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The search for WIMP annihilation in the Sun

Title: First Search for Dark Matter Annihilation in the Sun Using the ANTARES Neutrino Telescope
Authors: ANTARES Collaboration: S. Adrián-Martinez, I. Al Samarai, A. Albert, et al.
First Author Institution: Institut d’Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC) – Universitat Politècnica de València.

The quest for identifying the dark matter particle is well underway. Many experiments are relying on different detection methods to look for this elusive particle. In this paper, we discuss the work of the ANTARES (Astronomy with a Neutrino Telescope and Abyss environmental RESearch project) collaboration, which is using a neutrino telescope to search for signals of dark matter annihilation in the Sun.

Elusive WIMPs

Most of the matter in the Universe is not visible, it does not interact light. Think about it: casting light on something and seeing what we get back is the main physical mechanism we have of knowing it is there. In astronomy, we observe the light emitted by the object or the inverse, we notice light being absorbed by an object.  However, most of the matter in the Universe will not allow us to perform that experiment. We know of its existence because of its gravitational influence on the evolution of the Universe, the dynamics of galaxies or its lensing signatures. The leading theory for “dark” matter is that it is made of WIMPs, weakly interacting massive particles that naturally arise in supersymmetry (SUSY), which is an extension of the Standard Model of particle physics.

In spite of all the gravitational evidence in favor of dark matter, we still have not had a definitive detection of dark matter particles. The literature on these searches is vast, with experiments looking for dark matter directly, through the recoil of targets that collide with dark matter particles or indirectly, through products of the annihilation or decay of dark matter particles. We gave a short overview of the recent advances of this field in this astrobite. We also described an interesting experimental design of a new type of dark matter detector here.

The WIMP annihilation signal

If dark matter is indeed a supersymmetric particle, when two dark matter particles collide, they annihilate into other particles (including photons, neutrinos and antimatter). Indirect dark matter experiments search for those products by looking at regions where we expect the dark matter density to be high. WIMPs can become gravitationally trapped in the center of the Sun, annihilate and produce neutrinos that can escape and reach the Earth. Neutrino telescopes, such as ANTARES, can be used to search for this signal.

How does ANTARES work?

Neutrino telescopes do not resemble optical telescopes at all. When neutrinos interact with the Earth or the atmosphere, they produce charged particles (muons). If the particles have very high energies (10 GeV-100TeV), they emit Cherenkov light as they traverse water.

The  ANTARES telescope is located at ~2500 m underwater in the Mediterranean Sea. Its array of photomultipliers collects the Cherenkov light with the aim of reconstructing the direction of the original incoming muon. The figure below shows a diagram of the experiment underwater.

The experimental setup of the ANTARES neutrino telescope, with its 12 lines of photomultipliers, under the sea. Credit: F.Montanet, CNRS/IN2P3 and UJF for Antares. Produced with POV-ray.

The experimental setup of the ANTARES neutrino telescope: a dozen of detection lines of 450 m in length and separated by approximately 70 m from one another, with 75 photomultipliers each. Credit: F.Montanet, CNRS/IN2P3 and UJF for Antares. Produced with POV-ray.

 

The background, always the background

As usual in this business, one needs to be careful in distinguishing signal from background. In this particular case, cosmic rays entering the Earth atmosphere can produce downgoing muons and both downgoing and upgoing neutrinos that could mimic the muons from dark matter annihilation. The most significant contribution to the background comes from the downgoing atmospheric muons. To avoid them, the best strategy is to only take into account measurements that were triggered at night, when the muons from dark matter annihilation come from the opposite direction to the background, from below the detector.

Moreover, to increase the signal-to-background ratio, one can place a cut on the inferred direction of the muons (not the original neutrino!) with respect to that of the Sun. This cut depends on the energy of the muon: at high energies, the direction of the muon and the neutrino are more similar than for low energy muons. The trade-off is that a more stringent cut on the direction gives a cleaner signal, but at the same time it removes information from the low energy muons. Nevertheless, there is always a remaining background signal that you need to model to see if the data are in excess of (which would be a detection of dark matter annihilation) or consistent with the background.

Results

From January 2007 to December 2008, the experiment took an effective total of 294.6 days of data. We reproduce here Figure 4 in the paper, where the main results are presented. This figure shows the distribution of separations between the inferred direction of the muon and the Sun. The number of muons coming from the direction of the Sun is consistent with the background expectation. There is no detection of dark matter annihilation in the Sun by ANTARES. In the next section, we explore what constraints can be placed on the properties and models of dark matter particles using these results. If you are brave enough, carry on reading!

Results of dark matter annihilation search by ANTARES

Distribution of incidence angles of inferred muon tracks with respect to the direction of the Sun. The solid blue line is the expected background and the black triangles are the data, with 1-sigma Poissonian error bars. Figure 4 from Adrián-Martinez et al. (2013).

 

For the brave at heart: Constraints on SUSY parameter space

What do these results tell us about the dark matter particle candidates? Different models for dark matter particles predict different production mechanisms for neutrinos. The Minimal Supersymmetry models (MSSM) considered in this work predict that the neutrino signature comes mostly from the decay of tau particles, W bosons or bottom quarks that are produced when the dark matter particles annihilate.

The measurements of the previous section allow the authors to place an upper limit on the neutrino flux from dark matter annihilation in the Sun. This is to say, if there were dark matter annihilation happening in the interior of the Sun, the neutrino flux from this process would have to be below a certain threshold to be consistent with the observations by ANTARES.

This information comes in handy. In the interior of the Sun, the rate of dark matter annihilation depends on the rate of capture of dark matter: you need to be capturing dark matter to have anything to annihilate. This is just an equilibrium argument, but a very useful one, since it allows us to set constraints on the cross-section of the interaction dark matter with nucleons in the Sun, most abundantly, protons. The cross-section has a spin-dependent (SD) and a spin-independent (SI) contribution, based on whether the interaction depends or not on the spin of the nucleon. We already have very stringent limits on the SI cross-section of the interactions by means of direct detection experiments. Neutrino telescopes are thus ideal for constraining SD WIMP-proton cross-sections. For a more technical explanation, see this paper.

In the left panels of Figure 6 (reproduced below), the ANTARES collaboration presents their bounds on the parameter space defined by the SD cross-section of the interaction and the WIMP mass. Overall, even if we have not had a detection of annihilating dark matter in the Sun, the constraints on the parameter space of SUSY models are getting tighter day by day.

90% confidence limits on the spin-dependent WIMP-proton cross section as a function of WIMP mass. Neutrino telescopes are able to place a more stringent constraint on this magnitude than direct detection experiments. The two panels correspond to different SUSY models. The grey areas are the parameter spaced allowed by the theory and the different lines correspond to different experiments. Figure 6, left panels, from ...

90% confidence limits on the spin-dependent WIMP-proton cross section as a function of WIMP mass. The two panels correspond to different SUSY models. The grey areas are the parameter spaced allowed by the theory. The results from ANTARES are shown in solid red, blue and green for the different annihilation channels. The other lines shown correspond to results from other experiments. Figure 6, left panels, from Adrián-Martinez et al. (2013).

 

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I am a 5th year graduate student in Astrophysics at Princeton University. My current research focuses on the intrinsic shapes and alignments of galaxies and galaxy clusters. Aside from cosmology, I love roller skating, tango and going to the art museum.

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Discussion

5 Responses to “The search for WIMP annihilation in the Sun”

  1. I’m confused. People have been studying solar neutrinos for decades. One can derive theoretically the flux of neutrinos produced by nuclear reactions in the sun. Famously, there was a big discrepancy between this theoretical prediction and the flux measured experimentally at e.g. the Homestead Mine. But my impression was that this issue had been more or less resolved by accounting for neutrino oscillations, right? And that subsequent experiments (like Super-K?) which were sensitive to more flavors of neutrinos were able to find them?

    Anyway, the point is that people have been studying this stuff for awhile. I’m confused because as far as I can understand from what you’re saying, it sounds like ANTARES is trying to constrain dark matter in the sun via constraining excess solar neutrino flux. But this doesn’t make any sense, because other experiments have already measured the solar neutrino flux pretty accurately — far more accurately than the 20 or so events that ANTARES has seen according to the graph above.

    So what am I missing? Is there some additional feature that distinguishes neutrinos of dark matter origin from those of nuclear origin? Something that ANTARES is sensitive to that detectors like Super Kamiokande are not?

    Posted by Tim Campion | March 8, 2013, 12:32 am
    • Sorry, that’s the Homestake Mine experiment, not “Homestead”.

      Posted by Tim Campion | March 8, 2013, 12:42 am
    • Great question! Indeed, several experiments have measured solar neutrinos coming from nuclear reactions in the Sun. In this paper, the authors are looking for another production mechanism. The annihilation of dark matter in the interior of the Sun could also produce neutrinos.

      How do you distinguish them from the solar neutrinos produced by fusion? The neutrinos produced by nuclear reactions in the Sun have lower energies (up to several MeV) than those produced by the annihilation of dark matter (above 10 GeV). In fact, the ANTARES experiment is not designed to detect low energy neutrinos from fusion in the Sun, it was built to detect high energy neutrinos coming from extragalactic sources or from dark matter annihilation. I hope this answers your question!

      Posted by Elisa Chisari | March 8, 2013, 11:17 am
  2. Ah! That does make much more sense. Thanks. Incidentally, why does the expected background in the graph above have zero events coming directly from the direction of the Sun? Is most that background coming from atmospheric muons?

    Posted by Tim Campion | March 8, 2013, 5:32 pm
    • Indeed, the dominant source of background are atmospheric muons. I think the blue curve is obtained from the observations themselves. My interpretation was that, since you take measurements when the Sun is below the horizon, you expect to have a larger background for directions that traverse a shorter distance through the Earth; on average, away from the direction of the Sun.

      Posted by Elisa Chisari | March 11, 2013, 9:47 pm

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