Early Planet Formation in Embedded Disks (eDisk) XII: Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63

Christian Flores Gonzalez^1*, Nagayoshi Ohashi¹, John J Tobin², Jes K Jorgensen³, Shigehisa Takakuwa⁴, Zhi-Yun Li⁵, Zhe-Yu Daniel Lin⁵, Merel L.R. van ’t Hoff⁶, Adele L. Plunkett², Yoshihide Yamato⁷, Jinshi Sai (Insa Choi)¹, Patrick M. Koch¹, Hsi-Wei Yen¹, Yuri Aikawa⁷, Yusuke Aso⁸, Itziar de Gregorio-Monsalvo⁹, Miyu Kido⁴, Woojin Kwon¹⁰, Jeong-Eun Lee¹⁰, Chang Won Lee⁸, Leslie W. Looney¹¹, Alejandro Santamaria-Miranda⁹, Rajeeb Sharma³, Travis J. Thieme¹², Jonathan P. Williams¹³, Ilseung Han⁸, Suchitra Narayanan¹³, Shih-Ping Lai¹²

¹Astronomy and Astrophyisics, Academia Sinica, Taipei, Taiwan
²NRAO, USA
³Niels Bohr Institute, Denmark
⁴Kagoshima University, Japan
⁵University of Virginia, USA
⁶University of Michigan, USA
⁷The University of Tokyo, Japan
⁸KASI, Korea
⁹ESO, Chile
¹⁰Seoul National University, Korea
¹¹University of Illinois, USA
¹²National Tsing Hua University, Taiwan
¹³University of Hawaii at Manoa, USA

* Presenter:Christian Flores Gonzalez, email:caflores@asiaa.sinica.edu.tw

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.

Keywords: Protostars, Protoplanetary disks, Star formation, Planet formation