2000ApJ...538..275J


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET17:21:58

2000ApJ...538..275J - Astrophys. J., 538, 275-288 (2000/July-3)

The properties of molecular hydrogen toward the Orion belt stars from observations by the interstellar medium absorption profile spectrograph.

JENKINS E.B., WOZNIAK P.R., SOFIA U.J., SONNEBORN G. and TRIPP T.M.

Abstract (from CDS):

Absorption features from the Lyman and Werner bands of interstellar molecular hydrogen were recorded by the Interstellar Medium Absorption Profile Spectrograph (IMAPS) at λ/Δλ=80,000 in the spectra of δ Ori A and ε Ori. The objective was to find and study more examples of an unusual phenomenon found for one of the velocity components of H2 in the spectrum of ζ Ori by Jenkins & Peimbert (1997ApJ...477..265J). Specifically, they detected a gradual shift in velocity and broadening for features arising from progressively higher rotational excitations J. This effect appears to be absent in the spectra of both δ and ε Ori, which are only a few degrees away in the sky from ζ Ori. The absence of atomic material at a large negative velocity in the spectra of δ and ε Ori (and its presence in ζ Ori) supports a proposal by Jenkins & Peimbert that the line of sight to ζ intercepts a bow shock facing away from us, perhaps created by the collision of windlike material with some foreground obstruction. One edge of the molecular cloud complex Lynds 1630 is situated close to ζ Ori in the sky, but we present some evidence that seems to indicate that the cloud is more distant, in which case it could not serve as the obstruction. However, it is possible that the outermost extension of a high-speed jet from a star forming within the cloud can explain the high-velocity material and the shock front created by it.

For both stars, the H2 absorption features are separated into two velocity components. Total H2 column densities toward δ and ε Ori are 5.5x1014 and 1.9x1016 cm–2, respectively. When these values are compared to the column densities of H I, the fractions of H atoms bound in molecular form 2N(H2)/[2N(H2)+N(H I)]=7x10–6 for δ and 1.3x10–4 for ε. The rotation temperatures of the molecules with J>2 toward ε Ori indicate that the gas is in the general vicinity of the stars that emit UV fluxes capable of rotationally pumping the molecules. For the strongest component of H2 toward δ Ori, the pumping rate is lower and consistent with a general UV flux level in the plane of the Galaxy.


Abstract Copyright:

Journal keyword(s): ISM: Molecules - stars: individual (δ Orionis A, ε Orionis, ζ Orionis A) - Ultraviolet: ISM

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Barnard's Loop HII 05 27.5 -03 58           ~ 110 1
2 UCAC3 180-24383 * 05 31 58.7429520991 -00 18 18.746218247     14.0 12.99 12.25 ~ 25 0
3 * del Ori Al* 05 32 00.40009 -00 17 56.7424 0.96 2.02 2.41 2.32 2.54 B0III+O9V 751 0
4 * del02 Ori SB* 05 32 00.4062922775 -00 17 04.345829128 5.97 6.67 6.83     B2Vsn 268 0
5 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 241 0
6 * eps Ori s*b 05 36 12.81335 -01 12 06.9089 0.48 1.51 1.69 1.76 1.93 B0Ia 867 0
7 NAME Ori I As* 05 38 -02.8           ~ 566 0
8 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 754 0
9 * zet Ori ** 05 40 45.52666 -01 56 33.2649 0.50 1.56 1.77 1.85 2.05 O9.7Ib+B0III 334 0
10 * zet Ori A ** 05 40 45.527143 -01 56 33.26036   1.79 1.90     O9.2IbvarNwk 647 0
11 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 457 0
12 IC 434 HII 05 41 -02.5           ~ 79 1
13 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 692 1
14 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1213 0
15 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1084 1
16 LDN 1630 DNe 05 45.5 -00 59           ~ 356 0
17 NAME Ori Belt reg ~ ~           ~ 69 0

    Equat.    Gal    SGal    Ecl

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