A novel algorithm and hardware architecture for fast video-based shape reconstruction of space debris
© Di Carlo et al.; licensee Springer. 2014
Received: 28 February 2014
Accepted: 12 September 2014
Published: 25 September 2014
In order to enable the non-cooperative rendezvous, capture, and removal of large space debris, automatic recognition of the target is needed. Video-based techniques are the most suitable in the strict context of space missions, where low-energy consumption is fundamental, and sensors should be passive in order to avoid any possible damage to external objects as well as to the chaser satellite.
This paper presents a novel fast shape-from-shading (SfS) algorithm and a field-programmable gate array (FPGA)-based system hardware architecture for video-based shape reconstruction of space debris. The FPGA-based architecture, equipped with a pair of cameras, includes a fast image pre-processing module, a core implementing a feature-based stereo-vision approach, and a processor that executes the novel SfS algorithm.
Experimental results show the limited amount of logic resources needed to implement the proposed architecture, and the timing improvements with respect to other state-of-the-art SfS methods. The remaining resources available in the FPGA device can be exploited to integrate other vision-based techniques to improve the comprehension of debris model, allowing a fast evaluation of associated kinematics in order to select the most appropriate approach for capture of the target space debris.
KeywordsSpace debris Active space debris removal Stereo vision Image processing Features extraction Shape from shading FPGA Hardware acceleration
The challenge of removal of large space debris, such as spent launcher upper stages or satellites having reached the end of their lifetime, in low, medium, and geostationary earth orbits, is already well-known. It is recognized by the most important space agencies and industries as a necessary step to make appreciable progresses towards a cleaner and safer space environment [1, 2]. This is a mandatory condition for making future space-flight activities safe and feasible in terms of risks.
Space debris, defined as non-functional objects or fragments rotating around or falling on the earth , are becoming a critical issue. Several studies and analyses have been funded in order to identify the most appropriated approach for their removal. Recent studies demonstrated that the capability to remove existing space debris, over preventing the creation of new ones, is necessary to invert the growing trend in the number of debris that lie in orbits around the earth. Nowadays, the focus is on a specific space debris, weighting about 2 tons and spanning about 10 meters . This class of orbiting debris is the most dangerous for aircrafts and satellites, representing a threat to manned and unmanned spacecrafts, as well as a hazard on earth because large-sized objects can reach the ground without burning up in the atmosphere. In case of collision, thousands of small fragments can potentially be created or even worst, they can trigger the Kessler syndrome . An example of this class of debris is the lower stage of solid rocket boosters, such as the third stage of Ariane 4, the H10 module, usually left from European Space Agency (ESA) as space orbiting debris [6, 7].
In general, the procedure for removing a space debris consists of three steps. The first phase is the debris detection and characterization, in terms of size, shape profile, material identification, and kinematics. The second phase, called non-collaborative rendezvous, exploits the information gathered from the first phase in order to identify the best approach (e.g., trajectory) to capture the identified debris. Finally, in the capture and removal phase, depending on the on-board functionalities of the chaser satellite, the debris is actually grappled and de-orbited from its position [8, 9].
The work presented in this paper is related to the first phase of the debris removal mission. In order to collect the required information about the object to be removed, three main operations must be performed: (i) the debris three-dimensional shape reconstruction, (ii) the definition of the structure of the object to be removed and the identification of the composing material, and (iii) the computation of the kinematic model of the debris. In particular this paper focuses on the first of these three phases.
Since space applications impose several constraints regarding allowed equipments, in terms of size, weight, and power consumption, many devices commonly used for three-dimensional (3D) object shape reconstruction cannot be used when dealing with space debris removal (e.g., laser scanners  and LIDARs ). Moreover, the chosen device should be passive, not only for power constraints, but also because passive components are more robust against damages caused by unforeseen scattering of laser light.
Digital cameras, acquiring visible wavelengths, are suitable for space missions since they provide limited size, weight, and lower power consumption with respect to active devices. Either based on CCD or CMOS technology, digital cameras can be used for 3D shape reconstruction exploiting several techniques. For example, a stereo-vision system can be developed, making use of a pair of identical cameras fixed on a well-designed support.
However, its limitations arise when the object to be captured is monochromatic and texture-less . Since several types of space debris fall into this category, shape-from-shading algorithms that work by exploiting pixel intensities in a single image , combined to stereo-vision, could represent an efficient solution [14–16]. Moreover, in this type of missions, high performances are required to maximize the throughput of processed frames that enables an increase of the extracted information and, consequently, the accuracy of the reconstructed shape models. Moreover, thanks to the high processing rate, the system can quickly react depending on the extracted information.
Since image processing algorithms are very computational intensive, a software implementation of these algorithms running on a modern fault-tolerant space-qualified processor (e.g., LEON3-FT ) cannot achieve the required performances. In this context, hardware acceleration is crucial and devices such as field-programmable gate arrays (FPGAs) best fit the demand of computational capabilities. In addition, a current trend is to replace application-specific integrated circuits (ASICs) with more flexible FPGA devices, even in mission-critical applications .
In , we presented a preliminary work on a stereo-vision system architecture suitable for space debris removal missions, based on a FPGA device, including tightly coupled programmable logic and a dual-core processor. In this paper, we improve the work presented in  by proposing a novel fast shape- from-shading algorithm, and a system architecture that includes: (i) hardware accelerated modules, implementing the image pre-processing (i.e., image noise filtering and equalization) and the feature-based stereo-vision, and (ii) a processor running the proposed novel shape-from-shading (SfS) algorithm. In order to combine and improve SfS results with information extracted by the stereo-vision hardware, other vision-based algorithms routines can be integrated in this hardware architecture.
In the next sections, we first summarize the state of the art about 3D video-based shape reconstruction techniques, including stereo-vision and SfS approaches, and their related hardware implementations. Then, the novel fast SfS algorithm and the proposed system hardware architecture are detailed. Afterwards, experimental results are reported and, eventually, in the last section, the contributions of the paper are summarized, proposing future works and improvements.
In the last years, the interest in creation of virtual worlds based on reconstruction of contents from real world objects and scenes increased more and more. Nowadays, stereo-vision techniques are the most used when dealing with 3D video-based shape reconstruction. These techniques mimic the human visual system. They exploit two (or more) points of view (i.e., cameras) and provide in output a so-called dense map. The dense map is a data structure that reports the distance of each pixel composing the input image from the observer.
Several steps are required to compute the dense map of objects from a couple of images taken from different points of view. Knowing the relative orientation between the two cameras, the images acquired must be first rectified. This first mandatory step aims at removing the radial and tangential distortion effects due to lenses and to align the left and right images in order to apply the epipolar geometry . It is a simple step that moves pixels taking them from one place in the original image and locating them in another position in a new rectified image. The rectification process can be efficiently implemented in hardware exploiting a look-up table (LUT) approach, as proposed in [21, 22].
The rectification process is essential to reduce the complexity of the second task, that is the searching for correspondences of pixels between the two rectified images. In fact, by applying the epipolar geometry, the two-dimensional matching task becomes a one-dimensional problem, since it is sufficient to search for matching pixels in the same lines of the two images . Correspondence algorithms can be classified into two basic categories: feature-based and block-based. The former methods extract characteristic points in the images (e.g., corners, edges, etc), called features, and then try to match the extracted features between the two acquired images [23, 24]. Instead, block-based methods consider a window centered in a pixel in one of the images and determine correspondence by searching the most similar window in the other image [25, 26].
In both cases, based on the disparity between corresponding features, or windows, and on stereo camera parameters, such as the distance between the two cameras and their focal length, one can extract the depth of the related points in space by triangulation . This information can be used to compute the dense map, in which points close to the camera are almost white, whereas points far away are almost black. Points in between are shown in grayscale.
Nowadays, the research community focused more on block-based methods. They provide a complete, or semi-complete, dense map, while feature-based methods only provide depth information of some points .
In literature, several real-time FPGA-based hardware implementations of stereo-vision algorithms have been presented. As aforementioned, most of them focus on the implementation of block-matching algorithms [28–31] that, in general, are more complex than feature-based algorithms, thus leading to a large resource consumption. Moreover, even if this type of algorithms provides fast and accurate results for a wide range of applications, they cannot be effectively employed in the context of space debris shape reconstruction. In fact, space debris are often monochromatic and texture-less. In these conditions, both feature-matching and block-matching methods fail, since it is almost impossible to unambiguously recognize similar areas or features between the two acquired images .
When dealing with monochromatic and texture-less objects, under several assumptions, SfS algorithms are the most recommended . Contrary to stereo-vision methods, SfS algorithms exploit information stored in pixel intensities in a single image. Basically, these algorithms deal with the recovery of shape from a gradual variation of shading in the image, that is accomplished by inverting the light reflectance law associated with the surface of the object to be reconstructed .
Commonly, SfS algorithms assume as reflectance model the Lambertian law . In the last years, algorithms based on other more complex reflectance laws (e.g. Phong model and Oren-Nayar model) have been proposed. However, the complexity introduced requires a high computational power, leading to very low performances, in terms of execution times. Nonetheless, the surface of the biggest debris (e.g., Ariane H10 stage) is characterized by an almost uniform surface that can be effectively modeled with the Lambertian model. For these reasons, in the following, we will focus on the analysis of the most important SfS algorithm based on the Lambertian law.
These SfS algorithms can be classified in three main categories: (i) methods of resolution of partial differential equations (PDEs), (ii) optimization-based methods, and (iii) methods approximating the image irradiance equation (this classification follows the one proposed in  and ).
The first class contains all those methods that receive in input the partial differential equation describing the SfS model (e.g., eikonal equation) and provide in output the solution of the differential equation (i.e., the elevation map of the input image).
The optimization-based methods include all the algorithms that compute the shape by minimizing an energy function based on some constraints on the brightness and smoothness . Basically, these algorithms iterate until the cost function reaches the absolute minimum . However, in some of these algorithms, in order to ensure the convergence and reduce the execution time, the iterations are stopped when the energy function is lower than a fixed threshold , not guaranteeing accurate results.
Finally, the third class includes all the SfS methods that make an approximation of the image irradiance equation at each pixel composing the input image. These methods, thanks to their simplicity, allow to obtain acceptable results, requiring a limited execution time .
Nevertheless, all the aforementioned SfS algorithms present three main limitations: (i) they are very far from real-time behaviors, (ii) their outputs represent the normalized shape of the observed object with respect to the brightness range in the input image, without providing information on its absolute size and absolute distance from the observer, and (iii) they create artifacts if the surface is not completely monochromatic.
To overcome the first problem, we propose a novel fast SfS algorithm which exploits the knowledge on the input light direction (that is easily retrievable during space missions), with respect to the image plane, to reduce the computational load of the shape reconstruction problem. On the other hand, the last two problems can be solved by merging stereo-vision and SfS approaches. In particular, depth data can be exploited to correct and de-normalize the shape extracted by the SfS algorithm, in order to increase the robustness of the entire shape reconstruction process.
While the idea of merging sparse depth data, obtained by the stereo-vision, with SfS output data is not new [15, 16], this paper proposes, for the first time, a comprehensive system hardware architecture implementing the two orthogonal approaches.
We also improve our architecture, presented in , by completely hardware accelerating the image pre-processing and the feature-based stereo-vision algorithms, in order to reach real-time performances. Instead, to compare and highlight the timing improvements of the proposed SfS algorithm with respect to other existing methods, we choose to run it in software on an embedded processor, since, to the best of our knowledge, no hardware implementations of SfS algorithms are available in the literature. However, as will be explained in the following section, the proposed SfS algorithm can be also effectively and easily implemented in hardware.
Novel fast shape-from-shading algorithm
This section describes the proposed novel fast SfS algorithm, hereafter called Fast-SfS.
The basic idea of Fast-SfS is to suppose, as for the regular SfS algorithms, that the surface of the captured object follows the rules of the Lambertian model . However, a first main differentiation from the standard SfS algorithms, concerning the light direction, is introduced. Considering the specific space debris removal application, the dominant source that lights the observed object is the sun. In fact, the albedo of the earth (i.e., the percentage of the sun light reflected by the earth surface and atmosphere back to the space) can vary from the 0% (e.g., ocean, sea, and bays) to 30% (e.g., clouds) . Thus, also in the worst case, the sun represents the dominant light source. Since data concerning the actual environmental conditions in space debris removal missions are still not available, in this work we initially assume that the earth reflection is negligible. Taking into account the data about the earth albedo, this assumption can be considered valid, indeed the elements that provide the lower reflection factor (e.g., ocean, sea, and bays) are also the ones that cover the major part of the earth surface (i.e., around the 71% of the overall earth surface ). Knowing the position and the orientation of the system which captures the images with respect to the sun, it is possible to determine the mutual direction between the camera axis and the sunlight direction. This information can be extracted by computing the attitude of the spacecraft, which is provided by sun sensors  or star trackers , that are commonly available on spacecrafts.
A second assumption is about the light properties, which is supposed to be perfectly diffused, since the sun is far enough to be considered as an illumination source situated at infinite distance. This means that sunlight rays can be considered parallel among each other.
First, the algorithm crops the input image following the object borders, in order to exclude the background pixels from the following computations. Cropping is performed by means of a single thresholding algorithm that, for each row of the image, finds the first and the last pixel in that row that are greater than a given threshold, representing the background level. Moreover, Fast-SfS searches for the minimum and the maximum brightness values inside the cropped image.
Afterwards, in order to extract the elevation map of each pixel, i.e., Δ H in Figures 4 and 5, the tangent of each αP(x,y) is computed. In this step, only the module of the resulting tangent value is taken into account, since from the brightness of a pixel it is not possible to define the sign of the slope (as surfaces (2a) and (2b) in Figure 1).
Finally, the Δ H values are merged together to create the complete elevation map (or the object profile) associated with the horizontal component.
This is done by integrating pixel-by-pixel the Δ H values. Thus, the final elevation of each pixel is the sum of all Δ H associated to the pixels that precede it in the current image row. This operation is repeated for each row of the cropped image.
To discriminate if the object profile decreases or increases (i.e., if Δ H is positive or negative), the brightness value of the currently considered pixel I(x,y) is compared with the one of the previous in the row I(x−1,y). If I(x,y)≥I, the Δ H is considered positive (i.e., the profile of the object increases); otherwise, it is negative.As shown in the flow diagram of Figure 2, all the aforementioned operations are repeated for the vertical component.
where H(i,j) represents the output elevation map matrix, and are the two components of the elevation map in the horizontal and vertical axis, respectively, while (i,j) represents the pixel position in the image.
The most complex operation that the algorithm must perform is represented by the tangent computation. However, to allow a fast execution, this function can be approximated using a LUT approach. Moreover, compared to the SfS algorithms introduced in the previous section, Fast-SfS is not iterative, it does not present any minimization function, and it can be parallelized.
Obviously, Fast-SfS presents the same problems, in terms of output results, as all the other SfS algorithms that rely on the Lambertian surface model. Nonetheless, these problems can be overcome, resorting to stereo-vision depth measures [15, 16].
Proposed hardware architecture
The stereo-vision camera provides in output two 1024 × 1024 grayscale images, with 8 bit-per-pixel resolution. The camera is directly connected to the FPGA subsystem (i.e., an FPGA device), that is in charge of acquiring the two images at the same time, and pre-processing them in order to enhance their quality. Moreover, the FPGA also implements a feature-based matching algorithm to provide a ‘sparse’ depth map of the observed object (i.e., it provides depth information of extracted features, only). In parallel to the feature-based matching algorithm, the processor subsystem performs the novel fast SfS algorithm, presented in the previous section, and provides in output the reconstructed shape of the actual observed object portion. The FPGA and the processor subsystems share an external memory, used to store results and temporary data, and they communicate between each other in order to avoid any collision during memory reads or writes. As aforementioned, the results obtained by the stereo-vision algorithm can be merged to the ones in output from the Fast-SfS algorithm to correct them and to enhance their accuracy [15, 16].
The following subsections detail the functions and the internal architecture of the two subsystems.
Its internal architecture can be split in two main stages. The first, called image pre-processing stage, encloses the input controller, the noise filters, the image enhancers, and the rectifiers, while the second, called stereo-vision processing stage, includes the feature extractors, the feature matcher, and the feature depth calculator. Moreover, a main control unit coordinates all the activities of the different modules, providing also the interface with the external bus to communicate with the shared memory.
An FPGA-based hardware implementation of these algorithms has been preferred with respect to a software implementation running on an embedded processor since, when dealing with 1024×1024 pixels images, the software alternative can lead to execution times in the order of tens of seconds (see Section ‘Experimental results’ for further details). On the contrary, custom FPGA-based hardware acceleration of these algorithms can lead to very high performances.
The data stream from the stereo camera is managed by the input controller (Figure 8). The input controller manages the communication between the stereo camera and the FPGA subsystem, depending on the protocol supported by the camera. Moreover, it provides two output data streams, each one associated to one of the two acquired images. Each pixel stream is organized in 8-bit packets. Since the camera has a resolution of 8 bit-per-pixel (bpp), every output packet contains one pixel. The output packets associated with the right and left image are provided in input to the two noise filter modules.
The arithmetic stage performs the 7 × 7 matrix convolution using the MUL/ADD tree architecture, similar to the one presented in . The tree executes 49 multiplications in parallel and then adds all 49 results. It contains 49 multipliers and 6 adder stages, for a total of 48 adders.
Finally, all filtered pixels are sent both to the image enhancer and to the external shared memory. Storing filtered pixels in the external memory is mandatory since this information is needed during the following features matching phase.
Since the illumination conditions in the space environment cannot be predicted a priori and, at the same time, the proposed architecture must always be able to properly work, an image enhancement is required. The enhancement process aims at increasing the quality of the input images in terms of illumination and contrast. In , it has been demonstrated that this operation allows to increase the features extraction capability, also in bad illumination conditions.
This task can be performed exploiting spatial-domain image enhancement techniques. Among the available spatial-domain techniques, the histogram equalization is the best one to obtain a high contrasted image with an uniform tonal distribution. This technique modifies the intensity value of each pixel to produce a new image containing equally distributed pixel intensity values. Thus, the output images have always similar tonal distribution, reducing the effect of the illumination variations. However, this technique does not work well in every condition. In fact, it works properly on images with backgrounds and foregrounds that are both bright or both dark (smoothed image histogram) but becomes ineffective in the other cases.
If the image histogram is peaked and narrow, the histogram stretching  that allows to redistribute the pixel intensities to cover the entire tonal spectrum, provides better results. On the contrary, if the image histogram is peaked and wide, it means that the input image already has a good level of details and it contains an object on a solid color background (i.e., the image can be provided in output without modification).
Thus, in order to design a system able to work autonomously, the image enhancer module must be able to manage these three different cases and to provide in output the best enhanced image. This task can be accomplished, exploiting the hardware module proposed in , called self-adaptive frame enhancer (SAFE), and used in . SAFE is a high-performance FPGA-based IP core that is able to enhance an input image autonomously, selecting the best image enhancement technique (i.e., histogram equalization, histogram stretching, or no enhancement) to be applied.
The histogram calculator counts the occurrences of each pixel intensity, in order to compute the histogram bar values. In this way, when a complete image has been received, it is able to provide in output the histogram associated with the received image.
The histogram analyzer scans the image histogram in order to extract the maximum difference between two consecutive histogram bars and the histogram width. These two values are compared with the input thresholds (i.e., HW and BW), in order to select the best image to be provided in output.
The equalizer/stretcher module performs both histogram equalization and histogram stretching on the input image, but it provides in output only the best image (i.e., equalized image, stretched image, or input image without modifications) depending on the information provided by the histogram analyzer.
After image enhancement, the rectifier modules perform the rectification of the left and right image, respectively. Image rectification is essential (i) to remove the image distortion induced by the camera lens (especially in the borders of the image) and (ii) to align the images acquired by two different points of view in order to subsequently apply the epipolar geometry during the feature-matching task . Since the rectification parameters are fixed by the camera type and by the relative orientation between the two cameras, the rectification process can be performed using a simple LUT plus a bilinear interpolation approach, as done in [21, 22], where the two LUTs (one for each image) are stored in the external shared memory. Basically, each input pixel in position (x,y) in the original image is moved to a new position (x1,y1) in the new rectified image. The value of the rectified pixel is computed, interpolating the four adjacent pixels in the original image. Since for resources efficiency reasons, the LUT is stored in the external memory, and the coordinates must be translated in an absolute address value. This task is accomplished by simply adding a constant offset that is equal to the memory base address at which the LUTs are stored.
After image pre-processing, the feature-based stereo-vision algorithm can be applied in order to obtain the features depth map. The algorithm performs feature extraction, feature matching, and finally, feature depth computation. Among these three activities, feature extraction is the most complex one. Several feature extraction algorithms have been proposed in the literature. Beaudet , smallest univalue segment assimilating nucleus (SUSAN) , Harris , speeded up robust features (SURF) , and scale-invariant feature transform (SIFT)  are just some examples. In , we used a software implementation of SIFT as feature extractor since, from the algorithmic point of view, along with SURF, it is probably the most robust solution due to its scale and rotation invariance. This means that features can be matched between two consecutive frames even if they have differences in terms of scale and rotation. However, due to their complexity, their hardware implementations are very resource hungry, as reported in [51–53]. Among the available feature extraction algorithms, Harris is probably the best trade-off between precision and complexity . In this specific case, since the two images acquired by the two cameras can present only very small differences in terms of rotations and almost no differences in terms of scale, its accuracy is comparable to the one provided by SURF and SIFT. Its complexity makes it affordable for a fast FPGA-based hardware implementation requiring limited hardware resources.
where k is an empirical correction factor equal to 0.04, and N(x,y) is the second-moment matrix, which depends on the spatial image derivatives L x and L y , in the respective directions (i.e., x and y) . Pixels with high corner response have high probability to represent a corner (i.e., an image feature) of the selected frame and can be selected to search for matching points between consecutive frames.
The features extractors in Figure 8 implement the Harris corner detection algorithm . It is worth noting that the spatial image derivatives of the filtered image in the horizontal (L x ) and vertical (L y ) direction are performed by convolving the pre-processed image, read-out from the shared memory, with the 3 × 3 Prewitt kernels , using an architecture similar to the one proposed for the noise filters, guaranteeing high throughput. The extracted features are stored inside an internal buffer, implemented resorting to the FPGA internal memory resources.
where patch identifies the pixels window on which the correlation must be calculated (i.e., correlation window) and I1 and I2 identify the pixel intensity associated with the two input images. The less is the value of C, the more correlated will be the two points.
The computed cross-correlation results are thresholded, in order to eliminate uncorrelated features couples. If the calculated cross-correlation value is less than a given threshold, the coordinates of the correlated features are stored inside an internal buffer.
Finally, the depth results are stored in the external shared memory in order to be accessible by the processor subsystem for following computations.
The processor subsystem includes a processor that executes the novel fast SfS algorithm presented in the previous section. Even if implementing the proposed algorithm directly in hardware, as the modules described in the previous subsection, could lead to a boost of the performances, in this paper a software implementation has been preferred to highlight the differences, in terms of execution time, with respect to other state-of-the-art SfS algorithms.
To perform the proposed approach, the processor reads from the shared memory one of the two rectified images. The results of the algorithm represent the shape of the observed object, with respect to a reference plane.
Eventually, the same processor subsystem can be exploited to execute the algorithm that aims at merging the depth information gathered from the FPGA subsystem, with the results obtained by the fast SfS approach. This can allow (i) to correct the reconstructed shape in the features points neighbourhoods and (ii) to extract the absolute size and distance of the object under evaluation.
To prove the feasibility of the proposed architecture, we implemented both the FPGA subsystem and the processor subsystem on a single FPGA device exploring the Aeroflex Gaisler GR-CPCI-XC4V development board, which is equipped with a Xilinx Virtex-4 VLX100 FPGA device and a 256 MB SDRAM memory . The choice of using a Virtex-4 FPGA, instead of a more advanced device, fits the considered space debris removal applications. In fact, modern radiation-hardened space-qualified FPGAs exploit the same device architecture . Moreover, the processor subsystem has been implemented using the Aeroflex Gaisler LEON3 soft-core processor that represents the standard processor architecture used in space applications .
In the following, experimental results are separately reported for the FPGA subsystem and the processor subsystem.
FPGA subsystem results
FPGA subsystem modules logic and memory hardware resources consumption for a Xilinx Virtex-4 VLX100 FPGA device
Noise filter (× 2)
Image enhancer (× 2)
Rectifier (× 2)
Features extractor (× 2)
Features depth calculator
The numbers in brackets represent the percentages of resources used with respect to the total available in the FPGA device. It is worth noting that noise filters, image enhancers, rectifiers, and features extractors are instantiated twice in the design.
To emulate the camera, the images are supposed to be pre-loaded in an external memory. Thus, the input controller consists of a direct memory access interface that autonomously reads the images pre-loaded into the shared memory.
The entire processing chain is able to process a couple of images and to provide the associated depth map in about 32 ms, leading to a throughput of 31 image couples per second.
The bottleneck of the system is represented by the external shared memory that in some time slots is simultaneously requested by different modules. Using a dual-port memory can help to avoid the stall of the processing chain, leading to a greater throughput.
To highlight the speed-up obtained by resorting to hardware acceleration, the algorithm implemented by the proposed hardware modules has also been described in C and compiled (using the maximum possible optimization level) for the LEON3 processor. The processor has been implemented, enabling the floating-point unit and the internal data/instruction cache memories of 4 and 16 KB, respectively. The overall software execution time attests around 42 s, when the processor runs at 60 MHz (i.e., the maximum operating frequency of the LEON3 processor implemented on the selected FPGA device). The major contribution in the execution time is given by the Gaussian filtering and feature extraction functions that perform 2D convolution.
Comparing the overall software and hardware execution times, hardware acceleration provides a speed-up of 1,300 ×.
Finally, focusing on the features extractor and features matcher modules, we can highlight the gain, in terms of hardware resources consumption, of using the Harris algorithm, with respect to more complex SIFT or SURF extractors. As an example,  and  propose two FPGA-based implementations of the SURF algorithm. The architecture proposed in  consumes almost 100% of the LUTs available on a medium-sized Xilinx Virtex 6 FPGA, without guaranteeing real-time performances. Similarly, the architecture proposed in  consumes about 90% of the internal memory of a Xilinx Virtex 5 FPGA. It saves logic resources, but it is able to process in real-time only images with a limited resolution of 640×480 pixels. Another example is presented in  where an FPGA-based implementation of the SIFT algorithm is presented. It is able to process in real-time 640×480 pixel images, consuming about 30,000 LUTs and 97 internal digital signal processor hard macros in a Xilinx Virtex 5 FPGA. Instead, taking into account the reduced complexity of the Harris algorithm, the feature extraction for the two 1024 × 1024 input images, and the matching task can be performed in real-time using only 21,594 LUTs and 31 BRAMs resources, representing the 22% and the 12.9% of the considered Virtex-4 FPGA device, respectively.
An explicit comparison with other state-of-the-art FPGA-based stereo-vision architecture has not been made since they focus on block-based methods [28–31]. Even if they provide more dense results, due to their increased complexity, they incur in a greater hardware resources consumption (not including the resources needed for the image pre-processing) [28, 52, 53].
Processor subsystem results
The processor subsystem has been implemented resorting to the LEON3 soft-core processor architecture  and integrated in the same FPGA device as the FPGA subsystem. The processor has been implemented, enabling the floating-point unit and the internal data and instruction cache memories of 4 and 16 KB, respectively. The maximum operating frequency of the processor, synthesized on a Xilinx Virtex-4 VLX 100 FPGA device, is equal to 60 MHz.
The chosen processor configuration leads to an hardware resources usage of 21,395 LUTs, 8,750 FFs, and 32 BRAMs. Thus, the overall resources consumption of the proposed system (FPGA and processor subsystems) is around 60% of the overall logic resources available in the FPGA device.
The proposed algorithm has been compared, in terms of execution time, to other SfS approaches proposed in the literature. Durou et al.  reports execution times of the fastest SfS algorithms presented in the literature. The algorithms are executed on a Sun Enterprise E420 machine , equipped with four UltraSparc II processors running at 450 MHz, each one with 4 MB of dedicated cache. From , the fastest SfS algorithm is the one presented in , that is an iterative algorithm, requiring 0.29 s for 5 iterations and 1.17 for 20 iterations (to ensure better results), to process a 256 × 256 images. Even if running on a processor running at 1/6 of the operating frequency and equipped with a cache of 3 orders of magnitude smaller, the algorithm proposed in this paper requires almost the same time of .
The algorithm applied on the two synthetic images provides good results since they are characterized by a diffused light and a monochromatic surface. This characteristics completely match the assumptions on which the proposed algorithm is based (see Section ‘Novel fast shape-from-shading algorithm’).
On the other hand, in the real image the target object is illuminated by direct light, since diffused light cannot be easily reproduced in laboratory. Moreover, due to the reflective material composing the object, the image presents some light spots (see the upper central part of the drinking bottle in Figure 19a). As can be noted in Figure 19b,c, these light spots lead to some peaks in the reconstructed shape. Nevertheless, the resulting shape provided by the Fast-SfS algorithm follows the profile of the real object and the peaks can be efficiently corrected by merging the reconstructed shape with the information gathered from the stereo-vision algorithm (as discussed in Section ‘Related works’).
This paper presented a novel fast SfS algorithm and an FPGA-based system architecture for video-based shape reconstruction to be employed during space debris removal missions. The FPGA-based architecture provides fast image pre-processing, depth information exploiting a feature-based stereo-vision approach, and SfS results employing a processor that executes the proposed novel SfS algorithm.
Experimental results highlight the achieved timing and resources consumption improvements with respect to other state-of-the-art solutions. Moreover, the limited hardware resources consumption of the entire system allows to implement it in a single FPGA device, leaving free more than the 40% of overall hardware resources in the selected device.
The remaining part of the FPGA device can be exploited (i) to improve the reliability of the design, employed in space applications, e.g., applying some fault tolerance techniques; (ii) to hardware accelerate the proposed SfS algorithm, avoiding the usage of a processor; and (ii) to include the following vision-based algorithms that aim at merging the results obtained by the stereo-vision and the novel fast SfS approach.
When more detailed requirements of the space debris removal missions will be available, future work will focus on the improvement of the proposed algorithm, taking also into account the earth albedo effect during the shape model computation.
a Det(X) denotes the determinant of matrix X, and Tr(X) denotes the trace of matrix X
The authors would like to express their sincere thanks to Dr. Walter Allasia and Dr. Francesco Rosso of Eurix company for their helpful hints and fruitful brainstorming meetings.
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