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It is slightly strange that they decided to use a subset of all the available spectra (There are currently 104 in the BAA, 392 in the ARAS and 113 in the AAVSO databases, most of which would meet the resolution criterion though many are likely duplicates) I wonder what the selection criterion was.
On it now with the ALPY200. I make it roughly mag 13.5 unfiltered off the spectrograph guider so significantly brighter than at quiescence.
EDIT: I see that is consistent with the 13.64 V (APASS) at 16:20 today in the Gaia follow up data
They used to be even smaller I think (AstroTech 65mm/70mm refractors) They also had at least one with a Star Analyser 200 in the filter wheel which Arne Henden and I sorted. Unfortunately that does not work well with the new Takahashi E-180 astrographs which at f2.8 are too fast for the SA200
Raising the public profile through funding permanent BAA sponsored exhibits promoting the role of amateurs in science museums and similar venues perhaps? Or perhaps taking a stake in the rebuilding of the Galloway Forest Dark Sky Observatory which (was) burnt down earlier this year?
and we have a member with expertise in this area
A remote spectrograph in the southern hemisphere could be productive and is not something that the existing “telescopes for hire” provide. There is 2SPOT, a proof of concept dedicated remotely operated spectrograph on a telescope farm in Chile run by an amateur group, funded from commercial donations, individual personal investment and crowd funding. (The equipment was shipped out and commissioned on site and is maintained locally)
I see fellow amateur supernova classifier Claudio Balcon took a spectrum last night and classified as a CV (with a blue continuum and weak Balmer absorption at ~0 redshift)
Yes I saw that this morning. It is a pity it took 10 hours to report. It was clear here last night so could have grabbed a confirming spectrum.
Looking at the full paper, I see that they found deconvolving the images using the actual measured stellar point spread function gave artifacts so they resorted to tuning the PSF using a parameterised function. The reference to the validation of the technique using Vesta might be interesting for planetary imagers.
Well let’s just say i’ve seen a lot worse ! It would make a good template for anyone considering undertaking a similar sort of project
Cheers
Robin
Despite poring over the radar maps looking for gaps between the rain showers I have only managed 10 min on this so far.
Only the Balmer lines in emission are clear in the noisy spectrum but it does perhaps seem to be intermediate between the low and high state spectra in the literature. Here for example in the high state from L. Rosino et al 1993 PASP 105 51
and the low state (blue end only) from Voikhanskaia, N. F. 1988, A&A, 192, 128
(Both low state spectra, showing interesting variation during the 0.13 day orbit)
Cheers
Robin
Another low resolution R~500 spectrum last night (low SNR due to bright full moon) continues to show no evidence of H alpha (in emission or absorption) but the higher Balmer absorption lines have increase in depth. V mag for the two spectra were ~12.8/13.7 (AAVSO)
Robin
Hi Hugh,
Looks good. I identified the coronal lines lines in a 2006 Star Analyser spectrum using this reference
This time round I’ve used ISIS to make a little animated gif (attached) showing the [FeX] line emerging based on 4 observations between 25th Aug and 11th Sept
Cheers
Robin
The legal restrictions have been lifted but the wearing of face masks and social distancing where possible is still advised by both the government and NHS as ways to limit the spread. Personal freedom works both ways. A poll of members would be interesting. It could be that actually more members would attend provided modest precautions like face masks and social distancing were in place than would not attend because they do not wish to follow the guidelines.
Thanks Gary.
The Taichi Kato paper was not published until 2004.
https://ui.adsabs.harvard.edu/abs/2004PASJ…56S.135K/abstract
I will send a correction to CDS
Cheers
Robin
Here is the spectrum of BD+25 103, also identified (likely incorrectly) in SIMBAD as Nova And 1979, compared with an F2v standard
Hi Gary,
Could “Nova And 1979” actually have been LL And with a position error? See VSSC #83 1995 p7 and separate thread on “N And 1979”
https://britastro.org/vss/VS0083.pdf
(Your first VSSC after you took over directorship in 1995 by the looks)
Robin
The TA article
http://articles.adsabs.harvard.edu/pdf/1979Astr…16..152.
confusingly IAUC 3412 covers reports on several diverse objects including asteroid 1979QB
http://www.cbat.eps.harvard.edu/iauc/03400/03401.html
Cheers
Robin
