2002ApJ...567..391M

Query : 2002ApJ...567..391M

2002ApJ...567..391M - Astrophys. J., 567, 391-406 (2002/March-1)

Observations of H3 in the diffuse interstellar medium.

McCALL B.J., HINKLE K.H., GEBALLE T.R., MORIARTY-SCHIEVEN G.H., EVANS II N.J., KAWAGUCHI K., TAKANO S., SMITH V.V. and OKA T.

Abstract (from CDS):

Surprisingly large column densities of H+3 have been detected using infrared absorption spectroscopy in seven diffuse cloud sight lines (Cygnus OB2 12, Cygnus OB2 5, HD 183143, HD 20041, WR 104, WR 118, and WR 121), demonstrating that H+3 is ubiquitous in the diffuse interstellar medium. Using the standard model of diffuse cloud chemistry, our H+3 column densities imply unreasonably long path lengths (∼1 kpc) and low densities (∼3 cm–3). Complimentary millimeter-wave, infrared, and visible observations of related species suggest that the chemical model is incorrect and that the number density of H+3 must be increased by 1-2 orders of magnitude. Possible solutions include a reduced electron fraction, an enhanced rate of H2 ionization, and/or a smaller value of the H+3 dissociative recombination rate constant than implied by laboratory experiments.

Abstract Copyright: ∼

Journal keyword(s): ISM: Cosmic Rays - Infrared: ISM: Lines and Bands - ISM: Clouds - ISM: Molecules - Molecular Processes

Simbad objects: 21

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Number of rows : 21
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 20041 * 03 15 47.9705004096 +57 08 26.243459556 6.61 6.52 5.79     A0Ia 146 1
2 * chi02 Ori s*b 06 03 55.1843706432 +20 08 18.428141364 4.24 4.91 4.63 4.32 4.10 B2Ia 465 0
3 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1610 0
4 * bet01 Sco bC* 16 05 26.2319826 -19 48 19.630018 1.68 2.55 2.62 2.60 2.69 B1V 577 0
5 * 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
6 * eta Oph ** 17 10 22.68689 -15 43 29.6639 2.56 2.47 2.42 2.39 2.38 A2IV-V 271 0
7 MR 80 WR* 18 02 04.1244400656 -23 37 42.168277056   15.002 13.155 12.056   WC9 241 1
8 HD 168607 s*b 18 21 14.8856951904 -16 22 31.763755236 10.23 9.82 8.28 8.55   B9Ia+ 196 1
9 RAFGL 2179 WR* 18 31 42.2111779224 -09 59 16.687233168   25.0 22.0     WC9 91 0
10 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0V 2787 1
11 EM* AS 320 WR* 18 44 13.1526105048 -03 47 57.775268904 13.7 13.340 13.983     WC9d 121 0
12 * pi. Sgr ** 19 09 45.8329260 -21 01 25.010335 3.46 3.22 2.88 2.54 2.30 F2II-III 142 0
13 HD 183143 s*b 19 27 26.5636061496 +18 17 45.193019136 8.25 8.08 6.86 5.74 4.79 B7Ia+ 464 0
14 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 919 1
15 * P Cyg s*b 20 17 47.2019733389 +38 01 58.549132671 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1200 1
16 HD 194279 s*b 20 23 18.1647782064 +40 45 32.598481500 8.01 8.04 7.01 5.98 5.17 B2Ia 200 0
17 BD+40 4220 s*b 20 32 22.4238071594 +41 18 18.942475904 11.32 10.61 9.185     O7Iafep 414 0
18 Schulte 12 s*b 20 32 40.9572199728 +41 14 29.279036940 16.1 14.45 11.702     B3-4Ia+ 453 0
19 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 1023 0
20 * alf Cyg sg* 20 41 25.91514 +45 16 49.2197 1.11 1.34 1.25 1.14 1.04 A2Ia 778 0
21 * alf Cep PM* 21 18 34.77233 +62 35 08.0681 2.770 2.680 2.460 2.22 2.11 A8Vn 374 0

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