Skip to main content


Front. Phys., 07 May 2024
Sec. High-Energy and Astroparticle Physics
This article is part of the Research Topic New Developments In The Quest For Discovering Axions And Axion-like Particles. View all 4 articles

Split-cavity tuning of a rectangular axion haloscope operating around 8.4 GHz

Jessica Golm,
Jessica Golm1,2*Jose María García-Barcelo
Jose María García-Barcelo3*Sergio Arguedas CuendisSergio Arguedas Cuendis1Sergio CalatroniSergio Calatroni1Walter WuenschWalter Wuensch1Babette DobrichBabette Dobrich3
  • 1CERN—European Organization for Nuclear Research, Geneva, Switzerland
  • 2Institute for Optics and Quantum Electronics, Friedrich Schiller University Jena, Jena, Germany
  • 3Max-Planck-Institut für Physik (Werner-Heisenberg-Institut), Garching bei München, Germany

The axion haloscope is the currently most sensitive method to probe the vanishingly small coupling of this prominent Dark Matter candidate to photons. To scan a sizeable axion Dark Matter parameter space, the cavities that make up the haloscope need to be tuned efficiently. In this article, we describe a novel technique to tune axion haloscopes around 8.4 GHz in a purely mechanical manner without the use of dielectrics. We achieve tuning by introducing a gap along the cavity geometry. A quality factor reduction of less than 20% is achieved experimentally for a tuning range of around 600 MHz at room temperature and at cryogenic temperatures for around 300 MHz. A larger tuning range would require an improved alignments mechanism. We present the results of a corresponding prototype and outline prospects to further develop this technique.

1 Introduction

An axion haloscope is an experimental apparatus used in the search for axions, hypothetical particles that could make up Dark Matter in the Universe as discussed in Peccei and Quinn [1, 2]. In recent years, there has been a large increase in the number of experiments and approaches that aim to find or exclude the axion as Dark Matter, see, e.g., here Irastorza and Redondo [3].

Axions are very light, neutral particles that are expected to interact very weakly with ordinary matter and electromagnetic fields. Axion haloscopes are designed to detect axions by converting them into detectable electromagnetic signals (photons) in the presence of a strong magnetic field by the inverse Primakoff effect, cf. Primakoff [4]. To improve this conversion process, haloscopes use high-quality factor resonators, such as microwave cavities, see, e.g., here Sikivie [5]. The conversion of axions into photons occurs when the mass of the axion matches approximately the resonant frequency of the apparatus.

The primary goals of an effective axion detection system involve maximising the power generated from the axion-photon interaction and expanding the range of analysed axion masses (i.e., the range of frequencies scanned). The detected radio frequency (RF) power (Pd) relies on inherent axion properties and experimental cavity characteristics, as outlined in Díaz-Morcillo et al. [6] (see Eq. 1):


Here, κ signifies the coupling to the external receiver (κ = 0.5 for critical coupling operation), g represents the unknown axion-photon coupling, ρa denotes Dark Matter density, ma stands for axion mass, Be represents the external static magnetic field (dependent on the magnet used in the experiment), C is a label for the so-called “form factor,” V is the cavity volume, and Ql represents the loaded quality factor of the cavity. In contrast to Ql, the unloaded quality factor Q0 is a common metric in characterising resonant cavities as it is independent of external coupling, see, e.g., here Pozar [7]; Rezaee et al. [8]. The form factor (C), measuring the coupling between the external magnetostatic field and the RF electric field induced by axion-photon conversion, is expressed in Eq. 2:


Here, ɛr represents the relative electrical permittivity within the cavity of volume V. The sensitivity measure of the haloscope is the axion-photon coupling detectable for a given signal-to-noise ratio (SN), which can be calculated using:


In this equation, kB represents the Boltzmann constant, Tsys is the noise temperature of the system, Qa represents the quality factor of the axion resonance, and Δt is the data-taking time window, cf. Díaz-Morcillo et al. [6]. To summarise, the controllable parameters in a given experimental set-up encompass κ, C, V, and Ql.

On the other hand, the mass of axions, if they exist, is not known. To maximise the chances of detecting axions, the haloscope needs to be tuned to the resonant frequency that corresponds to the expected mass range of axions being searched for. Tuning ensures that the cavity is effectively only sensitive to the specific axion masses under investigation, improving the chances of successful detection. Thus, the scanning rate dmadt is commonly employed to assess the performance of a haloscope, a value derived from Eq. 3, cf. Kim et al. [9] (see Eq. 4):


Also, κ is usually rewritten in terms of the coupling coefficient β, which can be extracted from the expression from Eq. 5


A tuning step must not require the opening of the cryostat as this is very time and energy-consuming. Until today, most of the adjustment techniques applied in haloscope experiments for frequency tuning have relied on mechanical systems. Various collaborations such as ADMX (cf. Boutan et al. [10] and Yi et al. [11]), and HAYSTAC (cf. Zhong et al. [12]), utilise cylindrical cavities with metallic rods. Also, other teams like IBS/CAPP (cf. Choi et al. [13]) employ dielectric rods. These rods are rotated inside the cavities, altering the electromagnetic field distribution and, consequently, the resonant frequency of the operating mode. This rotation is achieved either through several gears connected to a motor or by employing piezoelectric elements. A slightly different technique was, for example, employed by the QUAX collaboration (cf. Alesini et al. [14]), by using adjustable sapphire shells to modify the resonant frequency of the cavity. In a different example, the CAST-CAPP/IBS group uses two movable dielectric sapphire plates positioned symmetrically at the cavity sides (see, e.g., here Miceli [15]). In Kuo [16] tunable conic shell-cavities have been investigated, providing good tuning results for large cavities operating around 7.5 and 20 GHz. Table 1 gives an examination of some current tuning systems for frequencies between 4 and 11 GHz, in comparison with the outcomes obtained in this work. The percentage value of tuning has been calculated according to Eq. 6.


where f2 is the upper limit in the frequency tuning range and f1 is the lowest frequency. It is worth mentioning that the ADMX Sidecar experiment has conducted axion data taking campaigns using two different resonance modes. For Run B, this group has employed the TM010 mode, while for Run C they have used TM020, to explore higher frequencies, where significantly lower form factor values are achieved. On the other hand, the CADEx collaboration proposed in Aja et al. [17] the use of a sliding or tunable wall mechanism in rectangular cavities. The ORGAN group, in McAllister et al. [18], also describes this type of mechanical tuning in detail, comparing it with the tuning technique using metal rods usually employed in the axion community. In addition, the QUAX group has explored in Braggio et al. [19] opening techniques in a cylindrical cavity using angular misalignment on the longitudinal axis, achieving satisfactory results at frequencies above 10 GHz, using a so-called “clamshell” cavity. A tunable rectangular axion cavity is described in McAllister et al. [18]. It was used in The ORGAN experiment Phase 1b, where the axion search was focused on the 26–27 GHz band. A movable side wall (moving plunger) provided the tuning.

Table 1

Table 1. Overview of some existing tunable haloscopes operating at frequencies between 4 and 11 GHz.

It should be mentioned that there is also the possibility of broad-band search, which removes the need of tuning, but typically cannot achieve a signal amplification comparable to the resonant haloscopes. Examples of such experiments are BRASS (magnetic mirror), see Bajjali et al. [20], MADMAX (with a set of movable dielectric disks in Brun et al. [21]), ALPHA (using metamaterials), cf. Gelmini et al. [22], or BREAD, see Knirck et al. [23].

Over the past 5 years, the RADES (Relic Axion Dark-Matter Exploratory Setup) research group has extensively explored haloscopes, engaging in the conceptualisation, production, and physics analysis of axion detectors in the pursuit of detecting Dark Matter axions with masses approximately around 1 and 34 μeV, cf. Álvarez Melcón et al. [2426]; Díaz-Morcillo et al. [6]; Ahyoune et al. [27]. This team has developed a mechanical tuning technique where the haloscope volume is increased by mechanically moving the cavity halves split symmetrically (cf. Arguedas-Cuendis et al. [28]), operating at X-band frequencies. This set-up can work similarly to the clamshell technique (cf. Braggio et al. [19]), but a symmetric opening is more favourable, giving a bigger frequency tuning range, as shown below. Also, the RADES group is currently exploring other methods based on electrical tuning by the use of ferroelectric materials (see, e.g., here García Barceló et al. [29]).

In this work, our goal is to build a tuning mechanism that can tune the resonant frequency of the first RADES cavity (cf. Álvarez Melcón et al. [24]) by using the tuning technique presented in Arguedas-Cuendis et al. [28] with a custom made support structure which gives the capability of tuning and quality factor measurements at cryogenic temperatures. This halo scope is based on an array of five subcavities interconnected by waveguide irises to increase the total volume while maintaining a high resonant frequency for operation in dipole magnets. The frequency tuning approach presented in this study relies on the separation of two symmetrical halves until RF leakage through the aperture becomes the primary factor affecting Q0. In the case of small apertures in this haloscope, the effect of a vertical cut along the longitudinal direction is negligible, as the microwave currents of the fundamental mode TE101 are parallel to this plane. This movement effectively increases the width of the cavity, thereby altering the search range for axion frequencies. According to Arguedas-Cuendis et al. [28], the theoretical tuning range value for this haloscope is around 10%. Similar values are also obtained in García-Barceló et al. [30] for this type of tuning at X-band frequencies in other cavities. For this study, experiments are carried out at cryogenic temperatures, and simulations using the finite element method are employed to comprehend how the cavity behaves at various openings.

2 Cavity design for mechanical tuning

Figure 1 shows the schematics of the mechanical tuning idea. By introducing a gap between two cavity halves the geometry can be widened which shifts the resonant frequency to lower frequencies.1

Figure 1

Figure 1. Schematics of the tuning concept. The left side shows the cavity in the closed position with no gap and at its highest resonant frequency. On the right side, a gap was introduced between the two cavity halves, tuning the cavity to a lower frequency depending on the gap size.

2.1 Cavity design

The tuning mechanism will be exemplified using multi-cell cavities, which were developed by the RADES team, as described in Álvarez Melcón et al. [24]. This design allows an increase in cavity volume while maintaining a high resonant frequency as a single element of the cavity mostly determines the frequency. A prototype resonating at 8.4 GHz was built by joining five cells with all-inductive irises (vertical windows in waveguide technology). While the tuning will be demonstrated with this prototype, it works in principle for other designs as well.

Figure 2 shows the electric field distribution of the five configuration modes. The coherence between the cavities is maintained only in the first mode which is the only mode that couples to the axion. To tune this type of cavity, it was cut along the symmetry plane as indicated in Figure 3A. The surface currents do not cross this plane of symmetry (they are parallel to this plane); therefore, it is possible to cut the cavity without intercepting the current. Thus, one can expect to retain a high Q0 value despite the introduction of the manufacturing cut and even when separating both halves. This paper aims to study and measure to what extent this is possible.

Figure 2

Figure 2. Electric field pattern for the five electromagnetic modes of the cavity. Red colour refers to a maximum and blue colour to a minimum in the electric field. Taken from Álvarez Melcón et al. [24].

Figure 3

Figure 3. (A) Mode pattern with symmetry plane. The fabrication is done in two halves defined by this symmetry plane. 3D model housing of the vertical cut inductive irises cavity to be manufactured (B). This piece is one of the two symmetrical halves, which must be parallel. SMA coaxial ports are situated at the 4.1 holes. Dimensions given in Table 2.

To enable vertical cut tuning, small changes in the design of the 5-cell cavity (with manufacturing horizontal cut), described in Álvarez Melcón et al. [24], were necessary. This cut can be used to introduce a gap that increases the volume and moves the resonant modes to lower frequencies, as shown in Figure 1, without a significant loss of quality factor, as will be shown in the following. In general terms, the gap should be small enough with gap < λ/2, where λ is the wavelength at the operation frequency, see, e.g., here Torrisi et al. [31]. However, in our case, as a more conservative scenario, a gap has been set to be small compared to the cavity dimensions (<10 % of the width, a value extracted from García-Barceló et al. [32], where a similar tuning mechanism is employed). Figure 3B depicts the 3D model and dimensions of the analysed haloscope.2 In Table 2, the dimension values are shown.

Table 2

Table 2. Dimension values of the vertical cut haloscope for cryogenic conditions analysed in this study.

2.2 Simulations of losses introduced due to mechanical tuning

2.2.1 Parallel cavity halves

Before the manufacturing and measurements of this haloscope, a study was carried out using the Computer Simulation Technology (CST) Studio Suite software [33], to study the behaviour of this structure in terms of Q0 and C factors against different openings that can cause radiation losses.

Figure 4 depicts the results obtained with a sweep of vertical cut gaps from 0 to 4 mm. For these simulations, an electrical conductivity value in the copper cavity of σc = 109 S/m was used, as this is a realistic value according to Golm et al. [34] where the same coating and frequency were applied. In addition, coaxial antenna lengths have been chosen to be critically coupled (β = 1) for Port 1 and very undercoupled (β ≃ 0) for Port 2, in the closed scenario (gap = 0 mm). The antenna lengths have been maintained for the study of all the gap values.

Figure 4

Figure 4. Results from CST simulations for the vertical cut tuning study applied in the haloscope depicted in Figure 3B: frequency and tuning versus gap (A), unloaded quality and form factors versus gap (B), and volume and figure of merit (Q0V2C2) versus gap (C).

As can be seen, the obtained form factor follows a relatively constant value, close to C = 0.66, for the whole range. However, the unloaded quality factor suffers a small detriment when the gap increases. For the full range of gaps analysed, the figure of merit Q0V2C2 remains almost constant at around 11.5 L, so it can be guaranteed that the tuning range is adequate, obtaining a frequency tuning range of 1.07 GHz (or 12.6%), which is a very satisfactory tuning compared to the results of other experimental groups shown in Table 1, and even more so for operating frequencies close to 8.4 GHz.

In addition, since this structure has a tuning system that connects to the outside environment, a study has been made of possible signals that could enter its interior. After several simulations, it has been verified that there are no resonance echoes of a potential dipole magnet with a bore diameter of about 50 mm where this haloscope could be installed.

2.2.2 Misalignment studies

A simulation study has been conducted to consider possible misalignment effects when separating the two halves. Due to the position of the coaxial ports, the number of possible main misalignments is reduced to the following: angular y − axis, angular z − axis, and lineal y − axis. Figure 5 shows an example of misalignment for each scenario. In addition, to reduce complexity, this tuning technique is based on leaving the coaxial ports attached to one of the halves of the haloscope. This introduces a small asymmetry between the two halves which can be neglected (see Appendix A).

Figure 5

Figure 5. Misalignment effect in the vertical cut haloscope for three scenarios: angular y − axis (A), angular z − axis (B), and lineal y − axis (C).

Also, to simplify this investigation of misalignments, a gap of 1 mm has been chosen. Figure 6 depicts the results obtained for each case as a function of the misalignment variables: θy for the angular y − axis, θz for the angular z − axis, and gy for the linear y − axis. As can be seen, the results show a degradation in the form factor value of 40 % in the case of angular misalignment in the y − axis. The main reason for this reduction is because the individual resonant frequencies of the subcavities are very sensitive to their widths, which are modified with θy, in turn changing the optimised condition for the operating mode (see more on this concept in Álvarez Melcón et al. [24]). Furthermore, for this type of misalignment, the resonant frequency changes considerably (around 1.2%). However, the unloaded quality factor remains relatively stable.

Figure 6

Figure 6. Results obtained in the simulation of the misalignment study in the angular y − axis (first column), in the angular z − axis (second column), and in the lineal y − axis (third column). The first row of graphs shows the variation of the quality and form factors versus the variation of the misalignment variable. The second row plots the variation in frequency and figure of merit Q0V2C2 versus misalignment. The quality factor and figure of merit parameters are given in terms of the percentage change from the aligned scenarios (θy = θz = gy = 0).

On the other hand, for angular z − axis misalignment, the form factor remains very high, although the quality factor suffers a reduction of more than 7% for negative values of θz. However, as the form factor becomes more important here for the figure of merit of the experiment, the latter remains relatively high. In the case of frequency, it is also maintained around stable values.

Finally, in the case of linear misalignment in the y − axis, it is seen that this causes the largest decrease of the unloaded quality factor (more than 80% for values of gy = 0.5 mm), while the form factor remains high for the entire range, and this in turn reduces the figure of merit the most of the three cases analysed. Fortunately, the outcomes show a resonant frequency that is relatively stable for the entire range.

3 Proof of principle

The tuning idea was first implemented by separating the cavity halves of a prototype with spacers that do not penetrate the cavity hollow volume or disturb the electromagnetic field pattern. The prototype was made of non-magnetic stainless steel (316 LN) coated with a 30 μm copper layer. The reason for choosing stainless steel as a base material for the cavity and not producing it from pure copper is the forces the cavity can be exposed to during a quench of the magnet (eddy currents). Cavities for axion Dark Matter searches are usually installed in multitesla fields.

A photograph of the prototype and spacers is shown in Figure 7. The top picture shows the disassembled cavity halves and the spacers made of brass. These spacers generate a gap of around 1.25 mm and they are mounted on the screws that connect the two cavity halves. The bottom picture depicts the assembled cavity with spacers made of stainless steel. After a characterisation of the tuning properties of the cavity at room temperature, the cavity was installed in a cryostat, and the unloaded quality factor Q0 was measured below 10 K for a gap size of 0 and 1.25 mm. The brass spacers were used during the cryogenic characterisation. In none of the described mounting situations, the spacers entered the cavity structure. The alignment of the two halves of the cavity with each other depended only on the two spacers and the force with which the screws were tightened on each side. Both cavity ports were kept on one cavity half when a gap was applied.

Figure 7

Figure 7. Photograph of the vertical cut haloscope coated with copper before assembly and brass spacers (A) and after assembly with a gap between the two halves introduced with stainless steel washer spacer (B). Note that for the characterisation both ports were attached to one cavity half unlike shown on the picture in which each port is attached to another cavity half.

Figure 8 shows measurements of the tuning range and quality factor at ambient conditions and compares it with simulation. For this characterisation of the cavity, washers of known thickness were used to create a gap while a vice pressed the cavity halves together There is a linear dependence between gap size and frequency, as expected, and the total tuning range at ambient conditions is 711 MHz for a gap opening of 2.5 mm, as shown in Figure 8B. There is only a small deviation between measurement and simulation in the unloaded quality factor of Figure 8A, but by differently assembling the cavity halves losses can increase. From simulations in Section 2.2.2 we know these losses can be attributed to misalignment.

Figure 8

Figure 8. Comparison of measurement with uncertainty (blue) and simulation (black) of the unloaded quality factor Q0 (A) and the resonant frequency (B) for different gap openings. For the simulations a copper conductivity at room temperature of 5.8 × 107 S/m was assumed.

For the characterisation at low temperature, the cavity was installed in a vacuum chamber which was introduced in a helium cryostat. The cavity was suspended in the cryostat by clamping it in a support structure on one extremity and subsequently attached to a long rod. It was measured in two configurations during cool-down for a gap size of 0 and 1.25 mm (half the maximum possible opening within the holding structure mechanics) separated by the brass spacers shown in Figure 7A. The results from the cryogenic measurements of the quality factor with spacers below 10K are shown in Table 3. From those measurements, the electrical conductivity of the copper coating can be deduced assuming that the pieces are aligned. These conductivity values are also shown in Table 3 and agree well with those measured from previous coatings on other samples (100 × 107 S/m). The copper coating of this cavity was applied by DC (Direct Current) galvanic plating with an organic brightener and the RRR (residual-resistance ratio) is expected to be 38 ± 2.

Table 3

Table 3. Unloaded quality factor Q0 and resonant frequency f from a cavity measurement and uncertainty for temperatures below 10 K and gap sizes of 0 and 1.25 mm. An electrical conductivity was deduced from these measurements.

Misalignment of the cavity halves can result in high losses. This was observed when remeasuring the cavity after reassembly. The unloaded quality factor obtained at low temperatures was measured to Q0 (gap = 0 mm) = 23,200 ± 800 and Q0 (gap = 1.25 mm) = 20,500 ± 1,100. The quality factor decreased by more than 20% which is consistent, for example, with a misalignment in direction gy of about 100 μm according to Section 2.2.2.

Due to the form factor studies in simulation considering misalignments of the cavity halves, we can justify that this parameter will move around the ranges shown in Figure 6. Thus, an argument for explaining the real form factor value arises. Two measurements at cryogenic temperatures gave Δf0 (difference in the resonant frequency between both measurements) of less than 0.03% for both gaps 0 and 1.25 mm (see Table 3). Compared to the misalignment simulations this low Δf0 gives us that we have a very low misalignment scenario with θy (see Figure 6), so the form factor is not affected by this. Also, due to the high ΔQ0 (difference in the unloaded quality factor between both measurements) (20%) we can affirm that we have linear misalignments gy (probably around 0.1 mm), but the form factor is neither affected by this misalignment. Thus, observing Figure 6 and considering the above information the C-factor should be around 0.62.

4 Tuning mechanism for cryogenic environment

4.1 Set-up and sliding mechanism

After demonstrating that the tuning concept is viable in principle, a gear system was designed to allow for translating the movement in a cryogenic environment. For data-taking, haloscope axion cavities will be installed in dipole magnets where the space for tuning is typically limited by small bore diameters. Furthermore, the measurement takes place in a vacuum or liquid helium environment at temperatures of 4.2 K. These conditions make it challenging to realise cavity tuning during data-taking. Therefore, two possible solutions were deliberated. One option is to install a piezo actuator in the bore to generate the movement. However, two challenges have to be overcome: first, the space in the bore does not allow for a larger actuator. Secondly, an actuator with sufficient force to move the cavity halves is needed. Considering the size of the currently existing actuators that can move our cavity halves, a gear system to generate the movement would be necessary. Another possibility is to generate the movement from the outside of the magnet by a long rod connected via gears to the two cavity halves. This solution is also not without problems as complex feedthroughs are required to propagate the rotational movement from the 300 K to the 4 K environment.

To study the gear-based tuning mechanism, a test stand was built in the CERN Central Cryogenic Laboratory, and different aspects of this tuning were investigated. Figure 9 shows a schematic drawing of the test stand. The cavity and the RF cables were installed in a vacuum chamber immersed in liquid helium. To characterise the cavity two RF cables (green) coming from the cavity were connected to a feedthrough in the vacuum flange at ambient temperature, to which a Vector Network Analyser (Keysight N9918A) was connected for quality factor measurements. To tune and change the gap size of the cavity a long rod (about 1.5 m long, 2 mm diameter, stainless steel) (red) was connected by a gear system to the cavity at the bottom of the vacuum chamber. The rod had an adjusting screw at the end and by turning it the cavity opened or closed, depending on the direction in which the gear is turned. The movement of the rod for this test was generated by hand, but the adjusting screw could be easily attached to a small motor which would allow more precision in movements. A gas inlet on the cryostat provided the possibility of measuring in a helium gas environment instead of in vacuum.

Figure 9

Figure 9. Cavity tuning test stand in the CERN Central Cryogenic laboratory with adjusting screw and rod (red), RF cables (green), temperature sensor (yellow), and the cavity (grey).

Photographs of the cavity installed in the holding system with gears to transmit the movement can be seen in Figure 10. In Figure 11, the individual parts of the tuning mechanism are shown. In (a), the holding pieces for the cavities are illustrated. The cavity halves can slide into these holding pieces, which are held by positioning screws. The holding piece has on both sides sliding bars. In Figure 11B, the sliding structure is shown. The assembly consists of two of those structures that will be connected by long stainless steel bars, which have on one side long holes for easier positioning. The sliding bars shown in (a) have to be inserted in the sliding rails shown in (b). Figure 11C shows the assembly of (a) and (b) without cavities, and (d) shows the complete assembly with the cavity halves installed. The assembly shows the two gear racks that are screwed to holding piece (a) and a tuning rod with two gears glued to it. Thus, by turning this tuning rod outside of the cryostat, the rotation will be transmitted to the gears on the cavity inside the cryostat and converted into a linear, parallel translation of one cavity half.

Figure 10

Figure 10. Photographs of the cavity halves installed in the tuning holding structure with gears. Top view with RF ports (A) and bottom view (B). The bottom view displays the gear mechanism that moves the cavity halves to each other.

Figure 11

Figure 11. Drawings of the cavity support structure with (A) holding piece for the cavity halves, (B) the sliding structure for alignment, (C) the assembly of the sliding structure, and (D) the complete assembly with the gear system.

To guarantee a smooth movement of the cavity halves with the described tuning mechanism at cryogenic temperatures and in vacuum, the materials have to be chosen carefully. In vacuum, parts of the same material can easily adhere to each other because there are no thin layers of other elements between the parts. Under mechanical pressure, e.g., thermal contraction, they can bond. Also, the friction coefficients between the same materials, i.e., aluminium on aluminium (friction coefficient 1.6–2.2, c.f. Deulin et al. [35]) or stainless steel on stainless steel (friction coefficient 2.9, see Deulin et al. [35]), in vacuum are very high. Thus, it was decided to produce the holding pieces for the cavity and the holding structure out of different materials. The holding piece for the cavity was made of stainless steel (see Figure 11A) and the structure on which the cavity slides back and forth inside was made of aluminium (friction coefficient 0.3, see Deulin et al. [35]; Figure 11B). The gear and gear rack were made of PTFE (Polytetrafluoroethylene) which has a very low friction coefficient of 0.04 for PTFE on PTFE, cf. Deulin et al. [35].

After a first functionality test of the described mechanism and material, some optimisations have been made. The sliding structure (see Figure 11A) was re-fabricated using brass as it has a more similar expansion coefficient to aluminium than stainless steel. Furthermore, the holding pieces for the cavity were optimised by replacing the sliding bars with sliding pins, which have less surface area touching the sliding rail, resulting in reduced friction and less material deforming during cool-down.

4.2 Tuning results with the sliding mechanism

The tuning mechanism described in the previous section was tested on functionality at 77 K by immersing the set-up in liquid nitrogen. For testing a tuning mechanism where pieces are made of materials with different thermal expansion coefficients, it is crucial to wait for thermalisation. After a 5-min thermalisation time in the liquid bath, an opening and closing of the cavity halves were demonstrated. The cavity spectrum and the tuning range were measured at ambient conditions, see Figure 12A, and in liquid nitrogen, see Figure 12B. The spectrum of the cavity shows five peaks, one for each of the small subcavities, while the axion only couples to the first mode. For explanations, see Álvarez Melcón et al. [24]. The difference in frequency between the first peak of each spectrum (and thus the tuning range) in the open (gap = 2.5 mm) and closed (gap = 0 mm) positions of the cavity halves was measured to be 670 MHz at ambient condition and 540 MHz in liquid nitrogen at 77 K. The tuning range in liquid nitrogen is smaller compared to air because the higher dielectric constant of LN2 decreases the resonant frequency by a factor of 1/ε. The dielectric constant of liquid nitrogen is 1.431, see Mathes [36], and therefore a tuning range of 540 MHz between 6.48 and 7.02 GHz corresponds to a tuning range in vacuum of about 650 MHz between 7.75 and 8.40 GHz.

Figure 12

Figure 12. Tuning range measured with the cavity embedded in the sliding structure at ambient conditions (A) and in liquid nitrogen (B) with a maximum gap size of 2.5 mm (blue) and no gap (red). At 77 K disturbances of the spectra due to the boiling of liquid nitrogen are visible, most clearly for the second cavity peak in the spectra of the cavity with a 2.5 mm gap.

In Figure 12B some disturbances in the second peak of the blue spectrum are visible. Those have their origin in gaseous Nitrogen bubbles that enter the cavity from time to time. Those bubbles are the result of the boiling of the liquid nitrogen and change the spectra while entering the cavity.

After demonstrating that the mechanism worked in a 77 K environment, the whole set-up was implemented in a cryostat with a 2 mm thick tuning rod of about 1.5 m length going from 4 to 300 K. The cavity and all elements were placed in a vacuum chamber inside the cryostat that was filled with liquid helium. A schematic of the experimental set-up is shown in Figure 9. It was possible to reach temperatures around 20 K in the vacuum chamber with this setup. The reason for not reaching lower temperatures is the RF cables which are made of copper, a very good thermal conductor, as well as the tuning rod of 1.5 m length (stainless steel, 2 mm diameter) conducting heat from the outside of the cryostat at ambient temperature to the cold vacuum chamber. For measurements with spacers between the cavity halves, described in Section 3, a minimum temperature of 6 K could be reached. However, this was only possible due to a complex thermalisation of the RF cables to intercept the conducted heat into the vacuum chamber. Those cables need to be moveable during tuning so as not to obstruct the mechanism, therefore they were not thermalised. Instead, thinner, more flexible cables were used with the disadvantage of higher RF losses.

The same results in terms of tuning are expected at 4 and 20 K, as previous measurements showed that the resonant frequency (= thermal contraction of the cavity) and quality factor (= electrical conductivity) for the cavity are constant below 30 K, see Figure 8B. To use the cavity as a haloscope in an axion search, the temperature should be as low as possible. One possibility to solve the issue of not reaching the minimum temperature is to let a small amount of exchange gas (about 1 mbar of helium) in the vacuum chamber, allowing convective heat transfer from the wall of the vacuum chamber to the cavity. By adding the exchange gas, the cavity properties remain the same, and the gas will not affect the haloscope data taking.

Figure 13 shows the tuning results at 20 K. It was demonstrated that the cavity can be tuned in a cryogenic environment without performing a warm-up achieving a tuning range of 667 MHz. This result confirms the tuning range predicted from the measurement in liquid nitrogen described before. Besides the tuning range, a high scanning resolution is important to investigate all possible frequencies while a haloscope is data-taking. Therefore, frequency steps in the range of the 3 dB points of the resonant frequency should be realised. The frequency step size required to achieve this depends on the cavity properties: the unloaded quality factor (Q0) and the coupling of the port. Assuming critical coupling and a Q0 of 27,000 (as measured for this specific cavity, see Section 3) we aim for a step size of 0.6 MHz (8.4 GHz/13500) per step.

Figure 13

Figure 13. Tuning range measured with the cavity embedded in the sliding structure at 20 K with maximum gap size (blue) and without gap (red) (A). Zoom in on the first cavity peak (axion mode) for a selected set of cavity openings, demonstrating the minimum step size achieved for this measurement (B).

The described set-up reached a minimum step size of 3 MHz while the rotation was applied, turning an adjustment screw by hand; see Figure 13B. Using a motor turning the adjustment screw at ambient conditions will lead to higher precision. Furthermore, high-precision gears and gear racks can help to decrease the frequency step size. To maximise the detection rate during tuning, over-coupling (i.e., β = 2) instead of critical coupling is more advantageous, cf. Kim et al. [9]. In that case, the minimum required step size required for our cavity increases to 0.9 MHz.

The cavity must maintain a high-quality factor during tuning. Therefore, Q0 of the cavity was observed while changing the resonant frequency with the tuning mechanism and compared with the results obtained with the spacers, described in Section 3. The result of the unloaded quality factor determination for different resonant frequencies of the cavity is illustrated in Figure 14.

Figure 14

Figure 14. Unloaded quality factor (Q0) of the cavity for different gap sizes generated by the tuning mechanism (yellow), by spacers (blue) and without tuning (red) measured at cryogenic temperatures below 20 K.

From the simulation in Section 2.2.1 we expect a quality factor of about 27,000 at cryogenic temperatures which does not degrade too much for a gap of 1.25 mm, cf. Figure 4B. Figure 14 shows that this is hard to achieve. The blue triangles mark the measurements done with a spacer (gap = 1.25 mm) and the red points the cavity bolted together with screws (gap = 0 mm). The measurements of those configurations were already discussed in Section 3, where we observed different quality factor values, during repeated assembly cycles. Only considering the maximum Q0 measured for both spacer configurations (gap = 0 and 1.25 mm) the results are in good agreement with the simulations from Section 2.2.1 for parallel cavities. The lower values for Q0 for the same spacer configurations are attributed to misalignments. The simulations of Section 2.2.2 showed how sensitive the cavity is to certain misalignment directions. The results underline the importance of a good alignment mechanism for the tuning, as a good-aligned setup is already hard to achieve with spacers.

The yellow triangles are the results obtained when changing the resonant frequency with the tuning mechanism described in Section 4.1. The quality factor is for all measurements below the values obtained with spacers and varies for the same resonant frequency. The maximum decrease in quality factor measured with the tuning mechanism compared to its optimal values for no gap (Q0 about 27,000) is about 45%. These losses are also attributed to misalignments of the two cavity halves, which leads to the conclusion that the alignment mechanism still needs to be improved and tolerances for the production of future assemblies need to be reduced.

5 Conclusion and outlook

We have presented a concept to tune rectangular cavities for haloscope searches mechanically. The concept foresees cutting cavities along a symmetry plane of the field lines. We have qualitatively validated this mechanism in practice and simulation. Assuming that the cavities are kept parallel, the simulations in Section 2.2.1 predict a tuning range of up to 1.1 GHz (12.6%) with nearly no degradation in the figure of merit (Q0V2C2) over the whole range.

The cavity could be tuned in a range of 667 MHz 9.5 % at 20 K using the sliding mechanism outlined in Section 4.1. The available bore size limited the maximum gap size (2.5 mm) and hence the tuning range for the presented configuration. The obtained unloaded quality factor varied between (1.5–2.1) × 104 while tuning. From the simulations in Section 2.2.1 higher quality factors were expected. As can be observed from the simulations in Section 2.2.2, the misalignment of the two cavity halves contributes to the losses (up to 45%) in this assembly. However, there could be other sources of losses like manufacturing tolerances or the electrical conductivity of the housing material. Previous measurements in Section 1 showed that greater values of Q0 (2.7 × 104 at 7 K, gap = 1.25 mm) are possible for parallel cavity-halves (separated by spacers). This number is consistent with the parallel cavity-half simulations shown in Section 2.2.1.

Moreover, misalignment can cause a 60% decrease in form factor C; see Figure 6. This is particularly relevant for cavity designs with subcavities connected by irises, as the misalignment alters the ideal operating mode conditions. Examining the same misalignment for a long single cavity, merely a minor deterioration of the form factor (0.66–0.63) is discernible.

The minimum step size achieved for this mechanism was 3 MHz. To have continuous tuning steps overlapping in their 3 dB range a step size of less than 0.9 MHz (3 μm) is required. To improve the step size of the assembly, high-precision gears and a motor-driven adjustment of the tuning rod are required.

The state of the art of various current tuning methods for different axion groups and the outcomes of this effort were displayed in Table 1 of Section 1. The mechanical tuning presented in this work is a competitive way to tune an axion haloscope because it can achieve the same tuning percentage as the ADMX Sidecar—Run B while also having a larger form factor and quality factor. However, it is necessary to make improvements to the current tuning design to produce a smaller step size and handle the misalignment more effectively. Further studies using an improved gear mechanism, combined with a mechanism that moves the coupler are ongoing in the group.

Data availability statement

The raw data supporting the conclusion of this article will be made available by the authors, without undue reservation.

Author contributions

JG: Writing–review and editing, Writing–original draft, Investigation. JG-B: Writing–review and editing, Writing–original draft, Investigation. SA: Investigation, Writing–review and editing. SC: Writing–review and editing, Supervision. WW: Writing–review and editing, Supervision. BD: Writing–review and editing, Writing–original draft, Supervision, Funding acquisition.


The authors declare that financial support was received for the research, authorship, and/or publication of this article. This work was funded by the European Research Council under grant ERC-2018-StG-802836 (AxScale project). JG is also funded by the “Physics Beyond Collider” initiative. This work has also been funded by MCIN/AEI/10.13039/501100011033/and by “ERDF A way of making Europe,” under grants PID2019-108122GB-C33 and PID2022-137268NB-C53. JG-B thanks the grant FPI BES-2017-079787, funded by MCIN/AEI/10.13039/501100011033 and by “ESF Investing in your future.”


This work was performed in the RADES group and we acknowledge the contribution and invaluable help of its members. Additionally, we would like to thank the entire CERN cryolab team, especially Agostino Vacca for helping to modify the mechanical components of the tuning mechanism.

Conflict of interest

The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

Publisher’s note

All claims expressed in this article are solely those of the authors and do not necessarily represent those of their affiliated organizations, or those of the publisher, the editors and the reviewers. Any product that may be evaluated in this article, or claim that may be made by its manufacturer, is not guaranteed or endorsed by the publisher.


1In García-Barceló et al. [29], preliminary investigations have been conducted with this technique for rectangular long single cavities, and 1D and 2D multicavity structures operating at X-band frequencies. A similar research is expected for the long single cavities, and 1D and 2D haloscopes with cylindrical shapes explored in García-Barceló et al. [30].

2In the fabrication of these parts, alignment pins were included in the x − axis, in the thickness tz of the housing at both ends in length. In addition, screw holes were implemented both in the port sections (y − axis) and in the tz-thickness (x − axis). The latter to test the behaviour of the completely closed and screwed-together structure.


1. Peccei R, Quinn H, CP conservation in the presence of pseudoparticles. Phys Rev Lett (1977) 38:1440–3. doi:10.1103/PhysRevLett.38.1440

CrossRef Full Text | Google Scholar

2. Peccei R, Quinn H, Constraints imposed by CP conservation in the presence of pseudoparticles. Phys Rev D (1977) 16:1791–7. doi:10.1103/PhysRevD.16.1791

CrossRef Full Text | Google Scholar

3. Irastorza IG, Redondo J, New experimental approaches in the search for axion-like particles. Prog Part Nucl Phys (2018) 102:89–159. doi:10.1016/j.ppnp.2018.05.003

CrossRef Full Text | Google Scholar

4. Primakoff H, Photoproduction of neutral mesons in nuclear electric fields and the mean life of the neutral meson. Phys Rev (1951) 81:899. doi:10.1103/PhysRev.81.899

CrossRef Full Text | Google Scholar

5. Sikivie P, Experimental tests of the invisible axion. Phys Rev Lett (1983) 51:1415–7. doi:10.1103/PhysRevLett.51.1415

CrossRef Full Text | Google Scholar

6. Díaz-Morcillo A, García Barceló JM, Lozano Guerrero AJ, Navarro P, Gimeno B, Arguedas Cuendis S, et al. Design of new resonant haloscopes in the search for the dark matter axion: a review of the first steps in the rades collaboration. Universe (2022) 8:5. doi:10.3390/universe8010005

CrossRef Full Text | Google Scholar

7. Pozar DM, Microwave engineering. Hoboken, New Jersey, United States: John Wiley and Sons, Inc. (2012).

Google Scholar

8. Rezaee P, Knöchel R, Tayarani M, Simple, fast, and accurate parametric modeling of the coupling and external quality factor for microstrip filter design using active learning method. AEU - Int J Elect Commun (2012) 66:668–76. doi:10.1016/j.aeue.2011.12.007

CrossRef Full Text | Google Scholar

9. Kim D, Jeong J, Youn S, Kim Y, Semertzidis YK, Revisiting the detection rate for axion haloscopes. J Cosmology Astroparticle Phys (2020) 2020:066. doi:10.1088/1475-7516/2020/03/066

CrossRef Full Text | Google Scholar

10. Boutan C, Jones M, LaRoque BH, Oblath NS, Cervantes R, Du N, et al. Piezoelectrically tuned multimode cavity search for axion dark matter. Phys Rev Lett (2018) 121:261302. doi:10.1103/PhysRevLett.121.261302

PubMed Abstract | CrossRef Full Text | Google Scholar

11. Yi AK, Ahn S, Kutlu i. m. c. b. u., Kim J, Ko BR, Ivanov BI, et al. Axion dark matter search around 4.55 μeV with dine-fischler-srednicki-zhitnitskii sensitivity. Phys Rev Lett (2023) 130:071002. doi:10.1103/PhysRevLett.130.071002

PubMed Abstract | CrossRef Full Text | Google Scholar

12. Zhong L, Al Kenany S, Backes KM, Brubaker BM, Cahn SB, Carosi G, et al. Results from phase 1 of the HAYSTAC microwave cavity axion experiment. Phys Rev D (2018) 97:092001. doi:10.1103/PhysRevD.97.092001

CrossRef Full Text | Google Scholar

13. Choi J, Ahn S, Ko B, Lee S, Semertzidis Y, CAPP-8TB: axion dark matter search experiment around 6.7 μev. Nucl Instrum Methods Phys Res B (2021) 1013:165667. doi:10.1016/j.nima.2021.165667

CrossRef Full Text | Google Scholar

14. Alesini D, Braggio C, Carugno G, Crescini N, D’ Agostino D, Di Gioacchino D, et al. Realization of a high quality factor resonator with hollow dielectric cylinders for axion searches. Nucl Instrum Methods Phys Res B (2020) 985:164641. doi:10.1016/j.nima.2020.164641

CrossRef Full Text | Google Scholar

15. Miceli L, Haloscope axion searches with the cast dipole magnet: the CAST-CAPP/IBS detector. In: 11th Patras Workshop on Axions, WIMPs and WISPs; June, 2015; Zaragoza, Spain (2015). p. 164–8.

Google Scholar

16. Kuo C-L, Symmetrically tuned large-volume conic shell-cavities for axion searches. J Cosmology Astroparticle Phys (2021) 2021:018. doi:10.1088/1475-7516/2021/02/018

CrossRef Full Text | Google Scholar

17. Aja B, Cuendis SA, Arregui I, Artal E, Barreiro RB, Casas FJ, et al. The canfranc axion detection experiment (cadex): search for axions at 90 ghz with kinetic inductance detectors. J Cosmology Astroparticle Phys (2022) 2022:044. doi:10.1088/1475-7516/2022/11/044

CrossRef Full Text | Google Scholar

18. McAllister BT, Quiskamp AP, Tobar ME (2023). Tunable rectangular resonant cavities for axion haloscopes

Google Scholar

19. Braggio C, Carugno G, Di Vora R, Ortolan A, Ruoso G, Seyler D, A tunable clamshell cavity for wavelike dark matter searches. Rev Scientific Instr (2023) 94:045111. doi:10.1063/5.0137621

CrossRef Full Text | Google Scholar

20. Bajjali F, Dornbusch S, Ekmedžić M, Horns D, Kasemann C, Lobanov A, et al. First results from BRASS-p broadband searches for hidden photon dark matter. JCAP (2023) 8:077. doi:10.1088/1475-7516/2023/08/077

CrossRef Full Text | Google Scholar

21. Brun P, Caldwell A, Chevalier L, Dvali G, Freire P, Garutti E, et al. A new experimental approach to probe QCD axion dark matter in the mass range above 40 μeV. Eur Phys J (2019) 79:186. doi:10.1140/epjc/s10052-019-6683-x

CrossRef Full Text | Google Scholar

22. Gelmini GB, Millar AJ, Takhistov V, Vitagliano E, Probing dark photons with plasma haloscopes. Phys Rev D (2020) 102:043003. doi:10.1103/PhysRevD.102.043003

CrossRef Full Text | Google Scholar

23. Knirck S, Hoshino G, Awida MH, Cancelo GI, Di Federico M, Knepper B, et al. First results from a broadband search for dark photon dark matter in the 44 to 52 μeV range with a coaxial dish antenna. Phys Rev Lett (2024) 132:131004. doi:10.1103/PhysRevLett.132.131004

PubMed Abstract | CrossRef Full Text | Google Scholar

24. Álvarez Melcón A, Arguedas-Cuendis S, Cogollos C, Díaz-Morcillo A, Döbrich B, Gallego JD, et al. Axion searches with microwave filters: the RADES project. J Cosmology Astroparticle Phys (2018) 040:040–22. doi:10.1088/1475-7516/2018/05/040

CrossRef Full Text | Google Scholar

25. Álvarez Melcón A, Arguedas-Cuendis S, Cogollos C, Díaz-Morcillo A, Döbrich B, Gallego JD, et al. Scalable haloscopes for axion dark matter detection in the 30 μeV range with RADES. J High Energ Phys (2020) 084:84–28. doi:10.1007/JHEP07(2020)084

CrossRef Full Text | Google Scholar

26. Álvarez Melcón A, Arguedas-Cuendis S, Baier J, Barth K, Bräuninger H, Calatroni S, et al. First results of the CAST-RADES haloscope search for axions at 34.67 μeV. J High Energ Phys (2021) 2021:75. doi:10.1007/JHEP10(2021)075

CrossRef Full Text | Google Scholar

27. Ahyoune S, Álvarez Melcón A, Arguedas Cuendis S, Calatroni S, Cogollos C, Devlin J, et al. A proposal for a low frequency axion search in the 1-2 μeV range and below with the BabyIAXO magnet. Annalen Der Physik (2023) 535:2300326. doi:10.1002/andp.202300326

CrossRef Full Text | Google Scholar

28. Arguedas-Cuendis S, Álvarez Melcón A, Cogollos C, Díaz-Morcillo A, Döbrich B, Gallego JD, et al. The 3 cavity prototypes of RADES: an axion detector using microwave filters at CAST. Microwave Cavities Detectors Axion Res Springer Proc Phys (2020) 245:45–51. doi:10.1007/978-3-030-43761-9_6

CrossRef Full Text | Google Scholar

29. García-Barceló JM, Díaz-Morcillo A, Gimeno B, Enhancing resonant circular-section haloscopes for dark matter axion detection: approaches and limitations in volume expansion. J High Energ Phys (2023) 159. doi:10.1007/JHEP11(2023)

CrossRef Full Text | Google Scholar

30. García Barceló JM, Álvarez Melcón A, Arguedas Cuendis S, Díaz-Morcillo A, Gimeno B, Kanareykin A, et al. On the development of new tuning and inter-coupling techniques using ferroelectric materials in the detection of dark matter axions. IEEE Access (2023) 11:30360–72. doi:10.1109/ACCESS.2023.3260783

CrossRef Full Text | Google Scholar

31. Torrisi G, Leonardi O, Mauro GS, Celona L, Sorbello G, Synthesis of open structures starting from closed-cross-section waveguide devices. IET Microwaves, Antennas and Propagation (2020) 14:1522–9. doi:10.1049/iet-map.2019.0879

CrossRef Full Text | Google Scholar

32. García-Barceló JM, Álvarez Melcón A, Díaz-Morcillo A, Gimeno B, Lozano-Guerrero AJ, Monzó-Cabrera J, et al. Methods and restrictions to increase the volume of resonant rectangular-section haloscopes for detecting dark matter axions. J High Energ Phys (2023) 98:98. doi:10.1007/JHEP08(2023)098

CrossRef Full Text | Google Scholar

33. Computer Simulation Technology (CST). Studio suite software (2023). Available from: Accessed at 25th January 2024.

Google Scholar

34. Golm J, Arguedas Cuendis S, Calatroni S, Cogollos C, Döbrich B, Gallego J, et al. Thin film (high temperature) superconducting radiofrequency cavities for the search of axion dark matter. IEEE Trans Appl Superconductivity (2022) 32:1–5. doi:10.1109/TASC.2022.3147741

CrossRef Full Text | Google Scholar

35. Deulin EA, Mikhailov VP, Panfilov YV, Nevshupa RA, Friction in vacuum. Dordrecht: Springer Netherlands (2010). p. 33–67. doi:10.1007/978-90-481-2520-3_3

CrossRef Full Text | Google Scholar

36. Mathes KN, Dielectric properties of cryogenic liquids. IEEE Trans Electr Insul (1967) EI-2:24–32. doi:10.1109/TEI.1967.298846

CrossRef Full Text | Google Scholar

37. Adair CM, Altenmüller K, Anastassopoulos V, Arguedas Cuendis S, Baier J, Barth K, et al. Search for dark matter axions with CAST-CAPP. Nat Commun (2022) 13:6180. doi:10.1038/s41467-022-33913-6

PubMed Abstract | CrossRef Full Text | Google Scholar

38. Calatroni S, A Mathematica Notebook for the calculation of the anomalous skin effect in copper (2020). Available from: Accessed at 25th January 2024.

Google Scholar

39. Calatroni S, Materials and properties: thermal and electrical characteristics (2020). Available from: Accessed at 25th January 2024.

Google Scholar


Misalignment due to coaxial ports

In this work, an additional misalignment study has been carried out on the haloscope with vertical cut tuning. The results obtained in Section 2.2 are based on a system in which the coaxial ports are screwed to one of the two halves, causing a small misalignment or asymmetry in the total system. In this case, the behaviour of the structure has been analysed in simulation by positioning the coaxial ports centred in the middle of the opening of the structure (gap/2).

In Figure 15 the results obtained in quality factor with a range of openings from gap = 0–2.5 mm are depicted. We can therefore conclude that this misalignment has practically no effect on this parameter and can be ignored in our system.


FIGURE 15. (A) 3D model of the vertical cut structure with gap = 2 mm applying symmetry with the coaxial ports laying in the middle of the gap (centred at gap/2 = 1 mm), and (B) quality factor results from CST simulations for this structure without (blue solid line) and with (red dashed line) centring the coaxial ports.

Misalignment in a long single cavity

In addition, the simulation of an individual cavity with the same dimensions of width, height and total length as the vertical cut multicavity (simply eliminating the inductive irises inside) has been carried out to observe the behaviour in form factor with angular misalignment in the y − axis (this is θy), which is the most relevant effect studied for this parameter [see Figure 6 (top-left corner plot)]. The width of the single cavity is 22.86 mm, the width is 10.16 mm, and the length is 136.36 mm.

Applying a misalignment of θy = 0o to 0.6o, a range of detriment form factor values from 0.659 to 0.634 was obtained, confirming that the effect is not high for individual cavities. Thus, we can conclude that the low form factor results obtained for the vertical cut haloscope with angular y − axis misalignment are due to the asynchrony of the individual frequencies of the subcavities of which it is composed.

Keywords: axion, haloscope, tuning, cryogenics, dark matter

Citation: Golm J, García-Barcelo JM, Arguedas Cuendis S, Calatroni S, Wuensch W and Dobrich B (2024) Split-cavity tuning of a rectangular axion haloscope operating around 8.4 GHz. Front. Phys. 12:1372846. doi: 10.3389/fphy.2024.1372846

Received: 18 January 2024; Accepted: 09 April 2024;
Published: 07 May 2024.

Edited by:

Yannis K. Semertzidis, Institute for Basic Science, Republic of Korea

Reviewed by:

Gu Chen, Guangzhou University, China
Giuseppe Torrisi, Laboratori Nazionali del Sud (INFN), Italy
SungWoo Youn, Institute for Basic Science (IBS), Republic of Korea

Copyright © 2024 Golm, García-Barcelo, Arguedas Cuendis, Calatroni, Wuensch and Dobrich. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

*Correspondence: Jessica Golm,; Jose María García-Barcelo,

Disclaimer: All claims expressed in this article are solely those of the authors and do not necessarily represent those of their affiliated organizations, or those of the publisher, the editors and the reviewers. Any product that may be evaluated in this article or claim that may be made by its manufacturer is not guaranteed or endorsed by the publisher.