2021ApJS..256...25T

Query : 2021ApJS..256...25T

2021ApJS..256...25T - Astrophys. J., Suppl. Ser., 256, 25-25 (2021/October-0)

Molecular cloud cores with high deuterium fractions: Nobeyama mapping survey.

TATEMATSU K., KIM G., LIU T., EVANS II N.J., YI H.-W., LEE J.-E., WU Y., HIRANO N., LIU S.-Y., DUTTA S., SAHU D., SANHUEZA P., KIM K.-T., JUVELA M., TOTH L.V., FEHER O., HE J., GE J., FENG S., CHOI M., KANG M., THOMPSON M.A., FULLER G.A., LI D., RISTORCELLI I., WANG K., DI FRANCESCO J., EDEN D., OHASHI S., KANDORI R., VASTEL C., HIROTA T., SAKAI T., LU X., NGUYEN LU'O'NG Q., SHINNAGA H., KIM J. (The JCMT Large Program "SCOPE" Collaboration)

Abstract (from CDS):

We present the results of on-the-fly mapping observations of 44 fields containing 107 SCUBA-2 cores in the emission lines of molecules N2H+, HC3N, and CCS at 82-94 GHz using the Nobeyama 45 m telescope. This study aimed at investigating the physical properties of cores that show high deuterium fractions and might be close to the onset of star formation. We found that the distributions of the N2H+ and HC3N line emissions are approximately similar to the distribution of the 850 µm dust continuum emission, whereas the CCS line emission is often undetected or is distributed in a clumpy structure surrounding the peak position of the 850 µm dust continuum emission. Occasionally (12%), we observe CCS emission, which is an early-type gas tracer toward the young stellar object, probably due to local high excitation. Evolution toward star formation does not immediately affect the nonthermal velocity dispersion.

Abstract Copyright: © 2021. The American Astronomical Society. All rights reserved.

Journal keyword(s): Interstellar clouds

VizieR on-line data: <Available at CDS (J/ApJS/256/25): table4.dat table6.dat tablea1.dat tablea2.dat tablea3.dat tablea4.dat tablea5.dat>

Status at CDS : All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 LDN 1498 DNe 04 11.0 +24 58           ~ 306 0
2 NAME [BM89] L1521B cor 04 24 12.7 +26 36 53           ~ 76 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
4 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1872 0
5 LDN 1512 MoC 05 04 09.7 +32 43 09           ~ 184 0
6 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 965 0
7 NAME lam Ori Complex SFR 05 35 06 +09 56.0           ~ 86 0
8 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 212 0
9 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 623 0
10 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
11 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1498 0
12 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1227 1
13 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3969 1
14 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 336 1
15 LDN 492 DNe 18 15 51 -03 44.4           ~ 50 0
16 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1195 1
17 NAME Aql Region reg 18 31.1 -02 10           ~ 456 0
18 NAME Gould Belt PoG ~ ~           ~ 956 1

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