On-The-Fly Observing System of the Nobeyama 45-m and ASTE 10-m Telescopes

Sawada, Tsuyoshi; Ikeda, Norio; Sunada, Kazuyoshi; Kuno, Nario; Kamazaki, Takeshi; Morita, Koh-Ichiro; Kurono, Yasutaka; Koura, Norikazu; Abe, Katsumi; Kawase, Sachiko; Maekawa, Jun; Horigome, Osamu; Yanagisawa, Kiyohiko

doi:10.1093/pasj/60.3.445

Cited by 138 publications

(121 citation statements)

References 11 publications

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“…The spectral resolution was 15.26 kHz (corresponding to 0.05−0.06 km s −1 ) for TZ1 and T70, and 3.81 kHz (corresponding to ∼0.05 km s −1 ) for H22. Observations with receiver TZ1 were conducted in the on-the-fly (OTF) mapping mode (Sawada et al 2008) with data sampling intervals along a strip of 5 and separations between strips of 5 . We have made orthogonal scans in RA and DEC to minimize scan effects.…”

Section: Nobeyama 45 M Telescopementioning

confidence: 99%

Astrochemical Properties of Planck Cold Clumps

Tatematsu

Ohashi

Sanhueza

et al. 2017

ApJS

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We observed thirteen Planck cold clumps with the James Clerk Maxwell Telescope/SCUBA-2 and with the Nobeyama 45 m radio telescope. The N 2 H + distribution obtained with the Nobeyama telescope is quite similar to SCUBA-2 dust distribution. The 82 GHz HC 3 N, 82 GHz CCS, and 94 GHz CCS emission are often distributed differently with respect to the N 2 H + emission. The CCS emission, which is known to be abundant in starless molecular cloud cores, is often very clumpy in the observed targets. We made deep single-pointing observations in DNC, HN 13 C, N 2 D + , cyclic-C 3 H 2 toward nine clumps. The detection rate of N 2 D + is 50%. Furthermore, we observed the NH 3 emission toward 15 Planck cold clumps to estimate the kinetic temperature, and confirmed that most of targets are cold ( 20 K). In two of the starless clumps observe, the CCS emission is distributed as it surrounds the N 2 H + core (chemically evolved gas), which resembles the case of L1544, a prestellar core showing

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Section: Nobeyama 45 M Telescopementioning

confidence: 99%

Astrochemical Properties of Planck Cold Clumps

Tatematsu

Ohashi

Sanhueza

et al. 2017

ApJS

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“…Although the wind conditions contributed to the pointing uncertainties, the pointing is better than a third of the beam. For the data reduction we used NOSTAR (Sawada et al 2008), a software package provided by the NRO for OTF data. The data were sampled to a spatial grid of 7.5 and smoothed to a spectral resolution of 0.5 km s −1 .…”

Section: Nobeyama 45 M Observationsmentioning

confidence: 99%

Kinematic structure of massive star-forming regions

Tackenberg

Beuther

Henning

et al. 2014

A&A

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Context. The mid-and far-infrared view on high-mass star formation, in particular with the results from the Herschel space observatory, has shed light on many aspects of massive star formation. However, these continuum studies lack kinematic information. Aims. We study the kinematics of the molecular gas in high-mass star-forming regions. Methods. We complemented the PACS and SPIRE far-infrared data of 16 high-mass star-forming regions from the Herschel key project EPoS with N 2 H + molecular line data from the MOPRA and Nobeyama 45 m telescope. Using the full N 2 H + hyperfine structure, we produced column density, velocity, and linewidth maps. These were correlated with PACS 70 μm images and PACS point sources. In addition, we searched for velocity gradients. Results. For several regions, the data suggest that the linewidth on the scale of clumps is dominated by outflows or unresolved velocity gradients. IRDC 18454 and G11.11 show two velocity components along several lines of sight. We find that all regions with a diameter larger than 1 pc show either velocity gradients or fragment into independent structures with distinct velocities. The velocity profiles of three regions with a smooth gradient are consistent with gas flows along the filament, suggesting accretion flows onto the densest regions. Conclusions. We show that the kinematics of several regions have a significant and complex velocity structure. For three filaments, we suggest that gas flows toward the more massive clumps are present.

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“…The channel width of the spectrometers was 31 kHz, corresponding to a velocity resolution of ∼0.1 km s −1 at 110 GHz. The observations were performed using the OTF mapping technique (Sawada et al 2008). Data were calibrated with the standard chopper-wheel method (Ulich & Haas 1976;Kutner & Ulich 1981).…”

Section: Observations With the Nro 45 M Telescopementioning

confidence: 99%

“…Data reduction and map generation were performed using the software package NOSTAR (Sawada et al 2008). A linear baseline was fitted and subtracted from the individual spectra.…”

Section: Observations With the Nro 45 M Telescopementioning

confidence: 99%

Molecular Clumps and Infrared Clusters in the S247, S252, and Bfs52 Regions

Shimoikura

Dobashi

Saito

et al. 2013

ApJ

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We present results of the observations carried out toward the S247, S252, and BFS52 H ii regions with various molecular lines using the 1.85 m radio telescope and the 45 m telescope at Nobeyama Radio Observatory. There are at least 11 young infrared clusters (IR clusters) within the observed region. We found that there are two velocity components in 12 CO (J = 2-1), and also that their spatial distributions show an anti-correlation. The IR clusters are located at their interfaces, suggesting that two distinct clouds with different velocities are colliding with each other, which may have induced the cluster formation. Based on 13 CO (J = 1-0) and C 18 O (J = 1-0) observations, we identified 16 clumps in and around the three H ii regions. Eleven of the clumps are associated with the IR clusters and the other five clumps are not associated with any known young stellar objects. We investigated variations in the velocity dispersions of the 16 clumps as a function of the distance from the center of the clusters or the clumps. Clumps with clusters tend to have velocity dispersions that increase with distance from the cluster center, while clumps without clusters show a flat velocity dispersion over the clump extents. A 12 CO outflow has been found in some of the clumps with IR clusters but not in the other clumps, supporting a strong relation of these clumps to the broader velocity dispersion region. We also estimated a mean star formation efficiency of ∼30% for the clumps with IR clusters in the three H ii regions.

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On-The-Fly Observing System of the Nobeyama 45-m and ASTE 10-m Telescopes

Cited by 138 publications

References 11 publications

Astrochemical Properties of Planck Cold Clumps

Astrochemical Properties of Planck Cold Clumps

Kinematic structure of massive star-forming regions

Molecular Clumps and Infrared Clusters in the S247, S252, and Bfs52 Regions

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