The possibility and feasibility of future drone-based shallow subsurface GPR radar survey for Mars have been examined. SHARAD data indicates shallower features are expected to be present, while HiRISE based analysis of outcrops confirm there are several target features, waiting for radar identification. Targets for an airborne shallow subsurface radar were evaluated including ice content of indurated dunes, internal layering of fluvial deposits, mid- and high latitude ice containing features, former crater lake sediments and lava caves; as well as expected dielectric constant values. The proposed instrument will be able to explore discontinuities in the underground to measure thickness, volume and stratigraphic sequence. Airborne GPR is expected to provide such information what is not achievable by rovers with limited traverse capability and inability of crossing several terrain types.The radar penetration will be increased compared to those characteristics on the Earth by the low humidity expected in the Martian subsurface, while the iron-oxides could decrease the signal with scattering effect and the normal attenuation due to imaginary part of dielectric constant. As radar signals are strongly affected by the presence of liquid water that is very common of Earth, the FlyRadar instrument will be tested mostly in dry areas that are arid hot deserts, karsts or cold arid areas where water is frozen. The suggested trade off according to the geology of the investigated areas was found for the survey of the top 50 m of subsurface could be done at 20 MHz of bandwidth with 80 MHz of transmitted frequency. The mass of such an instrument could reach kilogram payload. The drone technology is available to do survey at 10 km scale distances, what neither an orbiter nor a surface rover could achieve, in order to support next missions for science and ISRU activities.

The possibility and feasibility of future drone-based shallow subsurface GPR radar survey for Mars have been examined. Various observations indicate shallower features are present on Mars, could be surveyed ideally from a low altitude flying airborne GPR with survey around 100 MHz transmitted frequency. Although there are uncertainties especially related to the role of iron-oxides – but in general better and deeper penetration is expected for the radar signals than it is characteristic on the Earth. The proposed instrument will be able to explore discontinuities in the underground to measure thickness, volume and stratigraphic sequence.IntroductionThis project aims to evaluate the feasibility and realization of a small mass drone based GPR survey on Mars to support next missions. Range of scientific questions on tectonics, volcanism, climate changes, water and ice could be answered of partly clarified with better knowledge on the shallow subsurface of Mars – all are ideal targets for GPR analysis. The discoveries of shallow subsurface ice on Mars (Dundas et al. 2021, Morgan et al. 2021, Mouginot et al. 2012, Schiff and Gregg 2022), and the mapping of these deposits (Putzing et al. 2023, Morgan et al. 2021), make shallow subsurface region especially important recently. While the top surface is influenced by UV- plus charged particle irradiation, as well as heavily oxidized, the few meters deep region is not influenced by these effected, thus ideal for the acquisition of astrobiology relevant samples.Radar observations are important for Mars and based on the former MARSIS (Jordan et al. 2009, Picardi et al. 2004, Seu et al. 2007) and SHARAD instruments used from orbit, the RIMFAX instrument onboard the Perseverance and RoPeR instrument onboard Zhurong rovers could provide a range of such discoveries. Internal structure of the polar caps (Jawin et al. 2022), thickness so some depositional units (Li et al. 2022), occurrence of buried ice masses (Nerozzi and Holt 2019) have already demonstrated the success of GPR-like technology for Mars.Targets on Mars it is expected that the shallow subsurface consists mainly porous basaltic materials together with various salts beside sedoments. The porous voids if filled by brine or ice could increase electrical conductivity and cause strong radar reflection (Stillman et al. 2022). Porosity exhibits an elevated value at shallow depths in the regolith. Using InSight mission pores are expected to be closed around 9 km depth (Gyalay and Nimmo 2022), and close to the surface the porosity might be up to about 50-60% (Grott et al. 2022). Brines are expected also on Mars, permittivity of salty solutions depends on temperature. Brine mixtures in JSC Mars-1 regolith simulant also show a range of permittivity values depending on temperature and concentration (Kobayashi et al. 2023).Considering the morphology of target features, surveying about HiRISE images the existence of subsurface structures in the top 10-20 m layer. Some examples are indicated in Figure 1.Figure 1: Surface exposed shallow subsurface structures on HiRISE images. First column shows 100 km diameter terrain using THEMIS images for context, second column shows about 4 km diameter part of the HiRISE images, while third column shows 1x1 km magnified section of the images.Required technical parametersAiming the top 1-40 m of the Martian regolith the wavelength range 100-200 MHz is idel. The spatial resolution is expected in the range of meters horizontally (controlled by the pulse frequency and UAV (drone) velocity). Duricrust, hydration-related mineral filled voids and air-filled voids are expected (Spray 2004). Earth based studies showed iron-oxide lower wave velocity, bound water content also has an effect, controlling permittivity (Van Dam et al. 2002).Identification of bulk liquids water might be moderately straightforward (Wu et al. 2019), as it absorbs the radar signal – but could be rare or absent on Mars today. Thus radar signal could penetrate deeper on Mars than in the case of the Earth. The elevated abundance of iron containing minerals on Mars could potentially affect the interpretability of GPR signal by signal attenuation caused of magnetic minerals (Heggy et al. 2001) could still be too provide useful data (Pettinelli et al. 2007).Considering such a “FlyRadar” mission with the technical capabilities listed above, an airborne shallow subsurface radar would provide range of new information on ice content of indurated dunes, internal layering of fluvial deposits, mid- and high latitude ice, former crater lake sediments, lava caves, and subsurface tectonic structures and volcanic plumbing systems, or source region of volcano-ice interaction.ConclusionsDrone based GPR survey on Mars could explore a poorly known domains: large (10-100 km) size area at 1-50 m shallow subsurface, what is and was in close contact with the atmosphere and volatile circulation. Enhanced mobility and accessibility even at rough, steep and dangerous areas are supported by drone-based survey. Rapid mapping of large areal in a short period with repeated observations at different daily and seasonal cycles would provide unique results.For drones there are limitations on the size and weight of the antenna that can be carried, 100 MHz looks to be ideal. Additionally, at these wavelengths, the attenuation of the electromagnetic waves in the Martian subsurface is still acceptable, based on the attenuation at frequencies of SHARAD and MARSIS.AcknowledgementThis work was supported by the FlyRadar EU project (No 101007973). The support from Internal fund from Thales Alenia Space Italia is also acknowledged.ReferencesDundas et al. 2021. JGR 126, e06617.Grott et al. 2021. 52nd LPSC #1237.Gyalay and Nimmo 2022. 53rd LPSC #1633Heggy et al. 2001. Icarus 154, 244–257.Jawin et al. 2022. GRL 49, e99896.Jordan et al. 2009. PSS 57, 1975–1986.Kobayashi et al. 2023. Earth, Planets and Space 75, id.8.Morgan et al. 2021. Nat Astron 5, 230–236.Mouginot et al. 2012. GRL 39, L02202.Nerozzi and Holt 2019. GRL 46, 7278-7286.Pettinelli et al. 2007. IEEE Trans. 45, 1271-1281.Schiff and Gregg 2022. Icarus 383, 115063.Spray 2004. AGU, id.P33B-05Picardi G. et al., in Mars Express, ed. by Wilson and Chicarro. SP-1240 (ESA, Noordwijk, 2004), 51–69.Putzig 2017. 5th International Planetary Dunes Workshop #3054.Seu et l. 2007. JGR 112(E5), E002745.Stillman et al. 2022. JGR 127, E007398.Van Dam et al. 2002. Geophysics 67(2):536-545.

Introduction: The Tharsis dome is the main volcanic province on Mars. Being the locus of volcanism since at least the lower Hesperian, the age of emplacement and succession of its lava flows gives insights onto the thermal evolution of the planet since that time. Late Amazonian volcanic activity has taken the form of a large number of long and narrow lava flows, the vast majority of which unmapped to date. Mapping them is critical to characterize the recent dynamics of the Tharsis volcanism and relationships with tectonic activity. We focus on a group of fresh-looking lava flows located SE of Arsia Mons (Fig. 1). We map individual flows and determine their crater retention age, correlate with stratigraphy.Geological Setting: Arsia Mons is the southernmost shield volcano of the Tharsis Montes. The edifice is ~400 km wide and rises 10 km above the surrounding topography. Its eruptive history includes explosive and effusive episodes [1]. The youngest episodes are thought to have occurred within the caldera and in the southern rift zone, forming a large fan-shaped lava aprons at 130 Ma [2,3]. Mapping of individual lava flows around vents [4] constrains the intra-caldera activity between 200-300 Ma and 90-100 Ma, with a peak at 150 Ma. The SE lava field (Fig. 1) was previously dated using HRSC data, and inferred to be 189 Ma [3].Dataset and methods: Individual lava flows are mapped based on CTX images (6 m/px), THEMIS Night and Day-IR imagery (~100 m/px), and MOLA shots, and their succession is established using cross-cutting and stratigraphic relationships.Absolute ages are estimated using automated crater detection and counting based on machine learning technique [5]. This method was favoured over manual counting because of time efficiency on large surface areas, such as total extents of lava flow. The algorithm was trained on THEMIS images where database for craters >1 km already exists [6]. The algorithm is applied to CTX mosaic from Murray Lab [7] to detect impact craters of diameter >100 m. A second algorithm based on cluster analysis is used to clean clusters of secondary impact craters. Each crater detection is then checked manually by visual inspection. Crater ages and errors are derived from crater size frequency distribution plots using Craterstats II [8] and Hartmann’s chronology system [9].Results: We have mapped 37 individual lava flows and sorted them with respect to their stratigraphic relationships (Fig. 2). Flow length and width are in the range 20-300 km, and 0.7-21 km. Flows have typically a rugged surface with sometimes a medial channel system, while others display a smoother texture and wider extent. The flows originate from the southern lava apron of Arsia Mons. The flowing direction is toward ESE, the direction of the current regional slope of the Tharsis dome. In the NW, they overprint SW-NE-trending grabens, but are cut by other normal faults from the same graben system, implying syn-tectonic volcanism. The total number of craters retrieved by the counting algorithm and kept after visual inspection is 948. The age of 23 flows could be obtained. They range from 200±50 Ma to 54±20 Ma, with 80% of lava flows between 60 and 160 Ma. In the SE, the longest lava flows lie on a 470±100 Ma older flow.Discussion and perspectives: The obtained ages span 150 million years, with an apparent peak age at 150 Ma. This age corelates with the 150 Ma peak eruption age within the caldera [4]. It has been argued that a transition from explosive to effusive style occurred at Arsia Mons 200 Myrs ago [4]. Our results confirm that after effusive volcanism resumed, volcanic activity at Arsia Mons was not restricted to the caldera. Activity centered at the caldera and the southern flank followed a several hundred million years hiatus after main-flank building activity already noted by previous studies [3,4]. Crosscutting relationships between lava flows and bounding faults of concentric grabens indicate that extensional tectonics was coeval with some of the eruptions.Length compared to width suggests lavas of mafic compositions. Texture pattern visible in CTX shows similarity with flows located further SW and NE of Daedalia Planum and dated 100 Ma [10]. The bright and rugged textures indicate differences in viscosity, similarly to basaltic flows found on the flanks of terrestrial shield volcanoes (aa’ and pahoehoe texture – e.g. [11]).Morphometric study based on high-resolution digital terrain models will help confirm this interpretation and infer viscosity [12], a first step towards understanding the dynamics of the most recent eruptions at Arsia Mons.Acknowledgments: This work is supported by the TEAM program of the Foundation for Polish Science (TEAM/2016-3/20), co-financed by the European Union under the European Regional Development Fund. This study is also supported by Europlanet 2024 RI's GMAP project.References: [1] Ganesh I. et al. (2020) J. Volcanol. Geotherm. Res., 360. [2] Neukum G. et al. (2004) Nature, 432, 971-979. [3] Werner S.C. (2009), Icarus, 201, 44-68. [4] Richardson J.A. et al. (2017), EPSL, 458, 170-178. [5] Benedix, G. K. et al. (2020) Earth and Space Science 7, no. 3 [6] Robbins S. (2012), JGR, 117(E). [7] Dickson J.L. (2018), LPSC, Abstract #2480. [8] Michael G. G. and Neukum G. (2010) EPSL, 294, 223–229. [9] Hartmann W. K. (2005) Icarus, 174, 294–320. [10] Crown, D. A., & Ramsey, M. S. (2017). J. Volcanol. Geotherm. Res., 342, 13-28. [11] Holcomb, R. T. (1987) US Geol. Surv. Prof. Pap, 1350(1), 261-350. [12] Kolzenburg S. et al. (2018), J. Volcanol. Geotherm. Res., 357, 200-212. [13] Michael G. G (2016) Icarus 277:279–285

Introduction: One essential part of NASA´s planetary geologic mapping program [1] is to coordinate and standardize the geological map process and products in planetary science. This important role is taken by the Astrogeology Team as USGS since the early sixties.Within the scope of an EU project called PLANetary MAPping (PLANMAP, [2]), which ended this year, initial steps to develop complementary expertise in the EU was done. To continue addressing the major scientific and technological challenges facing modern planetary science and strengthen Europe´s position and the forefront of space exploration a new pan-EU infrastructure, the EUROPLANET 2024 Research Infrastructure (EPN-2024-RI), is coordinating mapping efforts in the EU and with international partners. One component of this 4-year-project is the Geologic MApping of Planetary bodies (GMAP). This aims to serve the European planetary community through an infrastructure to foster, support, and sustain the production of planetary geological maps and related products following standard procedures [e.g., 3]). In order to do so, GMAP is directly building on the PLANMAP work [2], and several partners and institutions with previous experience in planetary geologic mapping are involved. That means a planetary scientist can produce a geological map or a derived higher-level product through GMAP Virtual Access (VA) with the help and advice of the GMAP partner institutions, who will provide base-maps and technical aid as part of the Joint Research Activity (JRA). The maps will provide support for ongoing and future planetary missions, training activities, and non-standard science-driven mapping projects, such as space resource mapping.GMAP – motivation and focus: The primary focus of GMAP is to streamline the processes which are involved in the production of geological and geomorphological maps of planetary surfaces. Here, we are mainly collecting existent approaches and related documents which handle the standardization of GIS-based mapping processes to enable the European community in creating cartographic products. The aim is to describe, develop, store, combine (!), access, update, revise, and finally, visualize scientific cartographic products. As soon as these steps can be handled in well-defined workflow and distributed among researchers and mappers, the highest possible level of homogenization, and thus standardization, is reached. This is the essential step to use these research products as a basis for broader studies. During the first year, coordination activities targeted the planning and the initial setup of digital infrastructure services that will be needed for supporting VA and JRA activities. The domain europlanet-gmap.eu was acquired by GMAP and will serve as the entry point for presenting the GMAP initiative, collecting most notable resources, for users’ access, for providing basic guidance for publishing new maps, request support and contribute to the overall project. The website is built on the same open source Content Management System (WordPress, [4]) already employed for the main Europlanet website, on https://europlanet-society.org. The GMAP data portal (see figure 1, [5]) and additional services and tools are being setup.GMAP – requirements and developments: In order to extract the requirements to support the European community in streamlining their planetary geological maps, a document was produced during the last year of JRA activities. The document contains state of the art information in this field and addresses the geologic mapping and cartographic aspects of the various Solar System bodies.Geologic process-specific and body-specific best practice and published case studies are included in [1]. The approaches for two-dimensional mapping and three-dimensional geologic mapping and modelling are introduced, as well as the range of non-standard map types that are envisaged within GMAP activities.In particular the following main topics are in development: 1) a mapping guide with essential information for the GIS-based mapping process, including CRS symbology, metadata, and naming conventions; 2) mapping templates for GIS-based mapping and for final map layout, as well as instructions about naming conventions [6].Mapping review directions are indicated, as well data sharing, distribution and discovery. Proposed standards, best practices, and tools are based on those existing, as well as on additional or new developments and adaptations [e.g. 7]. The document will be periodically updated. GMAP – summary and outlook: The development of the GMAP data portal [5] was initiated, based on existing developments from PLANMAP. The availability of GMAP products and underlying datasets is going to be FAIR (findable, accessible, interoperable, and reusable [8]), as also recommended by the VA Review Board (see also [9]), and building on the practices of PLANMAP [10], see also e.g. [11]). The use of existing tools by NASA and USGS such as Integrated Software for Imagers and Spectrometers (ISIS, [12]), and Ames Stereo Pipeline (ASP, [13]) will be promoted. Moreover, in addition to the community support by the GMAP VA, interaction with the community via OpenPlanetary [14] is also planned. All further information and current developments are available via [15] and [16].Acknowledgments: GMAP and Europlanet 2024 RI have received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.References: [1] Astrogeology Team at USGS, https://www.usgs.gov/centers/astrogeology-science-center, [2] https://planmap.eu/, [3] Nass, et al., (2020) Standard definition Document 1st iteration, available online at https://www.europlanet-gmap.eu/about-gmap/deliverables, [4] https://de.wordpress.org/, [5] GMAP data portal, available online at https://data.europlanet-gmap.eu, [6] GMAP Consortium (2021) GMAP wiki documentation and service pages, available online at https://wiki.europlanet-gmap.eu/, [7] Penasa, L., et al. (2020) Europlanet Science Congress 2020, EPSC2020-1057, doi:10.5194/epsc2020-1057, 2020, [8] Wilkinson, M., et al. (2016) The FAIR Guiding Principles for scientific data management and stewardship. Sci Data 3, 160018, doi:org/10.1038/sdata.2016.18, [9] Raugh et al., (2020), VAs 1st year External Board Review report, available online at https://www.europlanet-society.org/europlanet-2024-ri/europlanet-2024-ri-deliverables/, [10] Brandt, C. H., et a., EGU General Assembly 2020, EGU2020-18839, doi: 10.5194/egusphere-egu2020-18839, [11] Luzzi, E., et al. (2020) JGR-Planets, 125, doi:10.1029/2019JE006341, [12] Gaddis, L., et al. (1997). An overview of the Integrated Software for Imaging Spectrometers (ISIS), in: Lunar and Planetary Science XXVIII. p. 1997, [13] Beyer, R. A., et al. (2018) Earth and Space Science, 5, 537-548, doi:10.1029/2018EA000409, [14] Manaud et al., (2019) EPSC-DPS Joint Meeting, EPSC Abstracts, Vol. 13, EPSC-DPS2019-1654-1, [15] https://wiki.europlanet-gmap.eu/bin/view/Main/Documentation/, [16] https://wiki.europlanet-gmap.eu/bin/view/Main/Services%20and%20tools/

ABSTRACTThis work presents a detailed volcano-geological map of the Northern region of Lanzarote (Canary Islands, Spain). This map is a synthesis of gathered and interpreted field data and geological maps. We have integrated information obtained from: (a) detailed geological field surveys, (b) high-resolution digital elevation models (DTMs), (c) aerial orthophotographs, (d) morphometric analysis of eruptive deposits and volcanic structure (i.e. lava tubes), and (e) integrated with data from previous publications (IGME – Instituto Geológico y Minero de España). This map provides a detailed view of the volcanic diversity of the region and an overview of the lava tube system of La Corona, both of which may be used as references for future research work.

Following the recent detection of HCl in the atmosphere of Mars by ExoMars/Trace Gas Orbiter, we present here the first measurement of the 37Cl/35Cl isotopic ratio in the Martian atmosphere using a set of Nadir Occultation for MArs Discovery (NOMAD) observations. We determine an isotopic anomaly of −6 ± 78‰ compared to Earth standard, consistent with the −51‰–−1‰ measured on Mars’ surface by Curiosity. The measured isotopic ratio is also consistent with surface measurements, and suggests that Cl reservoirs may have undergone limited processing since formation in the Solar Nebula. The examination of possible sources and sinks of HCl shows only limited pathways to short‐term efficient Cl fractionation and many plausible reservoirs of “light” Cl.

The analysis of rockfall distribution and magnitude is a useful tool to study the past and current endogenic and exogenic activity of Mars. At the same time, tracks left by rockfalls provide insights into the mechanical properties of the Martian surface. While a wealth of high-resolution spaceborne image data are available, manual mapping of displaced boulders with tracks is inefficient and slow, resulting in: 1) a small total number of mapped features; 2) inadequate statistics; and 3) a suboptimal utilization of the available big data. This study implements a deep learning-driven approach to automatically detect and map Martian boulders with tracks in high resolution imaging science experiment (HiRISE) imagery. Six off-the-shelf neural networks have been trained either on Martian or lunar rockfall data, or a combination of both, and are able to achieve a maximum overall recall of up to 0.78 and a maximum overall precision of up to 1.0, with a mean average precision of 0.71. The fusion of training data from different planets and sensors results in an increased detection precision, highlighting the value of domain generalization and multidomain learning. Average processing time per HiRISE image is ~45 s using an NVIDIA Titan Xp, which is more than one order of magnitude faster than a human operator. The developed deep learning-driven infrastructure can be deployed to map Martian rockfalls on a global scale and within a realistic timeframe.

Here we study rocks falling from exposed outcrops of bedrock, which have left tracks on the slope over which they have bounced and/or rolled, in fresh impact craters (1-10 km in diameter) on Mars. The presence of these tracks shows that these rocks have fallen relatively recently because aeolian processes are known to infill topographic lows over time. Mapping of rockfall tracks indicate trends in frequency with orientation, which in turn depend on the latitudinal position of the crater. Craters in the equatorial belt (between 15 degrees N and 15 degrees S) exhibit higher frequencies of mckfall on their north-south oriented slopes compared to their east-west ones. Craters >15 degrees N/S have notably higher frequencies on their equator-facing slopes as opposed to the other orientations. We computed solar radiation on the surface of crater slopes to compare insolation patterns with the spatial distribution of rockfalls, and found statistically significant correlations between maximum diurnal insolation and rockfall frequency. Our results indicate that solar-induced thermal stress plays a more important role under relatively recent climate conditions in rock breakdown and preconditioning slopes for rockfalls than phase transitions of H2O or CO2, at mid- and equatorial-latitudes. Thermal stress should thus be considered as an important factor in promoting mass-wasting process on impact crater walls and other steep slopes on Mars.

Individual block falls are one of the currently active surface processes on Mars. Similarly to Earth, clasts detach from upslope outcrops roll or bounce downslope, leaving a track on the substratum (Fig. 1). The trails show that the rockfalls are recent, as aeolian processes would infill topographic lows over time. Using rover-track erasure rates, these tracks are likely <100 ka. On Earth, slope instability is usually caused by phase changes of H2O [1]. However, solar-induced thermal stress could also play a key-role in rock breakdown leading to rockfalls [2]. Although liquid water is not stable at the surface of Mars today, sub-surface water ice is known to be present from mid- to high-latitudes [3]. Water ice and CO2 seasonal frost on shadowed pole-facing slopes may exist at latitudes down to 30° [4] or less [5]. On the other hand, insolation-related thermal stress has been used to explain fracture orientation patterns in martian boulders observed by the Mars Exploration Rovers [6] and other studies suggest that it could cause rock breakdown on airless bodies [7]. Therefore, both phase transitions and solar-induced thermal stress are plausible mechanisms for rock breakdown and preconditioning slopes for rockfalls on modern Mars. In this study we analyze distribution of rockfalls on impact crater walls to assess whether one of these mechanisms could be involved in local rock breakdown.

Here, we track annual changes in the global surface ice distribution on Mars. We present apparent thermal inertia maps for the first time using the PFS/MEX (Planetary Fourier Spectrometer of Mars Express) surface temperature dataset.

SPOTS. J. Ciazela 1 , D. Mège 1 , B. Pieterek 2 , M. Ciazela 1 , J. Gurgurewicz 1 , A. Lagain 3 , and P.-A. Tesson 1 , 1 Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw, Poland (jc@cbk.pan.wroc.pl), 2 Institute of Geology, Adam Mickiewicz University, ul. Bogumila Krygowskiego 12, 60-680 Poznan, Poland, 3 Space Science and Technology Centre, Curtin University, Kent Street, Bentley, Perth, Western Australia 6102, Australia.

We study rocks falling from exposed outcrops of bedrock in martian impact craters. Those rockfalls have left trails on the slope over which they have bounced and/or rolled. Craters at ~20°N/S have notably higher frequencies on their equator-facing slopes compared to other slope-orientations. Our interpretation is that thermal stress is playing a more important role than ice-presence in rock breakdown on modern Mars.

RECENT MAGMATIC PLUMBING SYSTEM B. Pieterek, J. Ciazela, D. Mège, P.-A. Tesson, M. Ciazela, J. Gurgurewicz, A. Lagain, and A. Muszyński Institute of Geology, Adam Mickiewicz University, ul. Bogumila Krygowskiego 12, 60-680 Poznan, Poland (barpie@amu.edu.pl), Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw, Poland, Space Science and Technology Centre, Curtin University, Kent Street, Bentley, Perth, Western Australia 6102, Australia.