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Looking at the light curve Stewart, there is not much difference. In any case, the objective of the project is to measure the time and duration of each outburst, rather than its precise mag. Thanks for your observation. If you are getting decent signal to noise ratio then stick with the V filter -after all, you are using a decent aperture scope. But no filter allows better SNR, so is often preferable with small telescopes.
Still worth following this nova in her while the field is well placed. Fading the mag 15 now, though, but perhaps leveling off:
I used EverBuild external frame sealant, Grant.
I applied both to the outside wall and inside. I overpainted the latter with the polymeric concrete sealant paint base I used for the rest of the floor.
Yes, definitely a bit brighter last night, Nick: ~0.25 mag brighter on Jul 20 in CV for me compared to 24 h earlier.
After a drop in brightness in the first 24 h, the nova has been at ~mag 13 the last 3 nights. Not much of a light curve so far as we are in the early days of this eruption. Further observations are encouraged.
Good to see the data rolling in for this star. Many thanks to all observers. It’s been faint for a few days: I’ve have it at 16.6 yo 16.7 the last couple of nights.
Now the nights are getting a bit longer, some time-series photometry runs become possible.
Christian Knigge (U of Southampton) notes:
“I just wanted to flag up that we’re
currently still trying to follow the outburst of V627 Peg — one of the
closest WZ Sge stars that erupts only every 5 years (at best) and has
just recently gone off. I’m involved in a campaign to get X-ray,
ultraviolet and radio coverage of the outburst, alongside, of course,
optical.The thing is really bright in outburst — V ~ 8-10 or so — so it’s
great for high-cadence photometry or even spectroscopy, for anybody who
has a spectrograph. For our campaign, any long sequences would be
useful. Ideally we’d have long runs covering the full outburst in 2
filters, say B and V.In terms of spectra, time-resolved spectroscopy would be awesome — I’m
particularly interested in the transition from a pure absorption line
spectrum near plateau to a pure emission line spectrum in quiescence.
Where and how fast does this happen, and does it correlate with other
things happening at other wavelengths.Thanks!
Christian “Further confirmation as nova: https://www.astronomerstelegram.org/?read=14793
Tim, the Variable Star Section CCD Target List has some shorter period eclipsing binaries that might be useful if your aim is to test your system. The Beginner’s Category has a few systems that are 1 day or less. Ones around atm include EG Cep and TZ Lyr.
Given the short nights atm, you would need very short periods.
You could also look at any SU UMa dwarf novae that are in outburst. CVnet lists current ones. V1227 Her (UGSU, eclipsing, orbital period 0.064419 d (92.763 min)) might be a good one for you. There is a Journal paper on it here.
A motorised Dome facility is not commercially available for the original 2.1m Pulsar dome. A few people have come up with diy solutions but way beyond my level of expertise.
A word of caution, Grant. I have that model and it is superb, but with one limitation. The slit is a bit narrow. They widened it in later models.
Consequence is that when the scope is pointing obliquely across the slit, it doesn’t take very long before you need to shift the dome round a bit. The wider the scope, the shorter the time. Can be a pain if you are doing a long time series run. I’ve long thought my C11 is at the practical limit. I wouldn’t like to use a 12-inch.
Kato-san (VSnet) notes that t3 (time to drop 3 mags) is ~ 2.3 days. Appears to be record breakingly fast!
Now confirmed as a Nova by Munari, Valisa and Dellaporta in an ATEL 14704: “Spectroscopic classification of TCP J18573095+1653396 as a nova bordering naked-eye brightness”
