We have performed a detailed analysis of such a CubeSat mission (“Q3Sat”), finding that cost and complexity can be reduced by sending the photons from ground to satellite, i.e. using an uplink. Calculations have been done for a prepare-and- send protocol (BB84 with decoy pulses) using polarization as information carrier. We have created a preliminary design of a 3U CubeSat including a detailed size, weight and power budget and a CAD to account for the assembly of the components. Deploying a 10 cm long mirror telescope covering the small surface of the satellite leaves enough space for a polarization analysis module and housekeeping, communication and computing electronics.
For one such CubeSat, we estimate the quantum secure key to be acquired between two ground stations during one year to be about 13 Mbit. A Bell test between ground and satellite would also be feasible. The uplink design allows to keep the more sensitive, computation-intensive and expensive devices on ground. The experiment proposed by us therefore poses a comparably low-threshold quantum space mission. For a two-year lifetime of the satellite, the price per kilobit would amount to about 20 Euro. In large constellations, Q3Sats could be used to establish a global quantum network, which would further lower the cost. Summarizing, our detailed design and feasibility study can be readily used as a template for global-scale quantum communication.
The security of quantum communication (Q.Com) is based on fundamental and immutable laws of physics and not on the assumption that a problem is and always will be too difficult for an adversary to solve. Naturally, this unconditionally secure communication technology has a large impact on global communications. Attempts to overcome the limits imposed by losses, such as Ref. , and attempts to create a global satellite based network, are underway3,4. The latter are large and complex satellites which can cost upwards of 100 M€ each. Small CubeSats however can be constructed and launched for 0.5 to 10 M€. We present a simple, small, light-weight and low power-consuming satellite system capable of Q.Com. Our CubeSat mission is called Q³Sat (pronounced Q-CubeSat). Previous long distance implementations via optical fiber such as Ref.  and free space terrestrial links like Ref.  have approached the limits of terrestrial Q.Com in terms of distance. The successful 600 kg class3 and 50 kg class7 large satellites have shown that Q.Com in space is feasible. By analyzing the results of these proof-of-concept missions and evaluating their performance in both the uplink and the downlink scenario, we find that a downlink scenario offers a larger key rate. In an uplink, only a relatively simple polarization analysis module needs to be on board the satellite and a ultra bright state-of-the-art quantum source can be used on ground. Thus, an uplink is more suitable for a low cost CubeSat mission. Additionally, an uplink allows for a larger variety of implementable Q.Com protocols. This is because many different Q.Com protocols (e.g., E918, BB849, decoy state protocol (DSP)10, BBM11, B9212) rely on nearly identical detection schemes for the receiver and can thus all be implemented on our CubeSat. Changes would only have to be made to the easily accessible ground module. The CubeSat design considered here will also be able to perform tasks beyond Q.Com, e.g. measuring light pollution stemming from ground with a narrow field of view (FoV) to establish a global map in unprecedented resolution at single-photon level. This is crucial to finding dark areas near potential Q.Com customers and for other, more general applications. Additionally, the timing resolution of the single photon detectors enables pulse position modulation in classical communication from ground to space with exceptionally fast data rates. The extremely sensitive single photon detectors can also be re-purposed for other terrestrial and astronomical observations requiring an exceptional cadence and narrow FoV. In this manuscript we nevertheless focus on Q.Com, since this objective drives the design for the satellite infrastructure.
The advantage of the uplink scenario is that most of the mission’s complexity is ground-based. Figure 1 shows an overview of the experiment consisting of space and ground segments.
The CubeSat requires several subsystems as shown in the CAD-design (Fig. 2). For a 3U CubeSat, its components must be arranged to fit within a total volume of 0.1 × 0.1 × 0.32 m3, have a combined mass of less than 4 kg and consume a maximum of 21 Wh per orbit (with deployable ≈30 × 30 cm2 off-the-shelf solar panels13).
In this section we focus on the quantum payload which consists of receiving telescope, basis choice, polarization analysis and detection subsystems (see Fig. 3). We estimate all optical losses within the CubeSat (between telescope and detectors) to be 1.0 dB, using only standard commercially available devices14-16. The most crucial performance parameters are the noise counts of the avalanche photo diodes (APDs), which we will discuss in more detail in the following sections.
Limiting noise counts
The most challenging aspect of designing a CubeSat is minimizing total noise counts RB+D which therefore influences many design parameters. Unavoidable stray light collected by the CubeSat’s receiving telescope (i.e., background counts RBG) and the intrinsic thermal/radiation damage counts of the detectors (i.e., dark counts per detector RDC) add up to RB+D = RBG + 2RDC and significantly degrade the signal-to-noise ratio (SNR). RDC, which we assume to be constant, has to be below 200 cps per detector to achieve a reasonable SNR. Firstly, the detector noise is reduced when operating at low temperatures. –30°C diode temperature is desirable. Two 250 cm2 radiators on the sun-averted sides of the CubeSat could dissipate the 0.6 W of thermal energy required to cool both detectors. A heating resistor should be used to further regulate the temperature to within ±1°C. While RDC of such a cooled detector can be less than 5 cps in laboratory conditions17, it is increased by damage due to energetic particles and ionizing radiation in space. This can be mitigated by using very small active detector areas dB. The smallest commercially available ones have a dB of 20 μm, which we expect to be small enough to keep RDC well below the 200 cps limit18 despite a radiation damage equivalent to a 2 year mission lifetime. Using other satellite components such as high density batteries accounts for additional radiation shielding. We therefore assume a constant 200 cps of thermal and radiation noise per detector which is, at least for the first months of operation, a conservative estimate.
RBG are the erroneous measurement clicks due to near-infrared noise photons originating from the ground area which are not blocked by the spectral filters. As a worst-case scenario, we account for scattered sunlight from a full moon (brightness: 4000 cd/m²)19 reflected from earth (mean albedo: 0.3)20 into to the CubeSat (we used the solar radiation spectrum). We then translate the luminous intensity into photons per second per m2 footprint impinging on the CubeSat telescope with aperture DB = 10 cm and calculate how many of these photons would pass through our 3 nm wide bandpass filters centered at 810 nm. We arrive at values of 0.55 photons s–1m–2 in zenith and 0.17 photons s–1m–2 for the lowest elevations (because of the larger distance between OGS and satellite). This effect of decreasing background counts per area for low elevations is however less significant than the increase in area because of the larger footprint on ground. The closer the CubeSat is to the horizon, the more ground area is covered by the satellite’s FoV since the circular footprint in zenith changes to a substantially larger elliptical one. Optical losses and detection efficiency of the CubeSat on the other hand reduce the background count value again (see below in this section). In total this gives us a worst-case estimate of total noise counts which we use for all orbits regardless of the moon phase: RB+D varies from ≈480 cps in zenith to ≈575 cps at 30° elevation from horizon. This assumption is very conservative, especially when considering the 350 cps total noise counts at full moon of a similar uplink experiment21.
Field of View (FoV) and attitude control
For a given orbit height of 500 km and imperfect filters, RBG can only be reduced by reducing the field of view (FoV = dB/fB where fB is the CubeSat telescope’s effective focal length). This has two additional benefits: A long fB improves the polarizing beam splitter’s (PBS) extinction ratio since it reduces the divergence of the impinging beam within the PBS. More importantly, a small dB strongly reduces the radiation damage to the detector due to its small cross sectional area. However, the FoV must be large enough to maintain the OGS in view despite the pointing errors of the CubeSat. Until recently, the attitude control of small CubeSats was too imprecise, requiring a large FoV that would have resulted in too many background counts to make the mission possible. The latest commercially available CubeSat attitude control systems based on star trackers have shown a body pointing precision σB of better than 40 μrad RMS (full angle)22,23. The resulting pointing losses ΛPB due to this error, which are caused by an effective spot size broadening on the detectors when averaging over time, can be shown to be
This attitude precision allows us to limit the FoV < 50 μrad while introducing pointing losses 1/ΛPB of 2.5 dB. These comparably high losses are outbalanced by the strongly reduced RBG because of the narrow FoV. Roll axis precision is about a factor of 10 worse24, however misalignment here only leads to an increase in erroneous detections ed on the CubeSat. Even with misalignment in the order of tens of mrad, its contribution to ed stays below 0.1%. Optically tracking the beacon signal holds the potential to further improve ΛPB. Another attitude system requirement is a sufficient slew rate. To keep the OGS in view, the CubeSat should be able to turn with up to 1°/s; this can easily be provided by the system in consideration (10°/s slew rate in pitch and yaw axes for a 4 kg 3U CubeSat22). To achieve an optimal fB, a Cassegrain-type reflector is a good choice for the receiving telescope despite the decreased telescope transmission due to the secondary mirror (which we estimate to be –1.5 dB in total). This is because the overall design is lightweight and the required fB of 40 cm can be realized with a 10 cm long telescope. The telescope covers the CubeSat’s square Z+ surface of about 9 × 9 cm. For simplicity, our calculations assume a circular telescope with DB = 10 cm.
Dead time and timing resolution
To ensure that saturation and dead time effects do not cause losses >0.1 dB, we require a maximum count rate of each CubeSat detector in the order of 100 kHz. The detectors consist of actively quenched silicon-based avalanche photo diodes (APDs) operated in Geiger mode, placed at the output ports of the PBS. The detector diameter dB of only 20 μm strongly reduces the cross sectional area for harmful radiation. Therefore little to no radiation shielding is required, which also has a positive effect on the mass budget.
Errors in Q.Com arise from accidental coincidences and are therefore related to the coincidence detection time window τ. To correctly identify and distinguish at least 98% of all pairs, τ has to be greater than ≈2√(tA2 + tB2), where tA = 10 ps is the timing jitter on ground and tB that on the CubeSat. Thus tB, including the jitter of the detectors17 and the time tagging electronics that note the arrival time of each pulse25,26, should be less than 40 ps to ensure that we can choose τ = 80 ps which is crucial to improving the SNR. The detection efficiency of the detectors ηB we chose is ≈15%. This might seem low, however we trade this for excellent temporal resolution.
In addition to the quantum payload, the CubeSat optics should also accommodate an earth-facing beacon diode to aid in the ground station’s tracking of the CubeSat. There should also be a dichroic mirror to separate the quantum signal from the OGS beacon. The latter assists in locating and tracking the OGS and can be detected by a fast quadrant photo diode. The OGS’s beacon signal is pulsed to facilitate clock synchronization, and the detection pulses from the fast photo diode (along with GPS signals) are used to discipline the local clock on board the CubeSat.
We now want to give an estimate on the amount of secret key the satellite could acquire with two sufficiently separated OGS over one year. To this end, we derive a model for geometric losses due to beam divergence while incorporating long-time measurements of atmospheric turbulence and weather influences to calculate different loss scenarios for our uplink. We also carry out an orbit assessment (see Fig. 5).
Lastly, we evaluate the requirements for an on board clock and estimate the data storage and -transmission needs as well as the computational requirements of the CubeSat. Measurements by the RoboDIMM seeing monitor on La Palma show that a Fried parameter r0 of larger than 5 cm can on average be observed on 228 nights per year (see Fig. 6) or 62% of the time. Therefore, assuming a circular orbit with 30° orbital inclination, it can be assumed that for a total of 44,300 s or 12:20 h each year, the link quality is sufficient to perform Q.Com. The average inclination in zenith as seen from the OGS is 28.3° (unlike the orbital pass shown in Fig. 6 where the zenith angle goes down to 0°). Computing for such an average orbit and taking the annual r0 values into account, the total key acquired in one year would therefore amount to 13.0Mbit for a DSP protocol.
Using our CubeSat design, a pair of ground stations can exchange 13x106 secure bits a year (ignoring finite key effects). Our CubeSat design consists of commercially available components that cost <200,000€27. A typical launch price is <300,000€28. Naturally, the research/development and manpower costs for the first such satellite would be higher and are not included. Assuming a lifetime of two years, information theoretic security could be bought for ≈20€/kbit, provided that an operational OGS is readily available. For DSP, such an OGS would be about 100,000€.
In the current design, the CubeSat is a trusted node. This is suitable for usage scenarios like communication between many branches of a single organization. The current state-of-the-art Q.Com satellites are prohibitively expensive trusted nodes, for communication across the globe, that can only be built by a few select industries. A CubeSat – such as we have shown above – is cheaper and interested organizations can build their own or carefully supervise the building of these trusted nodes for their own use. The proposed CubeSat can also be used for fundamental experiments such as Bell tests which require a SNR of only 4.8 (as opposed to the SNR of 15.1 needed by DSP QKD), clock synchronization, light pollution measurements and earth/atmosphere observation at the beacon wavelengths.
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