The circumstellar environment of IRAS 05327+3404

E. A. Magnier, L. B.F.M. Waters, P. J. Groot, M. E. Van Den Ancker, Y. J. Kuan, E. L. Martin

    Research output: Contribution to journalArticlepeer-review

    8 Citations (Scopus)

    Abstract

    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.

    Original languageEnglish
    Pages (from-to)441-452
    Number of pages12
    JournalAstronomy and Astrophysics
    Volume346
    Issue number2
    Publication statusPublished - 1999 Dec 1

    Keywords

    • Stars: circumstellar matter
    • Stars: evolution
    • Stars: formation
    • Stars: mass-loss
    • Stars: pre-main sequence

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Fingerprint Dive into the research topics of 'The circumstellar environment of IRAS 05327+3404'. Together they form a unique fingerprint.

    Cite this