Inner Warm Disk of ESO Hα 279a Revealed by NA i and CO Overtone Emission Lines

• Published in: The Astrophysical journal Vol. 844; no. 1; p. 4
• Main Authors: Lyo, A-Ran, Kim, Jongsoo, Lee, Jae-Joon, Kim, Kyoung-Hee, Kang, Jihyun, Byun, Do-Young, Mace, Gregory, Sokal, Kimberly R., Park, Chan, Chun, Moo-Young, Oh, Heeyoung, Yu, Young Sam, Oh, Jae Sok, Jeong, Ueejeong, Kim, Hwihyun, Pak, Soojong, Hwang, Narae, Park, Byeong-Gon, Lee, Sungho, Kaplan, Kyle, Lee, Hye-In, Le, Huynh Anh Nguyen, Jaffe, Daniel
• Format: Journal Article
• Language: English
• Published: Philadelphia IOP Publishing 20.07.2017
• Subjects: Accretion; Accretion disks; Astrophysics; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CALCIUM; CARBON MONOXIDE; Channel flow; COMPUTERIZED SIMULATION; DISTANCE; EMISSION; Emission analysis; Emission lines; Emission measurements; Gratings (spectra); HYDROGEN; Infrared analysis; INFRARED SPECTROMETERS; IRON; LUMINOSITY; MASS; Near infrared radiation; PROTOPLANETS; PROTOSTARS; RECOMBINATION; SODIUM; SPECTRA; Spectroscopy; Star formation; STARS; Submerging; SYMMETRY; WATER
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aa799e

Abstract We present an analysis of near-infrared, high-resolution spectroscopy toward the flat-spectrum young stellar object (YSO) ESO H α 279a (∼1.5 M ⊙ ) in the Serpens star-forming region at a distance of 429 pc. Using the Immersion GRating INfrared Spectrometer (IGRINS; R ≈ 45,000), we detect emission lines originating from the accretion channel flow, jet, and inner disk. Specifically, we identify hydrogen Brackett series recombination, [Fe ii ], [Fe iii ], [Fe iv ], Ca i , Na i , H 2 , H 2 O, and CO overtone emission lines. By modeling five bands of CO overtone emission lines and the symmetric double-peaked line profile for Na i emission lines, we find that ESO H α 279a has an actively accreting Keplerian disk. From our Keplerian disk model, we find that Na i emission lines originate between 0.04 and 1.00 au, while the CO overtone emission lines are from the outer part of the disk, in the range between 0.22 and 3.00 au. The model reveals that the neutral atomic Na gas is a good tracer of the innermost region of the actively accreting disk. We derive a mass accretion rate of M ⊙ yr −1  from the measured Br γ emission luminosity of 1.78(±0.31) × 10 31 erg s −1 .