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Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Left panel: radio luminosity light curve of AT 2024wpp  at ≈ 10 GHz in the context of other transients. FBOTs stand out for their luminosities that are intermediate between ultrarelativistic GRBs and SNe, while also showing a characteristic bell-shaped light curve peaking at ≈80 days followed by a very steep decay. This shared radio behavior is at the core of the “universal density profile” that we discuss in Section 8.1. Right panel: the (sparsely populated) millimeter-band (80–200 GHz) phase space of light curves of different extragalactic transients GRBs (T. Eftekhari et al. 2022, and references therein), tidal disruption events (E. Berger et al. 2012; Q. Yuan et al. 2016; Y. Cendes et al. 2021; I. Andreoni et al. 2022; D. A. Perley et al. 2022), CCSNe (K. W. Weiler et al. 2007; A. Horesh et al. 2013), and FBOTs (A. Y. Q. Ho et al. 2019, 2022, 2023a, 2023b). In stark contrast with the well-behaved 10 GHz emission, the millimeter emission from even this small sample of FBOTs displays remarkable diversity, likely mirroring the diverse properties of the innermost material the shock emission is emerging from.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Left panel: soft X-ray luminosity evolution of AT 2024wpp in the context of explosive transients capable of launching relativistic ejecta (long GRBs, tidal disruption events, H-poor SNe). FBOTs span the entire dynamical range of X-ray luminosity observed for long GRBs to date. Right panel: zoom-in of the region of luminous FBOTs with X-ray emission (stars) and fast transients (open gray circles). AT 2024wpp  is only the second FBOT for which we were able to sample the X-ray emission at δt < 10 days. While the initial Lx ≈  a few × 1043 erg s−1 is not dissimilar from AT 2018cow, AT 2020xnd, and AT 2023fhn, AT 2024wpp  stands out at later times δt ≳ 30 days for its longer-lived and spectrally harder X-ray emission. Similar to AT 2018cow is the remarkably fast late-time decay. We add to this panel other fast transients observed in the X-rays: of these, the very luminous and fast-evolving optical emission from “Dougie” bears close similarities to luminous FBOTs. References: R. Margutti et al. (2013, 2019), D. L. Coppejans et al. (2020), J. S. Bright et al. (2022), Y. Yao et al. (2022), D. Matthews et al. (2023), A. Y. Q. Ho et al. (2023b), A. A. Chrimes et al. (2024b), G. Migliori et al. (2024) and references therein.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: A cartoon diagram (not to scale) showing the geometry of AT 2024wpp and various emission components in the context of an engine-driven progenitor model. The physical picture is motivated by the models presented in D. Tsuna & W. Lu (2025) and B. D. Metzger (2022). Both these models invoke super-Eddington accretion onto a compact object (NS or BH) in different astrophysical contexts. The disk wind outflows from the accretion disk generate 56Ni-poor asymmetric ejecta with a range of velocities—fast outflow (v ≈ 0.4c) from the interior of the accretion disk and slow winds from the outer radii of the disk. In this framework, the X-ray emission originates from the central engine, while the optical emission arises from reprocessing of X-rays. Here we are agnostic about the reprocessing layer, whereas D. Tsuna & W. Lu (2025) assume it to be an SN ejecta and B. D. Metzger (2022) assumes it to be the fast disk wind ejecta. The low-velocity emission lines are from the slow disk winds from the outer radii of the accretion disk. Radio emission arises owing to the interaction between fastest disk wind and CSM at R ≳ 1016 cm.
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Radio spectra of AT 2024wpp in the time range δtrest ≈ 13–161 days acquired with MeerKAT, GMRT, ATCA, ATA, and ALMA. The purple diamonds denote the VLA flux measurements from G. Schroeder et al. (2024). Inverted triangles mark the 3σ flux density upper limits. Solid lines represent best-fit BPL models with smoothing parameter s = −1 and optically thin spectral index α1 = −1.5. AT 2024wpp shows a complex evolution with two unprecedented elements: (i) an extremely rapid and delayed rise of the millimeter emission captured by ALMA, and (ii) radio spectrum inversion in the last two ATCA epochs (emphasized with circles).
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Blast wave energy vs. shock velocity of FBOTs AT 2024wpp (δt ≈ 32–118 days), AT 2018cow (δt ≈ 22 days), CSS 161010 (δt ≈ 99 days), AT 2020xnd (δt ≈ 38 days), AT2022mrf (δt ≈ 261 days), and AT 2023fhn (δt ≈ 138 days). References: R. Margutti et al. (2019), A. Y. Q. Ho et al. (2019), D. L. Coppejans et al. (2020), J. S. Bright et al. (2022), A. Y. Q. Ho et al. (2022), Y. Yao et al. (2022), A. A. Chrimes et al. (2024a).
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Radio spectral luminosities of different astrophysical transients. Lp denotes the peak spectral luminosity in the 8–10 GHz band. νp and tp represent the peak frequency and peak time of the radio SED, respectively. The dashed lines denote the mean shock velocity in an SSA scenario (R. A. Chevalier 1998). References: R. Margutti et al. (2019), A. Y. Q. Ho et al. (2019), D. L. Coppejans et al. (2020), J. S. Bright et al. (2022), A. Y. Q. Ho et al. (2022), Y. Yao et al. (2022), A. A. Chrimes et al. (2024a).
Paper: The Most Luminous Known Fast Blue Optical Transient AT 2024wpp: Unprecedented Evolution and Properties in the X-Rays and Radio
Authors: Nayana A. J., Raffaella Margutti, Eli Wiston, Tanmoy Laskar, Giulia Migliori, Ryan Chornock, Timothy J. Galvin, Natalie LeBaron, Aprajita Hajela, Collin T. Christy, Itai Sfaradi, Daichi Tsuna, Olivia Aspegren, Fabio De Colle, Brian D. Metzger, Wenbin Lu, Paz Beniamini, Daniel Kasen, Edo Berger, Brian W. Grefenstette, Kate D. Alexander, G. C. Anupama, Deanne L. Coppejans, Luigi F. Cruz, David R DeBoer, Maria R. Drout, Wael Farah, Xiaoshan Huang, W. V. Jacobson-Galán, Dan Milisavljevic, Alexander W. Pollak, Nathan J. Roth, Huei Sears, Andrew Siemion, Sofia Z. Sheikh, James F. Steiner, Indrek Vurm
Figure caption: Evolution of the radius of the optical photosphere and radio photosphere of AT 2018cow (left panel; R. Margutti et al. 2019) and AT 2024wpp (right panel; Paper I). The size of the optical photosphere is derived by fitting a blackbody function to the bolometric luminosities. The size of the radio photosphere (rest frame) is estimated by modeling single-epoch radio SEDs adopting the SSA formalism (R. A. Chevalier 1998).
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: Distance and proper motion distributions for candidate pulsar–open cluster associations. Left panel: each row represents a pulsar–cluster pair, with open cluster distances shown as blue error bars (±5σoc, where σoc is the cluster distance uncertainty) and pulsar distances marked by red (±3σpsr) and light red (±5σpsr) error bars, with σpsr being the pulsar distance uncertainty. Right panel: proper motion vectors for open clusters (blue arrows) and pulsars (red arrows). Each row corresponds to the pair in the left panel, while segment lengths indicate proper motion magnitudes and arrows show directions.
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: Properties of the member stars of UBC 525 and the binary system PSR J1302−6350/LS 2883. In all panels, the color of the dots indicates the probability of cluster membership (as defined in the color bar); the black (red) star marks PSR J1302−6350 (LS 2883). In the upper right panel, the pulsar proper motion was measured in J. C. A. Miller-Jones et al. (2018). The lower left panel shows parallax vs. G magnitude, with the black and red stars indicating the parallax ranges of LS 2883 using Gaia DR2 (R. J. Jennings et al. 2018) and DR3, respectively. The lower right panel shows the color–magnitude diagram using Gaia DR3’s photometric bands. All data are taken from Gaia DR3 unless otherwise specified.
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: Past trajectories of PSR J0630−2834 and its potential birth open clusters—Collinder 132 and CWNU 45. The plus symbol marks a 0.5 Myr interval along the paths. Blue and black lines trace the past trajectories of the clusters, while magenta and green dots indicate the past positions of member stars in Collinder 132 and CWNU 45, respectively. Assuming a radial velocity of −151 km s−1, the pulsar’s trajectory (red line) crossed CWNU 45 about 0.86 Myr ago (solid line) and reached the region of Collinder 132 about 1.17 Myr ago (dashed line). The black dashed circle shows the 3r50 extent of CWNU 45.
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: The sky location of PSR J1302−6350, two open clusters (UBC 525 and HSC 2546), the stellar association Cen OB1, and their member stars. The magenta and green dashed ellipses mark the 3r50 regions of UBC 525 and HSC 2546, respectively, with their member stars shown as dots. The gray dashed ellipse indicates the region of Cen OB1 with a radius of 3°, and the gray triangles denote its member stars (M. A. Corti & R. B. Orellana 2013).
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: Distributions of minimum separation Δmin and corresponding encounter time τ for PSR J0630−2834 and Collinder 132, with an encounter time of ﹩1.{6}_{-0.3}^{+0.4}﹩ Myr. The solid red curve is the theoretically expected distribution of Δmin Equation (2), while the color bar indicates the probability of each pixel.
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: The spatial distribution of three possible pulsar–open cluster associations. The left panels display the sky location for pulsars (red stars), the center of open clusters (blue crosses), and cluster member stars (green points). Each open cluster is shown with a radius of 3r50 (the black dashed line). The right panels present three-dimensional Cartesian coordinates of pulsars (black dots). The red dots represent those within 3r50 from the center of the open cluster, while the green points show the cluster members assuming the same distance as the cluster center (but different R.A. and decl.).
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: The past trajectory of PSR J0630−2834 (with its current position marked by a red star) relative to the Antlia SNR and the open cluster Collinder 132. The blue dot indicates the position of Antlia SNR, with its extension marked by a blue dashed circle. The red solid line shows the pulsar trajectory up to 0.72 Myr ago for a radial velocity of 454 km s−1. The black dashed line assumes a pulsar radial velocity of −230 km s−1 and shows the pulsar trajectory up to 1.06 Myr ago, which coincides with Collinder 132, whose extent is shown by a green dashed circle and current position by a green dot.
Paper: A Census of Pulsars in Possible Association with Galactic Open Clusters
Authors: Lu Zhou, Zhi-Qiang You, Lu Li, Xiao-Jin Liu, Xing-Jiang Zhu, Zong-Hong Zhu
Figure caption: As is Figure 1 but for pulsar-moving group associations, showing (left) distance comparisons and (right) proper motion vector diagrams.
Paper: Azimuthal Misalignments in Stellar Warp Structure as Dynamical Tracers of Mergers in Milky Way–like Galaxies
Authors: Lekshmi Thulasidharan, Elena D'Onghia, Robert Benjamin
Figure caption: Azimuthal variation of the average vertical displacement 〈Z〉 for the present-day snapshot (t = 0) of each model galaxy. Top panel: for each galaxy that developed a warp due to a major merger, we analyze the stars contributing to the warp, separating them into populations formed before and after the merger. This plot reveals the differences in warp structure between these two stellar populations, highlighting an intriguing azimuthal misalignment in the warp signature between pre- and postmerger stars. Bottom panel: same as the top panel, except that we corrected for the misalignment due to the differential rotation for premerger and postmerger populations.
Paper: Azimuthal Misalignments in Stellar Warp Structure as Dynamical Tracers of Mergers in Milky Way–like Galaxies
Authors: Lekshmi Thulasidharan, Elena D'Onghia, Robert Benjamin
Figure caption: X–Y plane maps of average vertical displacement 〈Z〉 for present-day snapshots (t = 0) of Subhalo IDs 540920, 482889, and 476266. These visualizations contrast the warp signatures found within the gaseous disk, stars formed after the merger, and stars formed before the merger. Each map illustrates how the galaxy’s vertical structure varies among its distinct stellar populations and gas, shedding light on the influence of the merger event on the observed galactic warp. In each model, the warp in the postmerger stellar disk aligns with the gaseous warp. In contrast, the premerger stellar population exhibits a distinct warp signature, appearing at a different orientation.
Paper: Azimuthal Misalignments in Stellar Warp Structure as Dynamical Tracers of Mergers in Milky Way–like Galaxies
Authors: Lekshmi Thulasidharan, Elena D'Onghia, Robert Benjamin
Figure caption: Density projection of warped Milky Way analogs from IllustrisTNG50 in the X–Y and X–Z plane.
Paper: Azimuthal Misalignments in Stellar Warp Structure as Dynamical Tracers of Mergers in Milky Way–like Galaxies
Authors: Lekshmi Thulasidharan, Elena D'Onghia, Robert Benjamin
Figure caption: Azimuthal variation of the average vertical displacement 〈Z〉 for the present-day snapshot (t = 0) of the model galaxy 459557. As this galaxy does not undergo a significant merger, the stellar population is divided into three age bins, 0–4, 4–8, and >8 Gyr, to compare their respective warp structures. (a) Maps of 〈Z〉 in the X–Y plane for the gaseous disk and stars in each age bin at the present day. (b) Azimuthal profiles of 〈Z〉 for stars in each age bin, illustrating the similarities in the warp signature across stellar populations.
Paper: Water-driven Accessible Potential Karstic Caves in Hebrus Valles, Mars: Implications for Subsurface Habitability
Authors: Ravi Sharma, Chunyu Ding, Francesco Soldovieri, Jiangwan Xu, Zihang Liang, Yachen Xie, Yan Su, Changzhi Jiang, YuXiao Zhi, Tang Chuanhu, Xiaohang Qiu, Zhonghan Lei, Haoyu Chen, Li Qingquan
Figure caption: Geochemical and surface conditions favoring karstic cave formation in the Hebrus Valles region. (a) GRS-derived (W. Boynton et al. 2007) water-equivalent hydrogen abundance map showing broad regional context. (b) Zoomed-in hydrogen map (inset from black box in (a)) reveals localized enrichment up to 3.73 wt% near skylight candidates. (c) TES (J. L. Bandfield 2002) sulfate mineral abundance map, and (d) its zoomed-in counterpart, reveal elevated sulfate concentrations colocated with skylight features. (e) TES (J. L. Bandfield 2002) carbonate abundance map, and (f) its zoomed-in counterpart, display carbonate enrichment across multiple skylight sites. (g) TES-derived (J. L. Bandfield 2002) surface dust abundance map indicates spatial variation in dust cover, its zoom-in of the region highlighted in (h), showing skylight sites occurring in low-dust zones likely associated with indurated surfaces. (i) TES-derived thermal inertia difference map (day–night) indicates moderate ThI values in the skylight zone, higher than unconsolidated dust yet lower than intact rock. These contrasts reflect surface heterogeneity, with dust mantles overlying more consolidated substrates. Comparison with TES mineral maps further supports this interpretation, as localized enrichments in sulfates, carbonates, feldspars, pyroxenes, olivine, hematite, and dust occur in association with skylight candidates—consistent with conditions favorable for karstic processes. Data from GRS (W. Boynton et al. 2007) and TES (M. T. Mellon et al. 2000; J. L. Bandfield 2002; N. E. Putzig & M. T. Mellon 2007) instruments were used in this study, while extraction of values at skylight point locations and their interpretation represent the authors’ analysis (Tables 1–3).
Paper: Water-driven Accessible Potential Karstic Caves in Hebrus Valles, Mars: Implications for Subsurface Habitability
Authors: Ravi Sharma, Chunyu Ding, Francesco Soldovieri, Jiangwan Xu, Zihang Liang, Yachen Xie, Yan Su, Changzhi Jiang, YuXiao Zhi, Tang Chuanhu, Xiaohang Qiu, Zhonghan Lei, Haoyu Chen, Li Qingquan
Figure caption: Conceptual model illustrating water-driven karstic cave development and subsurface habitability potential in Hebrus Valles, Mars. J. A. P. Rodriguez et al. (2012) interpreted the initiation of outflow channels at two large source pits as evidence of groundwater-sourced paleofloods, recognized knick-point retreat as an indicator of collapse into large subsurface voids, noted alignments with possible mud-volcanic structures, and emphasized the absence of downstream outflows—implying that infiltration water and sediments were accommodated within cavities. They further linked the flood source pits to the Hephaestus Fossae trough system, where collapse-related pitted lineations, polygonal troughs, and mud-volcanic chains highlight structural control on water pathways and void formation. Building on this framework, the present study shows that carbonate- and sulfate-bearing lithologies provided soluble substrates (Table 1), with dissolutional processes contributing to cavity enlargement and skylight development (Figures 1, 2, and 3). Our analysis also confirms that no groundwater outflows beyond the sinkhole clusters were identified, consistent with the interpretation of large subsurface voids. Thermal inertia values, higher than unconsolidated dust yet lower than intact rock, together with mineralogical evidence (Figure 4; Tables 2 and 3), reveal heterogeneous layering in which surface dust mantles over more indurated karstic material. Collectively, these geomorphological (Figures 1, 2, and 3), mineralogical and geochemical (Tables 1, 2, and 3), and thermophysical (Figure 4) signatures support the interpretation of the Hebrus skylights as dissolutional karst caves. The potential presence of past water, subsurface ice, and accessible cave resources within these voids further underscores their significance for resource utilization, astrobiological exploration, and broad scientific investigation. These environments offer opportunities to probe Mars’ hydrologic and climatic history, unravel dissolution-driven geological processes, and test advanced exploration technologies. As such, the Hebrus skylights emerge as prime targets for future human missions, long-term habitation studies, robotic surveys, advanced robotic dog–based investigations, and high-resolution radar probing of their internal architecture. Such efforts could deliver the first detailed images and 3D maps of extraterrestrial caves, opening unprecedented opportunities for science, exploration, and the search for life beyond Earth.