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VHIRES-MO spectrum (R=48000) at high SNR (11 x 600 sec. exposure under good conditions) on C11 taken the 19.8 May.

Detail of Raman OIV line:



H alpha line (after H2O telluric removed):



He I line (fines structures evolution):



He II line (increase in intensity):



Christian Buil

Hello, here is my extracted result about variability of EWs on in the red part (same night as others already reported 05.17-18): This graph is showing error bars, calculated by EWs of conitnuum itself near to it at the same length of selected region, using the stddev formula for the overall result (all scripted via IRAF).
Got 0.15 for the Raman OVI 6825, and between 0.8-0.11 for the other lines (H-alpha is special here: division by 10 except the error).
Exposures was taken of 10 -> 8 -> 5 minutes decreasing in the 2nd half of the night (after scope turnover + took other bands spectra).
This reduction was due to H-alpha started to have a pixel reaching the max ADU on the ccd.
All in all, Raman profiles flicker by 10% during a night, shorter integration times are meaningful!

Cheers,
Peter

Evolution of Ag Dra in 4 days

The full spectrum


H Alpha(corrected for heliocentric velocity)


Raman OIV (corrected for heliocentric velocity)

Bonjour, voici le profil de l'observation de la nuit 21/05/2017.
Umberto

Dear all,
How impressiv are your spectra ! C'est fantastique. Olivier, tes spectres en très haute résolution sont incroyables.
J'ai un problème:
I can't saturate Halpha line with my small 200 mm Celestron and my 460EX Atik camera in binning 1x1 mode in 20 minutes. But I took spectra of AG Dra with 1200s exposure time. I show you my results (blue profil) in low resolution (Alpy 600 spectrograph), compared with 8x600s last month (black profil). Will I have more details in the blue part in binning 2x2 mode ?
For the blue plot: 8 x 1200s, R= 592 - HD145454 (A0Vs) is my reference star (not my favorite star...A joke).
I'm not sure about the identity of some emission lines (Calcium or some Balmer lines...Or blended lines ?)
Thank you for comments.
Cheers,
Michel Verlinden

Thanks to all for the very coverage and the quality of the spectra.

It looks like the event is already finished. Very weak and very short.
Of course, we go on the good job!

François

AG Dra low resolution spectrum taken the 20.89/05/2017 (C11 + Lhires III 150 g/mm):





Christian Buil

An update from Rudolf Galis:
The recent activity of AG Dra looks really strange. After promising increase of its brightness (around 0.1 mag/day in B filter), the magnitude stopped to raise and it is almost at same level as before this event, now. The event recalls the pre-outburst in 2015 with maximal brightness around 10.7 mag in B filter. Is this event another pre-outburst, as we have already recorded in the photometric history of AG Dra? There is still a chance for main outburst: if we assume that the last outburst occurred around JD 2 457 517 and the time interval between outbursts of AG Dra varies from 300–400 days, the outburst window is open until June 12, 2017. Another possibility is that AG Dra will return to quiescence stage as we have already detected such behaviour during the weak activity stage 1963–66.
In any case, I suggest to continue with daily monitoring of AG Dra at least to mid of June. Subsequently, we would redefine the observational schedule of AG Dra. Thank you for your cooperation.

Rudolf Gàlis


Let'us go on the good job
Thanks to all
François

Hello all

AG Dra spectra the 2017/05/24.980

Meade ACF 355mm f/d 7 + Alpy600 + Atik460EX
Cheers,

Echelle spectra after the weak burst
He I 5875 François