2005A&A...440..547W


Query : 2005A&A...440..547W

2005A&A...440..547W - Astronomy and Astrophysics, volume 440547-557 (2005/9-3)

NaI and CaII absorption components observed towards the Orion-Eridanus Superbubble.

WELSH B.Y., SALLMEN S. and JELINSKY S.

Abstract (from CDS):

We present medium-resolution spectra (R∼7.5km/s) of the interstellar NaI and CaII interstellar absorption lines observed towards 16 early-type stars with distances of 160-1kpc in the line-of-sight towards the Orion-Eridanus Superbubble (OE-S). These data have been supplemented with measurements of NaI absorption towards a further 13 stars with similar sight-lines taken from the literature. We detect two major absorption components with velocities of Vlsr~+7.0 and -8.0km/s. The former component, seen in 70% of the sight-lines is associated with the boundary to the Local Bubble cavity located at a distance of 140-150pc. The other absorption component is only detected towards a limited region of the sky bounded by (190°<l<215°) and (-50°<b←30°). If gas with this velocity is associated with an outer expansion shell of the OE-S, then we can place its distance at 163-180pc in agreement with the estimate by Guo et al. (1995ApJ...453..256G). Several other negative velocity components at Vlsr~-20.4, -28.5 and -33.5km/s have also been detected for sight-line distances >220pc within an area coincident with that of the 0.75keV X-ray enhancement of the OE-S. Column density ratios, N(NaI)/N(CaII), for the most negative velocity components have values <1.0, suggesting that this gas has been disrupted by a possible shock event. Our data do not support a simple model for the OE-S that involves a single stellar bubble cavity that stretches from the Orion Nebula to high galactic latitudes. Instead, our detection of multiple positive and negative velocity components suggests the presence of several gas shells produced by supernovae and/or stellar wind-driven shocks. We also confirm that the prominent ``hook-like'' feature of H-α emission that characterizes the OE-S, in in fact composed of two physically separate emission arcs, with the brighter Arc A being at a distance >500pc. Finally, we place a similar distance limit for any coherently structured rear shell of neutral gas associated with expansion of the OE-S towards the galactic halo.

Abstract Copyright: ∼

Journal keyword(s): ISM: bubbles - ISM: kinematics and dynamics

Simbad objects: 42

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Number of rows : 42
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 18873 * 03 02 00.6145205232 -02 56 24.943229412   9.32 8.88     F0/2IV/V 20 0
2 HD 19846 Pe* 03 11 42.0457482888 +08 07 07.596376356   8.62 8.57     B9IV-VEu 27 0
3 HD 20001 * 03 12 15.3787005048 -20 37 10.531422912   6.90 7.03     B3V 33 0
4 HD 20340 Be* 03 15 45.8644215984 -16 49 43.503765132 7.26 7.83 7.96     B3Ve 63 0
5 HD 20319 ** 03 16 00.85447 -05 55 07.3324   6.15 6.17     B9III 71 0
6 HD 20404 * 03 16 44.3897447760 -03 21 50.384593476   7.69 7.71     B9IV/V 23 0
7 [BDM2001] Arc B ISM 03 19 -06.8           ~ 7 0
8 * v Eri * 03 30 37.0583178770 -05 04 30.532729396   4.631 4.725     B9III 89 0
9 HD 22558 * 03 37 24.6051454272 -11 05 35.357970336   10.86 10.12     F5/6V 10 0
10 * 22 Eri a2* 03 40 38.3331139440 -05 12 38.555731188 4.81 5.38 5.53     B9IIIpSi4200 134 0
11 HD 23393 * 03 44 29.3765289024 -12 03 31.124662128   8.62 8.30     ApSrCrEu 39 0
12 * 24 Eri * 03 44 30.5105062824 -01 09 47.127478680 4.76 5.15 5.25     B7IV 83 0
13 * u Tau SB* 03 45 40.4433670200 +06 02 59.985349222   5.225 5.337     B3V 139 0
14 NAME Eri Bubble HI 03 52 -02.0           ~ 148 0
15 * 31 Tau ** 03 52 00.2291740237 +06 32 05.659794373 5.3         B3.5V+ 111 0
16 * 30 Eri * 03 52 41.6487441096 -05 21 40.417862076   5.378 5.475     B8III 61 0
17 * tau08 Eri SB* 03 53 42.7023562560 -24 36 44.021417544   4.496 4.623     B6V 123 0
18 HD 24819 ** 03 56 43.0313153760 -01 34 18.718824072   8.35 8.04     A5/7III 23 0
19 [BDM2001] Arc A ISM 04 02 +03.2           ~ 7 0
20 HD 25631 * 04 03 24.7472481504 -20 08 37.665824028   6.271 6.450     B3V 78 0
21 * 40 Tau ** 04 03 44.6044538328 +05 26 08.225802924 4.68 5.25 5.33     B5V 141 0
22 HD 26739 Em* 04 13 38.1466725144 -01 08 59.056715940 5.76 6.296 6.423     B4V 75 0
23 HD 26994 * 04 15 26.7506756520 -16 26 42.628567740 6.15 6.729 6.863     B7III 23 0
24 * d Eri * 04 20 42.8341039320 -07 35 32.985711240 5.23 5.710 5.838     B7II 78 0
25 * 228 Eri Be* 04 29 06.9254098152 -13 02 54.127769208 4.45 5.23 5.41 5.46 5.63 B2(V)ne 286 0
26 HD 28763 * 04 31 25.8505846032 -13 38 39.202938816   6.321 6.250     A2/3V 52 0
27 HD 28856 * 04 32 17.7545423832 -13 35 11.480811504   9.46 9.27     A1V 23 0
28 HD 29227 * 04 36 01.6702305600 -03 36 41.881055616 5.8 6.239 6.340     B5III 50 0
29 * nu. Eri bC* 04 36 19.1419185396 -03 21 08.857744927 2.82 3.737 3.928     B2III 407 0
30 V* V1148 Tau SB* 04 37 54.3391205928 +07 19 03.478947384   6.97 7.02     B3V 53 0
31 HD 29851 SB* 04 41 42.0315143376 -12 28 32.816965332   6.76 6.64     A2IV-V 27 0
32 * 56 Eri Be* 04 44 05.3207274312 -08 30 12.852684720 4.97 5.75 5.81 5.72 5.74 B2(V)nne 186 0
33 * mu. Eri SB* 04 45 30.1514281206 -03 15 16.775320589 3.26 3.87 4.00     B5IV 170 0
34 * b Eri ** 04 56 24.1867291992 -05 10 16.884454476   5.349 5.482     B5III 62 0
35 HD 31726 * 04 57 44.6845893336 -14 13 54.901969680   5.939 6.139     B2V 136 0
36 HD 32192 * 05 01 03.2558559024 -09 13 29.451471420   8.97 8.93     A0V 21 0
37 * psi Eri ** 05 01 26.3457823592 -07 10 26.273231188 3.87 4.61 4.78     B3IV 114 0
38 HD 34968 Pu* 05 20 26.9147809752 -21 14 23.148600180   4.684 4.729     A0V 59 0
39 M 42 HII 05 35 16.8 -05 23 15           ~ 4411 0
40 NAME Ori I As* 05 38 -02.8           ~ 653 0
41 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
42 NAME Local Bubble ISM ~ ~           ~ 1059 0

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