2020RAA....20...77T

Query : 2020RAA....20...77T

2020RAA....20...77T - Research in Astron. and astroph., 20, 77-77 (2020/May-0)

Pilot HI survey of Planck Galactic Cold Clumps with FAST.

TANG N.-Y., ZUO P., LI D., QIAN L., LIU T., WU Y.-F., LIU M.-T., YUE Y.-L., ZHU Y., LIU H.-F., YU D.-J., SUN J.-H., JIANG P., PAN G.-F., LI H., GAN H.-Q., YAO R., LIU S. (The FAST Collaboration)

Abstract (from CDS):

We present a pilot HI survey of 17 Planck Galactic Cold Clumps (PGCCs) with the Five-hundredmeter Aperture Spherical radio Telescope (FAST). HI Narrow Self-Absorption (HINSA) is an effective method to detect cold HI being mixed with molecular hydrogen H2 and improves our understanding of the atomic to molecular transition in the interstellar medium. HINSA was found in 58% PGCCs that we observed. The column density of HINSA was found to have an intermediate correlation with that of 13CO, following log(N(HINSA)) = (0.52 ± 0.26) log(N13CO) + (10 ± 4.1). HI abundance relative to total hydrogen [HI]/[H] has an average value of 4.4 x 10–3, which is about 2.8 times of the average value of previous HINSA surveys toward molecular clouds. For clouds with total column density NH > 5 x 1020 cm–2, an inverse correlation between HINSA abundance and total hydrogen column density is found, confirming the depletion of cold HI gas during molecular gas formation in more massive clouds. Nonthermal line width of 13CO is about 0 - 0.5 km s–1 larger than that of HINSA. One possible explanation of narrower non-thermal width of HINSA is that HINSA region is smaller than that of 13CO. Based on an analytic model of H2 formation and H2 dissociation by cosmic ray, we found the cloud ages to be within 106.7 - 107.0 yr for five sources.

Abstract Copyright: © 2020 National Astronomical Observatories

Journal keyword(s): ISM: clouds - ISM: evolution - ISM: molecules

Simbad objects: 22

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Number of rows : 22
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 PLCKECC G121.92-07.66 cor 00 44 27.2 +55 11 18           ~ 7 0
2 PLCKECC G122.01-07.48 cor 00 45 01.8 +55 22 43           ~ 7 0
3 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 296 0
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
5 LDN 1570 DNe 06 07 28.4 +19 28 04           ~ 46 0
6 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
7 PLCKECC G093.16+09.61 cor 20 36 31.5 +56 54 48           ~ 8 0
8 PLCKECC G092.79+09.14 cor 20 37 43.3 +56 20 14           ~ 7 0
9 PLCKECC G089.29+04.01 cor 20 50 37.9 +50 27 05           ~ 7 0
10 PLCKECC G089.62+02.16 cor 21 00 44.2 +49 30 30           ~ 6 0
11 PLCKECC G089.36-00.67 cor 21 12 19.4 +47 24 19           ~ 7 0
12 PLCKECC G089.75-02.16 cor 21 20 13.7 +46 39 03           ~ 8 0
13 PLCKECC G090.76-04.55 cor 21 34 00.1 +45 37 40           ~ 7 0
14 PLCKECC G089.64-06.86 cor 21 38 04.9 +43 10 21           ~ 7 0
15 PLCKECC G093.22-04.59 cor 21 44 47.8 +47 13 40           ~ 8 0
16 PLCKECC G093.31-11.68 cor 22 09 48.0 +41 42 42           ~ 7 0
17 PLCKECC G093.36-12.06 cor 22 11 10.9 +41 25 42           ~ 6 0
18 PLCKECC G101.14-15.28 cor 22 54 59.6 +42 36 11           ~ 6 0
19 PLCKECC G108.85-00.80 cor 22 58 48.640 +58 56 54.43           ~ 13 0
20 PGCC G089.05-41.27 MoC 23 08 43.430 +14 43 35.71           ~ 8 0
21 PLCKECC G107.64-09.29 cor 23 14 27.4 +50 40 44           ~ 6 0
22 PLCKECC G116.08-02.38 cor 23 56 41.8 +59 45 13           ~ 9 0

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