TY - JOUR
T1 - The circumstellar environment of IRAS 05327+3404
AU - Magnier, E. A.
AU - Waters, L. B.F.M.
AU - Groot, P. J.
AU - Van Den Ancker, M. E.
AU - Kuan, Y. J.
AU - Martin, E. L.
PY - 1999
Y1 - 1999
N2 - We continue our study of the young stellar object associated with IRAS 05327+3404. We have determined the spectral type of the central star to be K2. We show that the star is most likely seen directly, not via a reflection, and that the extinction is only Av ∼ 2.3 mag. The spectral energy distribution shows the presence of large amounts of circumstellar material. Near-IR and optical observations of the reflection nebula also demonstrate the presence of circumstellar material, and show the material to be arranged in a disk with a relatively wide central hole of ∼33° opening angle. The central hole and a CO outflow are co-aligned, and are roughly aligned with the ionized outflow. Several surprising aspects remain: Although the system has a strong ionized outflow, there is little or no evidence of active accretion in the form of UV excess, veiling, or strong high-Balmer line emission. Also, the spectral energy distribution is very wide, and suggests that the original birth cloud had a large rotational velocity. We propose that the relative isolation of the system from other star formation activity may explain the relatively large circumstellar disk for a system with a well-exposed central star.
AB - We continue our study of the young stellar object associated with IRAS 05327+3404. We have determined the spectral type of the central star to be K2. We show that the star is most likely seen directly, not via a reflection, and that the extinction is only Av ∼ 2.3 mag. The spectral energy distribution shows the presence of large amounts of circumstellar material. Near-IR and optical observations of the reflection nebula also demonstrate the presence of circumstellar material, and show the material to be arranged in a disk with a relatively wide central hole of ∼33° opening angle. The central hole and a CO outflow are co-aligned, and are roughly aligned with the ionized outflow. Several surprising aspects remain: Although the system has a strong ionized outflow, there is little or no evidence of active accretion in the form of UV excess, veiling, or strong high-Balmer line emission. Also, the spectral energy distribution is very wide, and suggests that the original birth cloud had a large rotational velocity. We propose that the relative isolation of the system from other star formation activity may explain the relatively large circumstellar disk for a system with a well-exposed central star.
KW - Stars: circumstellar matter
KW - Stars: evolution
KW - Stars: formation
KW - Stars: mass-loss
KW - Stars: pre-main sequence
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M3 - Article
AN - SCOPUS:4243239409
VL - 346
SP - 441
EP - 452
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
IS - 2
ER -