# Super-Resolution Remote Imaging Using Time Encoded Remote Apertures
## 5 Proof of Concept Experiments
One possible way to address overlapped peaks is to add a post processing step, where all of the discovered nodes are randomly tested for a potential double peak and added to the distance list for further reconstruction. It is an interesting approach and it is subject for further study. In addition to missing peaks, the collected data may contain incorrect peaks due to background noise from ambient light, dark count rate, after pulsing. Incorrect peaks may also be what we call orphaned peaks that are true peaks from a patch for which not enough peaks are available to reconstruct the patch. A wrong peak can create an invalid vertex in the point-cloud if it satisfies the vertex adding condition (Section 3.2). The algorithm would find an incorrect core and most likely only be able to account for a very small fraction of the detected peaks in a small network. Hence, it can lead to an incorrect reconstruction. In this case, the re-initialization of the algorithm that happens routinely as part of the described algorithm can help. Because all distances used for core build-up and vertex adding parts are randomized, there is a probability that the wrong peak will not be used in the core and would be left over after all of the correct nodes and edges have been identified. A small number of false peaks thus would not prevent a correct reconstruction. A better way to deal with incorrectly detected peaks is an interesting subject for further research. Figure 5: Imaging system and examples of the scene (**a,d**) The imaging system with co-located ultrafast pulsed laser and SPAD. We placed a diffuser in front of the laser to scatter the laser light into the scene. Note there is no lens before SPAD. On the right, the scene with illumination is shown. (**b,c,e,f**) Examples of the test scenes. All of the targets have a dimension approximately 4 \(\times\) 4 cm, except the plane, which has dimensions 8 \(\times\) 8 cm. Our SPAD's dark count rate is 10 photons per second. Coupled with 1 W laser, this dark count rate is negligible in our experiments. After pulsing probability is around 0.1-3% and can also be ignored in our experiments. One way to reduce after pulsing noise is to use fast time-gated SPADs. Gated mode allows a SPAD to be sensitive only during a short gate window of hundreds of picoseconds. The gating window can be moved in time. By progressively moving the active window through the scene in time, one can largely eliminate after pulsing. Figure 6: Resolution test using 2 targets (**a**) Circular patches with diameter 3 cm are placed at distance 15 cm from each other. First column shows ground truth image. Simulated image of the scene captured by an imaging system with 20-micron aperture size. Third column shows reconstructed image. Last column is acquired data. In the time response, we can see clearly three peaks. Two first and one second bounce. (**b**) Circular patches with diameter 3 cm are placed at distance 23 cm from each other. (**c**) Circular patches with diameter 3 cm are placed at distance 35 cm from each other. Figure 8: Experiments with different targets. (**a**) Two star targets of size 4 \(\times\) 4 cm are placed at distance 30 cm from each other. Stars are made of wood and surface color is brown. (**b**) Circular patch and a plane are placed at distance 30 cm from each other. (**c**) Three circular white patches with 4 cm diameter are placed in the scene. In the time response, we can find six peaks: three first and three s bounces. Figure 7: Ground truth distance vs reconstructed distance. Circular patches with diameter 3 cm are placed at distance 15 cm from each other and are moved apart from each other up to 35 cm. The green line is ground truth distance and blue line is reconstructed distance. The RMS error of total 21 sample is 0.03 cm.