Electronic transitions of valence electrons in atoms have typical energies of a few eV, whereas nuclear processes occur on the keV to MeV scale. This large gap in energy scales reflects in the fact that the realms of atomic and nuclear physics barely overlap, but there are a few exceptions.

One such exception is encountered in the nucleus of the isotope 229Th. This unique nucleus is believed to possess an extremely low-lying and long-lived excited state at an energy of a few eV, a property not found in any other known isotope1,2,3,4. While direct evidence of the existence of this isomeric state is still pending5,6,7 and its energy has only been determined with large uncertainty, the fascinating possibility to manipulate nuclei by laser light has spurred a wealth of proposals for various applications.

The most prominent application of the 229Th isomer transition might be an optical clock based on this transition8,9. This clock could feature a quality factor of Q = ν/Δν ≈ 1019, potentially outperforming today’s best optical clocks10. While such a clock might be highly immune to external perturbations, it would be very sensitive to variations of the fine-structure constant α and QCD parameters11,12,13, constituting an exquisite probe of possible drifts in fundamental constants. In further quantum optics applications, the isomeric state has been proposed as a primer for the field of nuclear quantum optics14,15 and as a robust qubit for quantum information16. More generally, the unique case of 229Th might be the pioneer of gamma-ray lasers17. The prerequisite for all of these experiments is an unambiguous proof of the existence of the isomeric state, a measurement of its energy and a demonstration of its optical addressability.

So far, most studies on 229Th employed high-resolution gamma spectroscopy1,2,3,4. Differencing schemes were used to indirectly determine the energy of the isomeric state. The latest measurement places the excitation energy at 7.8(5) eV, corresponding to a wavelength of 159(10) nm in the vacuum-ultra-violet (VUV) range4,18. Systematic errors of this measurement might be underestimated19. Additional evidence for the existence of an isomeric state has been obtained from collision experiments20.

A number of experiments were performed to observe the VUV-photon emitted during the decay of the isomeric state. These measurements generated either false results21,22 that were soon refuted23,24, or null6,7,25,26 results. The lifetime of the isomeric state is expected to be on the order of 1,000 s3,27,28. Two experiments set out to measure the isomer lifetime via alpha spectroscopy29 and through gamma decay30, but found no signal. A recent experiment claims observation of the VUV photon with an isomer lifetime of 6(1) hours5, but is highly disputed31.

There exist a large number of strategies to populate the isomeric state. So-called “indirect” pathways include the alpha decay 233U → 229mTh5,32, excitation via higher-lying nuclear states (e.g. at 29.19 keV)33, electron bridge processes34 and light-ion fusion reactions35. Direct optical excitation of the isomeric state via a photon with the correct wavelength has not yet been successful, nor has the wavelength of the transition been determined with sufficient precision to commence spectroscopy with narrow-linewidth lasers. Spectroscopy with synchrotron radiation may fill this apparent gap6.

Optical spectroscopy of the 229Th isomeric transition requires a platform to securely hold the nucleus for a sufficiently long time in a recoil-free environment. Radiation with a wavelength shorter than 196 nm ionizes the neutral Th atom (first ionization energy 6.32 eV), experiments should therefore employ positively charged Th ions for spectroscopy in the VUV. The extreme scarcity of the isotope 229Th, related to its half-life of τ = 7932 a36 and the minuscule cross section for optical excitation37 place further demands on the spectroscopy scheme. Two platforms have been proposed as hosts of 229Th ions: ion traps8,38,39 and VUV-transparent crystals8,40.

CaF2 is a promising candidate for such a host crystal37,41. Its fairly simple lattice has a band-gap of about 12 eV, which ensures optical transparency down to 120 nm. CaF2 readily accepts thorium as a dopant. Lattice structure calculations show that Th4+ ions replace Ca2+ ions, where the additional charges are compensated for by flourine interstitials42; see Fig. 1(b). Doping with Th may reduce the band-gap of CaF2 by a few percent42, but Th:CaF2 crystals with doping concentration below 10−4 remain transparent down to 125 nm. Broadening mechanisms caused by the lattice environment37 might limit the ultimate performance of clock operation with this platform, but the ability to place more than 1015 nuclei into a volume of 1 cm3 is a tremendous advantage for the initial optical search for the transition. This solid state approach thus enables optical Mössbauer spectroscopy and provides a very simple, robust and secure way to store the 229Th nuclei. Figure 1(a) summarizes the relevant properties of the isomer transition.

Figure 1
figure 1

(a) The nuclear two-level system in 229Th. (b) Lattice structure of Th:CaF2, where a Th4+ ion replaces a Ca2+ ion and the additional charge is compensated for by two F interstitials at 90° angle. (c) Experimental set-up: a spectrometer is used to measure the crystal’s luminescence spectrum. A deuterium lamp serves for both the excitation of the crystal and the calibration of the spectrometer. The instrumental resolution is about 1 nm. A manual actuator allows one to place different probes into the central region.

The long lifetime of the isomeric state can only be exploited if radiative M1 decay into the nuclear ground state is the dominant pathway of decay. Thus, competing pathways such as fast non-radiative relaxation and internal conversion need to be suppressed33,41. This requires the 229Th nucleus to be located at a well-defined lattice site, as the introduction of severe lattice defects in the vicinity of the Th nucleus would reduce the bandgap and lead to increased off-resonant de-excitation. The actual microscopic environment of Th ions in the crystal is still to be explored.

Pure CaF2 is widely used for UV optics and numerous studies have investigated scintillation properties in response to irradiation with hard X-rays, as well as resilience against intense pulsed VUV light (e.g. in Refs. 43, 44, 45). These studies only covered parameter regimes far away from the one relevant for the work presented here.

In this paper, we study the suitability of 229Th:CaF2 crystals for optical spectroscopy of the 229Th nuclear transition. We suspect that the nuclear signal might be masked by two types of background: VUV-photoluminescence of the crystal, caused by the interrogation light and radioluminescence, caused by radioactive decay of 229Th. We employ VUV light to induce photoluminescence and take advantage of the radioactivity of thorium nuclei doped into the crystal as an intrinsic source of radioluminescence. A spectrometer with nm-resolution is used to measure the emission spectrum of both kinds of luminescence. In time-resolved studies, we use photo-multiplier tubes (PMTs) to measure the duration of crystal scintillation. Details of the experimental set-up are given in the Methods Section.


Optical spectrum

We begin our studies by an investigation of the VUV-light induced luminescence. A deuterium lamp (peak emission around 160 nm) is used to simulate a synchrotron or a future tunable and narrow-band spectroscopy light source. A home-grown 232Th:CaF2 crystal is illuminated for 1 s and subsequently exposed to a CCD camera via a spectrometer for one second; see Fig. 1(c). This alternating cycle of crystal illumination and detection is repeated for an hour to improve the signal-to-noise (S/N) ratio. The measured spectrum shows distinct peaks between 260 and 500 nm, interpreted as self-trapped exciton (STE) emission, but no discernable features below 260 nm; see Fig. 2(a).

Figure 2
figure 2

VUV-photoluminescence of CaF2.

(a) The spectrum shows characteristic lines between 260 and 500 nm. The data below 250 nm is magnified by a factor of 1,000 to demonstrate the absence of crystal emission in this region. (b) Zoom into the self-trapped exciton (STE) feature, where the data (black dots) is fitted by nine Gaussian peaks of variable position, amplitude and width (colored lines). The positions of the Gaussian peaks, expressed in units of eV, are plotted in the inset. The instrumental resolution is 0.5 nm. (c, d) Time-dependent decay of the VUV-light induced luminescence, measured separately for timescales up to 100 s (c) and up to 20 hours (d). The data is fit by a double-exponential decay for short wait times and by a power law for longer times.

The STE spectrum consists of nine overlapping lines, which can be approximated by Gaussian functions. In the inset of Fig. 2(b), we plot the positions of the lines, where the wavelength λ has been converted into photon energy via E = hc/λ. The dependence of photon energy on peak number is almost linear, suggesting that each line represents an oscillator state in the harmonic STE potential. The width of the lines is between 5 and 10 nm (substantially larger than the instrumental resolution) and decreases linearly with increasing energy.

The positions of the lines are independent of crystal temperature, wait time after illumination, light intensity and emission spectrum of the deuterium lamp. Their relative amplitudes, however, do change with wait time after illumination and spectrum of the excitation source. Notably, we varied the illumination/exposure time between 250 ms and 10 hours and found only little change to the overall shape of the spectrum.

We do observe a weak temperature dependence of the emission strength. Between 20 and 110 °C, the emission increases by about 60% in a near-linear fashion, but the relative amplitudes of the individual lines are unchanged.

It should be noted that STEs are a well-known type of excitation in rare-earth halides45. The VUV light might not excite the STEs directly, but may induce various kinds of other crystal excitations, which quickly relax into STEs. The magnitude of the excitonic luminescence appears to depend on the purity of the crystal and therefore on the details of the crystal growing process. For our home-grown crystals, the amplitude of luminescence emission varies by about a factor of five within a large set of home-grown specimens, irrespective of the doping concentration. We probe various commercial CaF2 crystals (Hellma/Schott Lithotec and Korth) and find their VUV-photoluminescence to be a factor of at least 104 smaller than for our home-grown crystals. A 232Th:CaF2 crystal (doping concentration 2 × 10−4) produced by the Institut für Kristallzüchtung (IKZ, Berlin, Germany) using the Czochralski method shows negligible luminescence. We thus conclude that the emission amplitude depends only on the quality of the CaF2 production process, with no discernable influence of the thorium doping concentration.

An absolute quantification of the crystal’s photoluminescence in response to prior illumination with a well-defined light source is beyond the scope of this paper. We estimate that our home-grown CaF2 crystals (thickness 10 mm, diameter 17 mm), illuminated by a deuterium lamp with 200 mW optical power for 30 minutes, radiate 108 photons/s one minute after the end of illumination.


The decay of luminescence in CaF2 on ns- and μs-timescales has already been studied extensively43. In future spectroscopy and optical clock experiments, however, mechanical shutters have to be opened and closed in between crystal illumination and fluorescence measurement, introducing a delay of about 10 ms. Consequently, we limit our studies to timescales longer than 10 ms.

An excimer laser at 157 nm is used to illuminate the crystal for one minute and the subsequent luminescence detection is performed with a Cs-Te PMT (sensitivity range 115 and 320 nm; see Methods section). For detection times below one minute, we find a double-exponential decay with time constants τ1 = 450 ms and τ2 = 23 s; see Fig. 2(c). These values change slightly with varying experimental parameters, but the significant difference in timescales prevails. The amplitude of the faster decay is at least 10-times larger compared to the slower branch. For times in excess of one minute, we observe the familiar power-law decay of luminescence46,47. This decay that can be traced for times as long as a full day; see Fig. 2(d). We fit the data by I(t)/I0 = c + tk, where c is an offset related to radioluminescence and obtain an exponent k = 0.75(2) at room temperature.

To conclude, we find that the STE spectrum in CaF2 has an abrupt lower edge at 260 nm and we observe no emission in the relevant spectral region around 160 nm. Choosing PMTs with Cs-I (sensitive between 115 and 190 nm) or diamond photocathodes (115 to 220 nm) ensures maximum detection efficiency in the desired wavelength range and suppresses the luminescence background by at least three orders of magnitude. In addition, a vast fraction of the luminescence decays on timescales much shorter than the expected isomer lifetime. These findings suggest that both temporal and spectral filtering can be used to discriminate the nuclear spectroscopy signal from crystal luminescence.


The alpha decay of 229Th in the crystal is a violent process: the alpha particle and the remnant 225Ra nucleus obtain kinetic energies of 5.1 MeV and 90 keV, respectively. These fragments travel through the crystal lattice structure with ranges of about 30,000 and 30 lattice constants, respectively, leaving behind a track of defects. From an energy point of view, each alpha decay releases enough energy to create 106 photons. While most of the released kinetic energy Qα is eventually converted into phonons, some of the defects relax via emission of photons, known as scintillation. As we will show later, each alpha decay in CaF2 generates 1.0(2) × 104 photons in the UV range. In addition, all the daughter products of 229Th down to 209Bi are short-lived (half-lives between 3.7 μs and 15 days), such that each 229Th decay is followed by a chain of four alpha and three beta decays.

Radioluminescence thus poses a considerable background for both the initial search for the isomeric transition, as well as future operation of an optical clock, where the background inevitably scales linearly with the nuclear isomer signal. In the following, we will characterize the radioluminescence with respect to its spectrum and its dependence on time and temperature.

Optical spectrum

We place a 229Th:CaF2 crystal (thickness 20 mm, doping concentration 1.6 × 10−8, activity 5 kBq) into the spectrometer and integrate the emission spectrum for 100 hours. The radioluminescence spectrum is shown in Fig. 3(a); spectra obtained with highly-doped 232Th:CaF2 crystals are identical. Importantly, no emission is observed for wavelengths below 220 nm. These spectra show pronounced emission between 230 and 400 nm and differ significantly from the ones induced by VUV light. The crystal was heated to 300 °C prior to the measurement to remove emission related to thermoluminescence, which will be investigated later.

Figure 3
figure 3

Radioluminescence spectra of 229Th:CaF2 crystals.

(a) Spectrum of “prompt” scintillation (black line), compared to a scaled photoluminescence spectrum (gray line). The instrumental resolution is 15 nm. (b) Thermoluminescence spectrum, obtained while heating the crystal to 150 °C (black line). The heating anneals semi-permanent defects under emission of a spectrum comprised of individual peaks with positions identical to those observed in photoluminescence (gray line). The resolution here is 1.5 nm.


We use a Cs-Te PMT (sensitivity range 115 to 320 nm) to record the emission of a 229Th:CaF2 crystal (activity 1 kBq, temperature 20 °C) at the single-photon level. The bin width is set to 100 μs, a factor of 10 shorter than the average time difference between two successive alpha events. The total detection efficiency is about 2.5%. A typical histogram of counts per bin, using 5 minutes of integration, is shown in Fig. 4(a).

Figure 4
figure 4

Bursts of radioluminescence induced by alpha decay.

(a) Single photons emitted by a 229Th:CaF2 crystal are detected by a PMT and counted in bins of 100 μs width. The histogram shows a summation of 3 × 106 bins, the numbers label relevant features discussed in the text. A section of the data is also plotted on a linear scale (inset). (b) Similar measurement for a 232Th-doped crystal. The feature labelled “B” points to a 229Th contamination of the crystal; see the text for details. The dashed red lines in the inset are Gaussian fits to the three center peaks.

We observe five clearly distinguishable features. The vast majority of bins contain zero or very few counts, forming the Poissonian distribution labelled “1” in Fig. 4(a). Strikingly, about 13% of all bins make up feature 3I, each containing about 200 counts. We interpret this feature as a flash of photons, released in succession of an alpha decay inside the crystal, with a duration much shorter than 100 μs. The rate of such events matches the 229Th activity inferred by neutron activation analysis and gamma spectroscopy. Consequently, bins containing two and three of such events constitute features 3II and 3III in the figure. Feature 2 is a signature of the beta decay of 229Th daughters and possibly contaminations in the crystal.

The progenies of 229Th are short-lived, such that the entire decay chain is in equilibrium and one would expect the radioactive decays of all progenies to appear as individual features. Surprisingly, we do observe the beta decay of daughters (e.g. 225Ra), but not the alpha decay of further progenies. The reason for the absence of these features is not known.

Next, we sandwich the crystal in between two identical PMTs. We observe the appearance of “bursts” always in coincidence on both detectors, again supporting the hypothesis that such flashes are related to alpha decay in the crystal. We calculate that each decay gives birth to 1.0(2) × 104 photons, thus about 1% of Qα is radiated via photons.

We then exchange the 229Th:CaF2 crystal for a 232Th:CaF2 specimen. The doping concentration of 0.8% is nearly 6 orders of magnitude higher to account for the long half-life of 232Th (τ = 1.4 × 1010 a). We use a longer binning time of 500 μs; the obtained histogram is shown in Fig. 4(b). The fact that the main peak has shifted to a lower value of counts is explained by the reduced optical transmission properties of this specific crystal. The upshift of feature 2 can be explained as a signature of the beta decay of 228Ac in the 232Th decay chain: a comparably large amount of kinetic energy is released in this decay ( MeV). Interestingly, two separate peaks A and B are clearly visible and we speculate that they correspond to two types of alpha decay with different values of Qα. Fitting simple Gaussian distributions to the dominant peaks (dashed red lines in the inset of Fig. 4(b)), we obtain a difference in released photon number of 27.8(6)% between peaks A and B. Following the Geiger-Nuttall law, we assign feature A (lower Qα) to the very long-lived 232Th isotope. The 229Th value of Qα is 26.6% larger compared to 232Th48, very close to the difference in observed photon numbers. We thus identify feature B with a crystal contamination of 229Th at a level of 0.8(1) ppm relative to the 232Th content.

We repeat the same experiment with the 232Th:CaF2 specimen (doping concentration 2 × 10−4) produced at IKZ. This crystal shows the very same radioluminescence spectrum as our home-grown 232Th:CaF2. Taking a histogram equivalent to the one shown in Fig. 4(b), we recover the same feature labelled “A”. Note that the IKZ crystal showed negligible signs of photoluminescence. This lets us to believe that the observed radioluminescence is a generic scintillation feature of CaF2 and does not depend on the details of the crystal growing process.

We found that the characteristic “flashes” are substantially shorter than 100 μs. To measure their duration more precisely, we reduce the detector bin width to 250 ns and record the emission of a 229Th-doped crystal. We find that each flash lasts on the order of 1 μs, the average time interval between flashes being about 1 ms. From the PMT’s time trace, we extract sequences that contain about 200 counts within a few μs, thus fall into the prominent peak 3I in Fig. 4(a). To reduce the shot noise, we average over 100 of such flashes, where the first non-zero bin is taken as the onset of the flash. Typical time evolution curves are shown in Fig. 5(a).

Figure 5
figure 5

Temperature dependence of radioluminescence in 229Th:CaF2.

(a) Time evolution of a burst of photons initiated by an alpha decay, shown for two different temperatures. An exponential decay (red line) is fit to the tail of the distribution; the dotted line connects data points (black dots) to guide to the eye. (b) The duration of a burst depends on temperature, quantified here by the full width at half maximum (FWHM) and the decay time τ of the burst. (c) The integrated photon emission changes by a factor of 10 between 20 and 100 °C.

In view of the coarse timing resolution, as well as the lack of a profound model to explain the time evolution, we will restrict ourselves to a semi-quantitative analysis. A simple exponential decay fits the tail of the curve surprisingly well, yielding a value of 1.6(1) μs for a crystal at room temperature. The FWHM of the distribution gives a similar value, 2.3(1) μs. Substituting 229Th by 232Th in the crystal returns the same result. Changes to key parameters of the PMT set-up, such as the hold-off time and absolute count rate, evoke only mild changes. Note that even for the highest count rates of about 50 MHz during a flash, the average interval between counts is still larger than the PMT’s signal width (2 ns) and the typical holdoff-time (5 ns).

The near-unit efficiency in detecting alpha decays in the crystal can be turned into a powerful tool to reduce the radioluminescence background of 229Th nuclear spectroscopy measurements. A primary PMT, most sensitive around 160 nm, would be used to detect the sought-after emission of the isomeric state. This PMT would have a non-negligible relative sensitivity of 10−3 for radioluminescence photons. An ancilla PMT, sensitive around 300 nm, would be used to detect alpha decays with high efficiency, thus recording the time stamp of every event. When post-processing of the data, any signal registered by the primary PMT during a μs time window around the alpha event would be excluded. The same could be performed already on-line with a suitable gating scheme.


As a next step, we measure the duration of the flashes at different crystal temperatures; see Fig. 5(b). Between 0 and 70 °C, the two extracted measures of the flash duration decrease by a factor of about 4 in a near-linear fashion. This speed-up is identical for 229Th- and 232Th-doped crystals.

Not only the duration of each flash, but also the number of contained photons is strongly temperature-dependent: the ratio of radiative to non-radiative relaxation of STE defects changes drastically around room temperature45. Recording histograms as in Fig. 4, we find that the prominent peak shifts towards fewer counts for increased temperature: for every alpha decay, fewer photons are emitted. More quantitatively, we measure the total emission of a crystal by integrating over time intervals of 10 s, thereby detecting not only prompt emission following alpha decays, but also relaxation of long-lived defects and beta decays. Such a curve, taken with a Cs-Te PMT right after annealing a 229Th:CaF2 crystal at 300 °C, is shown in Fig. 5(c). Between 30 and 100 °C, the photon emission decreases exponentially with temperature, dividing in half every 24 K. The apparent increase above 110 °C is caused by black-body radiation emitted by the crystal heater.

We perform the same measurement using a PMT with a diamond photocathode, for which the spectral sensitivity has a plateau up to 170 nm and gradually decreases towards higher wavelengths. The signal amplitude is drastically reduced by a factor of 80, yet we find the same temperature dependence. This indicates that Cherenkov radiation between 115 and 220 nm, which we do not assume to be temperature-dependent, comprises less than 1% of the photons emitted as a result of radioactivity. This agrees with the spectrum shown in Fig. 3, where negligible Cherenkov radiation was observed.

This finding is again important for future 229Th spectroscopy measurements: Mild heating of the crystal to around 100 °C reduces its radioluminescence by a factor of 10 compared to its room temperature value. In addition, the duration of characteristic flashes decreases dramatically, which in turn reduces the veto time imposed onto the primary detector to reject unwanted counts during radioluminescence flashes.


Ionizing radiation can create semi-permanent defects in doped CaF2, exhibiting lifetimes of several weeks or months. Such excitations, often related to contaminations or crystal defects, can be healed by heating of the crystal, allowing excited electrons to leave their traps and relax into the ground state by photon emission. This behavior is widely used in thermoluminescent dosimeters (TLDs) based on CaF2.

We allow a 229Th:CaF2 crystal to accumulate long-lived defects for many weeks. Heating the crystal to 150 °C frees an enormous amount of photons. The spectrum, shown in Fig. 3(b), is markedly different from the one obtained with “prompt” photons. We observe a series of overlapping lines, where the positions of the individual lines (but not their relative amplitudes) coincide perfectly with the photoluminescence spectrum.

Next, we use the single photon counting capability of PMTs to access the absolute amount of photons radiated upon heating. Measuring an ordinary glow curve, we estimate that for each alpha decay, a few 104 semi-permanent defects are created in the crystal. These defects have a lifetime of months and slowly relax under emission of single uncorrelated photons. These photons (and not the PMT dark counts) are the origin for the features labelled “1” in Fig. 4. Thus, for every alpha event, there are more semi-permanent defects created than prompt photons released.

These “delayed” photons pose an unpleasant background to nuclear spectroscopy measurements, as they cannot be excluded by a veto in the time domain. Instead, periodic annealing of the crystal, e.g. once a day, has proven to reduce the emission of uncorrelated photons by a factor approaching 100 compared to a crystal stored dark and cold for months. After annealing, the emission increases with an initial rate of 0.27(1) %/day at room temperature. Note also that the onset of the delayed-photon spectrum appears about 40 nm towards longer wavelengths compared to the prompt-photon spectrum. This allows for more convenient spectral filtering with respect to the sought-after nuclear emission around 160 nm.


We have measured the photoluminescence spectrum of CaF2 upon irradiation with VUV light and, for the first time, resolved the substructure of the prominent STE feature. Spectral filtering will allow to remove the luminescence background, which extends down to 260 nm, from the nuclear isomer signal expected around 160 nm.

We have developed a consistent understanding of the radioluminescence emission, which comprises two components: intense flashes of μs duration following a radioactive decay in the crystal, as well as a constant background of single uncorrelated photons emitted by very long-lived crystal defects. The spectra of these two components are strikingly different with lower cut-offs at 220 and 260 nm, respectively. The number of “prompt” photons can be reduced by a factor of 10 through a mild temperature increase. Additionally, an auxiliary detector, sensitive around 300 nm, can be used to identify such events and thus provide the gating of a primary detector with peak sensitivity at the expected nuclear signal. The background of “delayed” photons can be removed almost entirely by periodic heating of the crystal.

These findings can be used to optimize the protocol of future searches for the nuclear VUV photon using synchrotron radiation and guide the selection of suitable photodetectors and optical filters.

Future work will include an absolute photoluminescence measurement using well-defined synchrotron radiation. Understanding the reason for the large photoluminescence level in our home-grown crystals will allow us to improve the crystal growing process in this regard. Considering MgF2 as a viable alternative to CaF2, we will assess the doping efficiency of Th into MgF2.


CaF2 crystals

We operate an in-house furnace to grow CaF2 single crystals by means of the vertical gradient freeze technique. The crystals have a volume of 7 cm3 and are cut and polished to disks of typically 5 mm thickness. For the studies presented here, we employ pure CaF2 crystals, 232Th:CaF2 crystals and 229Th:CaF2 crystals. The isotope 232Th (half-life τ = 1.4 × 1010 a) is readily available and chemically identical to 229Th and can therefore be used as a proxy. The doping concentration (fraction of Ca2+ ions replaced) can be varied from 10−8 to values as high as 1%. The limited availability of the isotope 229Th restricts the concentration in our crystals to 1.6 × 10−8, corresponding to a density of 4 × 1014 cm−3. As a result of the chemical processing of 229Th, the 229Th:CaF2 crystals also contain 232Th at a concentration of 10−4.

Pure CaF2 is commonly used for UV optics, therefore some of its scintillation properties have already been studied. Such studies found that self-trapped excitons (STEs) are the dominant type of excitation created by various kinds of radiation43,44,45. Any form of ionizing radiation absorbed by the crystal will create highly energetic electron-hole pairs, which quickly thermalize to form a myriad of various excitations with energies below the band gap. These may transfer their energy to various kinds of luminescence centers, which eventually decay under emission of photons. The temperature-dependent relaxation timescales range from ns to ms. A particular type of defect are STEs, which can heal by emission of UV photons at a wavelength of around 300 nm. The ratio of non-radiative (via lattice phonons) to radiative relaxation is temperature-dependent45.


Various sources of optical excitation are available, such as deuterium and noble gas lamps, excimer lasers, synchrotron radiation and solid state lasers. These light sources greatly differ in spectral photon flux, spectral width and tunability. In this work, we focus on deuterium lamps and excimer lasers.


Commonly used strategies for the detection of UV photons differ in their spectral and temporal resolution.

Photo-multiplier tubes (PMTs) offer single-photon detection and have excellent timing resolution down to well below 10 ns. To optimize detection efficiency at the desired wavelength, various materials can be chosen for the photocathode. Cs-I cathodes are sensitive between 115 nm (the transmission edge of the MgF2 window) and 190 nm, diamond cathodes operate up to 220 nm and Cs-Te cathodes up to 320 nm. The peak quantum efficiency of VUV PMTs is of order 10%. The sensitivity at higher wavelengths, however, is not zero, but about 1/1,000 of the peak sensitivity. PMTs thus offer a certain degree of spectral filtering with a bandwidth of order 100 nm, which might be improved by UV filters.

Adding a spectrometer to the detection system offers spectral resolution down to below 0.1 nm, however the light throughput is fairly small, reducing the signal by typically five orders of magnitude. The reduced S/N often leads to long integration times and poor temporal resolution.

Studies in the VUV range are hampered by the fact that molecular oxygen absorbs light at wavelengths below 180 nm, therefore all experiments take place in an oxygen-depleted environment. We operate two vacuum systems: one is equipped with a VUV spectrometer and a deuterium lamp, the other one holds a set of different PMTs and an excimer laser as light source.

Spectrometer set-up

Studies that require spectral resolution are performed in a UV spectrometer (McPherson model 234/302); see Fig. 1(c). The crystal is imaged onto a slit with a typical width of 600 μm and the slit in turn is imaged onto the sensor of a CCD camera by a concave holographic grating. We used various gratings with groove densities between 300 and 2,400 grooves/mm, but most measurements of this work were performed with a 600 grooves/mm grating (blaze angle optimized for 150 nm). The total efficiency of the spectrometer is 2 × 10−7, largely limited by the small solid angle and a grating efficiency of a few percent. We determine the instrumental resolution by setting the grating to the blaze angle, thereby imaging the spectrometer’s slit directly onto the camera. The best resolution obtained for minimum slit widths is 0.5 nm.

The camera is an ANDOR Newton 940 model with a pixel size of 13.5 μm, the chip is cooled to −95 °C. The chamber is pumped down to a pressure of 2 × 10−6 mbar to avoid spurious signals from atoms and molecules in the residual gas23,24. The entire chamber is housed in a lead shield of 20 mm thickness to protect the CCD camera from ambient gamma radiation of up to 1 MeV energy. This measure reduces the rate of “cosmic” background events by a factor of at least 4, consistent with literature values. Given the long exposure times and large binning areas used in most measurements, however, the signal background is still dominated by “cosmic” events, both massive high-energy particles and gammas. We develop a reliable protocol to detect and remove such events in our data sets.

The spectrometer is calibrated by a Hamamatsu L1835 deuterium lamp, which is also used for illumination of the crystal. The lamp has a strong characteristic emission spectrum between 120 and 170 nm, the light intensity on the crystal is a few W/cm2 with a spot size of 3 mm. The absolute calibration and its reproducibility are better than 1 nm.

PMT set-up

The time evolution of luminescence signals is investigated with PMTs. Measurements of the radioluminescence are performed in a dedicated vacuum chamber evacuated to 10−5 mbar. We employ PMTs with Cs-I, diamond and Cs-Te photocathodes (Hamamatsu models R6835, R7639 and R6836) in head-on and side-on configurations. The PMTs are cooled to 0 °C. Typical settings are a high voltage of −1500 V and a signal threshold of −7.8 mV, resulting in a dark count rate of 5 Hz. The voltage divider circuitry is placed inside the vacuum and the signals are counted by a Becker + Hickl card without prior amplification. The FWHM of a signal is below 2 ns and we allow for a hold-off time of 5 ns.

The crystal temperature can be controlled between 0 and 160 °C using peltier elements and heating wires and the distance between crystal and PMT can be varied to adjust the absolute count rate.

A 157-nm F2 excimer laser is attached to this chamber to induce photoluminescence in the crystal. The pulse energy and duration are 1 mJ and 7 ns, respectively, the repetition rate is set to 100 Hz and the size of the beam is 8 × 3 mm2. Mechanical shutters are used to protect the PMT from direct exposure to the excitation light.

Additional Information

How to cite this article: Stellmer, S. et al. Radioluminescence and photoluminescence of Th:CaF2 crystals. Sci. Rep. 5, 15580; doi: 10.1038/srep15580 (2015).