(cba:news) strike V1974 Cyg
jop at astro.columbia.edu
Tue Sep 12 03:12:06 EDT 2017
Delete V1974 Cygni from the menu. I finished the analysis of all the
data (dominated by David Cejudo's), and there is a very clear detection
of the orbital signal. In fact, two, separated by ~90 days (we never
had that before, and it's very useful to connect the years).
The detection and measurement of the phase of the orbital signal was the
goal... and we have it now. Especially nice since the detection is
uncontaminated by superhumps; we never had that before, also. Two other
things we'd *like* to know are:
(1) What is the phase of the radial velocity variation when the light
reaches its orbital max?
(2) Just how bright is the continuum? The 4000-8000 A region, where we
observe the star at "17.12", is probably dominated by the O III emission
at 5007 A. That emission from the shell needs to be subtracted to learn
how bright the central object is.
Only a very motivated spectroscopist could answer (1); so far, none have
piped up. (2) is best learned from a single high-quality spectrum;
someone might have that. But if you have a filter which excludes that
terrible monstrosity at 4959/5007 A, and preferably also H-alpha, you
might learn that. Might be worth an effort. You don't necessarily need
to detect the periodicity (at 0.08126 days); just measuring the
brightness of a clean, line-free continuum would allow us to correct our
measurement for all that unwanted and so-far-unmeasured nebular light.
Pretty nice result for "the nova of the century"!
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