The structure of the interstellar gas towards stars in the globular cluster M 55

Details The structure of the interstellar gas towards stars in the globular cluster M 55 The structure of the interstellar gas towards stars in the globular cluster M 55

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..535l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 286, no. 2, p. 535-542

Astronomy and Astrophysics

Astrophysics

11

Globular Clusters, H I Regions, Interstellar Gas, Line Spectra, Molecular Clouds, Potassium, Sodium, Stellar Spectra, Interstellar Chemistry, Spectrograms, Spectrographs

Scientific paper

Observations are presented of high resolution interstellar Na D line profiles towards 10 stars in the globular cluster M 55 and 6 foreground stars which lie within 3 deg from the cluster. The spectral region containing the K I (lambda 7699 A) line is simultaneously recorded but this line is detected only towards one of the foreground stars as a component having a relatively high K I/Na I abundance ratio. Two principal components are observed towards the cluster stars at velocities of approximately +1 and +15 km/s and weaker higher velocity gas is detected at approximately -21, +33 and +55 km/s. The +1 km/s component is at a distance of approximately less than 100 pc and we suggest that this is part of an extensive region of diffuse gas which connects the molecular and dark clouds observed closer to the galactic plane. The +15 km/s component lies at a distance between 130 to 300 pc and is identified with an anomalous velocity arc observed in HI. The higher velocity gas components are at a distance approximately greater than 700 pc. From a comparison with our previous observations in the general direction of the Carina-Sagittarius arm we suggest that these features have an origin in spiral arm gas, in which case their detection towards M 55 places them some 600 to 800 pc from the galactic plane.

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