Assuming that all their light is coming from stars, they have far too much stellar mass (with stellar masses similar to the Milky Way) to be the progenitors of today's globular clusters.
In globular clusters stars tend to have similar age in terms of main sequence progression. If most of the stars approach their brightest phase, the cluster will be extremely bright relative to its mass.
I've read the paper, those objects have all properties of AGNs, but since having AGNs so early doesn't fit current mainstream, authors try very hard to come up with a different explanation.
This seems very cool, but last release is from 2014, last commit is from 2018, and there are various bug fixing PR that have been waiting for years to be merged :(
What about https://github.com/jazzband/docopt-ng?
I just downloaded Transmission 4 via Github and it works on my M1 Macbook. I previously had problems with beta versions as well, so I guess they addressed that.
The sentence you’ve quoted, from the abstract of the paper, refers to the state of knowledge before this paper was written/published.
The results section of the paper updates this knowledge. It says:
“Compared to those with first infection, those with reinfection exhibited increased risk and excess burden of all-cause mortality, hospitalization, and at least one sequela in the acute phase and the post-acute phase of the reinfection.”
“… the risk was higher in those who had two infections (HR 2.11 (2.07, 2.15); burden 234.58 (227.08, 241.92)), and highest in those with three or more infections (HR 3.00 (2.71, 3.31) …”
Susceptibility is also a spectrum, though, which is what I meant to get at and failed to communicate clearly. Immunocompromised people are probably more susceptible than others? I don't have data on that, it's just a guess.
We have models for how much light a star of a given mass, age, chemical composition etc. puts out as a function of wavelength. We can then take mixtures of stars and predict the total light output of a stellar population in different bandpasses. So from observations of a galaxy in these different bandpasses, we can use these models to determine things like the age of the stars in the galaxy—from how old the stars in the best fit stellar population are—as well as the mass (or number) of stars—from how many are needed to match the observed brightness of the galaxy.
