Studying gaugino masses in supersymmetric model at future 100 TeV $pp$ collider

We discuss prospects of studying supersymmetric model at future $pp$ circular collider (FCC) with its centre-of-mass energy of $\sim 100\ {\rm TeV}$. We pay particular attention to the model in which Wino is lighter than other supersymmetric particles and all the gauginos are within the kinematical reach of the FCC, which is the case in a large class of so-called pure gravity mediation model based on anomaly mediated supersymmetry breaking. In such a class of model, charged Wino becomes long-lived with its decay length of $\sim 6\ {\rm cm}$, and the charged Wino tracks may be identified in particular by the inner pixel detector; the charged Wino tracks can be used not only for the discrimination of standard model backgrounds but also for the event reconstructions. We show that precise determinations of the Bino, Wino, and gluino masses are possible at the FCC. For such measurements, information about the charged Wino tracks, including the one about the velocity of the charged Wino using the time of the hit at the pixel detector, is crucial. With the measurements of the gaugino masses in the pure gravity mediation model, we have an access to more fundamental parameters like the gravitino mass.


Introduction
There are strong motivations to consider physics beyond the standard model (BSM) at TeV scale. One is dark matter that cannot be explained in the framework of the standard model; particularly, the scenario of thermal relic dark matter requires the annihilation cross section of the dark matter particle to be ∼ 1 pb, which is the typical cross section for particles with the mass scale ∼ 0.1-1 TeV. In addition, a large hierarchy between the electroweak scale and the Planck scale, i.e. the scale of the gravity, motivates us to consider some mechanism to relax the quadratic divergence in the Higgs mass parameter in the standard model.
High-energy-collider experiments are crucial for the study of BSM physics. LHC experiments have been searching for the BSM particles as an energy-frontier, but no direct sign has been discovered yet. Although LHC experiments will keep on exploring BSM particles at higher mass scale, BSM particles may be just above the discovery reach of the LHC. In this case, a collider with higher energy than the LHC is needed to discover and study the BSM physics. Among possibilities, we consider pp option of Future Circular Collider (FCC) with the centre-of-mass energy of ∼ 100 TeV [1][2][3] because it can drastically push up the energy frontier of high-energy experiments. Because the FCC is considered to be one of promising collider experiments, the understanding of the physics potential of the FCC is of high importance.
Here, we discuss the prospect of the FCC in the study of supersymmetric (SUSY) model. We concentrate on the so-called pure gravity mediation (PGM) model of SUSY breaking [4][5][6], which is strongly motivated from theoretical and phenomenological points of view. As we will discuss in the next section, in the PGM model, scalar particles in the minimal SUSY standard model (MSSM) have masses of O(100) TeV and may be too heavy to be studied at the FCC. However, gaugino masses are generated by the anomaly mediation [7,8] and are loop suppressed relative to the scalar masses. Typically, the gauginos are at the TeV scale and are within the reach of the FCC. Such a spectrum is easily obtained by a simple set up of the SUSY breaking sector. In addition, the PGM model has several advantages in cosmology. In particular, a thermally produced lightest superparticle (LSP) can be a viable candidate of dark matter under the assumption of R-parity conservation [9].
One important feature of the model of our interest, the PGM model, is that the Winos, which are the gauginos for SU (2) L gauge group, are likely to be lighter than other superparticles. In particular, due to the radiative correction, the neutral WinoW 0 is slightly lighter than charged onesW ± [10,11] and hence is the LSP. With such a mass spectrum, charged Wino has a relatively long lifetime and, once produced at the FCC, it may fly a macroscopic distance of ∼ 10 cm before its decay. The track of such a "long-lived" charged Wino may be identified by the inner pixel detector of the FCC, which provides a very characteristic and unique signal of the PGM model. The charged Wino tracks expected in the PGM model can be used not only for the discovery but also for the study of the properties of SUSY particles.
In this paper, we discuss the prospect of the study of SUSY particles at the FCC, paying particular attention to the PGM model of SUSY breaking. We mainly focus on a parameter region where all the gauginos, i.e, Bino, Winos, and gluino, are within the reach of the FCC, assuming that its centre-of-mass energy is 100 TeV. We propose procedures to measure Wino, Bino, and gluino masses at the FCC, using the pair production process of gluinos, pp →gg, and the pair production process of charged Winos associated with hard jets, pp →W +W − + jets. We show that information about the charged Wino tracks from the inner pixel detector is crucial not only for the background reduction but also for the reconstruction of SUSY events. We also point out that, for the gaugino mass determination, it is important to precisely determine the velocity of charged Wino, which is expected to be possible by using the time information available from the pixel detector.
The organization of this paper is as follows. In section 2, we introduce the PGM model and introduce several Sample Points for our Monte Carlo (MC) analysis. In section 3, we explain basic features of the SUSY events at the FCC. The results of the MC analysis for the gaugino mass determinations are shown in section 4. Implications of the gaugino mass determinations for the understanding of the underlying theory are discussed in section 5. Section 6 is devoted to conclusions and discussions.

Model
Let us first introduce the SUSY model we consider. Among various possibilities, we concentrate on the so-called pure gravity mediation (PGM) model of SUSY breaking [4][5][6] based on anomaly mediation [7,8]. In this model, the sfermion and Higgsino masses are generated by (tree-level) Planck-suppressed operators and are of the order of the gravitino mass m 3/2 . On the contrary, assuming that there is no singlet field in the SUSY breaking hidden sector so that tree-level gaugino masses in the MSSM sector are forbidden, the gaugino masses are obtained from the effect of anomaly mediation. In this model, the gaugino masses are one-loop suppressed compared to the gravitino mass. Then, the gauginos are relatively light and are the primary targets of collider experiments.
In the PGM model, the SUSY breaking gaugino mass parameters for U (1) Y , SU (2) L , and SU (3) C gauge interactions, denoted as M 1 , M 2 , and M 3 , respectively, are given as where g 1 , g 2 , and g 3 are gauge-coupling constants of U (1) Y , SU (2) L , and SU (3) C gauge interactions, respectively. Here, L denotes the effect of the threshold correction due to the Higgs and Higgsino loop and is given by where µ and m A are the SUSY invariant Higgs mass and the pseudo-scalar Higgs mass, respectively, while β being the angle parametrizing the relative sizes of vacuum expectation values of up-and down-type Higgses. In addition, M S is the mass scale of sfermions and Higgsinos, and hence M S ∼ m 3/2 . Here and hereafter, we take the convention such that m 3/2 is real and positive. We use the MS scheme for the calculation of gauge coupling constants and mass parameters. In general, M 1 , M 2 , and M 3 are complex and depend on the renormalization scale. The gaugino masses (i.e. mass eigenvalues) are determined from M 1 , M 2 , and M 3 at the renormalization scale close to the mass eigenvalues. The mass eigenvalues of Bino, Wino, and gluino, which are real and positive, are denoted as mB, mW , and mg, respectively. 1 We take into account the one-loop threshold correction to the gluino mass [12] where M G is the mass scale of gauginos, which we determine by solving M G = |M 3 (M G )| in our analysis. In addition, we neglect the small threshold corrections to Bino and Wino at the gaugino mass scale and just take mB = |M 1 (M G )| and mW = |M 2 (M G )|. When m 3/2 and L are of the same order of magnitude, Wino becomes lighter than Bino and gluino. 1 Because the Higgsino mass is much larger than the gaugino masses, the mixings between gauginos and Higgsinos are not important in the present case, and we regard Bino and Wino as mass eigenstates. In addition, as we will discuss, the masses of charged and neutral Winos are slightly different but their difference is much smaller than the expected accuracy of the Wino mass determination at the FCC. Thus, we neglect the mass difference unless it is important.
In our analysis, we consider the case where the gravitino mass is of O(100) TeV (and hence the sfermion and Higgsino masses are), while the gaugino masses are of O(1) TeV. Such a mass spectrum is phenomenologically viable and well-motivated: • The observed value of the Higgs mass (i.e. m h ≃ 125 GeV [13]) can be realized due to radiative corrections [14][15][16][17][18].
• Neutral Wino is a viable candidate of dark matter. In particular, if mW ≃ 2.9 TeV, thermal relic density of Wino becomes equal to the present dark matter density [19]. In addition, even if the Wino mass is smaller than ∼ 2.9 TeV, Wino dark matter is possible with non-thermal production [8,20].
• With the large gravitino mass of O(100) TeV, a dangerous cosmological gravitino problem can be avoided even if the reheating temperature after inflation is as high as O(10 9 ) GeV [21]. A simple scenario of leptogenesis [22] works with such reheating temperature [23,24].
• Even if the sfermion and Higgsino masses are as high as O(100) TeV, the gauge coupling constants still meet at ∼ 10 16 GeV, and the SUSY grand unified theory, which is one of the strong motivations to consider SUSY models, is still viable [12].
• Because of large sfermion masses, CP and flavour violations due to the loops of SUSY particles are suppressed. This will significantly relax the SUSY CP and flavour problems [25,26].
Because the neutralino dark matter is one of the strong motivations of low-energy SUSY, we consider the case that the Wino becomes lighter than the Bino and gluino so that neutral Wino becomes the candidate of dark matter. (Notice that, in the present framework, the Bino hardly becomes a viable candidate of dark matter even if it is the LSP. This is because, with heavy sfermions and Higgsinos, its pair annihilation cross section is too small to realize the correct relic density to be dark matter.) In particular, we assume that the Wino mass is ∼ 2.9 TeV so that the thermal relic density of Wino becomes consistent with the present dark matter density. In the following, we adopt several Sample Points for our MC analysis. The mass spectrum and fundamental parameters are summarized in table 1. As shown in table 1, mW < mB < mg in all Sample Points.
Assuming R-parity conservation, gluino decays as where q andq denote the standard-model quark and anti-quark, respectively. The branching ratio for each decay mode depends on the mass spectrum of sfermions. For simplicity, we assume that Br (g →qqB) = Br (g →qq (′)W ) = 0.5, 7.9 2.7 1.0 Table 1: Fundamental parameters (m 3/2 and L), gaugino masses, and the gluino pair production cross section (for the centre-of-mass of 100 TeV), for Sample Points 1, 2, and 3.
and that the decay process is flavour universal. The dominant decay modes of Bino are given byB The masses of charged and neutral Winos split after the electroweak symmetry breaking. When |µ| is much larger than the electroweak scale, which is the case in the present framework, the mass splitting is dominantly via radiative correction due to loop diagrams with electroweak gauge bosons [10,11], and the neutral Wino becomes lighter than the charged one. Based on the two-loop calculation, the mass splitting is δmW ≃ 165 MeV [27]; then charged Wino dominantly decays asW ± →W 0 π ± with cτW ± ≃ 5.75 cm, where τW ± is the proper lifetime of charged Wino while c is the speed of light.

SUSY events at the FCC
In this section, we discuss important features of SUSY events at the FCC which are used for our analysis. In the sample points of our choice, gluino is within the kinematical reach of the FCC, and its pair production process is the primary target. Hereafter, we consider the pair production process of gluinos, pp →gg, and the pair production process of charged Winos associated with a high-p T jet, pp →W +W − + jets. From these processes we extract information about the gaugino masses as we discuss in the following.

Background estimation
In order to eliminate standard-model backgrounds, we use the fact that charged Wino tracks, which are disappearing and high-p T , may be recognized by the inner pixel detector.
In the gluino pair production events, each gluino decays down to a charged or neutral Wino. Although charged Wino is unstable, it has a sizeable lifetime and its cτW ± is about 5.75 cm that is of the same order of the distance to the pixel detector from the interaction point. Thus, once a charged Wino is produced, it may hit several layers of the pixel detector before its decay into a neutral Wino and a pion. Charged Wino track is expected to be (i) short (i.e. disappearing in the tracker), and (ii) high-p T ; such a track is hardly realized by a single standard-model particle. Another source of fake Wino-like track is due to an accidental alignment of hits of particles mainly from pile-ups and it is the dominant source according to ref. [28]. In addition, in the signal events (i.e. the gluino pair production events), the missing transverse momentum evaluated only from jets is likely to be large because of the momenta carried away by Winos; this is not expected in the background events that have fake Wino-like tracks. The gaugino mass reconstruction in our analysis is based on the events satisfying the following requirements: • Requirement 1: There is a "long enough" Wino-like track. The transverse length of the track, denoted as L T,1 , should be longer than L (min) T,1 = 10 cm. In addition, the pseudo-rapidity (η) of the track is required to be |η| < 1.5.
• Requirement 2: There is another "long enough" Wino-like track. The transverse length of the track, denoted as L T,2 should be longer than L (min) T,2 . As we will discuss later, L (min) T,2 is set to be 10 cm but results with L (min) T,2 = 5 cm are also shown to see how the event selection affects on the mass determination. In addition, the pseudo-rapidity of the track is required to be |η| < 1.5.
• Requirement 3: The missing transverse momentum should be larger than 1 TeV.
We use signal events in which the decay chain of each gluino contains a charged Wino. We assume that the charged Wino with a longer (shorter) transverse flight length in an event can be fully identified when the transverse flight length is longer than L T,2 ). According to ref. [28], the probability to have one fake disappearing track in the pseudorapidity range of |η| < 1.5 is about 2×10 −5 per bunch crossing, requiring hits in five pixel layers for a particular setup of the FCC experiment. The background rate can be reduced therefore by ten orders of magnitude by requiring both Requirement 1 and Requirement 2. Additionally, the Requirement 3 can also reduce them as well. As a result, standard-model backgrounds can be negligible by applying these requirements.

Wino velocity measurement
We assume that the information about the velocity of the charged Wino will be available if the flight length is long enough. It may be possible that each pixel layer determines the time of the hit with the resolution of O(10) ps by utilizing, for example, low-gain avalanche detectors [29,30], with which the velocity relative to the speed of light (β) of the charged Wino could be determined with the accuracy of O(1) %. We estimate the expected accuracy of the β measurement via a simple MC analysis. We generate straight tracks, and smear the time of hits at each pixel-detector layers to determine the "observed" times of hits. The time of the pp collision (which can be identified as the time when Winos are produced) is assumed to be accurately determined by using associated jets. Then, the observed β is determined for each track by fitting the observed times of hits by a linear function assuming a constant β. The accuracy is estimated as the standard deviation of the distribution of the difference between the observed and the generator-level velocities as a function of the generator-level β. Then the average accuracy for Wino tracks is estimated by taking the weighted average using the generator-level β distribution in our Wino samples. We found that, assuming the hit-level time resolution of 20 ps (40 ps), the Wino velocity can be determined with the accuracy of 3.0 % and 3.3 % (6.1 % and 6.8 %) for charged Winos reaching the pixel layer located at the transverse length of 10 cm with β < 0.8 and 0.9, respectively. We require that the transverse flight length should be longer than 10 cm for the β measurement, and assume that the resolution of the observed Wino β is 6 %.

MC simulation
The flowchart of our MC analysis is shown in figure 1. We use MadGraph5_aMC@NLO (v2.6.3.2) [31,32] to generate pp →gg and pp →W +W − + jets events. Then, decay and hadronization processes are taken care of by PYTHIA8 [33]. A fast detector simulation is performed by Delphes (v3.4.1) [34]; we use the card FCChh.tcl included in the package. Because the velocity measurement of charged Wino cannot be simulated by the Delphes package by default, the information about Winos provided by PYTHIA8, as well as Delphes outputs, are passed to our original analysis code; the analysis code smears the velocities of charged Winos to determine observed velocities, applies kinematical cuts, reconstructs kinematical variables (including invariant masses that will be discussed in the following), and performs the hemisphere analysis. In particular, for charged Winos whose transverse flight length L T is longer than 10 cm, the observed value of the Wino velocity is determined by 2 where β and β (true) are observed and true values of the velocity, and Z is the (0, 1) Gaussian random variable. An accurate velocity determination may be difficult for charged Winos with a short transverse flight length, for example, L T < 10 cm; thus Winos with L T < 10 cm are not used in the mass determination. The fittings of invariant-mass distributions are performed by ROOT (v6.14) [35].

Gaugino mass determination
Now we are at the position of discussing how and how well we can determine the gaugino masses. In order to demonstrate that the gaugino mass determinations are possible, we generate pp →gg and pp →W +W − + jets events. Then, we study the reconstructions of gaugino masses using data sets which correspond to multiple experiments with a fixed integrated luminosity L for each experiment. As for pp →gg process, we take L = 10 ab −1 for Sample Points 1 and 2, while L = 30 ab −1 for Sample Point 3. For pp →W +W − + jets process, we take L = 30 ab −1 .

Wino mass determination
We first consider the measurement of the Wino mass. Using charged Winos identified as short high-p T tracks with velocity information, we may determine Wino mass if the momentum of the Winos are known. Even though the curvature of the track depends on the Wino momentum, most of the Winos are so high-p T that precise determination of the curvature is expected to be unlikely.
Instead of using the curvature information, we use the conservation of the transverse momentum to determine the Wino momenta. Because we use events with two charged Wino tracks, the directions of the Wino momenta (which we denote nW ± 1 and nW ± 2 ) are known. Then, the momenta of charged Winos, PW ± I with I = 1 and 2, are given in the following form: with c I being constants. The constants c 1 and c 2 can be obtained by using the transverse momentum conservation. Concentrating on events in which the decay products of gluinos contain only hadrons and Winos, the following relation should be held: where the subscript T denotes transverse components. In our analysis, we use Eq. (4.2) to calculate c 1 and c 2 , with which Wino momenta are determined. With PW ± I being given, the reconstructed Wino mass (in association with each track) is given by  where β I is the measured velocity of the I-th charged Wino.
In order to see how well the Wino mass can be reconstructed, we study the distribution of m (rec) W . For the Wino mass determination utilizing the above procedure, charged Wino samples with smaller uncertainties in the boost factor are necessary; this motivates us to use charged Winos with relatively low velocity. In addition, because the "missing" momentum evaluated using the jet momenta is assumed to be compensated by the Wino momenta, events with neutrino emission should be excluded in this study. Thus, we do not use events with an isolated lepton 3 because it may originate from the decay of W -boson. Thus, for the Wino mass determination, we use the events satisfying the following conditions (as well as Requirements 1, 2 and 3 in the previous section): (1a) There exists a charged Wino with L T > 10 cm and β < 0.8.
We calculate the reconstructed Wino mass m (rec) W for all the charged Winos satisfying (1a). In figures 2, 3, and 4, we show the distribution of the reconstructed Wino mass for Sample Points 1, 2, and 3, respectively, where not only L (min) T,2 = 10 cm but also 5 cm cases are shown as explained before. As mentioned earlier, the Wino with L (min) T,2 = 5 cm is not used for the mass determination; it is used to show impact on the mass determination from altering the event selections. This is also the case for Bino and gluino. For Sample Points 1 and 2 (Sample Point 3), we take the integrated luminosity L of 10 ab −1 (30 ab −1 ). The peak of the distribution is close to the true Wino mass. In order to determine the position      2925  2903  2881  2913  2899  2882  δmW  61  108  92  38 63 57 Table 2: The mean of the peak position based on 100 data sets of pp →gg events for each Sample Point, denoted as mW 100 , as well as the uncertainty in the Wino mass determination (in units of GeV).
of the peak, we use a fitting function in the form of a Gaussian function plus a constant: wherem, σ, A, and C are fitting parameters. In each figure, the fitting function with the best-fit parameters is shown in the red line. The best-fit value ofm, denoted as Mwno(Gauss), is also shown in each figure.
We expect to extract information about the Wino mass from the position of the Gaussian peak (i.e. the peak of the fitting function). The position of the peak may not exactly agree with the true Wino mass even with large enough statistics. We expect that this is due to our choice of the fitting function given in eq. (4.4), and that we may find a better fitting function without such a systematic effect. The detailed study of the fitting function is beyond the scope of this paper, and we simply assume that the relation between characteristic features of the fitting function (like the position of the peak) and the true mass can be well understood by, for example, a reliable MC analysis. In addition, as indicated in the figures, the statistical uncertainty in the measurement of the Wino mass is accounted for. Here, we evaluate the statistical uncertainty by using 100 independent data sets for each Sample Point; we determine the position of the Gaussian peak for each data set, and the standard deviation of the peak position is regarded as the statistical uncertainty in the Wino mass determination. The statistical uncertainty as well as the mean of the peak position based on 100 data sets are summarized in table 2.
So far, we have only considered the pp →gg process to determine the Wino mass. However, if gluino is so heavy that the cross section for the gluino pair production is significantly suppressed, it may be more efficient to use the electroweak production of charged Winos. In particular, the process pp →W +W − + jets may be used for the Wino mass determination, where a large missing transverse momentum is necessary to determine the Wino momenta as well as to pass the trigger selection. Here, we study such a possibility assuming that mW = 2.9 TeV and that the gluino is out of kinematical reach of the FCC. With this choice of the Wino mass, we performed the MC simulation of the processes up to two hard jets and obtained σ(pp →W +W − + jets) ≃ 0.15 fb for the missing transverse momentum larger than 1 TeV. As for the event selection, we require the same requirements as the previous analysis, i.e. Requirements 1, 2, and 3 in the previous section and conditions (1a) and (1b) in this section. We assume that standard-model backgrounds do not exist after    Table 3: The mean of the peak position based on 100 data sets pp →W +W − + jets events, denoted as mW 100 , as well as the uncertainty in the Wino mass determination (in units of GeV).
requiring two (long enough) charged Wino tracks. Then, we determine the reconstructed Wino mass using eq. (4.3) for each Wino track.
In figure 5, we show the distribution of the reconstructed Wino mass, taking the integrated luminosity L of 30 ab −1 . We can see that, with L ∼ 30 ab −1 , we may observe a peak close to the true Wino mass. We also perform a fit using the fitting function given in eq. (4.4). From the figure, one can see the statistical uncertainty in the fit and the difference between the true Wino mass and the position of the Gaussian peak. Although the difference is larger than in the case of pp →gg events, we again assume that the dependence of the position of the peak on the true mass can be well understood by a reliable MC analysis and so on. Under this assumption, we evaluate the statistical uncertainty with 100 independent event sets as we described before and summarize the result in table 3.

Bino mass determination
Next, we consider the Bino mass determination. Here, we use the decay modeB →W ± W ∓ , which has a sizeable branching ratio in the present case. Assuming that the Wino mass is known (see the previous subsection), the Wino four-momentum can be determined by using the velocity information (or by the conservation of the transverse momentum). Thus, we may reconstruct the Bino mass by calculating the invariant mass of theW ± plus W -boson system, if the decay products of the W -boson are identified.
For this purpose, we use the fact that the W -boson produced by the Bino decay may be highly boosted. The hadronic decay products of the boosted W -boson may result in a single fat jet with the jet mass m j close to the W -boson mass. In figure 6, we show the distribution of the jet mass for Sample Point 1 after applying Requirements 1, 2 and 3 and (2a) (see below). We can observe a peak at m j ∼ m W . Thus, if we require m j ∼ m W , we can obtain W -rich samples of jets. Using such a jet, with denoting its four-momentum as p j , the reconstructed Bino mass is defined as where uW is the four-velocity of the charged Wino:  Among the events with two charged Wino tracks (i.e. events that meet Requirements 1, 2, and 3 in the previous section), those satisfying the followings are used for the Bino mass reconstruction: 5 (2a) There exists a charged Wino with L T > 10 cm and β < 0.9. (In order to increase the number of samples, we adopt a larger value of the maximal velocity compared to the Wino mass determination.) (2b) There exists a fat jet with 70 GeV < m j < 90 GeV, with m j being the jet mass. We call such a jet as "W -jet." We calculate the reconstructed Bino mass given in eq. (4.5) for all the pairs of a charged Wino satisfying (2a) and a W -jet satisfying (2b). In figures 7 -9, we show the distribution of the reconstructed Bino mass for Sample Points 1 -3, respectively. Here, the true value of the Wino mass is used for the calculation of the four-momenta of charged Winos. We can see that, in each figure, the peak of the histogram is close to the true Bino mass and hence the Bino mass determination is possible via the method using the charged Wino track and the W -jet. We use the fitting function given in eq. (4.4) to estimate the position of the peak. The fitting function with the best-fit parameters is shown in the red line. For each Sample Point, the best-fit value of the position of the Gaussian peak (denoted as Mbno(Gauss)) and its statistical uncertainty are shown in the figure.        in quadrature.
There exist several sources of uncertainties in the reconstructed Bino mass. We observe a slight deviation of the position of the Gaussian peak from the true Bino mass. We found that the position of the peak of the fitting function is likely to be lower than the true Bino mass with the present choice of cut parameters. Such a systematic effect in the fitting is assumed to be corrected by, for example, a reliable MC analysis, and hence is not included in the estimation of the uncertainty in the Bino mass measurement. The position of the Gaussian peak should also have a statistical uncertainty. As in the case of the Wino mass determination, the statistical uncertainty (denoted as δm ) is determined by using 100 independent data sets for each Sample Point. Furthermore, so far, we have used the true Wino mass as an input for the analysis. As we discussed in the previous subsection, the Wino mass is also a parameter that should be experimentally determined, and the uncertainty in the measured Wino mass becomes a source of the uncertainty in the reconstructed Bino mass. In order to see how large such an effect is, we estimate the change of the reconstructed Bino mass with respect to the change of the input Wino mass. With varying the input Wino mass by 100 GeV, we found that the reconstructed Bino mass changes by ∼ 100 GeV. Thus, we take δm is the uncertainty associated with Wino mass uncertainty δmW in the reconstructed Bino mass. We add all the uncertainties in quadrature to estimate the expected accuracy of the Bino mass measurement. The uncertainties in the Bino mass reconstruction, as well as the mean of the peak position based on 100 data sets, are summarized in table 4.

Gluino mass reconstruction
The last subject is the gluino mass reconstruction. We consider the gluino pair production and use the hemisphere analysis to separate the decay products of one gluino from those of the other. The invariant mass of each hemisphere is regarded as the reconstructed gluino mass. We need to determine the Wino momenta by using the conservation of the transverse momentum (see eq. (4.2)). Thus, we should use events in which all the decay products of gluinos are detected. In order to eliminate events which might contain neutrino emission, we do not use events containing isolated leptons. We use the events that satisfy the next condition: (3a) There is no isolated lepton.
In the hemisphere analysis for the gluino mass reconstruction, two charged WinosW ± 1,2 and high-p T jets are assigned to one of two hemispheres, H 1 or H 2 . The assignment is performed as follows: 1. Two charged Winos are assigned to different hemispheres: 2. For each high-p T jet j with |η| < 2 (with η being pseudo-rapidity of the jet), where p j = (E j , p j ) is the four-momentum of j, and p H I = (E H I , p H I ) is the fourmomentum of the I-th hemisphere that is defined as The function d(p H , p j ) is given by with θ Hj being the angle between p H and p j [37].
3. Jets with |η| > 2 are not used for the analysis.
In our MC analysis, we determine the hemispheres by iteration. In the first step of the iteration, we take p H I = PW ± I , and all the high-p T jets are merged to one of the hemispheres which gives smaller d(p H I , p j ). Then, after the first step, we use Eq. (4.9) and repeat the iteration with re-calculating p H I . Compared to models in which particles responsible for the missing momentum are totally invisible, the hemisphere analysis in the present model is easier. This is because the momentum information of all the final state particles is available after reconstructing the Wino momenta. Once the hemispheres are determined, the reconstructed gluino mass for each hemisphere is defined as In figures 10 -12, we show the distribution of the reconstructed gluino mass; in the figures, the true Wino mass is used to determine the four-momenta of Winos.
We can see that the position of the Gaussian peak may have a sizeable deviation from the true gluino mass, although the position of the peak has a positive correlation with the true gluino mass. The deviation is partly a systematic effect due to our choices of the fitting       function and cut parameters. Such a systematic effect is assumed to be understood well so that it does not affect the accuracy of the observed gluino mass. The statistical uncertainty, δm (stat) g , is estimated by using 100 independent set of events for each Sample Point. Another source of the error in the gluino mass reconstruction is the Wino mass. In our procedure of determining the gluino mass, the Wino mass is needed as an input parameter to determine the four-momenta of charged Winos. In order to estimate the effect of the Wino mass uncertainty, we vary the input Wino mass by 100 GeV and find that the reconstructed gluino mass changes by ∼ 100 GeV. Thus, the uncertainty in the reconstructed gluino mass due to the Wino mass uncertainty is estimated to be δm (mW ) g ∼ δmW . Adding the uncertainties in quadrature, we estimate the expected accuracy of the gluino mass determination; in table 5, we summarize the uncertainties in the gluino mass reconstruction, as well as the mean of the peak position based on the analysis with 100 independent data sets for each Sample Point.

Implications
Let us discuss the implications of the gaugino mass determination. In the PGM model, the gaugino masses depend on the following three fundamental parameters: Thus, by checking if the gaugino masses obey the above relation, it provides a test of the PGM model. Simultaneously, with the gaugino mass measurements, m 3/2 , |L|, and φ L can be determined.
Here, we consider how well we can test the PGM prediction and how well we can determine fundamental parameters. For this purpose, we consider the parameter region consistent with observed gaugino masses, adopting Sample Point 1 as an example. To begin with, we plot contours of constant gaugino masses on the |L| vs. φ L plane in figure  13, with fixing m 3/2 = 250 GeV (i.e. the true value of the gravitino mass); the dotted lines are contours of true Bino and Wino masses, while the bands show the expected uncertainties given in tables 2 and 4. Notice that the gluino mass is independent of |L| and φ L , and is 6 TeV for m 3/2 = 250 GeV. We can estimate the uncertainties in the determination of these two parameters as δ|L| ∼ 25 TeV and δφ L ∼ π/5. 6 In figures 14 and 15, we also show the contours of constant gaugino masses on the |L| vs. m 3/2 plane and the m 3/2 vs. φ L plane, respectively. In each figure, the remaining parameter (φ L or |L|) is fixed to its input value; the dotted lines show the contours of true gaugino masses, while the bands stand for the expected uncertainty due to the uncertainties in the gaugino mass determination. Particularly from the gluino mass information, we can see that the gravitino mass m 3/2 can be determined with the accuracy of δm 3/2 ∼ 5 TeV.
Once |L| is determined, it will provide information about the masses of heavier MSSM particles. One of the important purposes of high energy colliders is to understand the mass scales of unknown particles; determination of |L| gives information about the mass scales of Higgsinos and heavy Higgses. From eq. (2.4), we can see that |L| depends on |µ|, m A , and tan β. In the PGM model, the masses of the Higgsinos and heavy Higgses are expected to be of the same order of magnitude, and hence information about |L| gives a good estimate of their mass scale as |µ| ∼ m A ∼ |L|/ sin 2β. More precisely, we may estimate an upper bound on the mass scale below which Higgisnos or heavy Higgses, whichever lighter, should exist. Such an upper bound depends on the hierarchy between |µ| and m A parameterized by where we consider the case of x min ≤ 1.
In figure 16, we plot min(|µ|, m A ) taking the input value of |L| (= 800 TeV) of Sample Point 1. Here, we take x min = 0.1, 0.3, and 1. The upper bound on the mass scale of Higgsinos and heavy Higgses becomes larger for a larger value of tan β. We comment here that tan β is also correlated with the sfermion mass scale M S (in particular that of stops) 6 Strictly speaking, there is a correlation among errors of gaugino mass determinations (see δm  through the observed value of the Higgs mass. At the sfermion mass scale, the Higgs quartic coupling λ is determined as [39,40] where δλ denotes the threshold correction from sfermions and Higgsinos. After taking into account the renormalization group effects, the value of λ at the electroweak scale determines the Higgs mass [41]. In figure 16, we also show M S as a function of tan β to realize the observed Higgs mass of m h = 125.18 GeV [13]. As is well known, M S becomes larger as tan β becomes smaller; this is due to the cancellation between the tan β dependence of the treelevel contribution to λ and the renormalization group effect on λ. Resultantly, |L|/ sin 2β and M S have opposite correlation with tan β. Then, two lines in figure 16 intersect with each other at the mass scale ∼ 10 3 TeV. This implies that, with the determination of |L|, we will acquire the mass scale below or at which a new particle (i.e. Higgsinos, heavy Higgs bosons, or sfermions) should exist. Notice that, since the qualitative behaviours of these two lines always hold, such a mass scale can be always acquired with the determination of |L|.

Conclusions and discussion
In this paper, we have discussed a prospect of the study of a SUSY model at the FCC. We have concentrated on the so-called PGM model of SUSY breaking, in which scalars in the MSSM sector have masses of O(100) TeV while gauginos are within the kinematical reach of the FCC, and have studied the SUSY signals at the FCC. We have paid particular attention to the case where Wino is lighter than other gauginos and neutral Wino is the LSP. In such a case, the charged Wino has its lifetime of cτW ± ≃ 5.75 cm and can give unique disappearing tracks in the inner pixel detector. The charged Wino tracks can be used not only for the reduction of standard-model backgrounds but also for the reconstruction of SUSY events.
In the model of our interest, gauginos are the only SUSY particles that are accessible with the FCC. We have proposed procedures to determine their masses.
• Once two charged Wino tracks are identified, the Wino mass can be determined by combining velocity and momentum information of each Wino; here, the velocity can be determined by using the time information from the pixel detector while the momentum of the Wino is determined by using the conservation of the transverse momentum.
• The Bino mass can be determined by using the fact that the decay processB → W ± W ∓ has sizeable branching ratio. In particular, at the FCC, the W -boson produced by the Bino decay can be highly boosted, and hence hadrons from the decay of W -boson may result in a single fat jet with the jet mass close to the W -boson mass.
Studying the invariant mass of the system consisting of a charged Wino (observed as a disappearing track) and a fat W -jet, information about the Bino mass can be obtained.
• For the gluino mass determination, we use the fact that, requiring two charged Wino tracks in the event, we can observe all the decay products of gluinos, i.e. charged Winos and jets, assuming that all the decay products of gluinos are hadrons and Winos. We have discussed the possibility to determine the gluino mass using the hemisphere analysis to recombine decay products of each gluino. A distribution of the invariant masses of hemispheres gives information about the gluino mass.
We emphasize here that there are several assumptions made in this paper. Charged Wino tracks can be reconstructed with high efficiency, even though the transverse flight length is as short as ∼ 10 cm. The velocity of charged Wino can be determined with the accuracy of O(1) %, which depends on the hit-level time resolution of the pixel detector. For the background, we consider only fake disappearing tracks because they are expected to be dominant in high pile-up conditions, but it should be kept in mind that physical background due to particle scattering also exists to some extent. The gaugino mass determination will be affected by contributions from additional energies deposited in jets such as pileups, but such contributions could be sufficiently suppressed by using pile-up mitigation techniques, as indicated in ref. [42]. The event selections that we have used in this paper are sufficient to characterize the properties of signal events while they might need to be altered if more realistic background is considered. All these conditions may affect the gaugino mass determination, and the details in realistic situation will be studied in the future.
Once three gaugino masses are known, the result can be used to understand the underlying theory of SUSY breaking and to reconstruct fundamental parameters behind the gaugino masses. In the PGM model of our interest, gaugino masses depend on three parameters, i.e.,m 3/2 , |L|, and φ L . Even though there are three free parameters for three gaugino masses, there exists a non-trivial constraint as shown in eq. (5.2). Thus, by checking if the observed gaugino masses are in agreement with the PGM relation, we can test the PGM model as a model of SUSY breaking. Simultaneously, we can determine the fundamental parameters m 3/2 , |L|, and φ L . In particular, with the determination of |L|, information about the masses of Higgsinos and heavy Higgses are obtained (see eq (2.4)). Furthermore, understanding of the gravitino mass m 3/2 will shed light on the mechanism of SUSY breaking. Determination of the gravitino mass has implications also for cosmology. For example, once the gravitino mass is known, an upper bound on the reheating temperature after inflation can be precisely determined in order not to spoil the success of big-bang nucleosynthesis. For the understanding of the thermal history of the universe, such an upper bound gives very important information.
In summary, we have demonstrated that the FCC can play crucial roles in the understanding of physics beyond the standard model. We have considered only the PGM model of SUSY breaking, and the importance of the FCC will become clearer with the studies of other cases.