Figure 1.
Map of the sky showing the clusters surveyed in KIWICS, and the eight clusters that have been already analysed.
Figure 2. Left panel: Example of UDGs found in different clusters,
the white lines show a scale of 5 arcsec. Upper right panel: The Sérsic
index distribution (a measure of the light concentration of a galaxy)
for central (red) and outer (blue) UDGs, showing that the galaxies in
the central regions are more concentrated. Lower right panel: Axis ratio
distribution of the two samples, showing that galaxies in the central
regions are rounder.
Credit: Pavel Mancera Piña. Large format: [PNG].
In preparation for the new multi-object survey spectrograph, WEAVE, on
the 4.2m William Herschel Telescope, the astronomical community is
working on deep imaging surveys to identify the astronomical objects
which will be studied later in more detail with WEAVE.
WEAVE will allow astronomers to take optical spectra of up to ~1000
targets at the same time in a single exposure, or to carry out
integral-field spectroscopy using 20 deployable mini integral-field
units or one large integral-field unit.
Galaxies, like our Milky Way, can live in large groups with many
others, the so-called galaxy clusters. Such associations contain a
potpourri of galaxies with many different properties such as colours,
ages, morphologies and brightness. Among this broad diversity there
exists a bewildering population of large but extremely faint galaxies,
called "ultra diffuse galaxies" (see e.g., news release "The Puzzle of Ultra-Diffuse Galaxies"),
and understanding their properties is important to understand how the
environment of galaxies affects their evolution. Since they are so
faint, they are easily perturbed by the cluster environment, and
therefore are ideal probes to study what happens with galaxies in the
dense cluster environment.
Using the capabilities of the WFC at the Isaac Newton Telescope
(INT) to explore large areas of the sky and detect faint ultra-diffuse
galaxies (UDGs), a collaboration of astronomers in the Netherlands and
Spain performed a study to investigate these galaxies in detail, the
Kapteyn IAC WEAVE INT Clusters Survey (KIWICS).
When finished, the KIWICS survey will contain 48 X-ray selected clusters. The results for 8 clusters have recently been published in the journal Monthly Notices of the Royal Astronomical Society.
By analysing the general properties of about 500 newly-found UDGs at different distances from the centres of the clusters the researchers found several signs of environmental effects. The first result was that the larger clusters show a lack of UDGs in their centres. This is proof that the enormous gravitational forces present there are tearing these fluffy galaxies apart.
Moreover they also found that UDGs away from the cluster centre are generally younger and have less concentrated stellar distributions, showing that the gravitational potential of the cluster, which is stronger close to the cluster centre, is changing the structure of galaxies, and is removing the interstellar gas, so that no new stars are being formed in the centres of clusters.
In addition, they see that, as UDGs approach the centres of their host clusters, their morphologies are transformed from irregular discs to more spheroidal systems. In fact, for dwarf galaxies, which are similar to UDGs, but much smaller, observations in the literature give the same results.
By analysing the general properties of about 500 newly-found UDGs at different distances from the centres of the clusters the researchers found several signs of environmental effects. The first result was that the larger clusters show a lack of UDGs in their centres. This is proof that the enormous gravitational forces present there are tearing these fluffy galaxies apart.
Moreover they also found that UDGs away from the cluster centre are generally younger and have less concentrated stellar distributions, showing that the gravitational potential of the cluster, which is stronger close to the cluster centre, is changing the structure of galaxies, and is removing the interstellar gas, so that no new stars are being formed in the centres of clusters.
In addition, they see that, as UDGs approach the centres of their host clusters, their morphologies are transformed from irregular discs to more spheroidal systems. In fact, for dwarf galaxies, which are similar to UDGs, but much smaller, observations in the literature give the same results.
It is expected that the whole KIWICS survey will be finished at the end of 2019, just before WEAVE will be installed on the William Herschel Telescope.
More information:
Pavel E. Mancera Piña, Reynier F. Peletier, J. Alfonso López Aguerri,
Aku Venhola, Scott C. Trager and Nelvy Choque Challapa, 2018,
"Reviewing the frequency and central depletion of ultra-diffuse galaxies
in galaxy clusters from the KIWICS survey", MNRAS, 481, 4381 [ ADS ]
Pavel E. Mancera Piña, J. Alfonso López Aguerri, Reynier F. Peletier,
Aku Venhola, Scott C. Trager and Nelvy Choque Challapa, 2019, "The
evolution of ultra-diffuse galaxies in nearby galaxy clusters from the
Kapteyn IAC WEAVE INT Clusters Survey (KIWICS)", arXiv:1901.07577 [ ADS ]
Contact:
Javier Méndez (Public Relations Officer)
