@article{20930,
  abstract     = {Context. Beta Pictoris is an A-type star that hosts a complex planetary system with two massive gas giants and a prominent debris disc. Variable absorption lines in its stellar spectrum have been interpreted as signatures of exocomets – comet-like bodies transiting the star. Stellar flybys can gravitationally perturb objects in the outer comet reservoir, altering their orbits and potentially injecting them into the inner system, thereby triggering exocomet showers.
Aims. We assessed the contribution of stellar flybys to the observed exocomet activity by reconstructing the stellar encounter history of β Pictoris in the past and future.
Methods. We used Gaia DR3 data, supplemented with radial velocities from complementary spectroscopic surveys, to compile a catalogue of stars currently within 80 pc of β Pictoris. Their orbits were integrated backwards and forwards in time in an axisymmetric Galactic potential (via the GALA package) to identify encounters within 2 pc of the system.
Results. We identified 99 416 stars currently within 80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including the eight components of five binaries) encounter β Pictoris within 2 pc between –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories also pass within 2 pc. We estimated the sample to be more than 60% complete within 0.5 Myr of today.
Conclusions. Despite β Pictoris being the eponym of its famous moving group, none of the identified encounters involved its moving group members; all are unrelated field stars. We found no encounter capable of shaping the observed disc structures, although stellar flybys may contribute to the long-term evolution of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction of the β Pictoris encounter history to date and provides a robust foundation for future dynamical simulations.},
  author       = {Gragera-Más, J. L. and Torres Rodriguez, Santiago and Mustill, A. J. and Villaver, E.},
  issn         = {1432-0746},
  journal      = {Astronomy & Astrophysics},
  publisher    = {EDP Sciences},
  title        = {{A kinematic history of stellar encounters with Beta Pictoris}},
  doi          = {10.1051/0004-6361/202555940},
  volume       = {704},
  year         = {2025},
}

@article{20932,
  abstract     = {Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial for understanding the properties of cosmic reionizers because the opacity of the intergalactic medium (IGM) prevents the direct detection of LyC emission from sources during the Epoch of Reionization (EoR). In this study, we confirm two new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03 and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively. These two LyC candidate leakers were detected in a catalog of 91 spectroscopically confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed properties that were proposed as indirect indicators of LyC emission, such as Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according to these properties, stacked the LyC observations of this subsample, and assessed the limits of the escape fractions in the stacks. We aim to enhance our understanding of LyC escape mechanisms and improve our predictions of the LyC fesc during the EoR by analyzing the individual candidates and the stacks in the context of the currently limited sample of known LyC leakers at z ∼ 3.},
  author       = {Liu, Y. and Mascia, Sara and Pentericci, L. and Watson, P. and Alavi, A. and Bergamini, P. and Bradač, M. and Calabrò, A. and Glazebrook, K. and Henry, A. and Llerena, M. and Merlin, E. and Metha, B. and Nanayakkara, T. and Napolitano, L. and Roy, N. and Siana, B. and Vanzella, E. and Vulcani, B. and Wang, X.},
  issn         = {1432-0746},
  journal      = {Astronomy & Astrophysics},
  publisher    = {EDP Sciences},
  title        = {{A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field}},
  doi          = {10.1051/0004-6361/202556410},
  volume       = {704},
  year         = {2025},
}

@article{20934,
  abstract     = { Supervised learning for causal discovery from observational data often achieves competitive performance despite seemingly avoiding the explicit assumptions that traditional methods require for identifiability. In this work, we analyze CSIvA (Ke et al., 2023) on bivariate causal models, a transformer architecture for amortized inference promising to train on synthetic data and transfer to real ones. First, we bridge the gap with identifiability theory, showing that the training distribution implicitly defines a prior on the causal model of the test observations: consistent with classical approaches, good performance is achieved when we have a good prior on the test data, and the underlying model is identifiable. Second, we find that CSIvA can not generalize to classes of causal models unseen during training: to overcome this limitation, we theoretically and empirically analyze \textit{when} training CSIvA on datasets generated by multiple identifiable causal models with different structural assumptions improves its generalization at test time. Overall, we find that amortized causal discovery still adheres to identifiability theory, violating the previous hypothesis from Lopez-Paz et al. (2015) that supervised learning methods could overcome its restrictions.},
  author       = {Montagna, Francesco and Cairney-Leeming, Maximilian T and Sridhar, Dhanya and Locatello, Francesco},
  issn         = {2835-8856},
  journal      = {Transactions on Machine Learning Research},
  publisher    = {ML Research Press},
  title        = {{Demystifying amortized causal discovery with transformers}},
  year         = {2025},
}

@article{20976,
  abstract     = {We present an experimental demonstration of an impedance-engineered Josephson parametric amplifier (IEJPA) fabricated in a single-step lithography process. Impedance-engineering is implemented using a lumped-element series LC circuit. We use a simpler lithography process where the entire device—impedance transformer and Josephson parametric amplifier (JPA)—is patterned in a single electron beam lithography step, followed by a double-angle Dolan-bridge technique for Al–AlOx–Al deposition. We observe amplification with 18 dB gain over a wide 400 MHz bandwidth centered around 5.3 GHz with added noise approaching the quantum limit, and a saturation power of −114 dBm. To accurately explain our experimental results, we extend existing theories for IEJPAs to incorporate the full sine nonlinearity of both the JPA and the transformer. Our work provides a route to simpler realization of broadband JPAs and a theoretical foundation for a regime of JPA operation that has been less explored in literature.},
  author       = {Patel, Lipi and Hawaldar, Samarth and Panikkar, Aditya and Shankar, Athreya and Suri, Baladitya},
  issn         = {1077-3118},
  journal      = {Applied Physics Letters},
  number       = {25},
  publisher    = {AIP Publishing},
  title        = {{Impedance-engineered Josephson parametric amplifier with single-step lithography}},
  doi          = {10.1063/5.0290636},
  volume       = {127},
  year         = {2025},
}

@article{20977,
  abstract     = {Hippocampal sharp-wave ripples (SPW-Rs) are high-frequency oscillations critical for memory consolidation. Despite extensive characterization in rodents, their detection in humans is limited by coarse spatial sampling, interictal epileptiform discharges (IEDs), and a lack of consensus on human ripple localization and morphology. Here, we demonstrate that mouse and human hippocampal ripples share spatial, spectral and temporal features, which are clearly distinct from IEDs. In recordings from male APP/PS1 mice, SPW-Rs were distinguishable from IEDs by multiple criteria. Hippocampal ripples recorded during NREM sleep in female and male surgical epilepsy patients exhibited similar narrowband frequency peaks and multiple ripple cycles in the CA1 and subiculum regions. Conversely, IEDs showed a broad spatial extent and wide-band frequency power. We developed a semi-automated, ripple curation toolbox (ripmap) to separate event waveforms by low-dimensional embedding to reduce false-positive rate in selected ripple channels. Our approach improves ripple detection and provides a firm foundation for future human memory research.},
  author       = {Maslarova, Anna and Shin, Jiyun N. and Navas Olivé, Andrea C and Vöröslakos, Mihály and Hamer, Hajo and Doerfler, Arnd and Henin, Simon and Buzsáki, György and Liu, Anli},
  issn         = {2041-1723},
  journal      = {Nature Communications},
  publisher    = {Springer Nature},
  title        = {{Spatiotemporal patterns differentiate hippocampal sharp-wave ripples from interictal epileptiform discharges in mice and humans}},
  doi          = {10.1038/s41467-025-66562-6},
  volume       = {16},
  year         = {2025},
}

@unpublished{20982,
  abstract     = {Plant cells respond to a wide range of stimuli through intracellular calcium (Ca2+) signaling. Cyclic nucleotide-gated channels (CNGCs) are a major class of plant Ca2+ channels, with 20 homologs in Arabidopsis. These tetrameric plasma membrane proteins act downstream of diverse signals, such as phytohormones, extracellular damage, cell wall integrity or temperature. Here, we identify a class of plant-specific proteins, Armadillo Repeat Only (ARO), as essential regulators of possibly all plant CNGCs. Abrogation of functional sporophytic AROs results in a phenotypic pattern strongly reminiscent of CNGC dysfunction, including defects in root gravitropism, root hair growth and morphology, stomatal movement, and responses to extracellular ATP and the phytohormone auxin. aro2/3/4 mutants are fully resistant to the toxic effects caused by overexpression of CNGCs. AROs colocalize and physically interact with multiple CNGCs and modulate CNGC-dependent currents in Xenopus oocytes. Structural modeling and site-directed mutagenesis reveal AROs tetramer formation surrounding the CNGC channel, interacting via its IQ domain. Taken together, plant CNGC channels don’t act alone, but in a larger complex - channelosome, first of a kind in plants.},
  author       = {Kulich, Ivan and Oulehlová, Denisa and Vladimirtsev, Dmitrii and Zou, Minxia and Lileikyte, Edita and Bondar, Alexey and Kulichová, Katarína and Janda, Martin and Iakovenko, Oksana and Neubergerová, Michaela and Studtrucker, Tanja and Pleskot, Roman and Dietrich, Petra and Fendrych, Matyas and Friml, Jiří},
  booktitle    = {bioRxiv},
  title        = {{Armadillo repeat only proteins are required for the function of plant CNGC channels}},
  doi          = {10.1101/2025.01.06.631460},
  year         = {2025},
}

@inproceedings{21020,
  abstract     = {Runtime verification offers scalable solutions to improve the safety and reliability of systems. However, systems that require verification or monitoring by a third party to ensure compliance with a specification might contain sensitive information, causing privacy concerns when usual runtime verification approaches are used. Privacy is compromised if protected information about the system, or sensitive data that is processed by the system, is revealed. In addition, revealing the specification being monitored may undermine the essence of third-party verification.
In this work, we propose two novel protocols for the privacy-preserving runtime verification of systems against formal sequential specifications. In our first protocol, the monitor verifies whether the system satisfies the specification without learning anything else, though both parties are aware of the specification. Our second protocol ensures that the system remains oblivious to the monitored specification, while the monitor learns only whether the system satisfies the specification and nothing more. Our protocols adapt and improve existing techniques used in cryptography, and more specifically, multi-party computation.
The sequential specification defines the observation step of the monitor, whose granularity depends on the situation (e.g., banks may be monitored on a daily basis). Our protocols exchange a single message per observation step, after an initialisation phase. This design minimises communication overhead, enabling relatively lightweight privacy-preserving monitoring. We implement our approach for monitoring specifications described by register automata and evaluate it experimentally.},
  author       = {Henzinger, Thomas A and Karimi, Mahyar and Thejaswini, K. S.},
  booktitle    = {Proceedings of the 2025 ACM SIGSAC Conference on Computer and Communications Security},
  isbn         = {9798400715259},
  location     = {Taipei, Taiwan},
  pages        = {2774--2787},
  publisher    = {Association for Computing Machinery},
  title        = {{Privacy-preserving runtime verification}},
  doi          = {10.1145/3719027.3765137},
  year         = {2025},
}

@inproceedings{21049,
  abstract     = {Post-hoc importance attribution methods are a popular tool for “explaining” Deep Neural Networks (DNNs) and are inherently based on the assumption that the explanations can be applied independently of how the models were trained. Contrarily, in this work we bring forward empirical evidence that challenges this very notion. Surprisingly, we discover a strong dependency on and demonstrate that the training details of a pre-trained model’s classification layer (<10% of model parameters) play a crucial role, much more than the pre-training scheme itself. This is of high practical relevance: (1) as techniques for pre-training models are becoming increasingly diverse, understanding the interplay between these techniques and attribution methods is critical; (2) it sheds light on an important yet overlooked assumption of post-hoc attribution methods which can drastically impact model explanations and how they are interpreted eventually. With this finding we also present simple yet effective adjustments to the classification layers, that can significantly enhance the quality of model explanations. We validate our findings across several visual pre-training frameworks (fully-supervised, self-supervised, contrastive vision-language training) and analyse how they impact explanations for a wide range of attribution methods on a diverse set of evaluation metrics.},
  author       = {Gairola, Siddhartha and Böhle, Moritz and Locatello, Francesco and Schiele, Bernt},
  booktitle    = {13th International Conference on Learning Representations},
  location     = {Singapore},
  publisher    = {ICLR},
  title        = {{How to probe: Simple yet effective techniques for improving post-hoc explanations}},
  year         = {2025},
}

@article{21057,
  abstract     = {Among the most puzzling early discoveries of JWST are “little red dots” (LRDs), compact red sources that host broad Balmer emission lines, and in many cases exhibit a “V-shaped” change in slope in the rest-optical. The physical properties of LRDs currently have order-of-magnitude uncertainties, because models to explain the continuum of these sources differ immensely. Here, we leverage the complete selection of red sources in the RUBIES program, supplemented with public PRISM spectra, to study the origin of this V shape. By fitting a broken power law with a flexible inflection point, we find that a large fraction of red Hα emitters at 2 < z < 6 exhibit a strong change in slope, and that all strong inflections appear associated with the Balmer limit (0.3645 μm). Using a simple model of a reddened active galactic nucleus (AGN) with an unobscured scattered-light component, we demonstrate that the observed V shape in LRDs is unlikely to occur at any specific wavelength if the entire continuum is dominated by light from a power-law AGN continuum. In contrast, models with an intrinsic feature at the Balmer limit, such as those that are dominated by an evolved stellar population, can produce the observed spectral shapes, provided that a reddened component picks up sufficiently redward of the break. While no model can comfortably explain the full LRD spectral energy distribution, the common inflection location suggests that a single component consistently dominates the rest-frame UV optical in LRDs, and that this component is associated with T ∼ 10^4 K hydrogen.},
  author       = {Setton, David J. and Greene, Jenny E. and de Graaff, Anna and Ma, Yilun 逸伦 and Leja, Joel and Matthee, Jorryt J and Bezanson, Rachel and Boogaard, Leindert A. and Cleri, Nikko J. and Katz, Harley and Labbe, Ivo and Maseda, Michael V. and McConachie, Ian and Miller, Tim B. and Price, Sedona H. and Suess, Katherine A. and van Dokkum, Pieter and Wang 王, Bingjie 冰洁 and Weibel, Andrea and Whitaker, Katherine E. and Williams, Christina C.},
  issn         = {1538-4357},
  journal      = {The Astrophysical Journal},
  number       = {1},
  publisher    = {IOP Publishing},
  title        = {{Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit}},
  doi          = {10.3847/1538-4357/ae1500},
  volume       = {995},
  year         = {2025},
}

@article{21058,
  abstract     = {Luminous broad Hα emission and red rest-optical spectral energy distributions (SEDs) are the hallmark of compact little red dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei (AGN). However, the lack of observed far-infrared (FIR) emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new Atacama Large Millimeter/submillimeter Array imaging, new and existing JWST/MIRI imaging, and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs (z = 3.1 and z = 4.47) to place the strongest constraints on the IR luminosity in LRDs to date. The detections at λrest = 1–4 μm imply flat slopes in the rest-IR, ruling out a contribution from hot (T ≳ 500 K) dust. Similarly, FIR nondetections rule out any appreciable cold (T ≲ 75 K) dust component. Assuming energy balance, these observations are inconsistent with the typical FIR dust emission of dusty starbursts and quasar tori, which usually show a mixture of cold and hot dust. Additionally, our [C ii] nondetections rule out typical dusty starbursts. We compute empirical maximum IR SEDs and find that both LRDs must have log(LIR/L ) 12.2 at the 3σ level. These limits are in tension with the predictions of rest-optical spectrophotometric fits, be they galaxy-only, AGN-only, or composite. It is unlikely that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature distribution that conspires to avoid current observing facilities. Rather, we favor an intrinsically redder LRD SED model that alleviates the need for strong dust attenuation.},
  author       = {Setton, David J. and Greene, Jenny E. and Spilker, Justin S. and Williams, Christina C. and Labbé, Ivo and Ma, Yilun 逸伦 and Wang, Bingjie 冰洁 and Whitaker, Katherine E. and Leja, Joel and de Graaff, Anna and Alberts, Stacey and Bezanson, Rachel and Boogaard, Leindert A. and Brammer, Gabriel and Cutler, Sam E. and Cleri, Nikko J. and Cooper, Olivia R. and Dayal, Pratika and Fujimoto, Seiji and Furtak, Lukas J. and Goulding, Andy D. and Hirschmann, Michaela and Kokorev, Vasily and Maseda, Michael V. and McConachie, Ian and Matthee, Jorryt J and Miller, Tim B. and Naidu, Rohan P. and Oesch, Pascal A. and Pan, Richard and Price, Sedona H. and Suess, Katherine A. and Weaver, John R. and Xiao, Mengyuan and Zhang, Yunchong and Zitrin, Adi},
  issn         = {2041-8213},
  journal      = {The Astrophysical Journal Letters},
  publisher    = {IOP Publishing},
  title        = {{A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots}},
  doi          = {10.3847/2041-8213/ade78b},
  volume       = {991},
  year         = {2025},
}

@article{21060,
  abstract     = {Compact, star-forming galaxies with high star formation rate surface densities (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigated the influence of galaxy morphology on LyC production and escape at redshifts 5 ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15 M), star-forming galaxies with ionizing photon efficiency (ξion) values consistent with canonical expectations. Since direct measurements of fesc are not possible during the Epoch of  Reionization (EoR), we predicted fesc for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit, on average, modest predicted escape fractions (∼0.04). In addition, we evaluated the correlation between morphological features and LyC emission. Our findings indicate that neither ξion nor the predicted fesc values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape. },
  author       = {Mascia, Sara and Pentericci, L. and Llerena, M. and Calabrò, A. and Matthee, Jorryt J and Flury, S. and Pacucci, F. and Jaskot, A. and Amorín, R. O. and Bhatawdekar, R. and Castellano, M. and Cleri, N. and Costantin, L. and Davis, K. and Di Cesare, Claudia and Dickinson, M. and Fontana, A. and Guo, Y. and Giavalisco, M. and Holwerda, B. W. and Hu, W. and Huertas-Company, M. and Jung, Intae and Kartaltepe, J. and Kashino, D. and Koekemoer, A. M. and Lucas, R. A. and Lotz, J. and Napolitano, L. and Jogee, S. and Wilkins, S.},
  issn         = {1432-0746},
  journal      = {Astronomy & Astrophysics},
  publisher    = {EDP Sciences},
  title        = {{Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe}},
  doi          = {10.1051/0004-6361/202553760},
  volume       = {701},
  year         = {2025},
}

@article{21061,
  abstract     = {Detecting the first generation of stars, Population III (Pop III), has been a long-standing goal in astrophysics, yet they remain elusive even in the JWST era. Here we present a novel NIRCam-based selection method for Pop III galaxies, and carefully validate it through completeness and contamination simulations. We systematically search ≃ 500 arcmin2 across JWST legacy fields for Pop III candidates, including GLIMPSE, which, assisted by gravitational lensing, has produced JWST’s deepest NIRCam imaging thus far. We discover one promising Pop III galaxy candidate (GLIMPSE-16043) at z=6.50 -0.24 +0.03, a moderately lensed galaxy (µ = + 2.9 -0.2 +0.1) with an intrinsic UV magnitude of MUV= -15.89 -0.14 +0.12. It exhibits key Pop III features: strong Hα emission (rest-frame EW 2810 ± 550 Å); a Balmer jump; no dust (UV slope β = −2.34 ± 0.36); and undetectable metal lines (e.g., [O III]; [O III]/Hβ < 0.44), implying a gas-phase metallicity of Zgas/Z⊙ < 0.5%. These properties indicate the presence of a nascent, metal-deficient young stellar population (<5 Myr) with a stellar mass of ≃105 M⊙. Intriguingly, this source deviates significantly from the extrapolated UV–metallicity relation derived from recent JWST observations at z = 4–10, consistent with UV enhancement by a top-heavy Pop III initial mass function or the presence of an extremely metal-poor active galactic nucleus. We also  derive the first observational constraints on the Pop III UV luminosity function at z ≃ 6–7. The volume density of GLIMPSE-16043 (≈10^−4 cMpc−3) is in excellent agreement with theoretical predictions, independently reinforcing its plausibility. This study demonstrates the power of our novel NIRCam method to finally reveal distant galaxies even more pristine than the Milky Way’s most metal-poor satellites, thereby promising to bring us closer to the first generation of stars than we have ever been before.},
  author       = {Fujimoto, Seiji and Naidu, Rohan P. and Chisholm, John and Atek, Hakim and Endsley, Ryan and Kokorev, Vasily and Furtak, Lukas J. and Pan, Richard and Liu, Boyuan and Bromm, Volker and Venditti, Alessandra and Visbal, Eli and Sarmento, Richard and Weibel, Andrea and Oesch, Pascal A. and Brammer, Gabriel and Schaerer, Daniel and Adamo, Angela and Berg, Danielle A. and Bezanson, Rachel and Bouwens, Rychard and Chemerynska, Iryna and Claeyssens, Adélaïde and Dessauges-Zavadsky, Miroslava and Frebel, Anna and Korber, Damien and Labbe, Ivo and Marques-Chaves, Rui and Matthee, Jorryt J and McQuinn, Kristen B. W. and Muñoz, Julian B. and Natarajan, Priyamvada and Saldana-Lopez, Alberto and Suess, Katherine A. and Volonteri, Marta and Zitrin, Adi},
  issn         = {1538-4357},
  journal      = {The Astrophysical Journal},
  publisher    = {IOP Publishing},
  title        = {{GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7}},
  doi          = {10.3847/1538-4357/ade9a1},
  volume       = {989},
  year         = {2025},
}

@article{21062,
  abstract     = {JWST observations have unveiled faint active galactic nuclei (AGNs) at high redshift that provide insights into the formation of supermassive black holes (SMBHs). However, disentangling their stellar from AGN light is challenging. Here, we use an empirical approach to infer the average stellar mass of five faint broad-line (BL) Hα emitters at z = 4–5 with BH masses ≈6 × 10^6 M⊙, with a method independent of their spectral energy distribution (SED). We use the deep JWST/NIRcam grism survey “All the Little Things” to measure the overdensities around BL-Hα emitters and around a spectroscopic reference sample of ∼300 galaxies. In our reference sample, we find that megaparsec-scale overdensity correlates with stellar mass. Their large-scale environments suggest that BL-Hα emitters are hosted by galaxies with stellar masses ≈5 × 10^7 M⊙, ≈40 times lower than those inferred from galaxy-only SED fits. Adding measurements around more luminous z ≈ 6 AGNs, we find tentative correlations between line width, BH mass, and the overdensity, suggestive of a steep BH to halo mass relation. The main implications are (1) when BH masses are taken at face value, we confirm extremely high BH to stellar mass ratios of ≈10%, (2) the galaxies of low stellar mass that host growing SMBHs are in tension with typical hydrodynamical simulations, except those without feedback, (3) a 1% duty cycle implied by the host mass hints at super-Eddington accretion, (4) the masses are at odds with an interpretation of the line broadening in terms of high stellar density, (5) our results imply a luminosity-dependent diversity of galaxy masses, environments, and SEDs among AGN samples.},
  author       = {Matthee, Jorryt J and Naidu, Rohan P. and Kotiwale, Gauri and Furtak, Lukas J. and Kramarenko, Ivan and Mackenzie, Ruari and Greene, Jenny and Adamo, Angela and Bouwens, Rychard J. and Di Cesare, Claudia and Eilers, Anna-Christina and de Graaff, Anna and Heintz, Kasper E. and Kashino, Daichi and Maseda, Michael V. and Tacchella, Sandro and Torralba Torregrosa, Alberto},
  issn         = {1538-4357},
  journal      = {The Astrophysical Journal},
  number       = {2},
  publisher    = {IOP Publishing},
  title        = {{Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5}},
  doi          = {10.3847/1538-4357/ade886},
  volume       = {988},
  year         = {2025},
}

@article{21063,
  abstract     = {We report the detection of a 13σ Hα emission line from HDF850.1 at z = 5.188 ± 0.001 using the FRESCO (First Reionization Era SpectroscopicallyComplete Observations) NIRCam F444W grism observations. Detection of Hα in HDF850.1 is noteworthy, given its high far-infrared (IR) luminosity, substantial dust obscuration, and the historical challenges in deriving its redshift.
HDF850.1 shows a clear detection in the F444W imaging data, distributed between a northern and southern component, mirroring that seen in [C II] from the Plateau de Bure Interferometer. Modelling the spectral energy distribution of each component separately, we find that the northern component has a higher mass, star formation rate (SFR), and dust extinction than the southern component. The observed Hα emission appears to arise entirely from the less-obscured southern component and shows a similar v∼ + 130 km s −1 velocity offset to that seen for [C II] relative to the source systemic redshift. Leveraging Hα-derived redshiftsfrom FRESCO observations, we find that HDF850.1 isforming in one of the richest environments identified to date at z > 5, with 100 z = 5.17–5.20 galaxies distributed across 13 smaller structures and a ∼(15 cMpc)3 volume. Based on the evolution of analogous structures in cosmological simulations, the z = 5.17–5.20 structures seem likely to collapse into
a single > 1014M cluster by z ∼ 0. Comparing galaxy properties forming within this overdensity with those outside, we find the masses, SFRs, and UV luminosities inside the overdensity to be clearly higher. The prominence of Hα line emission from HDF850.1 and other known highly obscured z > 5 galaxies illustrates the potential of NIRCam-grism programs to map both
the early build-up of IR-luminous galaxies and overdense structures.},
  author       = {Herard-Demanche, Thomas and Bouwens, Rychard J and Oesch, Pascal A and Naidu, Rohan P and Decarli, Roberto and Nelson, Erica J and Brammer, Gabriel and Weibel, Andrea and Xiao, Mengyuan and Stefanon, Mauro and Walter, Fabian and Matthee, Jorryt J and Meyer, Romain A and Wuyts, Stijn and Reddy, Naveen and Rowland, Lucie and van Leeuwen, Ivana and Haro, Pablo Arrabal and Dannerbauer, Helmut and Shapley, Alice E and Chisholm, John and van Dokkum, Pieter and Labbe, Ivo and Illingworth, Garth and Schaerer, Daniel and Shivaei, Irene},
  issn         = {1365-2966},
  journal      = {Monthly Notices of the Royal Astronomical Society},
  number       = {2},
  pages        = {788--808},
  publisher    = {Oxford University Press},
  title        = {{Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures}},
  doi          = {10.1093/mnras/staf030},
  volume       = {537},
  year         = {2025},
}

@inproceedings{21066,
  abstract     = {Causal discovery from observational data holds great promise, but existing methods rely on strong assumptions about the underlying causal structure, often requiring full observability of all relevant variables. We tackle these challenges by leveraging the score function ∇logp(X)
 of observed variables for causal discovery and propose the following contributions. First, we generalize the existing results of identifiability with the score to additive noise models with minimal requirements on the causal mechanisms. Second, we establish conditions for inferring causal relations from the score even in the presence of hidden variables; this result is two-faced: we demonstrate the score’s potential as an alternative to conditional independence tests to infer the equivalence class of causal graphs with hidden variables, and we provide the necessary conditions for identifying direct causes in latent variable models. Building on these insights, we propose a flexible algorithm for causal discovery across linear, nonlinear, and latent variable models, which we empirically validate.},
  author       = {Montagna, Francesco and Faller, Philipp and Blöbaum, Patrik and Kirschbaum, Elke and Locatello, Francesco},
  booktitle    = {Proceedings of the Fourth Conference on Causal Learning and Reasoning},
  issn         = {2640-3498},
  location     = {Lausanne, Switzerland},
  pages        = {552--605},
  publisher    = {ML Research Press},
  title        = {{Score matching through the roof: Linear, nonlinear, and latent variables causal discovery}},
  volume       = {275},
  year         = {2025},
}

@inproceedings{21089,
  abstract     = {Hypertrace logic is a sorted first-order logic with separate sorts for time and execution traces. Its formulas specify hyperproperties, which are properties relating multiple traces. In this work, we extend hypertrace logic by introducing trace quantifiers that range over the set of all possible traces. In this extended logic, formulas can quantify over two kinds of trace variables: constrained trace variables, which range over a fixed set of traces defined by the model, and unconstrained trace variables, which can be assigned to any trace. In comparison, hyperlogics such as HyperLTL have only constrained trace quantifiers. We use hypertrace logic to study how different quantifier patterns affect the decidability of the satisfiability problem. We prove that hypertrace logic without constrained trace quantifiers is equivalent to monadic second-order logic of one successor (S1S), and therefore satisfiable, and that the trace-prefixed fragment (all trace quantifiers precede all time quantifiers) is equivalent to HyperQPTL. Moreover, we show that all hypertrace formulas where the only alternation between constrained trace quantifiers is from an existential to a universal quantifier are equisatisfiable to formulas without constraints on their trace variables and, therefore, decidable as well. Our framework allows us to study also time-prefixed hyperlogics, for which we provide new decidability and undecidability results.},
  author       = {Chalupa, Marek and Henzinger, Thomas A and Oliveira da Costa, Ana A},
  booktitle    = {45th Annual Conference on Foundations of Software Technology and Theoretical Computer Science},
  location     = {Pilani, India},
  pages        = {20:1--20:18},
  publisher    = {Schloss Dagstuhl - Leibniz-Zentrum für Informatik},
  title        = {{Flavors of quantifiers in hyperlogics}},
  doi          = {10.4230/LIPICS.FSTTCS.2025.20},
  volume       = {360},
  year         = {2025},
}

@inproceedings{21091,
  abstract     = {Neural certificates have emerged as a powerful tool in cyber-physical systems control, providing witnesses of correctness. These certificates, such as barrier functions, often learned alongside control policies, once verified, serve as mathematical proofs of system safety. However, traditional formal verification of their defining conditions typically faces scalability challenges due to exhaustive state-space exploration. To address this challenge, we propose a lightweight runtime monitoring framework that integrates real-time verification and does not require access to the underlying control policy. Our monitor observes the system during deployment and performs on-the-fly verification of the certificate over a lookahead region to ensure safety within a finite prediction horizon. We instantiate this framework for ReLU-based control barrier functions and demonstrate its practical effectiveness in a case study. Our approach enables timely detection of safety violations and incorrect certificates with minimal overhead, providing an effective but lightweight alternative to the static verification of the certificates.},
  author       = {Henzinger, Thomas A and Kueffner, Konstantin and Yu, Zhengqi},
  booktitle    = {25th International Conference on Runtime Verification},
  issn         = {1611-3349},
  location     = {Graz, Austria},
  pages        = {54--72},
  publisher    = {Springer Nature},
  title        = {{Formal verification of neural certificates done dynamically}},
  doi          = {10.1007/978-3-032-05435-7_4},
  volume       = {16087},
  year         = {2025},
}

@inproceedings{21092,
  abstract     = {Formal verification provides assurances that a probabilistic system satisfies its specification—conditioned on the system model being aligned with reality. We propose alignment monitoring to watch that this assumption is justified. We consider a probabilistic model well aligned if it accurately predicts the behaviour of an uncertain system in advance. An alignment score measures this by quantifying the similarity between the model’s predicted and the system’s (unknown) actual distributions. An alignment monitor observes the system at runtime; at each point in time it uses the current state and the model to predict the next state. After the next state is observed, the monitor updates the verdict, which is a high-probability interval estimate for the true alignment score. We utilize tools from sequential forecasting to construct our alignment monitors. Besides a monitor for measuring the expected alignment score, we introduce a differential alignment monitor, designed for comparing two models, and a weighted alignment monitor, which permits task-specific alignment monitoring. We evaluate our monitors experimentally on the PRISM benchmark suite. They are fast, memory-efficient, and detect misalignment early.},
  author       = {Henzinger, Thomas A and Kueffner, Konstantin and Singh, Vasu and Sun, I},
  booktitle    = {25th International Conference on Runtime Verification},
  issn         = {1611-3349},
  location     = {Graz, Austria},
  pages        = {140--159},
  publisher    = {Springer Nature},
  title        = {{Alignment monitoring}},
  doi          = {10.1007/978-3-032-05435-7_9},
  volume       = {16087},
  year         = {2025},
}

@inproceedings{21093,
  abstract     = {We propose a monitoring approach for hyperproperties where the system’s observations range over infinite domains. The specifications are given as formulas of symbolic hypernode logic, an extension of earlier versions of hypernode logic that supports events with data. We demonstrate how to translate terms of symbolic hypernode logic into multi-tape symbolic transducers and we present a monitoring algorithm for universally quantified formulas that is based on this translation. We evaluate our approach against the previous approach for monitoring hypernode logic, and we also compare it to other monitors for hyperproperties.},
  author       = {Chalupa, Marek and Henzinger, Thomas A and Oliveira da Costa, Ana A},
  booktitle    = {25th International Conference on Runtime Verification},
  issn         = {1611-3349},
  location     = {Graz, Austria},
  pages        = {417--437},
  publisher    = {Springer Nature},
  title        = {{Monitoring hypernode logic over infinite domains}},
  doi          = {10.1007/978-3-032-05435-7_23},
  volume       = {16087},
  year         = {2025},
}

@article{21121,
  abstract     = {The relation between the masses of supermassive black holes (SMBHs) and their host galaxies encodes information on their mode of growth, especially at the earliest epochs. The James Webb Space Telescope (JWST) has opened such investigations by detecting the host galaxies of active galactic nuclei (AGN) and more luminous quasars within the first billion years of the Universe (z ≳ 6). Here, we evaluate the relation between the mass of SMBHs and the total stellar mass of their host galaxies using a sample of nine quasars at 6.18 ≤ z ≤ 6.4 from the Subaru High-z Exploration of Low-luminosity Quasars survey with NIRCam and NIRSpec observations. We find that the observed location of these quasars in the SMBH–galaxy mass plane (logMBH/M 8–9; logM*/M 9.5–11) is consistent with a nonevolving intrinsic mass relation with dispersion (0.80 +0.23 -0.28 dex) higher than the local value (∼0.3–0.4 dex) of their more massive descendants. Our analysis is based on a forward model of systematics and includes a consideration of the impact of selection effects and measurement uncertainties with an assumption on the slope of the mass relation. While degeneracies between parameters persist, the best-fit solution has a reasonable AGN fraction (2.3%) of galaxies at z ∼ 6 with an actively growing UV-unobscured black hole. In particular, models with a substantially higher normalisation in MBH would require an unrealistically low intrinsic dispersion (∼0.22 dex). Consequently, our results predict a large population of AGN at lower black hole masses, as are now just starting to be discovered in focused efforts with JWST.},
  author       = {Silverman, John David and Li, Junyao and Ding, Xuheng and Onoue, Masafusa and Strauss, Michael A. and Matsuoka, Yoshiki and Izumi, Takuma and Jahnke, Knud and Treu, Tommaso and Volonteri, Marta and Phillips, Camryn L. and Andika, Irham T. and Aoki, Kentaro and Arita, Junya and Baba, Shunsuke and Bosman, Sarah E. I. and Eilers, Anna-Christina and Fan, Xiaohui and Fujimoto, Seiji and Habouzit, Melanie and Haiman, Zoltán and Imanishi, Masatoshi and Inayoshi, Kohei and Iwasawa, Kazushi and Kashikawa, Nobunari and Kawaguchi, Toshihiro and Lee, Chien-Hsiu and Lupi, Alessandro and Nagao, Tohru and Schindler, Jan-Torge and Schramm, Malte and Shimasaku, Kazuhiro and Toba, Yoshiki and Trakhtenbrot, Benny and Umehata, Hideki and Vestergaard, Marianne and Walter, Fabian and Wang, Feige and Yang, Jinyi},
  issn         = {2041-8213},
  journal      = {The Astrophysical Journal Letters},
  number       = {2},
  publisher    = {IOP Publishing},
  title        = {{SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6}},
  doi          = {10.3847/2041-8213/ae279c},
  volume       = {995},
  year         = {2025},
}