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Here's a publication about spectroscopy and interferometry taken at the same time.
The spectroscopy part was made with my eShel spectrograph to have a very good calibration accuracy on the Balmer's lines.
The interferometry part was made with two telescopes of one meter in diameter.

https://academic.oup.com/mnras/advance- ... 17/6608892

Hi Olivier,
would you be so kind to send a copy of the paper?
Another question:
what about the evaluation of the del Sco spectra at BeSS?
Are there further not jet evaluated spectra of other observers? Because of the periastron passage radial velocity of the star as much spectra as possible would be helpful.

Ernst

Hi Olivier,
you write in capter 4.3.1:
In short, despite our ability to reproduce fairly well the Hα line profile of P Cygni observed in 2020 using such a less intense wind model, it is beyond the scope of the current paper to state that the intensity of the wind of P Cygni varied in this way during this two-year period.

I find this to be an unacceptable disregard for the facts. In fact, the intrinsic Halpha flux has changed dramatically during this period (see the attached ARAS long-term monitoring of the intrinsic Halpha flux of P Cyg)

It would be good if you could share this important observation with your fellow authors. It could be that your interpretation and summary of the results will change significantly as a result. Regards,
Ernst

Ernst Pollmann wrote:Hi Olivier,
would you be so kind to send a copy of the paper?
Another question:
what about the evaluation of the del Sco spectra at BeSS?
Are there further not jet evaluated spectra of other observers? Because of the periastron passage radial velocity of the star as much spectra as possible would be helpful.

Ernst

Ernst,
Bess database is down for the moment du to a hard disk failure, but submitting spectra is always possible and we have more than 700 spectra to validate and we can't validated the spectra at this time...

Ernst Pollmann wrote:Hi Olivier,
you write in capter 4.3.1:
In short, despite our ability to reproduce fairly well the Hα line profile of P Cygni observed in 2020 using such a less intense wind model, it is beyond the scope of the current paper to state that the intensity of the wind of P Cygni varied in this way during this two-year period.

I find this to be an unacceptable disregard for the facts. In fact, the intrinsic Halpha flux has changed dramatically during this period (see the attached ARAS long-term monitoring of the intrinsic Halpha flux of P Cyg)

It would be good if you could share this important observation with your fellow authors. It could be that your interpretation and summary of the results will change significantly as a result.

pcyg_intrinsic-flux.png

Regards,
Ernst

Dear Ernst,
Firtst it's not me, but others professional working on this paper whose wrote this sentence, then they precisely asked me to redo the spectra of P Cyg at the same time as their observations, to have a spectrum of the state of P Cyg at the same time as their observations. They just had a doubt about the stability of the anterior P Cyg profiles.

My work in this article consisted in providing them with spectra made at the same time as their interferometry measurement, but I have not written anything nor issued conclusions that go far beyond my knowledge of astrophysics.

Ok, I understand, Olivier,
but nevertheless, could you be so kind to pass them my posting?

Ernst

Ernst Pollmann wrote:Ok, I understand, Olivier,
but nevertheless, could you be so kind to pass them my posting?

Ernst

Of course, i will send your graph.

Olivier,
could you send me a corresponding eMail address of one of the authors?
Ernst