Star formation in the L1333 molecular cloud in cassiopeia

Ayano Obayashi, M. Kun, Fumio Sato, Yoshinori Yonekura, Yasuo Fukui

Research output: Contribution to journalArticle

22 Citations (Scopus)

Abstract

Radio and optical observations have been made in order to examine star formation in the dark cloud L1333 [α(1950) = 2h21m.0, δ(1950) = 75°15′]. A study of the cumulative distribution of field star distance moduli yields a distance value close to 180 pc for the L1333 molecular cloud. 13CO observations revealed two filamentary molecular clouds with distinct velocities of VLSR ∼ -2 and 3 km s-1, respectively. Thirteen C18O cores, characterized by an average molecular mass (MLTE) of ∼9 M and a mean density of ∼1.4 × 104 cm-3, are embedded in the two 13CO clouds. We have detected 18 Hα emission-line stars projected within or near the 13CO clouds on objective-prism plates. They can be regarded as candidate pre-main-sequence stars formed in the clouds. Five IRAS sources with flux density distributions characteristic of young stellar objects (YSOs) are found in the area of the cloud. Three of the IRAS sources coincide with Hα emission-line stars, the others with faint stars without detected Hα emission. One of the latter sources is associated with a C18O core and exhibits a protostar-type infrared spectrum. The IRAS source exhibits a winglike feature of ∼1.6 km s-1 (full width at zero intensity) in C18O, which may indicate that the YSO has an outflow. We note that the C18O core has the smallest ratio of virial mass (Mvir) to MLTE among the C18O cores in L1333, suggesting that star formation occurs preferentially in a core whose internal kinetic energy is low compared with the self-gravitational energy. A possible scenario for the past star formation activity is discussed.

Original languageEnglish
Pages (from-to)274-285
Number of pages12
JournalAstronomical Journal
Volume115
Issue number1
Publication statusPublished - Jan 1998

Fingerprint

molecular clouds
star formation
Infrared Astronomy Satellite
stars
pre-main sequence stars
star distribution
radio observation
protostars
prisms
kinetic energy
density distribution
outflow
infrared spectra
flux density
radio
energy
distribution
young

Keywords

  • ISM: clouds
  • ISM: individual (L1333)
  • ISM: molecules
  • Stars: pre-main sequence

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Obayashi, A., Kun, M., Sato, F., Yonekura, Y., & Fukui, Y. (1998). Star formation in the L1333 molecular cloud in cassiopeia. Astronomical Journal, 115(1), 274-285.

Star formation in the L1333 molecular cloud in cassiopeia. / Obayashi, Ayano; Kun, M.; Sato, Fumio; Yonekura, Yoshinori; Fukui, Yasuo.

In: Astronomical Journal, Vol. 115, No. 1, 01.1998, p. 274-285.

Research output: Contribution to journalArticle

Obayashi, A, Kun, M, Sato, F, Yonekura, Y & Fukui, Y 1998, 'Star formation in the L1333 molecular cloud in cassiopeia', Astronomical Journal, vol. 115, no. 1, pp. 274-285.
Obayashi A, Kun M, Sato F, Yonekura Y, Fukui Y. Star formation in the L1333 molecular cloud in cassiopeia. Astronomical Journal. 1998 Jan;115(1):274-285.
Obayashi, Ayano ; Kun, M. ; Sato, Fumio ; Yonekura, Yoshinori ; Fukui, Yasuo. / Star formation in the L1333 molecular cloud in cassiopeia. In: Astronomical Journal. 1998 ; Vol. 115, No. 1. pp. 274-285.
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