Star formation rates in the L 1482 filament of the California molecular cloud

Omodaká, Toshihiro; Nagayama, Tomonori; Dobashi, Kazuhito; Chibueze, James O.; Yamabi, Akifumi; Shimajiri, Yoshito; Inoue, Shinnosuke; Hamada, Shota; Sunada, Kazuyoshi; Ueno, Yuji

doi:10.1093/pasj/psaa048

Cited by 2 publications

(1 citation statement)

References 29 publications

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“…The OMC has 50 OB stars while Auriga-California has only one early B star, LkHα 101, a member of the embedded cluster in NGC 1579 (Herbig et al 2004). Using an H 2 O maser associated with L1482 where LkHα 101 is located, Omodaka et al (2020) measured parallax corresponding to the distance to the filament of 532±28 pc. Meanwhile, the distance to the B star LkHα 101 is estimated to be 567±68 pc with Gaia DR2 (Gaia Collaboration 2018).…”

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confidence: 99%

Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2

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Parsons

et al. 2021

ApJ

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We report the first high spatial resolution measurement of magnetic fields surrounding LkHα 101, a part of the Auriga-California molecular cloud. The observations were taken with the POL-2 polarimeter on the James Clerk Maxwell Telescope within the framework of the B-fields In Star-forming Region Observations (BISTRO) survey. Observed polarization of thermal dust emission at 850 µm is found to be mostly associated with the red-shifted gas component of the cloud. The magnetic field displays a relatively complex morphology. Two variants of the Davis-Chandrasekhar-Fermi method, unsharp masking and structure function, are used to calculate the strength of magnetic fields in the plane of the sky, yielding a similar result of B POS ∼ 115 µG. The mass-to-magnetic-flux ratio in critical value units, λ ∼ 0.3, is the smallest among the values obtained for other regions surveyed by POL-2. This implies that the LkHα 101 region is sub-critical and the magnetic field is strong enough to prevent gravitational collapse. The inferred δB/B 0 ∼ 0.3 implies that the large scale component of the magnetic field dominates the turbulent one. The variation of the polarization fraction with total emission intensity can be fitted by a power-law with an index of α = 0.82 ± 0.03, which lies in the range previously reported for molecular clouds. We find that the polarization fraction decreases rapidly with proximity to the only early B star (LkHα 101) in the region. The magnetic field tangling and the joint effect of grain alignment and rotational disruption by radiative torques are potential of explaining such a decreasing trend.

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Section: Introductionmentioning

confidence: 99%

Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2

Ngoc

Diep

Parsons

et al. 2021

ApJ

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The First VERA Astrometry Catalog

Hirota¹,

Nagayama²,

Honma³

et al. 2020

Publications of the Astronomical Society of Japan

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We present the first astrometry catalog from the Japanese VLBI (very long baseline interferometer) project VERA (VLBI Exploration of Radio Astrometry). We have compiled all the astrometry results from VERA, providing accurate trigonometric-annual-parallax and proper-motion measurements. In total, 99 maser sources are listed in the VERA catalog. Among them, 21 maser sources are newly reported, while the rest of the 78 sources are referred to in previously published results or those in preparation for forthcoming papers. The accuracy in the VERA astrometry is revisited and compared with that from the other VLBI astrometry projects such as BeSSeL (The Bar and Spiral Structure Legacy) Survey and GOBELINS (the Gould’s Belt Distances Survey) with the VLBA (Very Long Baseline Array). We have confirmed that most of the astrometry results are consistent with each other, and the largest error sources are due to source structure of the maser features and their rapid variation, along with the systematic calibration errors and different analysis methods. Combined with the BeSSeL results, we estimate the up-to-date fundamental Galactic parameters of $R_{0}=7.92\pm 0.16_{\rm {stat.}}\pm 0.3_{\rm {sys.}}\:$kpc and $\Omega _{\odot }=30.17\pm 0.27_{\rm {stat.}}\pm 0.3_{\rm {sys.}}\:$km$\:$s$^{-1}\:$kpc$^{-1}$, where $R_{0}$ and $\Omega _{\odot }$ are the distance from the Sun to the Galactic center and the Sun’s angular velocity of the Galactic circular rotation, respectively.

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Star formation rates in the L 1482 filament of the California molecular cloud

Cited by 2 publications

References 29 publications

Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2

Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2

The First VERA Astrometry Catalog

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