Photons, neutrinos, and gravitational-wave astronomy

Author here: this are my notes on what I mean to say in class, the website contain my whole course.

This particular lecture is still “in prep“, in fact the section "the problem" is just a bullet point and a figure. All other lectures are a bit more polished.

Unless I'm missing something - do the notes cover neutrino astronomy somewhere else? Aside from the general discussion on stellar evolution. Shame, because the detection of pre-optical neutrino emission from 1987A by Kamiokande (and others) was a fantastic theoretical confirmation. Essentially when the core collapses, the environment around the surroundings are optically opaque, but the neutrinos sail on through so you'd expect to see them before the photons.

https://ui.adsabs.harvard.edu/abs/1987ApJ...318L..63B/abstra...

I would recommend Telescope in the Ice as one of the best introductions to modern neutrino detectors - why and where they're built. Also provides a good insight into how a big collaboration is formed, funded and operates. I've worked for IceCube so I'm somewhat biased, but the book is great just for the history.

IceCube has an entire processing pathway (on ice) that is specifically designed to trigger on a supernova detection. One of the very few science results that would page us, and why uptime is absolutely critical to the experiment. On the one hand, we can't point the detector and we don't know where the signal will come from, so it's not predictable (and it's highly transient). On the other, becuase the burst happens shortly before the optical, we can use neutrinos to trigger optical observations as fast as possible - pretty much the whole observing community will drop what they're doing if a star blows up.

I believe we'd expect the whole flux through the detector to bump up above the background, at least at IceCube. PDF: https://iopscience.iop.org/article/10.1088/1742-6596/309/1/0...

After so many observations why is multi messenger still n=1?

Figure 3 is really nice!