As part of our search for emission-line objects in 26 Galactic globular clusters, we found a small emission nebula in M 22 (NGC 6656). Its spectral lines and mass indicate that it is the remnant of a nova.
A catalogue of ancient Chinese observations contains a record of a 'guest star' observed in the year 48 BCE very close to the position of the globular cluster.
Together with a remnant age of roughly 2,000 years estimated from its brightness, this suggests that the underlying nova has been observed by humans about 2,000 years ago.
This would be one of the oldest confirmed extrasolar observations recorded by humans.

A nova is an explosion caused by accreted matter on the surface of a white dwarf in a binary system.
The explosion increases the brightness of the white dwarf by several orders of magnitude, causing previously invisible stars to become much brighter, sometimes even visible to the naked eye. The white dwarf loses parts of its mass in the explosing, this ejected mass is distributed into the space surrounding the binary system. The ejected mass is illuminated by the UV radiation from the white dwarf and re-emits the energy in visible wavelengths, which can be observed as emission lines.
While a handful of novae are observed in the Milky Way each year, only two novae have been observed in Galactic globular clusters in the last 150 years.

Links to paper and data.

While searching for radial velocity variations and thus binary stars with our survey of 25 Galactic globular clusters, we came across with one curious star. After analysing the strong radial velocity signal and the observed properties of this star, the binary system appears to be most likely a main-sequence turn-off star orbiting around a detached stellar-mass black hole with at least four times the mass of the sun.

Links to paper and data.

Odd Behaviour of Star Reveals Lonely Black Hole Hiding in Giant Star Cluster
Created: 17 January 2018
ESO press release about our finding of a stellar-mass black hole candidate in the globular cluster NGC 3201:

Full article available on arxiv

Data for radial profiles are available here

In the media section of this homepage we present some visualisations which were created in the course of the PhD talk of Benjamin Giesers:

How a colour magnitude diagram (CMD) is created

The binary star content of NGC 3201

The 'chromosome map' of NGC 3201

ESO press release about the new adaptive optics facility for MUSE:

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