2018ApJ...858..111R

Query : 2018ApJ...858..111R

2018ApJ...858..111R - Astrophys. J., 858, 111-111 (2018/May-2)

The connection between different tracers of the diffuse interstellar medium: kinematics.

RICE J.S., FEDERMAN S.R., FLAGEY N., GOLDSMITH P.F., LANGER W.D., PINEDA J.L. and LAMBERT D.L.

Abstract (from CDS):

Using visible, radio, microwave, and submillimeter data, we study several lines of sight toward stars generally closer than 1 kpc on a component-by-component basis. We derive the component structure seen in absorption at visible wavelengths from Ca II, Ca I, K I, CH, CH+, and CN and compare it to emission from H I, CO and its isotopologues, and C+ from the GOT C+ survey. The correspondence between components in emission and absorption helps create a more unified picture of diffuse atomic and molecular gas in the interstellar medium. We also discuss how these tracers are related to the CO-dark H2 gas probed by C+ emission and discuss the kinematic connections among the species observed.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): ISM: atoms - ISM: clouds - ISM: molecules - ISM: structure - radio lines: ISM - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/ApJ/858/111): table1.dat table2.dat>

Simbad objects: 31

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Number of rows : 31
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 HD 29647 * 04 41 08.0448698568 +25 59 33.949206132 9.69 9.22 8.31 7.35 6.60 B9IIIpHgMn 217 0
2 V* IU Aur SB* 05 27 52.3995663216 +34 46 58.262388600 7.91 8.55 8.37     O9.5V+B0.2V 192 0
3 IC 443 SNR 06 17 00.0000000 +22 34 11.998901           ~ 1314 1
4 HD 260737 * 06 36 59.2616999664 +04 41 38.577734520   9.27 9.18     A2 8 0
5 HD 47073 * 06 36 59.7812319864 +04 42 48.708966888   8.57 8.34     A5/7 13 0
6 HD 55469 * 07 12 37.5315315480 -11 07 51.632450472   9.57 9.35     A2III 6 0
7 LDN 1658 DNe 07 14.4 -11 05           ~ 9 0
8 HD 55981 * 07 14 48.1454895480 -10 59 38.366022840   10.02 9.87     A0IV 8 0
9 HD 60146 * 07 32 22.1538561408 -18 52 26.209503876   9.48 9.49     B8II/III 11 0
10 * zet Oph Be* 16 37 09.5400587698 -10 34 01.509742704 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1908 0
11 HD 165783 Be* 18 08 27.0939756360 -19 52 07.946430240 8.20 8.69 8.37 9.11   B3/5Ib 32 0
12 HD 165918 * 18 09 04.6455519240 -19 52 30.817060860   8.22 8.11     B5IV/V 11 0
13 HD 167498 * 18 16 02.1396914640 -14 55 27.091267140   8.07 7.83     A2IV 16 0
14 HD 167812 * 18 17 26.0070612240 -14 50 56.464308420   8.19 7.97     B9.5V 12 0
15 HD 168607 s*b 18 21 14.8856951904 -16 22 31.763755236 10.23 9.82 8.28 8.55   B9Ia+ 196 1
16 LDN 413 DNe 18 26.6 -11 13           ~ 3 0
17 HD 169754 V* 18 26 42.6536643144 -11 21 24.830998092 9.61 9.64 8.60 7.63 6.86 B0.5Ia 54 1
18 BGPS G020.050+00.195 cor 18 26 55.2237 -11 21 13.478           ~ 8 0
19 BGPS G032.436-00.017 cor 18 50 35.6201 -00 26 58.645           ~ 5 0
20 HD 174509 * 18 50 49.2799736880 -00 33 29.623308552   9.48 9.27     B3V(n) 7 0
21 BGPS G032.411-00.099 cor 18 50 50 -00 30.6           ~ 11 0
22 BGPS G032.527-00.123 cor 18 51 08.3323 -00 24 58.055           ~ 5 0
23 BGPS G032.524-00.131 cor 18 51 09.8219 -00 25 17.602           ~ 5 0
24 BD+49 3482 gD* 21 14 13.1014949256 +50 07 02.769463560   9.40 9.09     A2 15 0
25 BD+49 3484 * 21 14 21.6317407416 +50 14 52.472742072   9.70 9.43     A0 5 0
26 DOBASHI 2934 DNe 21 15 03.1 +50 15 06           ~ 2 1
27 TGU H541 P30 DNe 21 15.4 +50 15           ~ 2 0
28 HD 210121 * 22 08 11.9027578440 -03 31 52.765490316   7.84 7.68     B7II 185 0
29 HD 240179 Pu* 23 03 58.0629546744 +60 05 16.260335088   9.50 9.28     B5V 10 0
30 HD 240183 * 23 04 10.2654108048 +60 05 19.589430552   9.97 9.85     B5V 7 0
31 IRAS 23033+5951 Y*O 23 05 25.1762883456 +60 08 15.374293800           ~ 97 0

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