Hi Jose! Welcome aboard!
Finally we got our first international colleague...that's great!
Your results are phantastic.
I was expecting an outcome with lower reds in the continuum.
Please keep in mind that you are not
observing a real continuum. The star has a completely optical dense environment in form of a radial symmetric wind in all atomic species. You can not see the stellar photosphere and WRs are not classified in the HR domain. What you see in the "continiuum" is just light from electron scattering within the wind.
What are the "corrected" and "uncorrected" spectra?
I'll post here when I have wr140 (==>) 1200 l/mm processed.
Yes, that is the probably most convenient setup. As you can see in our WR 140 web site. Berthold Stober was very successfull with LHIRES plus 1200 Grating. We are eager to see your output!!!
Just today I obtained the following message from Tony Moffat at Université de Montréal (I will place it into the WR site, too). He explicitely asks for spectra in all wavelengths beginning now
once every month (more would be even better) and more often later:
Two weeks ago I was in Madrid (well ESA/Vilspa actually) for a 3-day meeting with 6 others on WR140 - just WR140! Everyone could give a talk for 3 hours - great stuff. With lots of interaction and no such thing as dumb questions. But no time to stop off in Germany this trip.
During our discussions of all aspects of WR140 from radio through IR, optical, UV, X and gamma, one aspect which really came up often was getting the right orbit, based on both sets of lines (WR and O). For that we'll need good time coverage and good quality optical spectra. So the role of your amateyr friends could be quite crucial and we support their efforts. Ideally, we need steady coverage in time (once a month now), then by October 2008, increased to once every couple of nights and every night in Dec/Jan. Yellow spectra are good, but also blue would be useful, to get more O-absorption lines for a good orbit of the O star. S/N should be at least 150/pixel and no worse than ~1 A/pixel, if possible (to get good precision in RVs).
We should also get broadband (UBV best) photometry, around and after periastron passage, to look again for dust-caused dips, from which one can compare with dust models to constrain dust-grain size. Any chance of that, too?
I consider this request as a serious starting signal which includes carefull and exact
data reduction. We are now working with the pro's!!!
Greetings from Bonn, Thomas
As soon as we have an anglophone participant I ask everybody to switch to english within the respective discussion. - Sobald wir einen anglophonen Diskussionsteilnehmer haben, bitte ich alle um Beiträge in englisch innerhalb der entsprechenden Diskussion.