The WFI Halpha spectroscopic survey

Lines were also selected from the HARPS Procyon (HD 61421) spectrum, so that these could be used for hotter stars in addition to the main line list.. The line list was constructed

Several hypotheses could explain this discrep- ancy: a metallicity effect (Bergh¨ofer’s relation was determined for Galactic stars but SMC stars have weaker winds); X-ray emission

After summarizing the general importance of massive stars, we describe the spectroscopic observations of our program stars. We then detail the data analysis process, which

Figure 6 and 7 illustrate the clusters obtained for line segments and circles, and the sorted number of data points in each cluster for both object categories.... Clustering of

In the open clusters Trumpler 14, 15, 16, Collinder 232 and their vicinity in the Carina nebula; 6 of the 16 emission-line stars seem to be Herbig Ae/Be stars. For the 10 of

In order to further investigate the occurence of emission line stars in NGC6611 and to determine the nature of objects, we used the Wide Field Imager (WFI) at ESO in

The three-dimensional model of the dust dis- tribution of Drimmel & Spergel (2001) is used. Black represents all simulated stars, dark grey those for which the DIB line

We report molecular gas mass estimates obtained from a stacking analysis of CO line emission in the ALMA Spectroscopic Survey (ASPECS) using the spectroscopic redshifts from the