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Title:
Probable Association of T Tauri Stars with the L 1014 Dense Core
Authors:
Morita, Atsuko; Watanabe, Makoto; Sugitani, Koji; Itoh, Yoichi; Uehara, Mariko; Nagashima, Chie; Ebizuka, Noboru; Hasegawa, Takashi; Kinugasa, Kenzo; Tamura, Motohide
Affiliation:
AA(Graduate School of Natural Sciences, Nagoya City University, Nagoya 467-8501) AB(Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA) AC(Graduate School of Natural Sciences, Nagoya City University, Nagoya 467-8501) AD(Graduate School of Science and Technology, Kobe University, Kobe 657-8501) AE(Department of Astrophysics, Nagoya University, Nagoya 464-8602) AF(Department of Astrophysics, Nagoya University, Nagoya 464-8602) AG(RIKEN, Wako, Saitama 351-0198; National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588) AH(Gunma Astronomical Observatory, Takayama-mura Agatsuma-gun Gunma 377-0702) AI(Gunma Astronomical Observatory, Takayama-mura Agatsuma-gun, Gunma 377-0702) AJ(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588)
Publication:
Publications of the Astronomical Society of Japan, Vol.58, No.5, pp.L41-L45 (PASJ Homepage)
Publication Date:
10/2006
Origin:
PASJ
Keywords:
ISM: globules -- ISM: individual (L 1014) -- stars: distances -- stars: formation -- stars: low-mass, brown dwarfs -- stars: pre-main sequence
Bibliographic Code:
2006PASJ...58L..41M

Abstract

Using the Wide Field Grism Spectrograph 2 (WFGS2), we carried out slit-less spectroscopy, g'r'i' photometry, and slit spectroscopy on the L 1014 dense core. We detected three Hα emission-line stars. We interpret one as being a weak-line T Tauri star (WTTS) and the others as classical T Tauri stars (CTTS). Since their g'‑i' colors and/or classified spectral types are consistent with those of T Tauri stars and two of them show less extinction than the cloud, these three stars are likely to be T Tauri stars associated with L 1014. Adopting an age range for T Tauri stars, 1-10Myr, the color-magnitude diagram suggests a distance of ˜ 400-900 pc, rather than the previously assumed distance, 200pc. This could strongly affect the mass estimate of L 1014-IRS, which is thought to be either a very young protostar or proto-brown dwarf.
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