FS cma star, a pro am campaign

ARAS group has a pro am campaign concerning the B[e] FS cma star.

 They are not classical Be, bracket means forbidden emission lines in their spectra. Well this group is not very known and homogeneous as it concerns protostellar stars to proto planetary nebular star. From the birth to the Death.

 In this campaign we'll try to distinct some objects belonging to the FS cma star group. Prototype is FS cma, a hot blue star, showing a strong infrared excess. The question remaining is are these stars binaries with a cooler companion, explaing the dust infrared excess ? 

Here is the proposal by Anatoly Miroshnichenko of this campaign:

" This group I suggested to call FS CMa type objects (after the protype FS CMa = HD 45677). Indeed, they do not show some spectral lines that are sensitive to luminosity and appear only in supergiants. The group has already about 50 members and still grows, as I continue to look for candidates in various data bases. Most group objects are fainter than 11-th magnitude in the V-band. However, there is a fraction of group that is brighter. My hypothesis is that FS CMa objects are binaries with relatively large orbital periods (otherwise there is no room around stellar components to store circumstellar gas that is responsible for the strong line emission observed in the spectra of these objects). The periods can be from several weeks to years. Therefore, it is important to follow the objects for a long time. I have started such a monitoring 5-10 years ago and already accumulated a number of spectra. It wold be great if we can continue on selected objects together. This program requires observing frequencies of the order of once in a few weeks. There are only seven objects in my current list of this group that are brighter that ~10.5 magnitde. They are scattered all over the sky. So, if you think you can do some of them sometimes, it would be great. Let me know, and I share the information to get the observing running. This project can also be subject of a new campaign at a moderately large telescope (around the size of 1-m or so) to follow this brighter group and some fainter objects to study their short-term variability in order to understand what is going on in their gaseos envelopes."

Another comment by our PI:

They showed quick change like V/R ratio, profiles. Orbiting period maybe in months,  Here is the answer the PI in charge of this pro am campaign about V1972 cyg who has a strong asymmetric V profile double peak Ha emission

"The Halpha V/R ratio is most likely due to absorption by dust in front
of the star (which affects the blue-shifted peak more than the red
one). The asymmetry should be due to a certain density distribution
which we could probably find by modeling."