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

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 li...

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Bibliographic Details
Published in:The Astrophysical journal 2017-07, Vol.844 (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: Article
Language:English
Subjects:
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
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Summary: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 .
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa799e