The Local Interstellar Medium in Puppis‐Vela

Open Access
Publisher Website
Google Scholar
Abstract
The first study of the local interstellar medium (LISM) toward Puppis-Vela (l = 245° to 275°, b = -15° to +5°, d < 200 pc) is presented in this paper. A study of the locations, sizes, and physical characteristics of local interstellar gas, i.e."astronephography," is included, and relies upon the improved distance measurements provided by Hipparcos parallax measurements. All spectra of more distant sight lines contain absorption features due to intervening local gas, and more distant structures can only be studied accurately if components due to the LISM have been isolated. Towards this end, high-resolution (R ≈ 95,000), high signal-to-noise (S/N ~ 110 to 250) Na I λλ5889.951, 5895.924 spectra of 11 nearby stars in the direction of Puppis-Vela have been obtained with the Coudé Echelle Spectrograph on the 1.4 m Coudé Auxiliary Telescope at the European Southern Observatory. Toward Puppis-Vela, absorption due to the Local Interstellar Cloud (LIC) was not observed, but components at three distinct velocities were found, and the extent of the local gas producing the features was estimated. The three components have the following locations and velocities: component A—(l≈276° to 298°, b ≈ -5°to +4°), Vhelio = +6 to +9 km s-1, and d ~ 104 pc; component B—(l ≈ 264° to 276°, b ≈ -7° to +3°), Vhelio = +12 to +15 km s-1, and d ~ 115 pc; component C—(l ≈ 252° to 271°, b ≈ -8° to -6°), Vhelio = +21 to +23 km s-1, and d ~ 131 pc. The conclusions regarding the ultraviolet spectrum of γ2 Vel (l = 263°, b = -8°, d = 258 ± 35 pc) presented by Fitzpatrick & Spitzer were reexamined in light of this new LISM data, and the ambiguity in their conclusions about several absorption components is resolved. The stars in Puppis-Vela flank the region of the apparent extension of the Local Bubble (or Cavity) known as the β CMa tunnel, and measurements of the Na I column density towards the sample stars have been used to modify existing estimates of the extent of the tunnel. A compilation of all existing Na I observations of less than 200 pc sight lines around the tunnel reveal that low column densities have been exclusively detected within l ≈ 210° to 250°, and b ≈ -21° to -9°. Near the Galactic plane, at latitudes -10° < b < 0° and d 150 pc, the tunnel is confined to l < 270°, a lower longitude than was previously reported.
All Related Versions

This publication has 34 references indexed in Scilit: