Protostar IRAS 16253-2429

Author: Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jorgensen, Jes K., Tobin, John J., Aikawa, Yuri, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Sai, Jinshi, Saigo, Kazuya, Santamaria-Miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Yen, Hsi-Wei, Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jorgensen, Jes K., Tobin, John J., Aikawa, Yuri, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Sai, Jinshi, Saigo, Kazuya, Santamaria-Miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., and Yen, Hsi-Wei
Abstract: Precise estimates of protostellar masses are crucial to characterize the formation of stars of low masses down to brown-dwarfs (BDs; M* < 0.08 Msun). The most accurate estimation of protostellar mass uses the Keplerian rotation in the circumstellar disk around the protostar. To apply the Keplerian rotation method to a protostar at the low-mass end, we have observed the Class 0 protostar IRAS 16253-2429 using the Atacama Large Millimeter/submillimeter Array (ALMA) in the 1.3 mm continuum at an angular resolution of 0.07" (10 au), and in the 12CO, C18O, 13CO (J=2-1), and SO (J_N = 6_5-5_4) molecular lines, as part of the ALMA Large Program Early Planet Formation in Embedded Disks (eDisk). The continuum emission traces a non-axisymmetric, disk-like structure perpendicular to the associated 12CO outflow. The position-velocity (PV) diagrams in the C18O and 13CO lines can be interpreted as infalling and rotating motions. In contrast, the PV diagram along the major axis of the disk-like structure in the 12CO line allows us to identify Keplerian rotation. The central stellar mass and the disk radius are estimated to be ~0.12-0.17 Msun and ~13-19 au, respectively. The SO line suggests the existence of an accretion shock at a ring (r~28 au) surrounding the disk and a streamer from the eastern side of the envelope. IRAS 16253-2429 is not a proto-BD but has a central stellar mass close to the BD mass regime, and our results provide a typical picture of such very low-mass protostars., Comment: 41 pages, 14 figures
Published: 2023

26. Early Planet Formation in Embedded Disks (eDisk) IX: High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and its surrounding

Author: Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-Yu Daniel, Li, Zhi-Yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai, Jinshi, Kwon, Woojin, de Gregorio-Monsalvo, Itziar, Santamaría-Miranda, Alejandro, Yen, Hsi-Wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-Ping, Lee, Jeong-Eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., Williams, Jonathan P., Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-Yu Daniel, Li, Zhi-Yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai, Jinshi, Kwon, Woojin, de Gregorio-Monsalvo, Itziar, Santamaría-Miranda, Alejandro, Yen, Hsi-Wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-Ping, Lee, Jeong-Eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., and Williams, Jonathan P.
Abstract: We present high-resolution, high-sensitivity observations of the Class 0 protostar RCrA IRS5N as part of the Atacama Large Milimeter/submilimeter Array (ALMA) large program Early Planet Formation in Embedded Disks (eDisk). The 1.3 mm continuum emission reveals a flattened continuum structure around IRS5N, consistent with a protostellar disk in the early phases of evolution. The continuum emission appears smooth and shows no substructures. However, a brightness asymmetry is observed along the minor axis of the disk, suggesting the disk is optically and geometrically thick. We estimate the disk mass to be between 0.007 and 0.02 M$_{\odot}$. Furthermore, molecular emission has been detected from various species, including C$^{18}$O (2$-$1), $^{12}$CO (2$-$1), $^{13}$CO (2$-$1), and H$_2$CO (3$_{0,3}-2_{0,2}$, 3$_{2,1}-2_{2,0}$, and 3$_{2,2}-2_{2,1}$). By conducting a position-velocity analysis of the C$^{18}$O (2$-$1) emission, we find that the disk of IRS5N exhibits characteristics consistent with Keplerian rotation around a central protostar with a mass of approximately 0.3 M$_{\odot}$. Additionally, we observe dust continuum emission from the nearby binary source, IRS5a/b. The emission in $^{12}$CO toward IRS5a/b seems to emanate from IRS5b and flow into IRS5a, suggesting material transport between their mutual orbits. The lack of a detected outflow and large-scale negatives in \tlvco~observed toward IRS5N suggests that much of the flux from IRS5N is being resolved out. Due to this substantial surrounding envelope, the central IRS5N protostar is expected to be significantly more massive in the future., Comment: 25 pages, 24 figures. Accepted for publication in ApJ
Published: 2023
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27. Early Planet Formation in Embedded Disks (eDisk) V: Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System

Author: Sai, Jinshi, Yen, Hsi-Wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-Yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Sai, Jinshi, Yen, Hsi-Wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-Yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, and Williams, Jonathan P.
Abstract: We have observed the Class 0/I protostellar system Ced110 IRS4 at an angular resolution of $0.05''$ ($\sim$10 au) as a part of the ALMA large program; Early Planet Formation in the Embedded Disks (eDisk). The 1.3 mm dust continuum emission reveals that Ced110 IRS4 is a binary system with a projected separation of $\sim$250 au. The continuum emissions associated with the main source and its companion, named Ced110 IRS4A and IRS4B respectively, exhibit disk-like shapes and likely arise from dust disks around the protostars. The continuum emission of Ced110 IRS4A has a radius of $\sim$91.7 au ($\sim0.485''$), and shows bumps along its major axis with an asymmetry. The bumps can be interpreted as an shallow, ring-like structure at a radius of $\sim$40 au ($\sim0.2''$) in the continuum emission, as demonstrated from two-dimensional intensity distribution models. A rotation curve analysis on the C$^{18}$O and $^{13}$CO $J=2$-1 lines reveals the presence of a Keplerian disk within a radius of 120 au around Ced110 IRS4A, which supports the interpretation that the dust continuum emission arises from a disk. The ring-like structure in the dust continuum emission might indicate a possible, annular substructure in the surface density of the embedded disk, although the possibility that it is an apparent structure due to the optically thick continuum emission cannot be ruled out., Comment: 32 pages, 23 figures. Accepted for publication in ApJ as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023
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28. Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS

Author: Hoff, Merel L. R. van 't, Tobin, John J., Li, Zhi-Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe-Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Sai, Jinshi, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih-Ping, Phuong, Nguyen Thi, Yen, Hsi-Wei, Hoff, Merel L. R. van 't, Tobin, John J., Li, Zhi-Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe-Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong-Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Sai, Jinshi, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih-Ping, Phuong, Nguyen Thi, and Yen, Hsi-Wei
Abstract: Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at $\sim$0.06" (8 au) resolution and molecular line emission at $\sim$0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures, but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of $^{12}$CO, $^{13}$CO, C$^{18}$O, H$_2$CO, c-C$_3$H$_2$, SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in $^{12}$CO. The $^{13}$CO brightness temperature and the H$_2$CO line ratio confirm that the disk is too warm for CO freeze out, with the snowline located at $\sim$350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100" or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks., Comment: 27 pages, 16 figures, 2 tables, 10 pages appendix with 12 figures. Accepted for publication in ApJ as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023
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29. Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS

Author: Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Sai, Jinshi, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, Hoff, Merel L. R. van 't, Yen, Hsi-Wei, Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Sai, Jinshi, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, Hoff, Merel L. R. van 't, and Yen, Hsi-Wei
Abstract: Constraining the physical and chemical structure of young embedded disks is crucial to understanding the earliest stages of planet formation. As part of the Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Large Program, we present high spatial resolution ($\sim$0$.\!\!^{\prime\prime}$1 or $\sim$15 au) observations of the 1.3 mm continuum and $^{13}$CO $J=$ 2-1, C$^{18}$O $J=$ 2-1, and SO $J_N=$ $6_5$-$5_4$ molecular lines toward the disk around the Class I protostar L1489 IRS. The continuum emission shows a ring-like structure at 56 au from the central protostar and a tenuous, optically thin emission extending beyond $\sim$300 au. The $^{13}$CO emission traces the warm disk surface, while the C$^{18}$O emission originates from near the disk midplane. The coincidence of the radial emission peak of C$^{18}$O with the dust ring may indicate a gap-ring structure in the gaseous disk as well. The SO emission shows a highly complex distribution, including a compact, prominent component at $\lesssim$30 au, which is likely to originate from thermally sublimated SO molecules. The compact SO emission also shows a velocity gradient along a slightly ($\sim15^\circ$) tilted direction with respect to the major axis of the dust disk, which we interpret as an inner warped disk in addition to the warp around $\sim$200 au suggested by previous work. These warped structures may be formed by a planet or companion with an inclined orbit, or by a gradual change in the angular momentum axis during gas infall., Comment: 24 pages, 12 figures. Accepted for publication in The Astrophysical Journal as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023
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30. Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247

Author: Lin, Zhe-Yu Daniel, Li, Zhi-Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, Hoff, Merel L. R. van 't, de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Phuong, Nguyen Thi, Sai, Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-Wei, Lin, Zhe-Yu Daniel, Li, Zhi-Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, Hoff, Merel L. R. van 't, de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Phuong, Nguyen Thi, Sai, Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-Wei
Abstract: While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array (ALMA) large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the ``Butterfly Star." With a resolution of 0.05" (8~au), the 1.3 mm continuum shows an asymmetry along the minor axis which is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.1" (16~au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for $^{12}$CO $J$=2--1, $^{13}$CO $J$=2--1, C$^{18}$O $J$=2--1, $H_{2}$CO $J$=$3_{0,3}$--$2_{0,2}$, and SO $J$=$6_{5}$--$5_{4}$, and constrain the CO midplane snow line to $\sim 130$ au. We find Keplerian rotation around a protostar of $1.6 \pm 0.4 M_{\odot}$ using C$^{18}$O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is $\sim 6$ au at a radius of 100~au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class~I source has yet to vertically settle significantly., Comment: 33 pages, 21 figures. Accepted for publication in ApJ as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023
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31. Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results

Author: Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi-Yun, Looney, Leslie W., Willians, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai, Jinshi, Yamato, Yoshihide, Lee, Jeong-Eun, Tomida, Kengo, Yen, Hsi-Wei, Encalada, Frankie J, Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe-Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., Hoff, Merel L. R. van 't, de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, Mori, Shoji, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi-Yun, Looney, Leslie W., Willians, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai, Jinshi, Yamato, Yoshihide, Lee, Jeong-Eun, Tomida, Kengo, Yen, Hsi-Wei, Encalada, Frankie J, Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe-Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., Hoff, Merel L. R. van 't, de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, and Mori, Shoji
Abstract: We present an overview of the Large Program, ``Early Planet Formation in Embedded Disks (eDisk)'', conducted with the Atacama Large Millimeter/submillimeter Array (ALMA). The ubiquitous detections of substructures, particularly rings and gaps, in protoplanetary disks around T Tauri stars raise the possibility that at least some planet formation may have already started during the embedded stages of star formation. In order to address exactly how and when planet formation is initiated, the program focuses on searching for substructures in disks around 12 Class 0 and 7 Class I protostars in nearby ($< $200 pc) star-forming regions through 1.3 mm continuum observations at a resolution of $\sim7$ au (0.04"). The initial results show that the continuum emission, mostly arising from dust disks around the sample protostars, has relatively few distinctive substructures, such as rings and spirals, in marked contrast to Class II disks. The dramatic difference may suggest that substructures quickly develop in disks when the systems evolve from protostars to Class II sources or alternatively that high optical depth of the continuum emission could obscure internal structures. Kinematic information obtained through CO isotopologue lines and other lines reveals the presence of Keplerian disks around protostars, providing us with crucial physical parameters, in particular, the dynamical mass of the central protostars. We describe the background of the eDisk program, the sample selection and their ALMA observations, the data reduction, and also highlight representative first-look results., Comment: This is a publication of a series of eDisk ALMA large program first-look papers
Published: 2023
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32. Early Planet Formation in Embedded Disks (eDisk). VII. Keplerian Disk, Disk Substructure, and Accretion Streamers in the Class 0 Protostar IRAS 16544-1604 in CB 68

Author: Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., K, Jes, Jørgensen, Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, Sai, Jinshi, Santamarîa-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Tomida, Kengo, Hoff, Merel L. R. van't, Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-Wei, Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., K, Jes, Jørgensen, Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-Ping, Lee, Chang Won, Lee, Jeong-Eun, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, Sai, Jinshi, Santamarîa-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Tomida, Kengo, Hoff, Merel L. R. van't, Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-Wei
Abstract: We present observations of the Class 0 protostar IRAS 16544-1604 in CB 68 from the ''Early Planet Formation in Embedded Disks (eDisk)'' ALMA Large program. The ALMA observations target continuum and lines at 1.3-mm with an angular resolution of $\sim$5 au. The continuum image reveals a dusty protostellar disk with a radius of $\sim$30 au seen close to edge-on, and asymmetric structures both along the major and minor axes. While the asymmetry along the minor axis can be interpreted as the effect of the dust flaring, the asymmetry along the major axis comes from a real non-axisymmetric structure. The C$^{18}$O image cubes clearly show the gas in the disk that follows a Keplerian rotation pattern around a $\sim$0.14 $M_{\odot}$ central protostar. Furthermore, there are $\sim$1500 au-scale streamer-like features of gas connecting from North-East, North-North-West, and North-West to the disk, as well as the bending outflow as seen in the $^{12}$CO (2-1) emission. At the apparent landing point of NE streamer, there are SO (6$_5$-5$_4$) and SiO (5-4) emission detected. The spatial and velocity structure of NE streamer can be interpreted as a free-falling gas with a conserved specific angular momentum, and the detection of the SO and SiO emission at the tip of the streamer implies presence of accretion shocks. Our eDisk observations have unveiled that the Class 0 protostar in CB 68 has a Keplerian rotating disk with flaring and non-axisymmetric structure associated with accretion streamers and outflows., Comment: 30 pages, 24 figures, accepted for publication in The Astrophysical Journal as one of the first-look papers of the eDisk ALMA Large Program
Published: 2023

33. Chemical Differentiation around Five Massive Protostars Revealed by ALMA -Carbon-Chain Species, Oxygen-/Nitrogen-Bearing Complex Organic Molecules

Author: Taniguchi, Kotomi, Majumdar, Liton, Caselli, Paola, Takakuwa, Shigehisa, Hsieh, Tien-Hao, Saito, Masao, Li, Zhi-Yun, Dobashi, Kazuhito, Shimoikura, Tomomi, Nakamura, Fumitaka, Tan, Jonathan C., Herbst, Eric, Taniguchi, Kotomi, Majumdar, Liton, Caselli, Paola, Takakuwa, Shigehisa, Hsieh, Tien-Hao, Saito, Masao, Li, Zhi-Yun, Dobashi, Kazuhito, Shimoikura, Tomomi, Nakamura, Fumitaka, Tan, Jonathan C., and Herbst, Eric
Abstract: We present Atacama Large Millimeter/submillimeter Array Band 3 data toward five massive young stellar objects (MYSOs), and investigate relationships between unsaturated carbon-chain species and saturated complex organic molecules (COMs). An HC$_{5}$N ($J=35-34$) line has been detected from three MYSOs, where nitrogen(N)-bearing COMs (CH$_{2}$CHCN and CH$_{3}$CH$_{2}$CN) have been detected. The HC$_{5}$N spatial distributions show compact features and match with a methanol (CH$_{3}$OH) line with an upper-state energy around 300 K, which should trace hot cores. The hot regions are more extended around the MYSOs where N-bearing COMs and HC$_{5}$N have been detected compared to two MYSOs without these molecular lines, while there are no clear differences in the bolometric luminosity and temperature. We run chemical simulations of hot-core models with a warm-up stage, and compare with the observational results. The observed abundances of HC$_{5}$N and COMs show good agreements with the model at the hot-core stage with temperatures above 160 K. These results indicate that carbon-chain chemistry around the MYSOs cannot be reproduced by warm carbon-chain chemistry, and a new type of carbon-chain chemistry occurs in hot regions around MYSOs., Comment: Accepted by the publication for The Astrophysical Journal Supplement Series, 32 pages,18 figures, 11 tables
Published: 2023
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34. Early Planet Formation in Embedded Disks (eDisk) XII: Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63

Author: Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Hoff, Merel L. R. van 't, Plunkett, Adele L., Yamato, Yoshihide, Sai, Jinshi, Koch, Patrick M., Yen, Hsi-Wei, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-Eun, Lee, Chang Won, Looney, Leslie W., Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, Lai, Shih-Ping, Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-Yun, Lin, Zhe-Yu Daniel, Hoff, Merel L. R. van 't, Plunkett, Adele L., Yamato, Yoshihide, Sai, Jinshi, Koch, Patrick M., Yen, Hsi-Wei, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-Eun, Lee, Chang Won, Looney, Leslie W., Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, and Lai, Shih-Ping
Abstract: We present ALMA observations of the Class I source Oph IRS63 in the context of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA observations of Oph IRS63 show a myriad of protostellar features, such as a shell-like bipolar outflow (in $^{12}$CO), an extended rotating envelope structure (in $^{13}$CO), a streamer connecting the envelope to the disk (in C$^{18}$O), and several small-scale spiral structures seen towards the edge of the dust continuum (in SO). By analyzing the velocity pattern of $^{13}$CO and C$^{18}$O, we measure a protostellar mass of $\rm M_\star = 0.5 \pm 0.2 $~$\rm M_\odot$ and confirm the presence of a disk rotating at almost Keplerian velocity that extends up to $\sim260$ au. These calculations also show that the gaseous disk is about four times larger than the dust disk, which could indicate dust evolution and radial drift. Furthermore, we model the C$^{18}$O streamer and SO spiral structures as features originating from an infalling rotating structure that continuously feeds the young protostellar disk. We compute an envelope-to-disk mass infall rate of $\sim 10^{-6}$~$\rm M_\odot \, yr^{-1}$ and compare it to the disk-to-star mass accretion rate of $\sim 10^{-8}$~$\rm M_\odot \, yr^{-1}$, from which we infer that the protostellar disk is in a mass build-up phase. At the current mass infall rate, we speculate that soon the disk will become too massive to be gravitationally stable., Comment: 26 pages and 17 figures
Published: 2023

35. Early Planet Formation in Embedded Disks (eDisk) X: Compact Disks, Extended Infall, and a Fossil Outburst in the Class I Oph IRS43 Binary

Author: Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jorgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-Yu Daniel, Hoff, Merel L. R. van't, Li, Zhi-Yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-Wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-Eun, Lai, Shih-Ping, Kwon, Woojin, de Gregorio-Monsalvo, Itziar, Sharma, Rajeeb, Lee, Chang Won, Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jorgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-Yu Daniel, Hoff, Merel L. R. van't, Li, Zhi-Yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-Wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-Eun, Lai, Shih-Ping, Kwon, Woojin, de Gregorio-Monsalvo, Itziar, Sharma, Rajeeb, and Lee, Chang Won
Abstract: We present the first results from the Early Planet Formation in Embedded Disks (eDisk) ALMA Large Program toward Oph IRS43, a binary system of solar mass protostars. The 1.3 mm dust continuum observations resolve a compact disk, ~6au radius, around the northern component and show that the disk around the southern component is even smaller, <~3 au. CO, 13CO, and C18O maps reveal a large cavity in a low mass envelope that shows kinematic signatures of rotation and infall extending out to ~ 2000au. An expanding CO bubble centered on the extrapolated location of the source ~130 years ago suggests a recent outburst. Despite the small size of the disks, the overall picture is of a remarkably large and dynamically active region., Comment: Paper 10 of the ALMA eDisk Large Program. Accepted for publication in ApJ
Published: 2023

36. Early Planet Formation in Embedded Disks (eDisk). X. Compact Disks, Extended Infall, and a Fossil Outburst in the Class I Oph IRS43 Binary

Author: Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jørgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-yu Daniel, Van’t Hoff, Merel L. R., Li, Zhi-yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-eun, Lai, Shih-ping, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Sharma, Rajeeb, Lee, Chang Won, Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jørgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-yu Daniel, Van’t Hoff, Merel L. R., Li, Zhi-yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-eun, Lai, Shih-ping, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Sharma, Rajeeb, and Lee, Chang Won
Published: 2023

37. Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low Mass and Young Class 0 Protostar IRAS 15398–3359

Author: Thieme, Travis J., Lai, Shih-ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., (insa Choi), Jinshi Sai, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Yen, Hsi-wei, Thieme, Travis J., Lai, Shih-ping, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., (insa Choi), Jinshi Sai, Aso, Yusuke, Williams, Jonathan P., Yamato, Yoshihide, Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kwon, Woojin, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, Plunkett, Adele L., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, and Yen, Hsi-wei
Published: 2023

38. Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63

Author: Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-yun, Lin, Zhe-yu Daniel, Van ’t Hoff, Merel L. R., Plunkett, Adele L., Yamato, Yoshihide, Sai (insa Choi), Jinshi, Koch, Patrick M., Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, De Gregorio-monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-eun, Lee, Chang Won, Looney, Leslie W., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, Lai, Shih-ping, Flores, Christian, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Li, Zhi-yun, Lin, Zhe-yu Daniel, Van ’t Hoff, Merel L. R., Plunkett, Adele L., Yamato, Yoshihide, Sai (insa Choi), Jinshi, Koch, Patrick M., Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, De Gregorio-monsalvo, Itziar, Kido, Miyu, Kwon, Woojin, Lee, Jeong-eun, Lee, Chang Won, Looney, Leslie W., Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Williams, Jonathan P., Han, Ilseung, Narayanan, Suchitra, and Lai, Shih-ping
Published: 2023

39. Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings

Author: Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-yu Daniel, Li, Zhi-yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai (insa Choi), Jinshi, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Santamaría-miranda, Alejandro, Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-ping, Lee, Jeong-eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., Williams, Jonathan P., Sharma, Rajeeb, Jørgensen, Jes K., Gavino, Sacha, Ohashi, Nagayoshi, Tobin, John J., Lin, Zhe-yu Daniel, Li, Zhi-yun, Takakuwa, Shigehisa, Lee, Chang Won, Sai (insa Choi), Jinshi, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Santamaría-miranda, Alejandro, Yen, Hsi-wei, Aikawa, Yuri, Aso, Yusuke, Lai, Shih-ping, Lee, Jeong-eun, Looney, Leslie W., Phuong, Nguyen Thi, Thieme, Travis J., and Williams, Jonathan P.
Published: 2023

40. Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System

Author: Sai, Jinshi, Yen, Hsi-wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Sai, Jinshi, Yen, Hsi-wei, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Saigo, Kazuya, Aso, Yusuke, Lin, Zhe-yu Daniel, Koch, Patrick M., Aikawa, Yuri, Flores, Christian, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Looney, Leslie W., Mori, Shoji, Phuong, Nguyen Thi, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, and Williams, Jonathan P.
Published: 2023

41. Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429

Author: Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jørgensen, Jes K., Tobin, John J., Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Saigo, Kazuya, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., Yen, Hsi-wei, Aso, Yusuke, Kwon, Woojin, Ohashi, Nagayoshi, Jørgensen, Jes K., Tobin, John J., Aikawa, Yuri, De Gregorio-monsalvo, Itziar, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Narayanan, Suchitra, Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Saigo, Kazuya, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Takakuwa, Shigehisa, Thieme, Travis J., Tomida, Kengo, Williams, Jonathan P., and Yen, Hsi-wei
Published: 2023

42. Early Planet Formation in Embedded Disks (eDisk). VII. Keplerian Disk, Disk Substructure, and Accretion Streamers in the Class 0 Protostar IRAS 16544–1604 in CB 68

Author: Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, De Gregorio-monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Thieme, Travis J., Tomida, Kengo, Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi-wei, Kido, Miyu, Takakuwa, Shigehisa, Saigo, Kazuya, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Aikawa, Yuri, Aso, Yusuke, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, De Gregorio-monsalvo, Itziar, Han, Ilseung, Hirano, Shingo, Koch, Patrick M., Kwon, Woojin, Lai, Shih-ping, Lee, Chang Won, Lee, Jeong-eun, Li, Zhi-yun, Lin, Zhe-yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Plunkett, Adele L., Phuong, Nguyen Thi, (insa Choi), Jinshi Sai, Santamaría-miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Thieme, Travis J., Tomida, Kengo, Van ’t Hoff, Merel L. R., Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi-wei
Published: 2023

43. Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results

Author: Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi Yun, Looney, Leslie W., Williams, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai (Insa Choi), Jinshi, Yamato, Yoshihide, Lee, Jeong Eun, Tomida, Kengo, Yen, Hsi Wei, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., van ’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, Mori, Shoji, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Sheehan, Patrick, Aikawa, Yuri, Li, Zhi Yun, Looney, Leslie W., Williams, Jonathan P., Aso, Yusuke, Sharma, Rajeeb, Sai (Insa Choi), Jinshi, Yamato, Yoshihide, Lee, Jeong Eun, Tomida, Kengo, Yen, Hsi Wei, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Kido, Miyu, Han, Ilseung, Lin, Zhe Yu Daniel, Narayanan, Suchitra, Phuong, Nguyen Thi, Santamaría-Miranda, Alejandro, Thieme, Travis J., van ’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Plunkett, Adele, Saigo, Kazuya, Hirano, Shingo, Lam, Ka Ho, and Mori, Shoji
Abstract: We present an overview of the Large Program, “Early Planet Formation in Embedded Disks (eDisk),” conducted with the Atacama Large Millimeter/submillimeter Array (ALMA). The ubiquitous detections of substructures, particularly rings and gaps, in protoplanetary disks around T Tauri stars raise the possibility that at least some planet formation may have already started during the embedded stages of star formation. In order to address exactly how and when planet formation is initiated, the program focuses on searching for substructures in disks around 12 Class 0 and 7 Class I protostars in nearby (<200 pc) star-forming regions through 1.3 mm continuum observations at a resolution of ∼7 au (0.″04). The initial results show that the continuum emission, mostly arising from dust disks around the sample protostars, has relatively few distinctive substructures, such as rings and spirals, in marked contrast to Class II disks. The dramatic difference may suggest that substructures quickly develop in disks when the systems evolve from protostars to Class II sources, or alternatively that high optical depth of the continuum emission could obscure internal structures. Kinematic information obtained through CO isotopologue lines and other lines reveals the presence of Keplerian disks around protostars, providing us with crucial physical parameters, in particular, the dynamical mass of the central protostars. We describe the background of the eDisk program, the sample selection and their ALMA observations, and the data reduction, and we also highlight representative first-look results.
Published: 2023

44. Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS

Author: Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Insa Choi, Jinshi Sai, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Li, Zhi Yun, Lin, Zhe Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, van ’t Hoff, Merel L.R., Yen, Hsi Wei, Yamato, Yoshihide, Aikawa, Yuri, Ohashi, Nagayoshi, Tobin, John J., Jørgensen, Jes K., Takakuwa, Shigehisa, Aso, Yusuke, Insa Choi, Jinshi Sai, Flores, Christian, de Gregorio-Monsalvo, Itziar, Hirano, Shingo, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Li, Zhi Yun, Lin, Zhe Yu Daniel, Looney, Leslie W., Mori, Shoji, Narayanan, Suchitra, Phuong, Nguyen Thi, Saigo, Kazuya, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Thieme, Travis J., Tomida, Kengo, van ’t Hoff, Merel L.R., and Yen, Hsi Wei
Abstract: Constraining the physical and chemical structure of young embedded disks is crucial for understanding the earliest stages of planet formation. As part of the Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Large Program, we present high spatial resolution (∼0.″1 or ∼15 au) observations of the 1.3 mm continuum and 13CO J = 2-1, C18O J = 2-1, and SO J N = 65-54 molecular lines toward the disk around the Class I protostar L1489 IRS. The continuum emission shows a ring-like structure at 56 au from the central protostar and tenuous, optically thin emission extending beyond ∼300 au. The 13CO emission traces the warm disk surface, while the C18O emission originates from near the disk midplane. The coincidence of the radial emission peak of C18O with the dust ring may indicate a gap-ring structure in the gaseous disk as well. The SO emission shows a highly complex distribution, including a compact, prominent component at ≲30 au, which is likely to originate from thermally sublimated SO molecules. The compact SO emission also shows a velocity gradient along a direction tilted slightly (∼15°) with respect to the major axis of the dust disk, which we interpret as an inner warped disk in addition to the warp around ∼200 au suggested by previous work. These warped structures may be formed by a planet or companion with an inclined orbit, or by a gradual change in the angular momentum axis during gas infall.
Published: 2023

45. Early Planet Formation in Embedded Disks (eDisk). III. A First High-resolution View of Submillimeter Continuum and Molecular Line Emission toward the Class 0 Protostar L1527 IRS

Author: van ’t Hoff, Merel L.R., Tobin, John J., Li, Zhi Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Insa Choi, Jinshi Sai, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih Ping, Phuong, Nguyen Thi, Yen, Hsi Wei, van ’t Hoff, Merel L.R., Tobin, John J., Li, Zhi Yun, Ohashi, Nagayoshi, Jørgensen, Jes K., Lin, Zhe Yu Daniel, Aikawa, Yuri, Aso, Yusuke, de Gregorio-Monsalvo, Itziar, Gavino, Sacha, Han, Ilseung, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Lee, Jeong Eun, Looney, Leslie W., Narayanan, Suchitra, Plunkett, Adele, Insa Choi, Jinshi Sai, Santamaría-Miranda, Alejandro, Sharma, Rajeeb, Sheehan, Patrick D., Takakuwa, Shigehisa, Thieme, Travis J., Williams, Jonathan P., Lai, Shih Ping, Phuong, Nguyen Thi, and Yen, Hsi Wei
Abstract: Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here we present Atacama Large Millimeter/submillimeter Array observations of dust continuum at ∼0.″06 (8 au) resolution and molecular line emission at ∼0.″17 (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of 12CO, 13CO, C18O, H2CO, c-C3H2, SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in 12CO. The 13CO brightness temperature and the H2CO line ratio confirm that the disk is too warm for CO freezeout, with the snowline located at ∼350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100″ or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.
Published: 2023

46. Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247

Author: Lin, Zhe Yu Daniel, Li, Zhi Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, van’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Phuong, Nguyen Thi, Sai (Insa Choi), Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, Yen, Hsi Wei, Lin, Zhe Yu Daniel, Li, Zhi Yun, Tobin, John J., Ohashi, Nagayoshi, Jørgensen, Jes Kristian, Looney, Leslie W., Aso, Yusuke, Takakuwa, Shigehisa, Aikawa, Yuri, van’t Hoff, Merel L.R., de Gregorio-Monsalvo, Itziar, Encalada, Frankie J., Flores, Christian, Gavino, Sacha, Han, Ilseung, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lai, Shih Ping, Lee, Chang Won, Lee, Jeong Eun, Phuong, Nguyen Thi, Sai (Insa Choi), Jinshi, Sharma, Rajeeb, Sheehan, Patrick, Thieme, Travis J., Williams, Jonathan P., Yamato, Yoshihide, and Yen, Hsi Wei
Abstract: While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the “Butterfly Star.” With a resolution of 0.″05 (8 au), the 1.3 mm continuum shows an asymmetry along the minor axis that is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.″1 (16 au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for 12CO J = 2-1, 13CO J = 2-1, C18O J = 2-1, H 2CO J = 30,3-20,2, and SO J = 65-54, and constrain the CO midplane snow line to ∼130 au. We find Keplerian rotation around a protostar of 1.6 ± 0.4 M ⊙ using C18O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is ∼6 au at a radius of 100 au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class I source has yet to vertically settle significantly.
Published: 2023

47. Early Planet Formation in Embedded Disks (eDisk). X. Compact Disks, Extended Infall, and a Fossil Outburst in the Class I Oph IRS43 Binary

Author: Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jørgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-yu Daniel, Van’t Hoff, Merel L. R., Li, Zhi-yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-eun, Lai, Shih-ping, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Sharma, Rajeeb, Lee, Chang Won, Narayanan, Suchitra, Williams, Jonathan P., Tobin, John J., Jørgensen, Jes K., Ohashi, Nagayoshi, Lin, Zhe-yu Daniel, Van’t Hoff, Merel L. R., Li, Zhi-yun, Plunkett, Adele L., Looney, Leslie W., Takakuwa, Shigehisa, Yen, Hsi-wei, Aso, Yusuke, Flores, Christian, Lee, Jeong-eun, Lai, Shih-ping, Kwon, Woojin, De Gregorio-monsalvo, Itziar, Sharma, Rajeeb, and Lee, Chang Won
Published: 2023

48. Vibrationally-excited Lines of HC$_{3}$N Associated with the Molecular Disk around the G24.78+0.08 A1 Hyper-compact H$_{\rm {II}}$ Region

Author: Taniguchi, Kotomi, Tanaka, Kei E. I., Zhang, Yichen, Fedriani, Rubén, Tan, Jonathan C., Takakuwa, Shigehisa, Nakamura, Fumitaka, Saito, Masao, Herbst, Eric, Taniguchi, Kotomi, Tanaka, Kei E. I., Zhang, Yichen, Fedriani, Rubén, Tan, Jonathan C., Takakuwa, Shigehisa, Nakamura, Fumitaka, Saito, Masao, and Herbst, Eric
Abstract: We have analyzed Atacama Large Millimeter/submillimeter Array Band 6 data of the hyper-compact H$_{\rm {II}}$ region G24.78+0.08 A1 (G24 HC H$_{\rm {II}}$) and report the detection of vibrationally-excited lines of HC$_{3}$N ($v_{7}=2$, $J=24-23$). The spatial distribution and kinematics of a vibrationally-excited line of HC$_{3}$N ($v_{7}=2$, $J=24-23$, $l=2e$) are found to be similar to the CH$_{3}$CN vibrationally-excited line ($v_{8}=1$), which indicates that the HC$_{3}$N emission is tracing the disk around the G24 HC H$_{\rm {II}}$ region previously identified by the CH$_{3}$CN lines. We derive the $^{13}$CH$_{3}$CN/HC$^{13}$CCN abundance ratios around G24 and compare them to the CH$_{3}$CN/HC$_{3}$N abundance ratios in disks around Herbig Ae and T Tauri stars. The $^{13}$CH$_{3}$CN/HC$^{13}$CCN ratios around G24 ($\sim 3.0-3.5$) are higher than the CH$_{3}$CN/HC$_{3}$N ratios in the other disks ($\sim 0.03-0.11$) by more than one order of magnitude. The higher CH$_{3}$CN/HC$_{3}$N ratios around G24 suggest that the thermal desorption of CH$_{3}$CN in the hot dense gas and efficient destruction of HC$_{3}$N in the region irradiated by the strong UV radiation are occurring. Our results indicate that the vibrationally-excited HC$_{3}$N lines can be used as a disk tracer of massive protostars at the HC H$_{\rm {II}}$ region stage, and the combination of these nitrile species will provide information of not only chemistry but also physical conditions of the disk structures., Comment: 21 pages, 13 figures, 5 tables, Accepted by The Astrophysical Journal
Published: 2022

49. A VLA View of the Flared, Asymmetric Disk around the Class 0 Protostar L1527 IRS

Author: Sheehan, Patrick D., Tobin, John J., Li, Zhi-Yun, Hoff, Merel L. R. van 't, Jorgensen, Jes K., Kwon, Woojin, Looney, Leslie W., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Williams, Jonathan P., Aso, Yusuke, Gavino, Sacha, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Lee, Chang Won, Plunkett, Adele, Sharma, Rajeeb, Aikawa, Yuri, Lai, Shih-Ping, Lee, Jeong-Eun, Lin, Zhe-Yu Daniel, Saigo, Kazuya, Tomida, Kengo, Yen, Hsi-Wei, Sheehan, Patrick D., Tobin, John J., Li, Zhi-Yun, Hoff, Merel L. R. van 't, Jorgensen, Jes K., Kwon, Woojin, Looney, Leslie W., Ohashi, Nagayoshi, Takakuwa, Shigehisa, Williams, Jonathan P., Aso, Yusuke, Gavino, Sacha, de Gregorio-Monsalvo, Itziar, Han, Ilseung, Lee, Chang Won, Plunkett, Adele, Sharma, Rajeeb, Aikawa, Yuri, Lai, Shih-Ping, Lee, Jeong-Eun, Lin, Zhe-Yu Daniel, Saigo, Kazuya, Tomida, Kengo, and Yen, Hsi-Wei
Abstract: 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.
Published: 2022

50. Increasing mass-to-flux ratio from the dense core to the protostellar envelope around the Class 0 protostar HH 211

Author: Yen, Hsi-Wei, Koch, Patrick, Lee, Chin-Fei, Hirano, Naomi, Ohashi, Nagayoshi, Sai, Jinshi, Takakuwa, Shigehisa, Tang, Ya-Wen, Tatematsu, Ken'ichi, Zhao, Bo, Yen, Hsi-Wei, Koch, Patrick, Lee, Chin-Fei, Hirano, Naomi, Ohashi, Nagayoshi, Sai, Jinshi, Takakuwa, Shigehisa, Tang, Ya-Wen, Tatematsu, Ken'ichi, and Zhao, Bo
Abstract: To study transportation of magnetic flux from large to small scales in protostellar sources, we analyzed the Nobeyama 45-m N2H+ (1-0), JCMT 850 um polarization, and ALMA C18O (2-1) and 1.3 mm and 0.8 mm (polarized) continuum data of the Class 0 protostar HH 211. The magnetic field strength in the dense core on a 0.1 pc scale was estimated with the single-dish line and polarization data using the Davis-Chandrasekhar-Fermi method, and that in the protostellar envelope on a 600 au scale was estimated from the force balance between the gravity and magnetic field tension by analyzing the gas kinematics and magnetic field structures with the ALMA data. Our analysis suggests that from 0.1 pc to 600 au scales, the magnetic field strength increases from 40-107 uG to 0.3-1.2 mG with a scaling relation between the magnetic field strength and density of $B \propto \rho^{0.36\pm0.08}$, and the mass-to-flux ratio increases from 1.2-3.7 to 9.1-32.3. The increase in the mass-to-flux ratio could suggest that the magnetic field is partially decoupled from the neutral matter between 0.1 pc and 600 au scales, and hint at efficient ambipolar diffusion in the infalling protostellar envelope in HH 211, which is the dominant non-ideal magnetohydrodynamic effect considering the density on these scales. Thus, our results could support the scenario of efficient ambipolar diffusion enabling the formation of the 20 au Keplerian disk in HH 211., Comment: 27 pages, 12 figures, accepted by ApJ
Published: 2022
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