Planck discovers filament of hot gas linking two galaxy clusters

Planck spots hot gas bridging galaxy cluster pair
This image shows the two galaxy clusters Abell 399 and Abell 401, which can be seen in the upper left corner (Abell 401) and in the central lower portion of the image (Abell 399), respectively. They are located at redshift z~0.07 – about one billion light-years away from us. In the optical image, obtained with ground-based telescopes, galaxies are visible as slightly elliptical, bright flecks. The two clusters can be seen as the two portions of the images that show a higher concentration of galaxies. The image is also dotted with several foreground stars that belong to our Galaxy, the Milky Way. Depicted in orange is the hot gas that pervades the two clusters and the space between them, based on data from ESA's Planck satellite. Planck can detect the hot gas via the Sunyaev-Zel'dovich effect. Credit: Sunyaev–Zel’dovich effect: ESA Planck Collaboration; Optical image: STScI Digitized Sky SurveI

(—ESA's Planck space telescope has made the first conclusive detection of a bridge of hot gas connecting a pair of galaxy clusters across 10 million light-years of intergalactic space.

Scanning the sky at microwave and sub- with Planck, astronomers have unambiguously detected a 'bridge' of hot gas connecting two galaxy clusters, Abell 399 and Abell 401. The filament extends over about 10 million light-years and contains gas with a temperature of about 80 million K. At least part of this gas might derive from the warm-hot intergalactic medium (WHIM) - the elusive web of gaseous filaments which is believed to pervade the Universe.

The current understanding of cosmology suggests that the Universe is dominated by dark matter and dark energy. The remaining 'normal' matter – or baryonic matter – of which stars and planets are made, accounts for just a tiny fraction of the cosmic budget, less than five per cent. Baryonic matter can, in principle, be detected through the it releases. But there's a problem: the amounts of baryonic matter detected via in the distant, ancient Universe and in the nearby one do not match. Astronomers have struggled to locate about half of the baryonic matter expected to be present in the local Universe.

A leading candidate for the location of these so-called 'missing ' is the warm-hot intergalactic medium or WHIM. The WHIM is the baryonic component of the , a filamentary network of both dark and baryonic matter that is believed to pervade the Universe. of the formation of predict that galaxies and galaxy clusters are embedded in the cosmic web, and that the WHIM might account for most of the baryonic matter in the local Universe. This network of tenuous gas ranges in temperature from 100,000 to several tens of millions of K and due to its extremely low density has proved very hard to detect.

In the past decade, astronomers have started to collect evidence supporting the WHIM hypothesis, mainly via X-ray observations and optical/ultraviolet spectroscopy. A recent study using data from ESA's Planck satellite has brought a new insight to the debate, opening a new spectral window for the study of the missing baryons based on observations at microwave and sub-millimetre wavelengths.

"Although the WHIM is mainly organised in long and diffuse , we expect to find it also in the proximity to galaxy clusters, which are the largest gravitationally-bound structures in the Universe," explains José M. Diego, a Planck Collaboration scientist from the Instituto de Fisica de Cantabria (UC-CSIC) in Santander, Spain.

Planck spots hot gas bridging galaxy cluster pair
This image shows how matter in the Universe is arranged on very large scales, forming a wispy network of clusters, filaments and voids known as the cosmic web. This image was extracted from a numerical simulation of the formation and evolution of cosmic structure. The colour scale indicates the density of gas in the cosmic web: blue indicates regions where the density is lower than average, whereas white and red correspond to increasingly denser structures. Galaxy clusters form at the densest knots in this network, where filaments intersect. The temperature of gas is higher in the denser portions of the cosmic web, ranging from about a million K in the blue regions to tens of millions of K in the white regions and hundreds of millions of K in the red regions. The image shows a portion of the cosmic web that spans almost 900 millions of light-years across. Credit: Klaus Dolag, Universitäts-Sternwarte

"Planck can detect galaxy clusters across the sky because the hot gas that fills them imprints a characteristic signature on the Cosmic Microwave Background known as the Sunyaev-Zel'dovich effect," Diego adds. "Based on the same principle, Planck could be sensitive to gas from the WHIM, too".

Astronomers in the Planck collaboration have been exploiting the Sunyaev-Zel'dovich effect in the search for galaxy clusters. The first results of Planck's hunt for these gigantic cosmic structures were presented in 2011, along with the public release of an extensive catalogue of clusters. Careful analysis of this rich data set is now starting to reveal the properties not only of galaxy clusters, but also of their surroundings.

"Detecting the WHIM via the Sunyaev-Zel'dovich effect is extremely challenging due to its low density," comments Juan Macias-Perez, a Planck Collaboration scientist from the Laboratoire de Physique Subatomique et de Cosmologie in Grenoble, France. "The best chance to detect it is to look at the regions between pairs of nearby galaxy clusters that are interacting with one another: as they approach each other, gas in the inter-cluster region becomes denser and hotter, hence easier for us to spot," he adds.

This movie shows the three-dimensional structure of the cosmic web, the wispy network of both dark and baryonic matter that is believed to pervade the Universe. The movie was extracted from a numerical simulation of the formation and evolution of cosmic structure. Galaxy clusters are visible where the concentration of galaxies (shown in white and purple) is higher. Clusters form in the densest knots of the cosmic web, where filaments intersect. The density of gas in the filaments that link the cluster is represented with different colours, with dark brown indicating less dense regions and brighter colours (from orange to yellow and green) indicating increasingly denser regions. The colour scale also shows the gas temperature, ranging from less than a million K in the darker regions up to several tens of million K in the green regions. Credit: Klaus Dolag, Universitäts-Sternwarte

With this aim, astronomers from the Planck Collaboration inspected the catalogue of clusters compiled from data collected by Planck during its first two surveys, and the beginning of the third. "We looked for pairs of clusters which are close enough for a possible intervening filament to be detected, but also separate enough, on the plane of the sky, for Planck to resolve them as individual sources," explains Macias. The astronomers then identified a handful of candidates, which are all at very low redshifts – hence cosmologically short distances – to fulfil these requirements.

"A careful analysis revealed a 'bridge' of hot gas connecting two of the clusters in the sample: Abell 399 and Abell 401," comments Diego. These two clusters are located at redshift z~0.07 – about one billion light-years away from us. In contrast, the bridge has a length of about 10 million light-years.

Hot gas can also be detected via its direct emission at X-ray wavelengths. A previous study of Abell 399 and Abell 401, based on X-ray data from ESA's XMM-Newton space observatory, hinted at the presence of hot gas not only within, but also between the clusters, but the evidence was not conclusive. The result based on Planck data is much more robust and confirms that the two structures are indeed connected by a bridge of material; this also represents the first detection of inter-cluster gas obtained via the Sunyaev-Zel'dovich effect.

"By combining Planck data with archival X-ray observations from the German satellite ROSAT, we estimated the temperature of gas in the bridge as about 80 million K," notes Torsten Enßlin, a Planck Collaboration scientist from the Max-Planck-Institut für Astrophysik in Garching bei München, Germany. This value is of the same order as the temperature of gas in the two clusters. Although it may be part of the WHIM, the origin of this inter-cluster gas is, as yet, unclear.

"It is still debated whether the gas derives from the WHIM or from the gas that was previously part of the two clusters; numerical simulations suggest that it could well be a mixture of both," explains Enßlin. "Further analysis of the complete Planck data might help to clarify this issue by revealing additional examples," he adds.

The astronomers have already identified another promising candidate: the composite system Abell 3391-Abell 3395, which is highly substructured and may in fact consist of three or four clusters. This system exhibits what appears to be a bridge of material linking its various components. Due to the complex nature of this object, a more detailed investigation will be needed to confirm this second detection.

"This discovery highlights the ability of Planck to probe out to their outskirts and even beyond, allowing us to investigate the connection between intra-cluster gas and gas that is part of the cosmic web," concludes Jan Tauber, Planck project scientist at ESA.

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More information: "Planck Intermediate Results. VIII. Filaments between interacting clusters", is accepted for publication in Astronomy & Astrophysics. The Planck maps from which the cluster data have been extracted will be released to the public in early 2013.
Journal information: Astronomy & Astrophysics

Citation: Planck discovers filament of hot gas linking two galaxy clusters (2012, November 20) retrieved 16 May 2022 from
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