@article{15194,
  abstract     = {AM Canum Venaticorum (AM CVn) systems are ultracompact binaries where a white dwarf accretes from a helium-rich degenerate or semidegenerate donor. Some AM CVn systems will be among the loudest sources of gravitational waves for the upcoming Laser Interferometer Space Antenna; yet the formation channel of AM CVns remains uncertain. We report the study and characterization of a new eclipsing AM CVn, SRGeJ045359.9+622444 (hereafter, SRGeJ0453), discovered from a joint Spektrum-Roentgen-Gamma (SRG) Extended Roentgen Survey with an Imaging Telescope Array (eROSITA) mission and Zwicky Transient Facility program to identify cataclysmic variables (CVs). We obtained optical photometry to confirm the eclipse of SRGeJ0453 and determine the orbital period to be 
. We constrain the binary parameters by modeling the high-speed photometry and radial-velocity curves and find Mdonor = 0.044 ± 0.024M⊙ and Rdonor = 0.078 ± 0.012R⊙. The X-ray spectrum is approximated by a power-law model with an unusually flat photon index of Γ ∼ 1 previously seen in magnetic CVs with SRG/eROSITA, but verifying that the magnetic nature of SRGeJ0453 requires further investigation. Optical spectroscopy suggests that the donor star of SRGeJ0453 could have initially been a He star or a He white dwarf. SRGeJ0453 is the ninth eclipsing AM CVn system published to date, and its lack of optical outbursts have made it elusive in previous surveys. The discovery of SRGeJ0453 using joint X-ray and optical surveys highlights the potential for discovering similar systems in the near future.},
  author       = {Rodriguez, Antonio C. and Galiullin, Ilkham and Gilfanov, Marat and Kulkarni, Shrinivas R. and Khamitov, Irek and Bikmaev, Ilfan and van Roestel, Jan and Yungelson, Lev and El-Badry, Kareem and Sunayev, Rashid and Prince, Thomas A. and Buntov, Mikhail and Caiazzo, Ilaria and Drake, Andrew and Gorbachev, Mark and Graham, Matthew J. and Gumerov, Rustam and Irtuganov, Eldar and Laher, Russ R. and Masci, Frank J. and Medvedev, Pavel and Purdum, Josiah and Sakhibullin, Nail and Sklyanov, Alexander and Smith, Roger and Szkody, Paula and Vanderbosch, Zachary P.},
  issn         = {1538-4357},
  journal      = {The Astrophysical Journal},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {1},
  publisher    = {American Astronomical Society},
  title        = {{SRGeJ045359.9+622444: A 55 minute period eclipsing AM Canum Venaticorum star discovered from a joint SRG/eROSITA + ZTF search}},
  doi          = {10.3847/1538-4357/ace698},
  volume       = {954},
  year         = {2023},
}

@article{15195,
  abstract     = {White dwarfs, the extremely dense remnants left behind by most stars after their death, are characterized by a mass comparable to that of the Sun compressed into the size of an Earth-like planet. In the resulting strong gravity, heavy elements sink towards the centre and the upper layer of the atmosphere contains only the lightest element present, usually hydrogen or helium1,2. Several mechanisms compete with gravitational settling to change a white dwarf’s surface composition as it cools3, and the fraction of white dwarfs with helium atmospheres is known to increase by a factor of about 2.5 below a temperature of about 30,000 kelvin4,5,6,7,8; therefore, some white dwarfs that appear to have hydrogen-dominated atmospheres above 30,000 kelvin are bound to transition to be helium-dominated as they cool below it. Here we report observations of ZTF J203349.8+322901.1, a transitioning white dwarf with two faces: one side of its atmosphere is dominated by hydrogen and the other one by helium. This peculiar nature is probably caused by the presence of a small magnetic field, which creates an inhomogeneity in temperature, pressure or mixing strength over the surface9,10,11. ZTF J203349.8+322901.1 might be the most extreme member of a class of magnetic, transitioning white dwarfs—together with GD 323 (ref. 12), a white dwarf that shows similar but much more subtle variations. This class of white dwarfs could help shed light on the physical mechanisms behind the spectral evolution of white dwarfs.},
  author       = {Caiazzo, Ilaria and Burdge, Kevin B. and Tremblay, Pier-Emmanuel and Fuller, James and Ferrario, Lilia and Gänsicke, Boris T. and Hermes, J. J. and Heyl, Jeremy and Kawka, Adela and Kulkarni, S. R. and Marsh, Thomas R. and Mróz, Przemek and Prince, Thomas A. and Richer, Harvey B. and Rodriguez, Antonio C. and van Roestel, Jan and Vanderbosch, Zachary P. and Vennes, Stéphane and Wickramasinghe, Dayal and Dhillon, Vikram S. and Littlefair, Stuart P. and Munday, James and Pelisoli, Ingrid and Perley, Daniel and Bellm, Eric C. and Breedt, Elmé and Brown, Alex J. and Dekany, Richard and Drake, Andrew and Dyer, Martin J. and Graham, Matthew J. and Green, Matthew J. and Laher, Russ R. and Kerry, Paul and Parsons, Steven G. and Riddle, Reed L. and Rusholme, Ben and Sahman, Dave I.},
  issn         = {1476-4687},
  journal      = {Nature},
  number       = {7972},
  pages        = {61--66},
  publisher    = {Springer Nature},
  title        = {{A rotating white dwarf shows different compositions on its opposite faces}},
  doi          = {10.1038/s41586-023-06171-9},
  volume       = {620},
  year         = {2023},
}

@article{15196,
  abstract     = {We report the discovery of ZTF J0127+5258, a compact mass-transferring binary with an orbital period of 13.7 minutes. The system contains a white dwarf accretor, which likely originated as a post–common envelope carbon–oxygen (CO) white dwarf, and a warm donor (Teff,donor = 16,400 ± 1000 K). The donor probably formed during a common envelope phase between the CO white dwarf and an evolving giant that left behind a helium star or white dwarf in a close orbit with the CO white dwarf. We measure gravitational wave–driven orbital inspiral with ∼51σ significance, which yields a joint constraint on the component masses and mass transfer rate. While the accretion disk in the system is dominated by ionized helium emission, the donor exhibits a mixture of hydrogen and helium absorption lines. Phase-resolved spectroscopy yields a donor radial velocity semiamplitude of 771 ± 27 km s−1, and high-speed photometry reveals that the system is eclipsing. We detect a Chandra X-ray counterpart with LX ∼ 3 × 1031 erg s−1. Depending on the mass transfer rate, the system will likely either evolve into a stably mass-transferring helium cataclysmic variable, merge to become an R CrB star, or explode as a Type Ia supernova in the next million years. We predict that the Laser Space Interferometer Antenna (LISA) will detect the source with a signal-to-noise ratio of 24 ± 6 after 4 yr of observations. The system is the first LISA-loud mass-transferring binary with an intrinsically luminous donor, a class of sources that provide the opportunity to leverage the synergy between optical and infrared time domain surveys, X-ray facilities, and gravitational-wave observatories to probe general relativity, accretion physics, and binary evolution.},
  author       = {Burdge, Kevin B. and El-Badry, Kareem and Rappaport, Saul and Sunny Wong, Tin Long and Bauer, Evan B. and Bildsten, Lars and Caiazzo, Ilaria and Chakrabarty, Deepto and Chickles, Emma and Graham, Matthew J. and Kara, Erin and Kulkarni, S. R. and Marsh, Thomas R. and Nynka, Melania and Prince, Thomas A. and Simcoe, Robert A. and van Roestel, Jan and Vanderbosch, Zach and Bellm, Eric C. and Dekany, Richard G. and Drake, Andrew J. and Helou, George and Masci, Frank J. and Milburn, Jennifer and Riddle, Reed and Rusholme, Ben and Smith, Roger},
  issn         = {2041-8213},
  journal      = {The Astrophysical Journal Letters},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {1},
  publisher    = {American Astronomical Society},
  title        = {{Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor}},
  doi          = {10.3847/2041-8213/ace7cf},
  volume       = {953},
  year         = {2023},
}

@article{15197,
  abstract     = {Recently, the inner main belt asteroid (152830) Dinkinesh was identified as an additional fly- by target for the Lucy mission. The heliocentric orbit and approximate absolute magnitude of Dinkinesh are known, but little additional information was available prior to its selection as a target. In particular, the lack of color spectrophotometry or spectra made it impossible to assign a spectral type to Dinkinesh from which its albedo could be estimated. We set out to remedy this knowledge gap by obtaining visible wavelength spectra with the Keck telescope on 2022 November 23 and with Gemini-South on 2022 December 27. The spectra measured with the Keck I/Low Resolution Imaging Spectrometer (LRIS) and the Gemini South/Gemini Multi-Object Spectrograph South (GMOS-S) are most similar to the average spectrum of S- and Sq-type asteroids. The most diagnostic feature is the ≈15 ± 1% silicate absorption feature at ≈0.9–1.0 μm. Small S- and Sq-type asteroids have moderately high albedos ranging from 0.17 to 0.35. Using this albedo range for Dinkinesh in combination with measured absolute magnitude, it is possible to derive an effective diameter and surface brightness for this body. The albedo, size and surface brightness are important inputs required for planning a successful encounter by the Lucy spacecraft.},
  author       = {Bolin, B.T. and Noll, K.S. and Caiazzo, Ilaria and Fremling, C. and Binzel, R.P.},
  issn         = {0019-1035},
  journal      = {Icarus},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  publisher    = {Elsevier},
  title        = {{Keck and Gemini spectral characterization of Lucy mission fly-by target (152830) Dinkinesh}},
  doi          = {10.1016/j.icarus.2023.115562},
  volume       = {400},
  year         = {2023},
}

@article{15198,
  abstract     = {The axion-nucleon coupling enables the production of axions through the decay of excited 57Fe nuclei, and axions produced in the Sun through this process are often a target of helioscope searches. We show for the first time that hot, highly magnetic white dwarfs such as ZTF J1901+1458 are a viable target to search for the x-ray signature of axions that were produced by the 57Fe transition in the core and then converted to photons in the magnetosphere. We calculate that a 100 ks observation of ZTF J1901+1458 with NuSTAR would constrain the coupling of axions to nucleons and photons at a level below the bounds of both current and future planned helioscopes.},
  author       = {Fleury, Leesa and Caiazzo, Ilaria and Heyl, Jeremy},
  issn         = {2470-0029},
  journal      = {Physical Review D},
  number       = {10},
  publisher    = {American Physical Society},
  title        = {{Constraining axions with ZTF J1901+1458}},
  doi          = {10.1103/physrevd.107.l101303},
  volume       = {107},
  year         = {2023},
}

@article{15199,
  abstract     = {Gaia Data Release 2 revealed a population of ultramassive white dwarfs on the Q branch that are moving anomalously fast for a local disc population with their young photometric ages. As the velocity dispersion of stars in the local disc increases with age, a proposed explanation of these white dwarfs is that they experience a cooling delay that causes current cooling models to infer photometric ages much younger than their true ages. To explore this explanation, we investigate the kinematics of ultramassive white dwarfs within 200 pc of the Sun using the improved Gaia Early Data Release 3 observations. We analyse the transverse motions of 0.95–1.25 M⊙ white dwarfs, subdivided by mass and age, and determine the distributions of the three-dimensional components of the transverse velocities. The results are compared to expectations based on observed kinematics of local main-sequence stars. We find a population of photometrically young (∼0.5–1.5 Gyr) ultramassive (∼1.15–1.25 M⊙) white dwarfs for which the transverse velocity component in the direction of Galactic rotation is more dispersed than for local disc stars of any age; thus, it is too dispersed to be explained by any cooling delay in white dwarfs originating from the local disc. Furthermore, the dispersion ratio of the velocity components in the Galactic plane for this population is also inconsistent with a local disc origin. We discuss some possible explanations of this kinematically anomalous population, such as a halo origin or production through dynamical effects of stellar triple systems.},
  author       = {Fleury, Leesa and Caiazzo, Ilaria and Heyl, Jeremy},
  issn         = {1365-2966},
  journal      = {Monthly Notices of the Royal Astronomical Society},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {1},
  pages        = {364--374},
  publisher    = {Oxford University Press},
  title        = {{The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3}},
  doi          = {10.1093/mnras/stad068},
  volume       = {520},
  year         = {2023},
}

@article{15200,
  abstract     = {Magnetic cataclysmic variables (CVs) are luminous Galactic X-ray sources, which have been difficult to find in purely optical surveys due to their lack of outburst behavior. The eROSITA telescope on board the Spektr-RG mission is conducting an all-sky X-ray survey and recently released the public eROSITA Final Equatorial Depth Survey (eFEDS) catalog. We crossmatched the eFEDS catalog with photometry from the Zwicky Transient Facility and discovered two new magnetic CVs. We obtained high-cadence optical photometry and phase-resolved spectroscopy for each magnetic CV candidate and found them both to be polars. Among the newly discovered magnetic CVs is eFEDS J085037.2+044359/ZTFJ0850+0443, an eclipsing polar with orbital period Porb = 1.72 hr and WD mass MWD = 0.81 ± 0.08M⊙. We suggest that eFEDS J085037.2+044359/ZTFJ0850+0443 is a low magnetic field strength polar, with BWD ≲ 10 MG. We also discovered a non-eclipsing polar, eFEDS J092614.1+010558/ZTFJ0926+0105, with orbital period Porb = 1.47 hr and magnetic field strength BWD = 36–42 MG.},
  author       = {Rodriguez, Antonio C. and Kulkarni, Shrinivas R. and Prince, Thomas A. and Szkody, Paula and Burdge, Kevin B. and Caiazzo, Ilaria and van Roestel, Jan and Vanderbosch, Zachary P. and El-Badry, Kareem and Bellm, Eric C. and Gänsicke, Boris T. and Graham, Matthew J. and Mahabal, Ashish A. and Masci, Frank J. and Mróz, Przemek and Riddle, Reed and Rusholme, Ben},
  issn         = {1538-4357},
  journal      = {The Astrophysical Journal},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {2},
  publisher    = {American Astronomical Society},
  title        = {{Discovery of two polars from a crossmatch of ZTF and the SRG/eFEDS x-ray catalog}},
  doi          = {10.3847/1538-4357/acbb6f},
  volume       = {945},
  year         = {2023},
}

@article{15201,
  abstract     = {We present a systematic study of the unbinned, photon-by-photon likelihood technique which can be used as an alternative method to analyse phase-dependent, X-ray spectro-polarimetric observations obtained with IXPE and other photoelectric polarimeters. We apply the unbinned technique to models of the luminous X-ray pulsar Hercules X-1, for which we produce simulated observations using the IXPEOBSSIM package. We consider minimal knowledge about the actual physical process responsible for the polarized emission from the accreting pulsar and assume that the observed phase-dependent polarization angle can be described by the rotating vector model. Using the unbinned technique, the detector’s modulation factor, and the polarization information alone, we found that both the rotating vector model and the underlying spectro-polarimetry model can reconstruct equally well the geometric configuration angles of the accreting pulsar. However, the measured polarization fraction becomes biased with respect to the underlying model unless the energy dispersion and effective area of the detector are also taken into account. To this end, we present an energy-dispersed likelihood estimator that is proved to be unbiased. For different analyses, we obtain posterior distributions from multiple IXPEOBSSIM realizations and show that the unbinned technique yields 
 smaller error bars than the binned technique. We also discuss alternative sources, such as magnetars, in which the unbinned technique and the rotating vector model might be applied.},
  author       = {González-Caniulef, Denis and Caiazzo, Ilaria and Heyl, Jeremy},
  issn         = {1365-2966},
  journal      = {Monthly Notices of the Royal Astronomical Society},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {4},
  pages        = {5902--5912},
  publisher    = {Oxford University Press},
  title        = {{Unbinned likelihood analysis for X-ray polarization}},
  doi          = {10.1093/mnras/stad033},
  volume       = {519},
  year         = {2023},
}

@article{15202,
  abstract     = {Magnetars are the most strongly magnetized neutron stars, and one of the most promising targets for X-ray polarimetric measurements. We present here the first Imaging X-ray Polarimetry Explorer observation of the magnetar 1RXS J170849.0-400910, jointly analyzed with a new Swift observation and archival NICER data. The total (energy- and phase-integrated) emission in the 2–8 keV energy range is linerarly polarized, at a ∼35% level. The phase-averaged polarization signal shows a marked increase with energy, ranging from ∼20% at 2–3 keV up to ∼80% at 6–8 keV, while the polarization angle remains constant. This indicates that radiation is mostly polarized in a single direction. The spectrum is well reproduced by a combination of either two thermal (blackbody) components or a blackbody and a power law. Both the polarization degree and angle also show a variation with the spin phase, and the former is almost anticorrelated with the source counts in the 2–8 and 2–4 keV bands. We discuss the possible implications and interpretations, based on a joint analysis of the spectral, polarization, and pulsation properties of the source. A scenario in which the surface temperature is not homogeneous, with a hotter cap covered by a gaseous atmosphere and a warmer region in a condensed state, provides a satisfactory description of both the phase- and energy-dependent spectro-polarimetric data. The (comparatively) small size of the two emitting regions, required to explain the observed pulsations, does not allow to reach a robust conclusion about the presence of vacuum birefringence effects.},
  author       = {Zane, Silvia and Taverna, Roberto and González–Caniulef, Denis and Muleri, Fabio and Turolla, Roberto and Heyl, Jeremy and Uchiyama, Keisuke and Ng, Mason and Tamagawa, Toru and Caiazzo, Ilaria and Di Lalla, Niccolò and Marshall, Herman L. and Bachetti, Matteo and La Monaca, Fabio and Gau, Ephraim and Di Marco, Alessandro and Baldini, Luca and Negro, Michela and Omodei, Nicola and Rankin, John and Matt, Giorgio and Pavlov, George G. and Kitaguchi, Takao and Krawczynski, Henric and Kislat, Fabian and Kelly, Ruth and Agudo, Iván and Antonelli, Lucio A. and Baumgartner, Wayne H. and Bellazzini, Ronaldo and Bianchi, Stefano and Bongiorno, Stephen D. and Bonino, Raffaella and Brez, Alessandro and Bucciantini, Niccolò and Capitanio, Fiamma and Castellano, Simone and Cavazzuti, Elisabetta and Chen, Chieng-Ting and Ciprini, Stefano and Costa, Enrico and De Rosa, Alessandra and Del Monte, Ettore and Di Gesu, Laura and Donnarumma, Immacolata and Doroshenko, Victor and Dovčiak, Michal and Ehlert, Steven R. and Enoto, Teruaki and Evangelista, Yuri and Fabiani, Sergio and Ferrazzoli, Riccardo and Garcia, Javier A. and Gunji, Shuichi and Hayashida, Kiyoshi and Iwakiri, Wataru and Jorstad, Svetlana G. and Kaaret, Philip and Karas, Vladimir and Kolodziejczak, Jeffery J. and Latronico, Luca and Liodakis, Ioannis and Maldera, Simone and Manfreda, Alberto and Marin, Frédéric and Marinucci, Andrea and Marscher, Alan P. and Massaro, Francesco and Mitsuishi, Ikuyuki and Mizuno, Tsunefumi and Ng, C.-Y. and O’Dell, Stephen L. and Oppedisano, Chiara and Papitto, Alessandro and Peirson, Abel L. and Perri, Matteo and Pesce-Rollins, Melissa and Petrucci, Pierre-Olivier and Pilia, Maura and Possenti, Andrea and Poutanen, Juri and Puccetti, Simonetta and Ramsey, Brian D. and Ratheesh, Ajay and Roberts, Oliver J. and Romani, Roger W. and Sgró, Carmelo and Slane, Patrick and Soffitta, Paolo and Spandre, Gloria and Swartz, Douglas A. and Tavecchio, Fabrizio and Tawara, Yuzuru and Tennant, Allyn F. and Thomas, Nicholas E. and Tombesi, Francesco and Trois, Alessio and Tsygankov, Sergey S. and Vink, Jacco and Weisskopf, Martin C. and Wu, Kinwah and Xie, Fei},
  issn         = {2041-8213},
  journal      = {The Astrophysical Journal Letters},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics},
  number       = {2},
  publisher    = {American Astronomical Society},
  title        = {{A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910}},
  doi          = {10.3847/2041-8213/acb703},
  volume       = {944},
  year         = {2023},
}

@article{15225,
  abstract     = {We argue that measurements of X-ray polarization using the recently launched Imaging X-ray Polarimetry Explorer will answer many open questions about magnetars in particular the physical state of their surfaces, whether vacuum birefringence exists, and the nature of the hard X-ray emission from these objects. We outline the capabilities of the instrument, specific models and the results of simulations for the magnetar 4U 0142+61.},
  author       = {Heyl, Jeremy and Caiazzo, Ilaria and González-Caniulef, Denis},
  issn         = {1743-9221},
  journal      = {Proceedings of the International Astronomical Union},
  keywords     = {Astronomy and Astrophysics, Space and Planetary Science},
  number       = {S363},
  pages        = {80--91},
  publisher    = {Cambridge University Press},
  title        = {{X-ray polarization at the crossroads}},
  doi          = {10.1017/s1743921322000916},
  volume       = {16},
  year         = {2023},
}

@article{15226,
  abstract     = {Due to the rich phenomenology and extreme magnetic conditions, magnetars will be targets of great interest for the upcoming polarimetry space missions. In particular, the Imaging X-ray Polarimetry Explorer (IXPE), recently launched in December 2021, will operate in the 2–8 keV range. This will open a new window to study the polarized, persistent X-ray emission from magnetars. In this talk, I will present simulations of IXPE observations of magnetars using the IXPEObsSim package. I will discuss future prospect to discriminate between different magnetar’s emission mechanisms, as well as a potential detection of the signal of vacuum birefringence using IXPE.

},
  author       = {González-Caniulef, Denis and Caiazzo, Ilaria and Heyl, Jeremy},
  issn         = {1743-9221},
  journal      = {Proceedings of the International Astronomical Union},
  keywords     = {Astronomy and Astrophysics, Space and Planetary Science},
  number       = {S363},
  pages        = {314--317},
  publisher    = {Cambridge University Press},
  title        = {{IXPE simulations for magnetars}},
  doi          = {10.1017/s1743921322000679},
  volume       = {16},
  year         = {2023},
}

@misc{15292,
  abstract     = {We present a rigid body animation technique which prevents solids from interpenetrating, dissipates energy through friction, and propagates shocks through contacts. We employ the Alternating Direction Method of Multipliers (ADMM) to couple non-smooth Coulomb friction with impact propagation, allowing efficient and accurate non-smooth dynamics along with a correct transmission of impacts through assemblies of rigid bodies. We further extend our method to model adhesion, dynamic friction and lubricated contact.},
  author       = {Chen, Yi-Lu and Ly, Mickaël and Wojtan, Christopher J},
  booktitle    = {Proceedings of the ACM SIGGRAPH/Eurographics Symposium on Computer Animation},
  location     = {Los Angeles, CA, United States},
  publisher    = {ACM},
  title        = {{Unified treatment of contact, friction and shock-propagation in rigid body animation}},
  doi          = {10.1145/3606037.3606836},
  year         = {2023},
}

@article{17074,
  abstract     = {We verify Bogoliubov's approximation for translation invariant Bose gases in the mean field regime, i.e. we prove that the ground state energy EN is given by EN=NeH+infσ(H)+oN→∞(1), where N is the number of particles, eH is the minimal Hartree energy and H is the Bogoliubov Hamiltonian. As an intermediate result we show the existence of approximate ground states ΨN, i.e. states satisfying ⟨HN⟩ΨN=EN+oN→∞(1), exhibiting complete Bose--Einstein condensation with respect to one of the Hartree minimizers.},
  author       = {Brooks, Morris and Seiringer, Robert},
  issn         = {2690-1005},
  journal      = {Probability and Mathematical Physics},
  number       = {4},
  pages        = {939--1000},
  publisher    = {Mathematical Sciences Publishers},
  title        = {{Validity of Bogoliubov’s approximation fortranslation-invariant Bose gases}},
  doi          = {10.2140/pmp.2022.3.939},
  volume       = {3},
  year         = {2023},
}

@article{17078,
  abstract     = {For the emergence of life, the abiotic synthesis of RNA from its monomers is a central step. We found that in alkaline, drying conditions in bulk and at heated air‐water interfaces, 2′,3′‐cyclic nucleotides oligomerised without additional catalyst, forming up to 10‐mers within a day. The oligomerisation proceeded at a pH range of 7–12, at temperatures between 40–80 °C and was marginally enhanced by K<jats:sup>+</jats:sup> ions. Among the canonical ribonucleotides, cGMP oligomerised most efficiently. Quantification was performed using HPLC coupled to ESI‐TOF by fitting the isotope distribution to the mass spectra. Our study suggests a oligomerisation mechanism where cGMP aids the incorporation of the relatively unreactive nucleotides C, A and U. The 2′,3′‐cyclic ribonucleotides are byproducts of prebiotic phosphorylation, nucleotide syntheses and RNA hydrolysis, indicating direct recycling pathways. The simple reaction condition offers a plausible entry point for RNA to the evolution of life on early Earth.},
  author       = {Dass, Avinash Vicholous and Wunnava, Sreekar and Langlais, Juliette and von der Esch, Beatriz and Krusche, Maik and Ufer, Lennard and Chrisam, Nico and Dubini, Romeo C. A. and Gartner, Florian and Angerpointner, Severin and Dirscherl, Christina F. and Rovo, Petra and Mast, Christof B. and Šponer, Judit E. and Ochsenfeld, Christian and Frey, Erwin and Braun, Dieter},
  issn         = {2570-4206},
  journal      = {ChemSystemsChem},
  number       = {1},
  publisher    = {Wiley},
  title        = {{RNA oligomerisation without added catalyst from 2′,3′‐cyclic nucleotides by drying at air-water interfaces}},
  doi          = {10.1002/syst.202200026},
  volume       = {5},
  year         = {2023},
}

@article{17079,
  abstract     = {We study moments of characteristic polynomials of truncated Haar distributed matrices from the three classical compact groups O(N), U(N) and Sp(2N). For finite matrix size we calculate the moments in terms of hypergeometric functions of matrix argument and give explicit integral representations highlighting the duality between the moment and the matrix size as well as the duality between the orthogonal and symplectic cases. Asymptotic expansions in strong and weak non-unitarity regimes are obtained. Using the connection to matrix hypergeometric functions, we establish limit theorems for the log-modulus of the characteristic polynomial evaluated on the unit circle.},
  author       = {Serebryakov, Alexander and Simm, Nick and Dubach, Guillaume},
  issn         = {2010-3271},
  journal      = {Random Matrices: Theory and Applications},
  number       = {01},
  publisher    = {World Scientific Publishing},
  title        = {{Characteristic polynomials of random truncations: Moments, duality and asymptotics}},
  doi          = {10.1142/s2010326322500496},
  volume       = {12},
  year         = {2023},
}

@unpublished{17100,
  abstract     = {Prophet inequalities are a central object of study in optimal stopping theory. A gambler is sent values online, sampled from an instance of independent distributions, in an adversarial, random or selected order, depending on the model. When observing each value, the gambler either accepts it as a reward or irrevocably rejects it and proceeds to observe the next value. The goal of the gambler, who cannot see the future, is maximising the expected value of the reward while competing against the expectation of a prophet (the offline maximum). In other words, one seeks to maximise the gambler-to-prophet ratio of the expectations.
The model, in which the gambler selects the arrival order first, and then observes the values, is known as Order Selection. In this model a ratio of 0.7251 has been proved to be attainable for any instance. In very recent work, this has been improved up to 0.7258. If the gambler chooses the arrival order (uniformly) at random, we obtain the Random Order model. The worst case ratio over all possible instances has been extensively studied for at least 40 years. In the recent work aforementioned, through simulations, this ratio has been shown to be at most 0.7254 for the Random Order model, thus establishing for the first time that carefully choosing the order, instead of simply taking it at random, benefits the gambler. We give an alternative, more rigorous proof of this fact, by showing mathematically that in the Random Order model, no algorithm can achieve a ratio larger than 0.7235. This sets a new state-of-the-art hardness for this model, and establishes more formally that there is a real benefit in choosing the order.},
  author       = {Giambartolomei, Giordano and Frederik Mallmann-Trenn, Frederik Mallmann-Trenn and Saona Urmeneta, Raimundo J},
  booktitle    = {arXiv},
  title        = {{Prophet inequalities: Separating random order from order selection}},
  doi          = {10.48550/arXiv.2304.04024},
  year         = {2023},
}

@article{18621,
  abstract     = {During neural development, cellular adhesion is crucial for interactions among and between neurons and surrounding tissues. This function is mediated by conserved cell adhesion molecules, which are tightly regulated to allow for coordinated neuronal outgrowth. Here, we show that the proprotein convertase KPC-1 (homolog of mammalian furin) regulates the Menorin adhesion complex during development of PVD dendritic arbors in Caenorhabditis elegans. We found a finely regulated antagonistic balance between PVD-expressed KPC-1 and the epidermally expressed putative cell adhesion molecule MNR-1 (Menorin). Genetically, partial loss of mnr-1 suppressed partial loss of kpc-1, and both loss of kpc-1 and transgenic overexpression of mnr-1 resulted in indistinguishable phenotypes in PVD dendrites. This balance regulated cell-surface localization of the DMA-1 leucine-rich transmembrane receptor in PVD neurons. Lastly, kpc-1 mutants showed increased amounts of MNR-1 and decreased amounts of muscle-derived LECT-2 (Chondromodulin II), which is also part of the Menorin adhesion complex. These observations suggest that KPC-1 in PVD neurons directly or indirectly controls the abundance of proteins of the Menorin adhesion complex from adjacent tissues, thereby providing negative feedback from the dendrite to the instructive cues of surrounding tissues.},
  author       = {Ramirez, Nelson and Belalcazar, Helen M. and Rahman, Maisha and Trivedi, Meera and Tang, Leo T. H. and Bülow, Hannes E.},
  issn         = {1477-9129},
  journal      = {Development},
  number       = {18},
  publisher    = {The Company of Biologists},
  title        = {{Convertase-dependent regulation of membrane-tethered and secreted ligands tunes dendrite adhesion}},
  doi          = {10.1242/dev.201208},
  volume       = {150},
  year         = {2023},
}

@article{18942,
  abstract     = {Photosynthesis is among the first processes negatively affected by environmental cues and its performance directly determines plant cell fitness and ultimately crop yield. Primarily sites of photosynthesis, chloroplasts are unique sites also for the biosynthesis of precursors of the growth regulator auxin and for sensing environmental stress, but their role in intracellular auxin homeostasis, vital for plant growth and survival in changing environments, remains poorly understood. Here, we identified two ATP-binding cassette (ABC) subfamily B transporters, ABCB28 and ABCB29, which export auxin across the chloroplast envelope to the cytosol in a concerted action in vivo. Moreover, we provide evidence for an auxin biosynthesis pathway in Arabidopsis thaliana chloroplasts. The overexpression of ABCB28 and ABCB29 influenced stomatal regulation and resulted in significantly improved water use efficiency and survival rates during salt and drought stresses. Our results suggest that chloroplast auxin production and transport contribute to stomata regulation for conserving water upon salt stress. ABCB28 and ABCB29 integrate photosynthesis and auxin signals and as such hold great potential to improve the adaptation potential of crops to environmental cues.},
  author       = {Tamizhselvan, Prashanth and Madhavan, Sharmila and Constan-Aguilar, Christian and Elrefaay, Eman Ryad and Liu, Jie and Pěnčík, Aleš and Novák, Ondřej and Cairó, Albert and Hrtyan, Mónika and Geisler, Markus and Tognetti, Vanesa Beatriz},
  issn         = {2223-7747},
  journal      = {Plants},
  number       = {1},
  publisher    = {MDPI},
  title        = {{Chloroplast auxin efflux mediated by ABCB28 and ABCB29 fine-tunes salt and drought stress responses in Arabidopsis}},
  doi          = {10.3390/plants13010007},
  volume       = {13},
  year         = {2023},
}

@article{18959,
  abstract     = {This workshop continues a series of workshops whose current format originated in 1981 under then-organizers Moser and Zehnder, and whose latest iteration took place in July 2023. The general goal of this series of workshops is to discuss the latest developments in the field of dynamical systems, broadly construed, and its connections with neighboring areas of mathematics such as differential geometry, partial differential equations, and more recently contact and symplectic geometry. We continued this tradition, bringing in new participants working in areas of dynamical systems and its connections with other areas of mathematics that are currently highly active and/or showing great promise for future development. Key focus areas for the 2023 workshop include spectral rigidity for planar domains, chaotic and oscillatory motions in celestial mechanics, conformal symplectic dynamics, and relations between dynamics.he workshop by the grant DMS-2230648, “US Junior Oberwolfach Fellows”.},
  author       = {Arnaud, Marie-Claude and Hutchings, Michael and Kaloshin, Vadim},
  issn         = {1660-8941},
  journal      = {Oberwolfach Reports},
  number       = {3},
  pages        = {1671--1730},
  publisher    = {EMS Press},
  title        = {{Dynamische Systeme}},
  doi          = {10.4171/owr/2023/30},
  volume       = {20},
  year         = {2023},
}

@article{19053,
  abstract     = {Building on previous works by Bilu, Chambert-Loir and Loeser, we study the asymptotic behaviour of the moduli space of sections of a given family over a smooth projective curve, assuming that the generic fiber is an equivariant compactification of a finite dimensional vector space. Working in a suitable Grothendieck ring of varieties, we show that the class of these moduli spaces converges, modulo an adequate normalisation, to a non-zero effective element, when the class of the sections goes arbitrary far from the boundary of the dual of the effective cone. The limit can be interpreted as a motivic Euler product in the sense of Bilu’s thesis. This result provides a positive answer to a motivic version of the Batyrev–Manin–Peyre conjectures in this particular setting.},
  author       = {Faisant, Loïs},
  issn         = {2191-0383},
  journal      = {Beiträge zur Algebra und Geometrie / Contributions to Algebra and Geometry},
  number       = {3},
  pages        = {783--850},
  publisher    = {Springer Nature},
  title        = {{Geometric Batyrev–Manin–Peyre for equivariant compactifications of additive groups}},
  doi          = {10.1007/s13366-022-00656-w},
  volume       = {64},
  year         = {2023},
}