On the night of Jul 29/30, 2025, under very good conditions, I acquired images of the recurrent nova T CrB. This star undergoes outbursts at long intervals of 80 years or so. Its next outburst is predicted to occur soon (but then again, it was also predicted to occur during 2024), and so I've joined the crowd who are monitoring it.
Conditions were good, and I improved the focus of the guide camera, which turned into slightly higher photometric quality. Rah! No outburst, though.
Two of the students who are visiting RIT for the REU in Multimessenger Astrophysics decided to do a little observing of their own tonight. They brought a telescope out to the concrete pad, set it up, and looked at some clusters and nebulae. Excellent!
This recurrent nova brightens by about 8 magnitudes (!), from V = 10 to about V = 2, around every 80 years. Will we see another outburst THIS summer?
These observations involved:
Notes from the night:
With the better focus, I think I can reduce the exposure time for T CrB's guide star from 5 seconds to 2 or 3 seconds. Short tests tonight suggest it might help. Do more tests on subsequent nights.
The picture below shows a cropped image of the field of T CrB from Jun 14/15, 2024. The field of view is about 20 arcminutes across.
I've marked the location of several comparison stars, with magnitudes and names taken from the AAVSO's table X40237AAS. Note that the magnitudes listed for stars "A" and "B" have changed from the ones I listed in last year's notes.
star name B V
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A 000-BJS-901 11.096 10.554
B 000-BBW-805 11.779 11.166
C 000-BPC-198 13.049 12.336
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When the target is centered, the finder TV shows this field:
Here's the sky background over the course of the run. Note the very brief clouds at 886.65.
The FWHM rose a bit later in the night.
The graph below shows changes in the photometric zeropoint of an ensemble solution of the instrumental magnitudes over the course of the run. Note the effects of the brief cloud bank.
Using aperture photometry with a radius of 7 pixels in V filter (binned 4x4, each pixel is 1.036 arcsec, so a radius of 7.3 arcsec), and 7 pixels in B filter (binned 4x4, each pixel is 1.036 arcsec, so a radius of 7.3 arcsec), I measured the instrumental magnitudes of a number of reference stars and the target. Following the procedures outlined by Kent Honeycutt's article on inhomogeneous ensemble photometry, I used all stars available in each image to define a reference frame, and measured each star against this frame.
Sigma-vs-mag plots show that the floor in V-band was about 0.006 mag in V -- pretty good. in B-band, it was 0.006, also good.
The measurements show that the target is still in quiescent phase.
I've submitted these measurements to the AAVSO.