The XENON experiment is a 3500kg liquid xenon detector to search for the elusive Dark Matter. Have a look at the description of our detection principle, our recent publications, some pictures, or materials for press contacts. Feel free to contact us with your questions.
On Tuesday 20th of June, we presented our latest results on Electronic Recoil Modulations with 4 years of Xenon100 data at the PASCOS 2017 conference held in Madrid. After a short introduction, by M.L. Benabderrahmane, to the dark matter modulation as a signal, the main results have been presented, namely the test statistics of unbinned profile likelihood to search for the modulation period using three different sets of data. The first set contains the single scatter events in the energy range 2-5.8keV, the second set contains Multiple scatter events in the same energy range and the last one contains single scatters in the energy range 6-20keV. The last two samples are used as a sideband. The results of the likelihood gives a period of 431 days which is different from the one observed by the DAMA/LIBRA collaboration. Our single scatter modulation at 431 days has a global significance below 2sigma. The local test statistics for one year period gives a 1.8sigma. Similarity of the spectra between the two control samples and the signal sample disfavors the possibility for a modulation due to Dark Matter interaction.
ReStoX is an original cryogenic system designed for experiments that make use of high quantities of liquid xenon. It allows to store the total amount of xenon in gaseous, liquid or solid phase and to fill it into the detector vessel under high purity conditions. The system is crucial in case of emergencies that might require a fast recovering of the whole xenon present in the detector. ReStoX is currently being used by the XENON1T experiment and a future upgrade for XENONnT has already started.
The traditional approach for WIMP nucleus interaction studies in direct detection experiment is to consider just two types of interactions, the spin independent (SI) and the spin dependent (SD) ones. However, these are not the only types of interactions possible. In recent years, a non-relativistic effective field theory approach has been studied. In this framework, 14 new interaction operators arise. These operators include the SI and SD ones among others. Some of these new operators are momentum dependent and predict a non-exponential event rate as function of energy, in contrast to the traditional expected signals. Moreover, some of these operators predict energy recoils above the upper threshold of the standard analyses done in direct detection experiments. For XENON100, this threshold is 43keV (nuclear recoil).
In this analysis, we extend the upper energy threshold up to ~240 keV. This value is dictated by low statistics in calibration data above it. We divide our signal region into two regimes, low recoil energy, on which we perform the same “standard” analysis done for the SI and SD cases, and high recoil energy, which is the main focus of this work.
We find that our data is compatible with background expectations. Using a binned profile likelihood, we thus produce 90% CL exclusion limits for both elastic scattering and inelastic WIMP scattering for each operator. Find the preprint of this study on the arxiv.
On Tuesday, May 30, we presented the first XENON1T results in a seminar at LNGS, the laboratory where our experiment is hosted. The seminar was presented by Marco Selvi (INFN Bologna) in the Fermi room, the main auditorium at LNGS, and introduced by the LNGS director prof. Stefano Ragazzi in front of about 40 scientists.
After a short introduction on Dark Matter (you may guess that at LNGS they are well aware of the details of this physics puzzle! ), we described the construction and commissioning phase of the various systems crucial to run our detector.
We then focused mainly on the performances of XENON1T in the first science run,
where we reached the lowest ER background ever achieved in a dark matter experiment.
Also our sensitivity is very good, being it also the best out of the various direct search dark matter experiment, even with just 34 days of data acquisition.
With our result, XENON1T (and LNGS with) is back at the frontline of the race to finally detect dark matter particles … we look forward to analyse the already acquired >70 days of data !
[Press Release May 2017 – for immediate release. Preprint is on the arxiv]
“The best result on dark matter so far! … and we just got started!”.
This is how scientists behind XENON1T, now the most sensitive dark matter experiment world-wide, hosted in the INFN Laboratori Nazionali del Gran Sasso, Italy, commented on their first result from a short 30-day run presented today to the scientific community.
Dark matter is one of the basic constituents of the Universe, five times more abundant than ordinary matter. Several astronomical measurements have corroborated the existence of dark matter, leading to a world-wide effort to observe directly dark matter particle interactions with ordinary matter in extremely sensitive detectors, which would confirm its existence and shed light on its properties. However, these interactions are so feeble that they have escaped direct detection up to this point, forcing scientists to build detectors that are more and more sensitive. The XENON Collaboration, that with the XENON100 detector led the field for years in the past, is now back on the frontline with the XENON1T experiment. The result from a first short 30-day run shows that this detector has a new record low radioactivity level, many orders of magnitude below surrounding materials on Earth. With a total mass of about 3200kg, XENON1T is at the same time the largest detector of this type ever built. The combination of significantly increased size with much lower background implies an excellent dark matter discovery potential in the years to come.
The XENON Collaboration consists of 135 researchers from the US, Germany, Italy, Switzerland, Portugal, France, the Netherlands, Israel, Sweden and the United Arab Emirates. The latest detector of the XENON family has been in science operation at the LNGS underground laboratory since autumn 2016. The only things you see when visiting the underground experimental site now are a gigantic cylindrical metal tank, filled with ultra-pure water to shield the detector at his center, and a three-story-tall, transparent building crowded with equipment to keep the detector running, with physicists from all over the world. The XENON1T central detector, a so-called Liquid Xenon Time Projection Chamber (LXeTPC), is not visible. It sits within a cryostat in the middle of the water tank, fully submersed, in order to shield it as much as possible from natural radioactivity in the cavern. The cryostat allows keeping the xenon at a temperature of -95°C without freezing the surrounding water. The mountain above the laboratory further shields the detector, preventing it to be perturbed by cosmic rays. But shielding from the outer world is not enough since all materials on Earth contain tiny traces of natural radioactivity. Thus extreme care was taken to find, select and process the materials making up the detector to achieve the lowest possible radioactive content. Laura Baudis, professor at the University of Zürich and professor Manfred Lindner from the Max-Planck-Institute for Nuclear Physics in Heidelberg emphasize that this allowed XENON1T to achieve record “silence”, which is necessary to listen with a larger detector much better for the very weak voice of dark matter.
A particle interaction in liquid xenon leads to tiny flashes of light. This is what the XENON scientists are recording and studying to infer the position and the energy of the interacting particle and whether it might be dark matter or not. The spatial information allows to select interactions occurring in the central 1 ton core of the detector. The surrounding xenon further shields the core xenon target from all materials which already have tiny surviving radioactive contaminants. Despite the shortness of the 30-day science run the sensitivity of XENON1T has already overcome that of any other experiment in the field, probing un-explored dark matter territory. “WIMPs did not show up in this first search with XENON1T, but we also did not expect them so soon!” says Elena Aprile, Professor at Columbia University and spokesperson of the project. “The best news is that the experiment continues to accumulate excellent data which will allow us to test quite soon the WIMP hypothesis in a region of mass and cross-section with normal atoms as never before. A new phase in the race to detect dark matter with ultra-low background massive detectors on Earth has just began with XENON1T. We are proud to be at the forefront of the race with this amazing detector, the first of its kind.”
As always, feel free to contact the XENON collaboration at firstname.lastname@example.org.
To attain the high sensitivity needed to detect a dark matter particle with a xenon time-projection chamber, all other sources of particle interactions need to be eliminated or minimized. These interactions are classified as background events. Radiogenic backgrounds, in particular, come from radioactive isotopes within the detector materials that decay and lead to alpha, beta, or gamma emissions. Neutrons from spontaneous fission of heavy isotopes or from secondary reactions within the detector materials also contribute to the radiogenic background and can mimic a dark matter signal.
To minimize the radiogenic background, the goal of the XENON1T radioassay program is to measure the radioactivity of all materials that are needed to build the detector and to select only the most radiopure materials for the final construction. To do this, we use mass spectrometry techniques and high-purity germanium spectrometers that are capable of measuring radioactivity at the level of 10-6 decays per second in a kilogram of material (Bq/kg). As comparison, a typical banana has an activity of ~102 Bq/kg!
Because natural radioactivity is present in the soil, the water, and in the air, it is also present in the XENON detector materials. The Figure shows a measurement obtained with a germanium spectrometer of the gamma rays emitted from a sample of photomultiplier tubes. The background (purple spectrum) is subtracted from the sample (pink spectrum) in order to quantify the expected activity from a XENON1T component or material sample.
The most common radioactive isotopes present in the Earth are primordial uranium and thorium, each of which decays into a series of other radioactive isotopes (marked in green in the Figure). Potassium (red) is also a common, primordial isotope that is found in soil, and subsequently in food and in your body. Other isotopes that are found in detector materials come from interactions with cosmic rays (yellow) or from man-made activities (blue), i.e. industrial or medical use, nuclear power plant emissions, nuclear accidents, and military testing.
The measured activities of each material selected for detector construction are used in simulations of XENON1T to determine the expected background. This allows for a prediction of the attainable sensitivity of the detector to dark matter interactions. The radioassay measurement results from over 100 material samples are presented in our new paper “Material radioassay and selection for the XENON1T dark matter experiment”.
With 2 tonnes of target material, XENON1T is currently the largest liquid xenon detector in the search for dark matter. The detector’s immense volume greatly increases our chances of successfully observing that rare scatter of a dark matter particle off a xenon atom that we have sought for more than a decade, like casting a larger net to catch more fish. However, the size also makes it considerably more difficult for us to know how our detector would respond to the scatters of dark matter or to the scatters of electrons or gamma rays that would obscure our view of dark matter. These electrons and gammas come from ambient radon, impurities in the xenon, and even the detector components themselves. While their effects can be reduced through an appropriate selection of location and the materials, they cannot be completely eliminated. Hence, it is necessary to understand how our detector responds to electrons and gammas in contrast to dark matter. A thorough understanding of these backgrounds is arguably the single most crucial part of our endeavor.
Historically, in XENON10 and XENON100, we used external radioactive sources of cobalt and thorium, which emit gammas. Unfortunately, a drawback of XENON1T’s size is that it hobbles the rate of interactions in the central region of the detector, which is the most important for us in understanding our detector. For this reason, we needed to identify an internal, or dissolved, radioactive source that can be injected directly into the detector’s liquid xenon target volume.
One possibility is a source of 220Rn, which we characterize using the XENON100 detector. The source is well suited to calibrate our detector because it can imitate the effects of ambient radon (222Rn). The radioactive decay of 212Pb (a daughter of 220Rn) generates an electron just like 214Pb (a daughter of 222Rn), and thus their responses are very similar. The only thing we have to verify is that we can spread the 212Pb atoms throughout the detector volume. Due to the particular design of XENON100, many gamma events from other 220Rn daughters prevent us from identifying which events arise from 212Pb. So, we use the distribution of 212Bi, the daughter of 212Pb, to clearly show that 212Pb reaches even the centermost part of the detector. This distribution is shown in the figure below. Once that calibration is done, we do not have to proactively clean our detector, as would be the case with alternatives. Since the half-life of 212Pb is about half a day, we just wait a few days for the detector to return to normal.
The source also provides alpha particles that prove useful in understanding our background. The alpha particles of 216Po and 220Rn enable us to easily pinpoint their locations at the time of decay. And because they happen in quick succession (about 0.1 seconds), the daughter 216Po can be paired with its parent 220Rn. These pairs show us the trajectory of 216Po in the liquid xenon and how long it takes to decay. With both the time and the displacement, we can calculate the average velocity of the 216Po atom. If we then determine the velocities of all identified RnPo pairs, we can create a map of atomic motion in the full xenon volume of a given detector, as shown here:
In the case of XENON100, we find that atoms move at speeds up to 8 mm/s. They move in a single convection cell with a small contribution that results from an electric field applied to the xenon volume. This aspect tells us that an appreciable fraction of 216Po atoms is left ionized after the decay of 220Rn.
In general, a known map of atomic motion motivates two additional techniques to help us understand the backgrounds. Firstly, such a map enables us to identify the presence of “dead regions” through which liquid xenon does not flow very well. This feature is important for keeping the xenon free of impurities. Secondly, with sufficiently slow atomic motion or sufficiently large detector volumes, we could match 214Pb to its parent 222Rn or 218Po following a method similar to the one described previously for 220Rn. This tagging process would clearly distinguish 214Pb background events from the coveted dark matter event.
All of the finer details about this dissolved radon source can be found in the dedicated publication in Phys. Rev. D: E. Aprile et al. (XENON), Results from a calibration of XENON100 using a source of dissolved radon-220, Phys. Rev. D 95, 072008 (2017). This publication is of course also available as a pre-print as arXiv:1611.03585.
Search for magnetic inelastic dark matter with XENON100
There is the long-standing claim of the DAMA/LIBRA collaboration about a detection of dark matter via the highly significant observation of an annually modulating signal in radiopure sodium iodide crystals. This signal, however, is in conflict with exclusion limits from various other dark matter experiments, including XENON100. Several alternatives to the classical WIMP scenario have thus been proposed in order to reconcile these null results with DAMA/LIBRA. One of these models is magnetic inelastic dark matter (MiDM). The MiDM model is motivated by comparing certain properties of the different detector targets and how they possibly influence the expected event rates. Iodine, used in DAMA/LIBRA, is distinguished by its high atomic mass and high nuclear magnetic moment. This enhances the signal of MiDM compared to other targets, such as xenon, and opens up new parameter space for the DAMA/LIBRA signal that is not in conflict with other null results.
In the framework of MiDM the dark matter particle is expected to scatter inelastically off the nucleus, thereby gets excited, and de-excites after a lifetime of the order of order μs with the emission of a photon with an energy of δ~100 keV. Given the mean velocity of the dark matter particle, it travels a distance of O(m) before it de-excites. Furthermore it is assumed that the dark matter particle has a non-zero magnetic moment, μχ. The combination of a low-energy nuclear recoil followed by an electronic recoil from the de-excitation creates a unique delayed coincidence signature which has been searched for the first time using the XENON100 science run II dataset with a total exposure of 10.8 ton × days. No MiDM candidate event has been found, thus we calculate an upper limit on the interaction strength. The Figure shows the resulting limit for a dark matter mass of 123 GeV/c2 which completely excludes the DAMA/LIBRA modulation signal as being due to MiDM.The sensitivity of this type of analysis will be greatly improved for current ton-scale (e.g., XENON1T) and future multi-ton dual-phase LXe TPCs (e.g., XENONnT, LZ and DARWIN). This is not only due to the increased target mass, but also thanks to the higher probability of detecting the de-excitation inside the larger active volume.