A high-resolution optical survey of interstellar absorption lines toward globular clusters and extragalactic objects. I - Basic data

1980 ◽  
Vol 242 ◽  
pp. 976 ◽  
Author(s):  
A. Songaila ◽  
D. G. York
Keyword(s):  
High Resolution ◽  
Globular Clusters ◽  
Absorption Lines ◽  
Basic Data ◽  
Interstellar Absorption

scholarly journals Interstellar Matter with Very Large Telescopes

1984 ◽  
Vol 79 ◽  
pp. 675-678
Author(s):  
J. Lequeux
Keyword(s):  
High Resolution ◽  
Absorption Lines ◽  
High Resolution Spectroscopy ◽  
Interstellar Matter ◽  
Large Telescope ◽  
Interstellar Absorption ◽  
Near Ir ◽  
Very Large Telescope ◽  
Large Telescopes ◽  
Diffuse Matter

Interstellar matter is certainly one of the fields where a very large telescope (VLT) will prove to be most fruitful. This includes (somewhat paradoxically, but this will be explained later) the study of extended emissions. I will now examine in turn the different domains of interest for a VLT.I. Neutral diffuse matterOptical and near IR observations will mainly contribute to this domain through high-resolution spectroscopy of interstellar absorption lines in the spectra of stars. These lines are resonant lines of atoms (NaI, KI, etc.) or ions (CaII, TiII, etc.) as well as of some molecules (CH+, CH, CN, CS+, C2 in the near IR). Clearly this kind of study is always photon - limited; a VLT will collect more photons than present telescopes, thus increase the possibilities considerably.

scholarly journals Atomic and Molecular Interstellar Absorption Lines toward the High Galactic Latitude Stars HD 141569 and HD 157841 at Ultra–High Resolution

1998 ◽  
Vol 504 (1) ◽  
pp. 522-532 ◽  
Author(s):  
M. S. Sahu ◽  
J. C. Blades ◽  
L. He ◽  
Dap Hartmann ◽  
M. J. Barlow ◽  
...  
Keyword(s):  
High Resolution ◽  
Absorption Lines ◽  
Galactic Latitude ◽  
High Galactic Latitude ◽  
Interstellar Absorption

Interstellar absorption lines in high-resolution IUE spectra of cataclysmic variables

1988 ◽  
Vol 335 ◽  
pp. 829 ◽  
Author(s):  
Christopher W. Mauche ◽  
John C. Raymond ◽  
France A. Cordova
Keyword(s):  
High Resolution ◽  
Cataclysmic Variables ◽  
Absorption Lines ◽  
Interstellar Absorption

Absorption of OH in the 1200 Å Region

1974 ◽  
Vol 52 (4) ◽  
pp. 318-323 ◽  
Author(s):  
A. E. Douglas
Keyword(s):  
High Resolution ◽  
Absorption Band ◽  
Rydberg State ◽  
Strong Absorption ◽  
Absorption Lines ◽  
Strong Absorption Band ◽  
Interstellar Absorption

A strong absorption band of OH has been observed near 1221 Å. From the analysis of high resolution spectra, it has been determined that the upper state is a 2Σ− Rydberg state and the constants of the OH and the corresponding OD state have been obtained. It is shown that the new absorption band will give interstellar absorption lines of OH at 1221.166, 1222.071, and 1222.524 Å. New constants have also been determined for the A2Σ+ and X2Π states of OD.

Echelle Spectroscopy of Interstellar Absorption toward μ Columbae with the Goddard High Resolution Spectrograph

1999 ◽  
Vol 117 (1) ◽  
pp. 400-409 ◽  
Author(s):  
J. C. Brandt ◽  
S. R. Heap ◽  
E. A. Beaver ◽  
A. Boggess ◽  
K. G. Carpenter ◽  
...  
Keyword(s):  
High Resolution ◽  
Interstellar Absorption ◽  
Echelle Spectroscopy

scholarly journals 10. Radio observations of interstellar neutral hydrogen clouds

1957 ◽  
Vol 4 ◽  
pp. 66-66
Author(s):  
R. S. Lawrence
Keyword(s):  
Angular Resolution ◽  
Neutral Hydrogen ◽  
Optical Component ◽  
Absorption Lines ◽  
Radio Observations ◽  
Interstellar Absorption ◽  
Peak Intensity

The detailed relationship between optical interstellar absorption lines and 21-cm. observations is investigated in this paper.Dr Guido Münch, of the Mount Wilson and Palomar Observatories, provided the list of six intermediate-latitude stars shown in Table 1. The spectra of these stars all show complex absorption lines due to interstellar Ca 11. The 21-cm. line is measurable in four of the six regions, although the peak intensity is low in each case. It is noteworthy that for the first two stars on the list the radio velocity agrees closely with the velocity of an intense optical component. In view of the great difference in angular resolution, the failure to find correspondence in every case is not surprising.

Sign in / Sign up

Export Citation Format

Share Document