Let K be a number field and let A be its ring of integers. Let G be a connected, noncommutative, absolutely almost simple algebraic K-group. If the K-rank of G equals 2, then G(A[t]) is not finitely presented.

Amir Mohammadi Kevin Wortman

In theories with spontaneous symmetry breaking, the conventional effective potential possesses a defective loop expansion. For such theories, the exact effective potential $V(\phi_c,T)$ is real and convex, but its perturbative series is complex and concave at small $\phi_c$ and $T$. A more effective potential is available.

Kevin Cahill

As evidenced by recent survey results, majority of asteroids are slow rotators (P>12 h), but lack spin and shape models due to selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 hours. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent. We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared data: large bodies are too bright for WISE mission. Therefore, we recently launched a campaign among stellar occultation observers, to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to stellar occultations resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, e.g. constitute a solid basis for density determinations when coupled with mass information. Spin and shape models continue to fill the gaps caused by various biases.

A. Marciniak J. Ďurech A. Choukroun J. Hanuš W. Ogłoza R. Szakáts L. Molnár A. Pál F. Monteiro E. Frappa W. Beisker H. Pavlov J. Moore R. Adomavičienė R. Aikawa S. Andersson P. Antonini Y. Argentin A. Asai P. Assoignon J. Barton P. Baruffetti K. L. Bath R. Behrend L. Benedyktowicz L. Bernasconi G. Biguet M. Billiani D. Błażewicz R. Boninsegna M. Borkowski J. Bosch S. Brazill M. Bronikowska A. Bruno M. Butkiewicz - Bąk J. Caron G. Casalnuovo J. J. Castellani P. Ceravolo M. Conjat P. Delincak J. Delpau C. Demeautis A. Demirkol M. Dróżdż R. Duffard C. Durandet D. Eisfeldt M. Evangelista S. Fauvaud M. Fauvaud M. Ferrais M. Filipek P. Fini K. Fukui B. Gährken S. Geier T. George B. Goffin J. Golonka T. Goto J. Grice K. Guhl K. Halíř W. Hanna M. Harman A. Hashimoto W. Hasubick D. Higgins M. Higuchi T. Hirose R. Hirsch O. Hofschulz T. Horaguchi J. Horbowicz M. Ida B. Ignácz M. Ishida K. Isobe E. Jehin B. Joachimczyk A. Jones J. Juan K. Kamiński M. K. Kamińska P. Kankiewicz H. Kasebe B. Kattentidt D. -H. Kim M. -J. Kim K. Kitazaki A. Klotz M. Komraus I. Konstanciak R. Könyves - Tóth K. Kouno E. Kowald J. Krajewski G. Krannich A. Kreutzer A. Kryszczyńska J. Kubánek V. Kudak F. Kugel R. Kukita P. Kulczak D. Lazzaro J. Licandro F. Livet P. Maley N. Manago J. Mánek A. Manna H. Matsushita S. Meister W. Mesquita S. Messner J. Michelet J. Michimani I. Mieczkowska N. Morales M. Motyliński M. Murawiecka J. Newman V. Nikitin M. Nishimura J. Oey D. Oszkiewicz M. Owada E. Pakštienė M. Pawłowski W. Pereira V. Perig J. Perła F. Pilcher E. Podlewska-Gaca J. Polák T. Polakis M. Polińska A. Popowicz F. Richard J. J. Rives T. Rodrigues Ł. Rogiński E. Rondón M. Rottenborn R. Schäfer C. Schnabel O. Schreurs A. Selva M. Simon B. Skiff M. Skrutskie J. Skrzypek K. Sobkowiak E. Sonbas S. Sposetti P. Stuart K. Szyszka K. Terakubo W. Thomas P. Trela S. Uchiyama M. Urbanik G. Vaudescal R. Venable Ha. Watanabe Hi. Watanabe M. Winiarski R. Wróblewski H. Yamamura M. Yamashita H. Yoshihara M. Zawilski P. Zelený M. Żejmo K. Żukowski S. Żywica

Context. The sizes of many asteroids, especially slowly rotating, low-amplitude targets, remain poorly constrained due to selection effects. These biases limit the availability of high-quality data, leaving size estimates reliant on spherical shape assumptions. Such approximations introduce significant uncertainties propagating, e.g. into density determinations or thermophysical and compositional studies, affecting our understanding of asteroid properties. Aims. This work targets poorly studied main-belt asteroids, most of which lacked shape models. Using only high-quality dense light curves, thermal IR observations (incl. WISE), and stellar occultations, we aimed to produce reliable shape models and scale them via two independent techniques, allowing size comparison. We conducted two campaigns to obtain dense photometric light curves and to acquire multi-chord stellar occultations. Methods. Shape and spin models were reconstructed using lightcurve inversion. Sizes were determined by (1) thermophysical modeling with the Convex Inversion Thermophysical Model (CITPM), optimizing spin and shape models to visible lightcurve and IR data, and (2) scaling shape models with stellar occultations. Results. We obtained precise sizes and shape models for 15 asteroids. CITPM- and occultation-derived sizes agree within 5% in most cases, demonstrating the modeling's reliability. Larger discrepancies usually stem from incomplete occultation chord coverage. The study also gives insights into surface properties incl. albedo, roughness and thermal inertia. Conclusions. Using high-quality data and an advanced TPM integrating thermal and visible data with shape adjustment enabled precise size estimates comparable to those from multi-chord stellar occultations. We resolved major inconsistencies in previous size estimates, providing solid input for future studies on asteroid densities and surfaces.

A. Choukroun A. Marciniak J. Ďurech J. Perła W. Ogłoza R. Szakats L. Molnar A. Pal F. Monteiro I. Mieczkowska W. Beisker D. Agnetti C. Anderson S. Andersson D. Antuszewicz P. Arcoverde R. -L. Aubry P. Bacci R. Bacci P. Baruffetti L. Benedyktowicz M. Bertini D. Blazewicz R. Boninsegna Zs. Bora M. Borkowski E. Bredner J. Broughton M. Butkiewicz - Bąk N. Carlson G. Casalnuovo F. Casarramona Y. -J. Choi S. Cikota M. Collins B. Cseh G. Csörnyei H. De Groot P. Delincak P. Denyer R. Dequinze M. Dogramatzidis M. Drozdz R. Duffard D. Eisfeldt M. Eleftheriou C. Ellington S. Fauvaud M. Fauvaud M. Ferrais M. Filipek P. Fini M. Frits B. Gährken G. Galli D. Gault S. Geier B. Gimple J. Golonka L. Grazzini J. Grice K. Guhl W. Hanna M. Harman W. Hasubick T. Haymes D. Herald D. Higgins R. Hirsch J. Horbowicz A. Horti - David B. Ignacz E. Jehin A. Jones R. Jones D. Dunham Cs. Kalup K. Kaminski M. K. Kaminska P. Kankiewicz M. Kaplan A. Karagiannidis B. Kattentidt S. Kidd B. Kirpluk D. -H. Kim M. -J. Kim I. Konstanciak G. Krannich M. Kretlow J. Kubanek V. Kudak P. Kulczak M. Lecossois R. Leiva M. Libert J. Licandro P. Lindner R. Liu Y. Liu G. Lyzenga M. Maestripieri C. Malagon P. Maley A. Manna S. Messner O. Michniewicz M. A. Miftah M. Mizutani N. Morales M. Murawiecka J. Nadolny T. Nemoto J. Newman V. Nikitin P. Nosal P. Nosworthy M. O'Connell J. Oey A. M. Ortiz-Ochoa A. Ossola D. Oszkiewicz E. Pakstiene M. Pawlowski V. Perig E. Petrescu F. Pilcher E. Podlewska-Gaca M. Polacek J. Polak T. Polakis M. Polinska A. Popowicz V. Reddy J. -J. Rives M. Rottenborn N. Ruocco A. Rutkowski K. Saci T. Santana-Ros K. Sarneczky O. Schreurs V. Sempronio B. Skiff J. Skrzypek D. Smith K. Sobkowiak E. Sonbas S. Sposetti C. Stewart W. Stewart T. Swift M. Szkudlarek K. Szyszka N. Takacs L. Tychoniec M. Uno S. Urakawa K. Vida C. Weber N. Wünsche H. Yamamura H. Yoshihara M. Zawilski P. Zeleny S. Zola M. Zejmo K. Zukowski

I discuss recent seminal work on the LARCS dataset: a panoramic study of rich clusters of galaxies at z~0.12. The importance of observing beyond the cluster core is illustrated by exploiting these data to examine colour gradients across the clusters.

Kevin A. Pimbblet

We study the completion of a group relative to a Zariski dense representation in a reductive algebraic group over a field $k$. The characteristic zero case was worked out previously by R. Hain; we extend his results to arbitrary characteristic. The primary application is to the study of the cohomology of groups such as $SL_n(k[[T]])$.

Kevin P. Knudson

We discuss a novel method of efficiently producing multi-photon states using repeated spontaneous parametric downconversion. Specifically, by attempting downconversion several times, we can pseudo-deterministically add photons to a mode, producing various several-photon states. We discuss both expected performance and experimental limitations.

Kevin T. McCusker Paul G. Kwiat

I summarize the status of the Sanford Underground Research Facility in South Dakota and present connections to Energy and Intensity Frontier that benefit from the establishment of SURF and the staging of US-funded experiments in a domestic facility.

Kevin T. Lesko

We construct a quasiconformal mapping of $n$-dimensional Euclidean space, $n \geq 2$, that simultaneously distorts the Hausdorff dimension of a nearly maximal collection of parallel lines by a given amount. This answers a question of Balogh, Monti, and Tyson.

Zoltán M. Balogh Jeremy T. Tyson Kevin Wildrick

Let $k$ be a perfect field of characteristic $p$ and set $K=k((t))$. In this paper we study the ramification properties of elements of Aut$_k(K)$. By choosing a uniformizer for $K$ we may interpret our theorems in terms of power series over $k$. The most important tool that we use is the field of norms construction of Fontaine and Wintenberger.

Kevin Keating