Miracle-dz/UniFAR-FTUs huggingface dataset:
Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25

Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2–0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects, and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec−2. The ICL and the cluster CG contribute 44% ± 17% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature—for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster R200m, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations.
A photoevaporative gap in the closest planet-forming disc

The dispersal of the circum-stellar discs of dust and gas surrounding young low-mass stars has important implications for the formation of planetary systems. Photoevaporation from energetic radiation from the central object is thought to drive the dispersal in the majority of discs, by creating a gap which disconnects the outer from the inner regions of the disc and then disperses the outer disc from the inside-out, while the inner disc keeps draining viscously on to the star. In this Letter, we show that the disc around TW Hya, the closest protoplanetary disc to Earth, may be the first object where a photoevaporative gap has been imaged around the time at which it is being created. Indeed, the detected gap in the Atacama large millimeter/submilli-meter array images is consistent with the expectations of X-ray photoevaporation models, thus not requiring the presence of a planet. The photoevaporation model is also consistent with a broad range of properties of the TW Hya system, e.g. accretion rate and the location of the gap at the onset of dispersal. We show that the central, unresolved 870 mu m continuum source might be produced by free-free emission from the gas and/or residual dust inside the gap.
Explicit solutions for a nonlinear model on the honeycomb and triangular lattices

We study a simple nonlinear model deﬁned on the honeycomb and triangular lattices. We propose a bilin-earization scheme for the ﬁeld equations and demonstrate that the resulting system is closely related to the well-studied integrable models, such as the Hirota bilinear difference equation and the Ablowitz-Ladik system. This result is used to derive the two sets of explicit solutions: the N-soliton solutions and ones constructed of the Toeplitz determinants.
Hydrogen recombination with multilevel atoms

Hydrogen recombination is one of the most important atomic processes in many astrophysical objects such as Type II supernova (SN II) atmospheres, the high redshift Universe during the cosmological recombination era and H II regions in the interstellar medium. Accurate predictions of the ionization fraction can be quite different from those given by a simple solution if one takes into account many angular momentum substates, non-resonant processes and calculates the rates of all atomic processes from the solution of the radiative transfer equation instead of using a Planck function under the assumption of thermal equilibrium. We use the general-purpose model atmosphere code PHOENIX 1D to compare how the fundamental probabilities such as the photoionization probability, the escape probability and the collisional de-excitation probability are affected by the presence of other metals in the environment, multiple angular momentum substates and non-resonant processes. Our comparisons are based on a model of SN 1999em, SNe Type II, 20 d after its explosion.
Life after eruption – V. Spectroscopy of eight candidate old novae with Gemini-South

We present the analysis of photometric and spectroscopic data on eight candidates for post-nova systems. Five post-novae, V528 Aql, HS Sge, BS Sgr, GR Sgr and V999 Sgr, are successfully recovered. We furthermore identify likely candidates for the fields of V1301 Aql, V1151 Sgr and V3964 Sgr. The spectroscopic properties of the confirmed post-novae are briefly discussed. We find that two of the oldest post-novae in our sample, GR Sgr and V999 Sgr, contain an optically thick accretion disc, and thus can be suspected to have a high mass-transfer rate, contrary to what one would expect from most models. HS Sge and V528 Aql show evidence for a (comparatively) high system inclination, which makes them attractive targets for time-series observations. Finally, the presence of particularly strong He II emission together with a small eruption amplitude suggests that BS Sgr is a good candidate for an intermediate polar.
Plant complexes and homological stability for Hurwitz spaces

We study Hurwitz spaces with regard to homological stabilization. By a Hurwitz space, we mean a moduli space of branched, not necessarily connected coverings of a disk with fixed structure group and number of branch points. We choose a sequence of subspaces of Hurwitz spaces which is suitable for our investigations. In the first part, we introduce and study plant complexes, a large new class of simplicial complexes, generalizing the arc complex on a surface with marked points. In the second part, we generalize a result by Ellenberg-Venkatesh-Westerland by showing that homological stabilization of our sequence of Hurwitz spaces depends only on properties of their zeroth homology groups.
MAGNETIC FIELD STRUCTURE IN THE FLATTENED ENVELOPE AND JET IN THE YOUNG PROTOSTELLAR SYSTEM HH 211

HH 211 is a young Class 0 protostellar system with a flattened envelope, a possible rotating disk, and a collimated jet. We have mapped it with the Submillimeter Array in the 341.6 GHz continuum and SiO J = 8–7 at ∼0. ″6 resolution. The continuum traces the thermal dust emission in the flattened envelope and the possible disk. Linear polarization is detected in the continuum in the flattened envelope. The field lines implied from the polarization have different orientations, but they are not incompatible with current gravitational collapse models, which predict a different orientation depending on the region/distance. Also, we might have detected for the first time polarized SiO line emission in the jet due to the Goldreich–Kylafis effect. Observations at higher sensitivity are needed to determine the field morphology in the jet.
Streamwise and doubly-localised periodic orbits in plane Poiseuille flow

Abstract We study localised exact coherent structures in plane Poiseuille flow that are relative periodic orbits. They are obtained from extended states in smaller periodically continued domains, by increasing the length to obtain streamwise localisation and then by increasing the width to achieve spanwise localisation. The states maintain the travelling wave structure of the extended states, which is then modulated by a localised envelope on larger scales. In the streamwise direction, the envelope shows exponential localisation, with different exponents on the upstream and downstream sides. The upstream exponent increases linearly with Reynolds number $\mathit{Re}$ , but the downstream exponent is essentially independent of $\mathit{Re}$ . In the spanwise direction the decay is compatible with a power-law localisation. As the width increases the localised state undergoes further bifurcations which add additional unstable directions, so that the edge state, the relative attractor on the boundary between the laminar and turbulent motions, in the system becomes chaotic.
Synthetic activity indicators for M-type dwarf stars

Abstract Here, we present a set of time-dependent 3D RMHD simulations of a M-dwarf star representative of AD Leo, which extend from the upper convection zone into the chromosphere. The 3D model atmospheres are characterized by a very dynamic and intermittent structure on small spatial and temporal scales and a wealth of physical processes, which by nature cannot be described by means of 1D static model atmospheres. Artificial observations of these models imply that a combination of complementary diagnostics such as Ca II lines and the continuum intensity from UV to millimeter wavelengths, probe various properties of the dynamics, thermal and magnetic structure of the photosphere and the chromosphere and thus provide measures of stellar activity, which can be compared to observations. The complicated magnetic field structure and its imprint in synthetic diagnostics may have important implications for the understanding and characterization of stellar activity and with it possibly for the evaluation of planetary habitability around active M-dwarf stars.
Historical Touchstones and Imagined Futures During COVID-19 in Aotearoa/New Zealand

ABSTRACT During the COVID-19 pandemic to date, particular histories have come to serve as touchstones for the pandemic experience. The specific form this historical imagination takes can be significant as it is likely to shape people’s understandings and responses to the pandemic with consequences for official policy, community action and public behaviour. This research examines this imaginative space in Aotearoa/New Zealand’s public media during COVID-19, asking what past epidemics have been invoked and how. We conducted a content and thematic analysis of media stories in Aotearoa/NZ from February 2020 to December 2021. This analysis reveals how historical experiences are made meaningful in the context of the present crisis, and how the COVID-19 pandemic has prompted New Zealanders to look back on their histories for lessons and cautionary tales as they imagine possible futures. While the 1918 flu was the most frequent touchstone in both years, the focus of the stories changed, reflecting changes in public health policies. In 2020, the stories mirrored the major public health measures enacted by the government, namely isolation and quarantine requirements and lockdowns. They focused on anchoring the present in past experiences, collectively framing the ‘extraordinary’ as something more ‘ordinary’ and thus helping people to cope with the new crisis. In 2021, the focus on Māori populations increased, reflecting the emerging disparities in vaccination rates, as did explicit messaging encouraging vaccination. The sense of urgency grew, with the past providing impetus for present action, to bring about—or avert—particular imagined futures.
A few remarks on invariable generation in infinite groups

A subset [Formula: see text] of a group [Formula: see text] invariably generates [Formula: see text] if [Formula: see text] is generated by [Formula: see text] for any choice of [Formula: see text]. A topological group [Formula: see text] is said to be [Formula: see text] if it is invariably generated by some subset [Formula: see text], and [Formula: see text] if it is topologically invariably generated by some subset [Formula: see text]. In this paper, we study the problem of (topological) invariable generation for linear groups and for automorphism groups of trees. Our main results show that the Lie group [Formula: see text] and the automorphism group of a regular tree are [Formula: see text], and that the groups [Formula: see text] are not [Formula: see text] for countable fields of infinite transcendence degree over a prime field.
CIRCUMBINARY GAS ACCRETION ONTO A CENTRAL BINARY: INFRARED MOLECULAR HYDROGEN EMISSION FROM GG Tau A

We present high spatial resolution maps of ro-vibrational molecular hydrogen emission from the environment of the GG Tau A binary component in the GG Tau quadruple system. The H2 v = 1–0 S(1) emission is spatially resolved and encompasses the inner binary, with emission detected at locations that should be dynamically cleared on several hundred year timescales. Extensions of H2 gas emission are seen to ∼100 AU distances from the central stars. The v = 2–1 S(1) emission at 2.24 μm is also detected at ∼30 AU from the central stars, with a line ratio of 0.05 ± 0.01 with respect to the v = 1–0 S(1) emission. Assuming gas in LTE, this ratio corresponds to an emission environment at ∼1700 K. We estimate that this temperature is too high for quiescent gas heated by X-ray or UV emission from the central stars. Surprisingly, we find that the brightest region of H2 emission arises from a spatial location that is exactly coincident with a recently revealed dust “streamer” which seems to be transferring material from the outer circumbinary ring around GG Tau A into the inner region. As a result, we identify a new excitation mechanism for ro-vibrational H2 stimulation in the environment of young stars. The H2 in the GG Tau A system appears to be stimulated by mass accretion infall as material in the circumbinary ring accretes onto the system to replenish the inner circumstellar disks. We postulate that H2 stimulated by accretion infall could be present in other systems, particularly binaries and “transition disk” systems which have dust-cleared gaps in their circumstellar environments.
EVIDENCE FOR DCO+ AS A PROBE OF IONIZATION IN THE WARM DISK SURFACE

In this Letter, we model the chemistry of DCO+ in protoplanetary disks. We find that the overall distribution of the DCO+ abundance is qualitatively similar to that of CO but is dominated by a thin layer located at the inner disk surface. To understand its distribution, we investigate the different key gas-phase deuteration pathways that can lead to the formation of DCO+. Our analysis shows that the recent update in the exothermicity of the reaction involving CH2D+ as a parent molecule of DCO+ favors deuterium fractionation in warmer conditions. As a result, the formation of DCO+ is enhanced in the inner warm surface layers of the disk where X-ray ionization occurs. Our analysis points out that DCO+ is not a reliable tracer of the CO snow line as previously suggested. We thus predict that DCO+ is a tracer of active deuterium and, in particular, X-ray ionization of the inner disk.
The structure of approximate two electron wavefunctions in intense laser driven ionization dynamics

The structure of approximate two-electron wavefunctions in strong-field-driven ionization dynamics is investigated in depth, both theoretically and numerically. Theoretical analyses clarify that for two-electron singlet systems, the previously proposed time-dependent extended Hartree–Fock (TD-EHF) method (1995 Phys. Rev. A 51 3999) is equivalent to the multiconfiguration time-dependent Hartree–Fock method with two occupied orbitals. The latter wavefunction is further transformed into the natural expansion form, enabling the direct propagation of the natural orbitals (NOs). These methods, as well as the conventional time-dependent Hartree–Fock (TDHF) method, are numerically assessed as regards providing a description of the ionization dynamics of a one-dimensional helium atom model. This numerical analysis (i) explains the reason behind the well-known failure of the TDHF method to describe tunneling ionization, (ii) demonstrates the interpretive power of the TD-EHF wavefunction in both the original nonorthogonal formulation and the NO-based formulation, and (iii) highlights different manifestations of the electron correlation (an effect beyond the single-determinant description), in tunneling ionization, high harmonic generation, and nonsequential double ionization. Possible extensions of the NO basis approach to multielectron systems are briefly discussed.
A birational Nevanlinna constant and its consequences

abstract:The purpose of this paper is to modify the notion of the Nevanlinna constant ${\rm Nev}(D)$ introduced by the first author for an effective Cartier divisor on a projective variety $X$. The modified notion is called the {\it birational Nevanlinna constant} and is denoted by ${\rm Nev}_{{\rm bir}}(D)$. The goal of ${\rm Nev}(D)$ and ${\rm Nev}_{{\rm bir}}(D)$ is to measure what is possible using the filtration method introduced by Faltings and W\"{u}stholz, and further developed by Corvaja and Zannier and, independently, by Evertse and Ferretti. By computing ${\rm Nev}_{{\rm bir}}(D)$ using subsequent work of Autissier, we establish a general result (see the General Theorem in Section 1), in both the arithmetic and complex cases, which extends the results of Evertse-Ferretti and of Ru to general divisors. The notion ${\rm Nev}_{{\rm bir}}(D)$ originally came from applications involving Weil functions, but it also can be defined in terms of local effectivity of Cartier divisors after lifting by a proper birational map.
MULTI-EPOCH MULTI-FREQUENCY VLBI STUDY OF THE PARSEC-SCALE JET IN THE BLAZAR 3C 66A

We present observational results of the γ-ray blazar 3C 66A at 2.3, 8.4, and 22 GHz at four epochs during 2004–2005 with the VLBA. The resulting images show an overall core-jet structure extending roughly to the south, with two intermediate breaks occurring in the region near the core. By model-fitting to the visibility data, the northmost component, which is also the brightest, is identified as the core according to its relatively flat spectrum and its compactness. Combining our results with previous results to investigate the proper motions of the jet components, we found the kinematics of 3C 66A to be quite complicated, with components of inward and outward, subluminal and superluminal motions all detected in the radio structure. The superluminal motions indicate strong Doppler boosting exists in the jet. The apparent inward motions of the innermost components last for at least 10 years and could not be caused by newborn components. A possible reason could be non-stationarity of the core due to opacity change.
Adiabatic quantum dynamics of the Lipkin-Meshkov-Glick model

The adiabatic quantum evolution of the Lipkin-Meshkov-Glick (LMG) model across its quantum critical point is studied. The dynamics is realized by linearly switching the transverse field from an initial large value towards zero and considering different transition rates. We concentrate our attention on the residual energy after the quench in order to estimate the level of diabaticity of the evolution. We discuss a Landau-Zener approximation of the finite size LMG model, that is successful in reproducing the behavior of the residual energy as function of the transition rate in the most part of the regimes considered. We also support our description through the analysis of the entanglement entropy of the evolved state. The system proposed is a paradigm of infinite-range interaction or high-dimensional models.
PDF4LHC recommendations for Run II

The interpretation of LHC measurements requires a careful estimate of various sources of uncertainties that affect theoretical calculations. In this contribution, we present the PDF4LHC Working Group recommendations for the usage of sets of parton distribution functions (PDFs) at the LHC Run II. We review the construction and validation of the PDF4LHC15 combined sets, and study some of their phenomenological implications. We also address some recent criticism of these recommendations.
Modelling the variable broad-band optical/UV/X-ray spectrum of PG1211+143: Implications for the ionized outflow

We present the results from a detailed analysis of the 2007 Swift monitoring campaign of the quasar PG1211+143. We constructed broad-band, optical/UV/X-ray spectral energy distributions over three X-ray flux intervals. We fitted them with a model which accounts for the disc and the X-ray coronal emission and the warm absorber (well established in this source). The three flux spectra are well fitted by the model we considered. The disc inner temperature remains constant at ~2 eV, while X-rays are variable both in spectral slope and normalization. The absorber covers almost 90% of the central source. It is outflowing with a velocity less than 2.3*10^4 km/s (3sigma upper limit), and has a column density of ~10^23.2. Its ionization parameter varies by a factor of 1.6, and it is in photo-ionizing equilibrium with the ionizing flux. It is located at a distance of less than 0.35 pc from the central source and its relative thickness, DR/R is less than 0.1. The absorber' s ionization parameter variations can explain the larger than average amplitude of the X-ray variations. The absence of optical/UV variations (consistent with the high black hole mass estimate) argues against the presence of inward propagating disc fluctuations and strong X-ray illumination of the disc (in agreement with the low ratio of X-ray over the bolometric luminosity of ~20-35). We estimate an upper limit for the mass outflow of ~5 solar masses per year (~2.3 times the Eddington mass accretion rate). If the outflow rate is indeed that high, then it must be a short-lived episode in the quasar's life time. Finally, we estimate an upper limit for the kinetic power of the outflow of ~1.4*10^43 ergs/s. This outflow cannot deploy significant mechanical energy to the surrounding ISM of the quasar's host galaxy, but is sufficient to heat the ISM to 10^7 K and to produce a fast decline to the star formation rate of the galaxy.
THE RADIO–GAMMA CORRELATION IN STARBURST GALAXIES

We present a systematic study of non-thermal electron–proton plasma and its emission processes in starburst galaxies in order to explain the correlation between the luminosity in the radio band and the recently observed gamma luminosity. In doing so, a steady state description of the cosmic-ray (CR) electrons and protons within the spatially homogeneous starburst is considered where continuous momentum losses are included as well as catastrophic losses due to diffusion and advection. The primary source of the relativistic CRs, e.g., supernova remnants, provides a quasi-neutral plasma with a power-law spectrum in momentum where we account for rigidity-dependent differences between the electron and proton spectrum. We examine the resulting leptonic and hadronic radiation processes by synchrotron radiation, inverse Compton scattering, Bremsstrahlung, and hadronic pion production. Finally, the observations of NGC 253, M82, NGC 4945, and NGC 1068 in the radio and gamma-ray bands as well as the observed supernova rate are used to constrain a best-fit model. In the case of NGC 253, M82, and NGC 4945 our model is able to accurately describe the data, showing that: (i) supernovae are the dominant particle accelerators for NGC 253, M82, and NGC 4945, but not for NGC 1068; (ii) all considered starburst galaxies are poor proton calorimeters in which for NGC 253 the escape is predominantly driven by the galactic wind, whereas the diffusive escape dominates in NGC 4945 and M82 (at energies >1 TeV); and (iii) secondary electrons from hadronic pion production are important to model the radio flux, but the associated neutrino flux is below the current observation limit.