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Data: H₂O, CH3OH_I

BAE11 - A Multi-epoch, Simultaneous Water and Methanol Maser Survey toward Intermediate-mass Young Stellar Objects

Short title: Bae et al. (2011)
Authors: Bae, Jae-Han Kim, Kee-Tae Youn, So-Young Kim, Won-Ju Byun, Do-Young Kang, Hyunwoo Oh, Chung Sik
Journal: The Astrophysical Journal Supplement, Volume 196, Issue 2, article id. 21, 18 pp. (2011).
Bibcode: 2011ApJS..196...21B

PDF: BAE11.pdf

• Target type: YSO
  Transitions: SiO_1-0v0,CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II)
  

• Abstract

  We report a multi-epoch, simultaneous 22 GHz H2O and 44 GHz Class I CH3OH maser line survey toward 180 intermediate-mass young stellar objects, including 14 Class 0 and 19 Class I objects, and 147 Herbig Ae/Be stars. We detected H2O and CH3OH maser emission toward 16 (9%) and 10 (6%) sources with one new H2O and six new CH3OH maser sources. The detection rates of both masers rapidly decrease as the central (proto)stars evolve, which is contrary to the trends in high-mass star-forming regions. This suggests that the excitations of the two masers are closely related to the evolutionary stage of the central (proto)stars and the circumstellar environments. H2O maser velocities deviate on average 9 km s-1 from the ambient gas velocities whereas CH3OH maser velocities match quite well with the ambient gas velocities. For both maser emissions, large velocity differences ( v_{H_{2O}} - v_{sys} > 10 {\,km\,s^{-1}} and v_{CH_{3OH}} - v_{sys} > 1 {\,km\,s^{-1}}) are mostly confined to Class 0 objects. The formation and disappearance of H2O masers is frequent and their integrated intensities change by up to two orders of magnitude. In contrast, CH3OH maser lines usually show no significant change in intensity, shape, or velocity. This is consistent with the previous suggestion that H2O maser emission originates from the base of an outflow while 44 GHz Class I CH3OH maser emission arises from the interaction region of the outflow with the ambient gas. The isotropic maser luminosities are well correlated with the bolometric luminosities of the central objects. The fitted relations are L_{H_{2O}} = 1.71 \times 10^{-9} (L_{bol})^{0.97} and L_{CH_{3OH}} = 1.71 \times 10^{-10} (L_{bol})^{1.22}. eprintid: arXiv:1108.3878

  Comments: 180 intermediate-mass young stellar objects. Sources from published studies satisfying one of the following two criteria: (1) protostellar or PMS objects, which are thought to be the precursors of intermediate-mass stars (2) known or candidate HAeBe stars.

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DSS colored 2MASS colored WISE colored SDSS color IRAC color I1,I2,I4 GLIMPSE 360 PACS color (70-160 um) SPIRE color (250-500 um) NVSS (1.4GHz) ATLASGAL 870 um ATLASGAL 870 um + Planck Bolocam 1.1 mm UKIDSS K 2MASS K