adsabs/AstroCLIMB huggingface dataset:
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: Regional context and geospatial distribution of potential karstic skylight features in Hebrus Valles, Mars. (a) Mars Orbiter Laser Altimeter (MOLA) global topography illustrating the location of Hebrus Valles relative to Tharsis and Elysium volcanic provinces. (b) Regional elevation map of the Hebrus Valles–Hephaestus Fossae region, highlighting skylight cave candidates identified in this study (pink stars) and previously reported features (black stars) by D. Sulcanese et al. (2018). (c) THEMIS IR mosaic overlaid with geomorphic features including outflow channels, troughs, pit lines, wrinkle ridges, and mapped skylights. The spatial correlation of skylights with tectonic and fluvial systems, especially at pit termini and trough intersections, suggests a possible aqueous and structural control on their formation.
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: HiRISE-based geomorphological analysis of SK1 supporting a karstic collapse origin linked to water-mediated processes. (a) Digital Terrain Model (DTM) elevation map with 1 m contour intervals reveals a closed, asymmetrical depression bounded by steep scarps. (b) Slope map derived from the same DTM highlights localized steep gradients along the cavity walls. (c) 3D point cloud model further illustrates the depression’s verticality and volume asymmetry. (d) HiRISE DTM (DTEEC 055209 2015 060260 2015 U01; M. C. Malin et al. 2007; A. S. McEwen et al. 2007; A. S. McEwen 2009) showing nested elevation zones (Areas 1–3) within a 500 m buffer highlights differential subsidence magnitudes. Collectively, these datasets support a karstic collapse origin involving lithological weakening and void formation in water-soluble substrate.
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: Geological context of skylight candidates in Hebrus Valles. Skylight candidates (yellow stars) are mapped in relation to pit lines, outflow channels, and sinkholes, revealing their spatial association with fluvial systems. Mapping builds on earlier interpretations (J. A. P. Rodriguez et al. 2012) and was refined in later analyses (D. Sulcanese et al. 2018; R. Sharma et al. 2019). THEMIS daytime infrared image data (P. R. Christensen et al. 2004) has been used for regional mapping.
Paper: The Photochemical Plausibility of Warm Exo-Titans Orbiting M Dwarf Stars
Authors: Sukrit Ranjan, Nicholas F. Wogan, Ana Glidden, Jingyu Wang, Kevin B. Stevenson, Nikole Lewis, Tommi Koskinen, Sara Seager, Hannah R. Wakeford, Roeland P. van der Marel
Figure caption: CH4 net chemical loss rate (﹩{L}_{{\,\rm{CH}\,}_{4}}﹩) and lifetime (﹩{\tau }_{{\,\rm{CH}\,}_{4}}﹩) as a function of the partial surface pressure of methane. The pink line corresponds to Photochem calculations. The yellow line corresponds to CH4 loss estimated via diffusion-limited escape of equivalent hydrogen, following M. A. Thompson et al. 2022. The black diamond corresponds to true Titan. The blue diamond corresponds to the assumption that ﹩{\tau }_{{\,\rm{CH}\,}_{4}}\propto \tfrac{1}{{F}_{\mathrm{EUV}}}﹩ (M. Turbet et al. 2018). The CH4 loss rate increases sublinearly with CH4 concentration, meaning that the lifetime increases with ﹩{p}_{{\,\rm{CH}\,}_{4}}﹩ and exceeds both the diffusion-limited hydrogen escape estimate and the FEUV estimate at high ﹩{p}_{{\,\rm{CH}\,}_{4}}﹩. However, the TRAPPIST-1e CH4 lifetime remains orders of magnitude below the true Titan CH4 lifetime across the range of ﹩{p}_{{\,\rm{CH}\,}_{4}}﹩ considered, meaning that a warm M dwarf exo-Titan is much less likely than a true Titan.
Paper: Unusually High Gas-to-dust Ratios Observed in High-redshift Quiescent Galaxies
Authors: Justin S. Spilker, Katherine E. Whitaker, Desika Narayanan, Rachel Bezanson, Sarah Bodansky, Vincenzo R. D'Onofrio, Robert Feldmann, Andy D. Goulding, Jenny E. Greene, Mariska Kriek, Yuanze Luo, David J. Setton, Katherine A. Suess, Arjen van der Wel, Margaret E. Verrico, Christina C. Williams, Charity Woodrum, Po-Feng Wu
Figure caption: SIMBA exhibits a tight relationship between sSFR and ﹩{f}_{{{\rm{H}}}_{2}}﹩ but often a sharp decrease in fdust in quenched galaxies (KW21a). These trends are in broad agreement with observations, including our own. Our measurements are shown as large diamonds, color-coded according to δGDR, and the stacked nondetection as a large square. Individual quiescent galaxies from the literature are shown as circles (for detections) or left-facing triangles (2σ upper limits). Literature stacking experiments are shown similarly as open symbols. The galaxy ALMA.14 (M. Hayashi et al. 2018) is the only literature source with a measured δGDR. Galaxies from SIMBA are shown as small dots, color-coded according to δGDR. The dotted lines in the left-hand panel are lines of constant gas depletion time ﹩{t}_{{\rm{dep}}}={M}_{{{\rm{H}}}_{2}}﹩/SFR; the lines in the right-hand panel show the same if one also assumes δGDR = 100. Note that the δGDR color scaling uses 2σ limits where needed; δGDR is more directly visualized in Figure 4.
Paper: Unusually High Gas-to-dust Ratios Observed in High-redshift Quiescent Galaxies
Authors: Justin S. Spilker, Katherine E. Whitaker, Desika Narayanan, Rachel Bezanson, Sarah Bodansky, Vincenzo R. D'Onofrio, Robert Feldmann, Andy D. Goulding, Jenny E. Greene, Mariska Kriek, Yuanze Luo, David J. Setton, Katherine A. Suess, Arjen van der Wel, Margaret E. Verrico, Christina C. Williams, Charity Woodrum, Po-Feng Wu
Figure caption: We find values of δGDR much higher than the typically assumed value of 100 in our sample of z ∼ 1 quiescent galaxies—even the most “dust-rich” object has δGDR ≈ 300, and we find a 2σ limit δGDR ≳ 1200 from our stack of undetected galaxies. Our observations, and others from the literature, are generally consistent with predictions from SIMBA. We highlight ALMA.14 (M. Hayashi et al. 2018) as the only other object with a measured δGDR, and MRG-2129 (K. E. Whitaker et al. 2021b; T. Morishita et al. 2022) with a 2σ upper limit δGDR ≲ 50. Symbols otherwise are as in Figure 3; all limits are 2σ.
Paper: Unusually High Gas-to-dust Ratios Observed in High-redshift Quiescent Galaxies
Authors: Justin S. Spilker, Katherine E. Whitaker, Desika Narayanan, Rachel Bezanson, Sarah Bodansky, Vincenzo R. D'Onofrio, Robert Feldmann, Andy D. Goulding, Jenny E. Greene, Mariska Kriek, Yuanze Luo, David J. Setton, Katherine A. Suess, Arjen van der Wel, Margaret E. Verrico, Christina C. Williams, Charity Woodrum, Po-Feng Wu
Figure caption: Our sample of z ∼ 1 quiescent galaxies (diamonds) is empirically faint in dust continuum emission, regardless of any calibration or conversion factors. Compared to star-forming galaxies at low (circles) or high redshifts (squares), our sample galaxies have rest-frame 850 μm continuum luminosities weaker by 0.4 to more than 0.8 dex (2σ limit) given the observed CO luminosity. The dashed line and gray shaded regions show the best-fit relation and inner ±1σ, 2σ scatter from N. Scoville et al. (2023).
Paper: Unusually High Gas-to-dust Ratios Observed in High-redshift Quiescent Galaxies
Authors: Justin S. Spilker, Katherine E. Whitaker, Desika Narayanan, Rachel Bezanson, Sarah Bodansky, Vincenzo R. D'Onofrio, Robert Feldmann, Andy D. Goulding, Jenny E. Greene, Mariska Kriek, Yuanze Luo, David J. Setton, Katherine A. Suess, Arjen van der Wel, Margaret E. Verrico, Christina C. Williams, Charity Woodrum, Po-Feng Wu
Figure caption: In contrast to the mild decline of ﹩{f}_{{{\rm{H}}}_{2}}﹩ with increasing Mstar at all sSFRs, SIMBA predicts no clear trend between fdust and Mstar for quiescent galaxies. Observed galaxies scatter both above and below the expected ﹩{f}_{{{\rm{H}}}_{2}}﹩, while the most massive quiescent galaxies have lower fdust than predicted. Circles and error bars/shaded regions correspond to the median and 1σ interval of SIMBA simulated galaxies, while diamonds, squares, and small circles are observed galaxies as in previous figures. All upper limits (downward triangles) are 2σ.
Paper: The Photochemical Plausibility of Warm Exo-Titans Orbiting M Dwarf Stars
Authors: Sukrit Ranjan, Nicholas F. Wogan, Ana Glidden, Jingyu Wang, Kevin B. Stevenson, Nikole Lewis, Tommi Koskinen, Sara Seager, Hannah R. Wakeford, Roeland P. van der Marel
Figure caption: Key photochemical modeling inputs.
Paper: Unusually High Gas-to-dust Ratios Observed in High-redshift Quiescent Galaxies
Authors: Justin S. Spilker, Katherine E. Whitaker, Desika Narayanan, Rachel Bezanson, Sarah Bodansky, Vincenzo R. D'Onofrio, Robert Feldmann, Andy D. Goulding, Jenny E. Greene, Mariska Kriek, Yuanze Luo, David J. Setton, Katherine A. Suess, Arjen van der Wel, Margaret E. Verrico, Christina C. Williams, Charity Woodrum, Po-Feng Wu
Figure caption: Tapered ALMA 345 GHz cutout images of our quiescent galaxy sample. Contours are drawn at ±2σ, 3σ, where σ varies from 20.6 to 22.6 μJy beam−1. Only C130284 and C132776 are detected at >3σ. Dashed white circles indicate the 2″ photometric apertures.
Paper: The Photochemical Plausibility of Warm Exo-Titans Orbiting M Dwarf Stars
Authors: Sukrit Ranjan, Nicholas F. Wogan, Ana Glidden, Jingyu Wang, Kevin B. Stevenson, Nikole Lewis, Tommi Koskinen, Sara Seager, Hannah R. Wakeford, Roeland P. van der Marel
Figure caption: Atmospheric COX on a warm exo-Titan TRAPPIST-1e (﹩{p}_{{\,\rm{CH}\,}_{4}}=3\times 1{0}^{-2}﹩ bar). The simultaneous presence of abundant CH4 and H2O in the warm exo-Titan scenario results in abundant CO and maybe CO2, which are potentially detectable.
Paper: The Photochemical Plausibility of Warm Exo-Titans Orbiting M Dwarf Stars
Authors: Sukrit Ranjan, Nicholas F. Wogan, Ana Glidden, Jingyu Wang, Kevin B. Stevenson, Nikole Lewis, Tommi Koskinen, Sara Seager, Hannah R. Wakeford, Roeland P. van der Marel
Figure caption: Equilibrium constant for the key reactions H2 + CH3 ↔ H + CH4, H + CH3 + M ↔ CH4 + M. We find Keq decreases with temperature for both reactions, implying reduced CH4 stability at higher temperatures.
Paper: Polar Filaments Capture High-latitude Solar Poloidal Field Interactions and Can Foretell the Future Sunspot Cycle Amplitude before Polar Field Precursors
Authors: Srinjana Routh, Shaonwita Pal, Dibyendu Nandy, Subhamoy Chatterjee, Dipankar Banerjee, Mohd. Saleem Khan
Figure caption: (Left panel) A representative Meudon hand-drawn synoptic chart after calibration corresponding to the Carrington rotation 1123. (Right panel) A binary segmented image showcasing the extracted filaments, while the polar filaments (∣θ∣ ≥ 50°) are separately identified with a red contour from the same filaments.
Paper: Polar Filaments Capture High-latitude Solar Poloidal Field Interactions and Can Foretell the Future Sunspot Cycle Amplitude before Polar Field Precursors
Authors: Srinjana Routh, Shaonwita Pal, Dibyendu Nandy, Subhamoy Chatterjee, Dipankar Banerjee, Mohd. Saleem Khan
Figure caption: Top panel: the red curve shows the time series of the polar filament area in the northern hemisphere from solar cycles 16–21, while the black curve represents the northern hemispheric sunspot area obtained from S. Mandal et al. (2020). The lighter red and black curves in the background indicate the Carrington-rotation-aggregated and monthly averaged polar filament area and sunspot area, respectively, while the darker red and black curves show their corresponding 13 month running averages. The magenta curve denotes the northern hemispheric polar flux generated from the data-driven optimized surface flux transport (SFT) model. Green dashed lines indicate the epochs of polar field reversal. Middle panel: this panel shows the spatiotemporal distribution of the radial magnetic field (Br) from solar cycles 16–21, generated using a data-driven optimized SFT model (S. Pal & D. Nandy 2025). Red and black colors represent regions of positive and negative magnetic polarity, respectively. Bottom panel: the red curve shows the time series of the polar filament area in the southern hemisphere from solar cycles 16–21, while the black curve represents the southern hemispheric sunspot area obtained from S. Mandal et al. (2020). The lighter red and black curves in the background indicate Carrington-rotation-aggregated and monthly averaged polar filament parameters and sunspot area, respectively, while the darker red and black curves represent their corresponding 13 month running averages. The blue curve denotes the southern hemispheric polar flux generated using the same SFT model . Green dashed lines indicate the epochs of polar field reversal.
Paper: Polar Filaments Capture High-latitude Solar Poloidal Field Interactions and Can Foretell the Future Sunspot Cycle Amplitude before Polar Field Precursors
Authors: Srinjana Routh, Shaonwita Pal, Dibyendu Nandy, Subhamoy Chatterjee, Dipankar Banerjee, Mohd. Saleem Khan
Figure caption: Correlation of polar filament remnant over solar cycle (SC) N and N − 1 with maximum sunspot area (SSA) of cycle N + 1. The top left panel shows the correlation between the remnant average polar filament area, Δ〈AN〉, and the maximum sunspot area of the N + 1th cycle. The top right panel displays the corresponding correlation between Δ〈LN〉 and the peak sunspot area of the next cycle. Red and blue circles represent data from the northern and southern hemispheres, respectively. The cycle number labeling each circle refers to cycle N. The black dashed line in both panels indicates the best linear fit to the data. Bottom panels show the result from sliding the correlation coefficient in time Δt before the end of cycle N calculated for the Δ〈AN〉 (left) and Δ〈LN〉 (right), showing statistically significant (p-value < 0.05) correlation with ﹩{\mathrm{SSA}}_{\max }^{N+1}﹩ for Δt ≤ 5 yr measured relative to the solar minimum of cycle N.
Paper: Polar Filaments Capture High-latitude Solar Poloidal Field Interactions and Can Foretell the Future Sunspot Cycle Amplitude before Polar Field Precursors
Authors: Srinjana Routh, Shaonwita Pal, Dibyendu Nandy, Subhamoy Chatterjee, Dipankar Banerjee, Mohd. Saleem Khan
Figure caption: Latitudinal distribution and temporal evolution of polar filament (a) area and (b) length, marked by hemisphere for solar cycles 16–21. (Middle panels) The latitudinal distribution of all filaments extracted is presented, revealing a characteristic butterfly-like pattern, with the polar filaments (∣θ∣ ≥ 50°) highlighted in red and blue for the northern and southern hemispheres, respectively. (Top panels) The temporal evolution of (a) area and (b) length of the polar filaments in the northern hemisphere (shown in red continuous lines), compared with the sunspot area (shown in dashed black lines) in the same. The comparatively lighter red and black curves in the background show Carrington-rotation-aggregated and monthly averaged polar filament parameters and sunspot area, respectively. Dim gray dotted lines indicate the end epoch of each cycle. (Bottom panels) The same is shown in the southern hemisphere. All time series have been smoothed using a 13 month running average to enhance clarity.
Paper: Polar Filaments Capture High-latitude Solar Poloidal Field Interactions and Can Foretell the Future Sunspot Cycle Amplitude before Polar Field Precursors
Authors: Srinjana Routh, Shaonwita Pal, Dibyendu Nandy, Subhamoy Chatterjee, Dipankar Banerjee, Mohd. Saleem Khan
Figure caption: The left panel shows the correlation between the remnant average polar filament area, Δ〈AN〉, and the polar flux at the end of the Nth cycle. The right panel displays the corresponding correlation between Δ〈LN〉 and the polar flux strength of the end of sunspot cycle N. Red and blue circles represent data from the northern and southern hemispheres, respectively. The cycle number labeling each circle refers to cycle N. The black dashed line in both panels indicates the best linear fit to the data.
Paper: The First RELHIC? Cloud-9 is a Starless Gas Cloud 
Authors: Gagandeep S. Anand, Alejandro Benítez-Llambay, Rachael Beaton, Andrew J. Fox, Julio F. Navarro, Elena D'Onghia
Figure caption: Top left: the spatial distribution of sources fulfilling our quality criteria. The green dashed circle indicates the effective radius (8﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 or 180 pc projected) of a Leo T analog at the distance of M94, and is centered at the location of Cloud-9. Top right: CMD of the field. The three sources within the green circle in the top left panel are shown in green. We also show an RGB isochrone for an old, metal-poor stellar population (10 Gyr, [Fe/H] = −2.0 dex) drawn from MIST, and placed at the distance of M94. The green crosses on the right-hand side indicate typical photometric uncertainties for various F814W magnitudes at the color of the RGB isochrone. Bottom left: photometric completeness distributions for both of our filters, as determined by the artificial star experiments. Bottom right: difference between input and output magnitudes from the artificial star experiments for the primary CMD filter (F814W).
Paper: The First RELHIC? Cloud-9 is a Starless Gas Cloud 
Authors: Gagandeep S. Anand, Alejandro Benítez-Llambay, Rachael Beaton, Andrew J. Fox, Julio F. Navarro, Elena D'Onghia
Figure caption: Top: a color composite of our ACS/WFC1 imaging (∼202″ × 100″). The green circle (r = 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩4) marks the VLA H I maximum column density, with a radius corresponding to the effective radius of a Leo T analog at the distance of M94. Bottom: simulated dwarf galaxies spanning a range of stellar masses, generated under the same observing conditions and shown at the same physical scale as the ACS data. A Leo T analog (M⋆ = 105 M⊙) would be readily detected, but no stellar counterpart is visible down to at least M⋆ ∼ 103.5M⊙.
Paper: The First RELHIC? Cloud-9 is a Starless Gas Cloud 
Authors: Gagandeep S. Anand, Alejandro Benítez-Llambay, Rachael Beaton, Andrew J. Fox, Julio F. Navarro, Elena D'Onghia
Figure caption: H I–stellar mass relation for the ALFALFA Sloan Digital Sky Survey catalog (isocontours; A. Durbala et al. 2020). Newly identified dwarf galaxies in the local volume detected with the FAST All Sky HI Survey (FASHI) are shown as green points (I. D. Karachentsev et al. 2024). For comparison, Leo T, KK 153, Leo P, and Cloud-9 are also shown. The stellar mass upper limit for Cloud-9 (red star symbol) underscores its extreme gas richness relative to its possible stellar mass, if interpreted as an ultrafaint galaxy.
Paper: The First RELHIC? Cloud-9 is a Starless Gas Cloud 
Authors: Gagandeep S. Anand, Alejandro Benítez-Llambay, Rachael Beaton, Andrew J. Fox, Julio F. Navarro, Elena D'Onghia
Figure caption: Histograms of 10,000 simulations performed for each of a range of input stellar masses (shown in the legend). The x-axis values show the remaining number of visible stars in the simulated CMDs after applying our observational systematics.
Paper: The First RELHIC? Cloud-9 is a Starless Gas Cloud 
Authors: Gagandeep S. Anand, Alejandro Benítez-Llambay, Rachael Beaton, Andrew J. Fox, Julio F. Navarro, Elena D'Onghia
Figure caption: Digitized Sky Survey image covering a 10′ × 10′ region around Cloud-9. The VLA H I contours (A. Benítez-Llambay et al. 2024) are shown in red, and the footprint of our HST/ACS observations is shown in blue.
Paper: Direct Observation of the X-Ray Counterpart of the Hα Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster
Authors: Adrien Picquenot, Fabio Acero, Valeria Olivares, Michela Negro, Gabriel W. Pratt
Figure caption: On top, the distribution of the X-ray and Hα filaments. On the left, a map of the X-ray filaments from Figure 2. On the right, Hα filaments observed by the WIYN 3.5 m telescope, first presented in C. J. Conselice et al. (2001). Superimposed, the green box regions we defined to extract the filament profiles. The white annular regions are the ones used in our template fit (see results in Table 1). For both images, the scale is in square root. On the bottom, normalized profiles extracted from the X-ray filamentary structures found in the X-ray and Hα filaments are shown in red and black, respectively. The X-ray filaments are obtained with the pGMCA method, while the Hα come from the WIYN 3.5 m telescope.
Paper: Direct Observation of the X-Ray Counterpart of the Hα Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster
Authors: Adrien Picquenot, Fabio Acero, Valeria Olivares, Michela Negro, Gabriel W. Pratt
Figure caption: Maps of the sloshing spiral and X-ray filaments. On the left, a map of the cold sloshing front retrieved by pGMCA between 0.5 and 4.5 keV on the spectrally rebinned, spatially native data, cleaned, and smoothed. On the right, a map of the X-ray filaments found by pGMCA between 0.5 and 4.5 keV on the spectrally rebinned, spatially native data, smoothed. For both images, the scale is in square root.
Paper: Direct Observation of the X-Ray Counterpart of the Hα Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster
Authors: Adrien Picquenot, Fabio Acero, Valeria Olivares, Michela Negro, Gabriel W. Pratt
Figure caption: Image of the sloshing spiral from Figure 2 superimposed with spectral analysis regions. The white annular regions are the ones used in our template fit (see results in Table 1); the green region is the one used in the traditional Xspec analysis (see Table 2).
Paper: Direct Observation of the X-Ray Counterpart of the Hα Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster
Authors: Adrien Picquenot, Fabio Acero, Valeria Olivares, Michela Negro, Gabriel W. Pratt
Figure caption: Best fit for the template fitting method on all annular regions combined. The regions are shown in Figure 3, left, and Figure 5.
Paper: Direct Observation of the X-Ray Counterpart of the Hα Filaments and of the Sloshing Spiral in the Perseus Galaxy Cluster
Authors: Adrien Picquenot, Fabio Acero, Valeria Olivares, Michela Negro, Gabriel W. Pratt
Figure caption: Three components found by the pGMCA algorithm between 0.1 and 1.8 keV on the spectrally native, spatially rebinned data. On the left, spatial maps in square root and on the right, the associated integrated spectrum.