Context. Supergiant fast X-ray transients (SFXTs) are a subclass of high-mass X-ray binaries (HMXBs) in which a compact object accretes part of the clumpy wind of the blue supergiant companion, triggering series of brief X-ray flares lasting a few kiloseconds. Currently, only about 15 SFXTs are known.Aims. The EXTraS (Exploring the X-ray Transient and variable Sky) catalog provides the timing signatures

We confirm, at the 5.7σ level, previous studies reporting cosmic microwave background (CMB) temperatures being significantly lower around nearby spiral galaxies than expected from the ΛCDM model. Results from our earlier work were disputed in a recent paper, however, that analysis included areas far beyond the galactic halos, while disregarding the neighbourhood of the galaxies where the main signal

Context. The Herbig Ae/Be star HD 190073 is one of the very few magnetic Herbig Ae/Be stars for which close low-mass companions have been reported. Previously published magnetic field measurements indicated an annual change in the field configuration.Aims. We aim to study in detail the spectral and magnetic variability of this star and characterise its magnetosphere for the first time.Methods. Newly

Data from the ongoing Euclid survey will map out billions of galaxies in the Universe, covering more than a third of the sky. This data will provide a wealth of information about the large-scale structure of the Universe and will have a significant impact on cosmology in the coming years. In this paper we introduce an emulator-based halo model approach to forward-modeling the relationship between cosmological

Context. ALeRCE (Automatic Learning for the Rapid Classification of Events) is currently processing the Zwicky Transient Facility (ZTF) alert stream, in preparation for the Vera C. Rubin Observatory, and classifying objects using a broad taxonomy. The ALeRCE light curve classifier is a balanced random forest (BRF) algorithm with a two-level scheme that uses variability features computed from the ZTF

We performed a detailed abundance analysis of ten red giant members of the heavily obscured bulge globular cluster HP 1 using high-resolution, high S/N, near-infrared spectra collected with the Apache Point Observatory Galactic Evolution Experiment II survey (APOGEE-2), obtained as part of the bulge Cluster APOgee Survey (CAPOS). We investigated the chemical abundances for a variety of species, including

The systemic velocity or redshift of galaxies is a convenient tool to calculate their distances in the absence of primary methods, but the uncertainties on these flow distances may be substantial due to galaxy peculiar motions. Here, we derived a simple and easily applicable method to assign uncertainties to flow distances from four different methodologies, namely the Hubble law with both heliocentric

Context. Alfvén wave solar models (AWSOMs) have been very successful in describing the solar atmosphere by incorporating the Alfvén wave driving as extra contributions in the global MHD equations. However, they lack the contributions from other wave modes.Aims. We aim to write governing equations for the energy evolution equation of kink waves. In a similar manner to AWSOM, we combine the kink-wave-evolution

Aims. Soft gamma repeaters (SGRs) are highly magnetised neutron stars (magnetars) notable for their gamma-ray and X-ray outbursts. We used near-infrared (NIR) imaging of SGR 0501+4516 in the days, weeks, and years after its 2008 outburst to characterise the multi-wavelength emission, and to obtain a proper motion from our long temporal baseline observations.Methods. We present short- and long-term

The demographics of sub-Jovian planets around low-mass stars is dominated by populations of sub-Neptunes and super-Earths, distinguished by the presence or absence of envelopes of volatiles with a low molecular weight, that is, H2, He, and H2O. The current paradigm is that sub-Neptunes on close-in orbits evolve into super-Earths via atmospheric escape driven by high-energy stellar irradiation. We used

Context. The stellar mass-star formation rate (M⋆ − SFR) plane is an essential diagnostic to separate galaxy populations. However, we still lack a clear picture of how galaxies move within this plane along cosmic time.Aims. This study aims to provide an observational description of galaxy migrations in the M⋆ − SFR plane based on the reconstructed star formation histories (SFH) of a sample of galaxies

The missing satellite problem remains a central issue of the Lambda cold dark matter (ΛCDM) model. On a small scale, the number of observed dwarf galaxies is still fewer than the number predicted by existing theories. Therefore, finding fainter dwarf galaxies in deeper images is crucial for refining the existing theoretical framework. In this study, we propose an end-to-end automatic identification

Context. Pluto possesses a tenuous, time-variable, N2-dominated atmosphere, with extensive haze. Previous spectroscopic observations from the ground at near-infrared (NIR) and submillimeter (submm) wavelengths and New Horizons in the ultraviolet (UV) have revealed a Titan-like atmosphere with rich N2-CH4 photochemistry. The mid-infrared (MIR) range of Pluto’s spectrum, however, has remained out of

Context. Models predict that atomic carbon occurs at the surface and in the process of the formation of molecular clouds. This makes its fine-structure transitions a diagnostic of cloud formation.Aims. We study the distribution of atomic carbon in a small inconspicuous region toward the outer Galaxy that might be representative for a large fraction of the molecular gas of the Milky Way that is not

Context. Radiation plays a significant role in solar and astrophysical environments, as it may constitute a sizable fraction of the energy density, momentum flux, and total pressure. Modeling the dynamic interaction between radiation and magnetized plasmas in such environments is an intricate and computationally costly task.Aims. The goal of this work is to demonstrate the capabilities of the open-source

Context. Radiative transfer (RT) effects need to be taken into account when analysing spectral line observations. When the data are not sufficient for detailed modelling, simpler methods are needed. The escape probability formalism (EPF) is one such tool.Aims. We wish to quantify the model errors in the EPF analysis of interstellar clouds and cores.Methods. We introduce PEP, a parallel programme for

Context. R-process enhanced metal-poor stars ([Eu/Fe] ≥ +0.3 and [Fe/H] ≤ −1.0) are rare objects, the study of which can provide clues as to the astrophysical sites of the rapid neutron capture process.Aims. In this study, we investigate the detailed chemical abundance patterns of two of these anomalous stars, originally identified among stars observed by the GALAH survey. Our aim is to obtain the

Aims. The United Kingdom Infrared Telescope (UKIRT) microlensing survey was conducted over four years, from 2016 to 2019, with the goal of serving as a precursor to future near-infrared microlensing surveys. Focusing on stars in the Galactic center and utilizing near-infrared passbands, the survey identified approximately one thousand microlensing events, 27 of which displayed anomalies in their light

Context. The field of high redshift galaxy formation has been revolutionised by the James Webb Space Telescope (JWST), which is yielding unprecedented insights into galaxy assembly at early times. In addition to global statistics, including the redshift evolution of the ultraviolet luminosity function (UV LF) and stellar mass function (SMF), new datasets are providing information on galaxy properties

High-cadence surveys of the sky are revealing that a large fraction of red-supergiant (RSG) stars, which are the progenitors of Type II-Plateau (II-P) supernovae (SNe), explode within circumstellar material (CSM). Such Type II SNe exhibit a considerable diversity, with interaction signatures lasting from hours to days. As a result, they might merge with the Type IIn subclass, for which longer duration

Context. V1298 Tau is a very young and magnetically active K1V star that hosts a benchmark multi-planetary system to study planet formation and evolutionary history at the earliest stages. Thanks to the high interest, it has been the target of a multi-wavelength follow-up.Aims. We selected V1298 Tau for a first targeted follow-up at radio frequencies with the Karl G. Jansky Very Large Telescope (JVLA)

The properties of isolated Galactic radio pulsars can be inferred by modelling their evolution, from birth to the present, through pulsar population synthesis. This involves simulating a mock population, applying observational filters, and comparing the resulting sources to the limited subset of detected pulsars. We specifically focus on the magneto-rotational properties of Galactic isolated neutron

Context. Deuterated molecules can be used to study the physical conditions and astro-chemical evolution of molecular clouds.Aims. Large-sample surveys for deuterated molecules are needed to understand the enhancement of deuterated molecules from diffuse molecular gas to cold cores.Methods. A single-pointing survey toward the 559 Planck cold clumps of the Early Cold Core Catalogue (ECC) was conducted

Context. The origin of λ Boo stars is currently unknown. Very few of them are known as members of multiple systems, which could provide benchmark laboratories to study their origin.Aims. Our goal is to find new candidate λ Boo stars that belong to binary systems. Then, a detailed abundance determination of some candidates could confirm their true λ Boo nature, while the composition of any late-type

The Sun is a magnetic star, and the only spatio-temporally resolved astrophysical system displaying turbulent magnetohydrodynamic thermal convection. This makes it a privileged object of study to understand fluid turbulence in extreme regimes and its interactions with magnetic fields. Global analyses of high-resolution solar observations provided by the NASA Solar Dynamics Observatory (SDO) can shed

Context. Planetary nebulae (PNe) that are physical members of open star clusters (OCs) provide us with highly valuable data for stellar evolution studies. Unfortunately, they are extremely rare, with only three such instances previously confirmed in our Galaxy.Aims. In this study, we confirm the physical association of PN NGC 2818 with OC NGC 2818A, an association long debated in literature studies

Context. The MeerKAT Fornax Survey (MFS) is a large survey project mapping the H I in the Fornax cluster. Most of the cluster members detected in H I show significant signs of interaction with the intracluster medium or other galaxies. The galaxy ESO 358-60, however, stands out as its large H I disk appears regular and undisturbed. Combined with the fact that the galaxy’s systemic velocity is at the

We analyze JWST NIRSpec+MIRI/MRS observations of the infrared (IR) polycyclic aromatic hydrocarbon (PAH) features in the central regions (∼0.26″ at 6 μm; ∼50–440 pc depending on the source) of local luminous IR galaxies. In this work, we examine the effect of nuclear obscuration on the PAH features of deeply obscured nuclei, predominantly found in local luminous IR galaxies, and we compare these nuclei

Context. The study of large-scale structure benefits from an accurate and robust identification of the cosmic web. Having access to such classifications can facilitate a more complete extraction of cosmological information encoded therein. This information can then help us to improve the mapping and our understanding of galaxy-environment interactions. Classification methods such as T-web and V-web

An open issue about multiple stellar populations in globular clusters (GCs) is the possible existence of metallicity spreads in first-generation (FG) stars. Recent estimates based on the HST pseudo-colour map (PCM) derived unlikely large spreads in [Fe/H] from spreads in the colour col = mF275W − mF814W. The inferred metallicity spreads for many GCs are comparable to or even larger than the ones observed

Context. Far-ultraviolet (FUV) observations of pulsars allow us to measure surface temperatures of neutron stars and study their thermal evolution. Some pulsars can exhibit FUV bow-shock nebulae (BSNe), providing an additional tool for probing the interstellar medium and studying the pulsar’s properties. The nearby middle-aged gamma-ray pulsar J1741–2054 and its pulsar wind nebula (PWN) have been studied

Strong magnetic fields in the core of red-giant branch stars are expected to suppress the amplitudes of the multipole modes. This occurs when the strength of the internal magnetic field approaches the critical field strength, at which the magnetic forces become comparable to the buoyancy. We performed Hamiltonian ray tracing simulations of magneto-gravity waves to investigate the suppression of the

Fuzzy (wave) dark matter (FDM), the dynamical model underlying an ultralight bosonic dark matter species, produces a rich set of nongravitational signatures that distinguishes it markedly from the phenomenologically related warm (particle) dark matter (WDM) scenario. The emergence of extended interference fringes hosted by cosmic filaments is one such phenomenon reported by cosmological simulations

Context. The origin of He II emission in galaxies remains a debated topic, requiring ionizing photons with energies exceeding 54 eV. While massive stars, such as Wolf-Rayet stars, have been considered potential sources, their UV flux often fails to fully explain the observed He II emission. Recent studies suggest that X-ray binaries (XRBs) might contribute significantly to this ionization.Aims. We

Coronal lines are forbidden emission lines with a ionisation potential χ ≳ 100 eV. They are linked to energetic phenomena triggered by active galactic nuclei (AGNs) in the circumnuclear medium. We present the first high-angular-resolution integral-field analysis of the [Fe VII] λ6087 coronal line in a sample of four nearby low-inclination Seyfert galaxies of which three are of Type 1 and one of Type

Context. Recent observations with the James Webb Space Telescope (JWST) have revealed unprecedented details of an intricate filamentary structure of unshocked ejecta within the young supernova remnant (SNR) Cassiopeia A (Cas A), offering new insights into the mechanisms governing supernova (SN) explosions and the subsequent evolution of ejecta.Aims. We aim to investigate the origin and evolution of

Context. The driving and excitation mechanisms of decay-less kink oscillations in coronal loops remain under active debate. The photospheric dynamics may provide the continuous energy supply required to sustain these oscillations.Aims. We aim to quantify and provide simple observational constraints on the photospheric driving of coronal loops in a few typical active region configurations: sunspot,

Context. Solar energetic particles such as electrons can be accelerated to mildly relativistic velocities in the solar corona. These electrons travel through the turbulent corona, generating radio waves, which are then severely affected by scattering.Aims. The physical interpretation of the discrepancies between the actual and observed radio sources is still subject to debate. We used radio emission

Context. Source extraction in HI radio surveys is still often performed using visual (by-eye) inspection, but the efficacy of the procedure lacks rigorous quantitative assessment due its laborious nature. Thus, algorithmic methods are often preferred due to their repeatable results and speed.Aims. This work attempts to quantitatively assess the completeness and reliability of visual source extraction

Context. Bridging theory and observations is a key task in modern astrophysics, aimed at improving our understanding of the formation and evolution of galaxies. With the advent of state-of-the-art observational facilities, the accurate modeling of galaxy observables via radiative transfer simulations coupled to hydrodynamic simulations of galaxy formation must be performed.Aims. We present a novel

We analyze the emission and absorption lines during photospheric radius expansion (PRE) X-ray bursts from the ultracompact binary 4U 1820–30, observed with the Neutron Star Interior Composition Explorer (NICER). Using Monte Carlo simulations to estimate the significance, we identified a 1 kiloelectron volt (keV) emission line from 14 bursts, a 3 keV absorption line from 12 bursts, and a 1.6 keV absorption

The evolution of quiescent galaxies is driven by numerous physical processes, often considered to be related to their stellar mass and environment over cosmic time. Tracing their stellar populations can provide insight into the processes that transformed these galaxies into their observed quiescent state. In particular, higher-redshift galaxies, being younger, exhibit more pronounced relative age differences

Context. Freshly injected interstellar pick-up ion (PUIs) are expected to exhibit a simple, torus-shaped velocity distribution function (VDF). The PUI velocity in the solar wind (SW) frame depends on the velocity of the interstellar neutral (ISN) population at the pick-up position.Aims. We directly compare PUI VDFs measured by the plasma and suprathermal ion composition (PLASTIC) instrument over the

Thermohaline mixing is one of the main processes in low-mass red giant stars that affect the transport of chemicals and, thus, the surface abundances along the evolution. The interplay of thermohaline mixing with other processes, such as downward overshooting from the convective envelope, needs to be carefully investigated. This study aims to understand the combined effects of thermohaline mixing and

Context. More than 200 A- and F-type stars observed with Kepler exhibit a distinctive hump and spike feature in their Fourier spectra. The hump is commonly interpreted as unresolved Rossby modes, while the spike has been linked to rotational modulation. This feature has led these stars to be referred to as ‘hump and spike’ stars. However, two competing interpretations exist for the spike.Aims. This

Context. Open cluster (OC) groups are collections of spatially close OCs originating from the same giant molecular cloud. The formation mechanism of the OC groups remains unclear due to limited sample size and data precision. Recent advances in astrometric data from the Gaia mission have provided an unprecedented opportunity to study OC groups in detail.Aims. We aim to extend the sample of OC groups

Context. The influence of magnetic fields on stellar evolution remains unresolved. It has been proposed that if there is a large-scale magnetic field in the stellar interior, torsional Alfvén waves could arise, efficiently transporting angular momentum. In fact, the observed variations in the rotation periods of some magnetic stars can be attributed to these torsional Alfvén waves’ standing waves.Aims

Context. Active galactic nuclei (AGNs) play a vital role in the evolution of galaxies over cosmic time, significantly influencing their star formation and growth. As obscured AGNs are difficult to identify due to obscuration by gas and dust, our understanding of their full impact is still under study. It is essential to investigate their properties and distribution, in particular type II quasars (QSO2s)

Context. Understanding the configuration of galactic magnetic fields is essential for interpreting feedback processes in galaxies. Despite their importance, the exact structure of these fields, particularly in galactic halos, remains unclear. Accurate descriptions are crucial for understanding the interaction between star formation and halo magnetisation.Aims. By systematically analysing the polarisation

A recent study shows that if the power spectra (PS) of accreting compact objects consist of a combination of Lorentzian functions that are coherent in different energy bands but incoherent with each other, the same is true for the real and imaginary parts of the cross spectrum (CS). Using this idea, we discovered imaginary quasi-periodic oscillations (QPOs) in NICER observations of the black hole candidate

Context. Searching for planets analogous to Earth in terms of mass and equilibrium temperature is currently the first step in the quest for habitable conditions outside our Solar System and, ultimately, the search for life in the universe. Future missions such as PLAnetary Transits and Oscillations of stars or Large Interferometer For Exoplanets will begin to detect and characterise these small, cold

Aims. Using public data collected by the Fermi Large Area Telescope (LAT) over 16 years and the 1523 days of survey data (3HWC) from the High Altitude Water Cherenkov (HAWC) observatory, we searched for possible GeV-TeV connections in globular clusters (GCs).Methods. Excluding 44 confirmed γ-ray detections of GCs in the latest Fourth Fermi-LAT point source catalog (4FGL-DR4), we searched for possible

Context. Pulsars represent one of the possible final stages in the evolution of massive stars. If a supernova explosion is anisotropic, it can give the pulsar a powerful “kick”, propelling it to supersonic speeds. The resulting pulsar wind nebula is significantly reshaped by its interaction with the surrounding medium as the pulsar moves through it. First, the pulsar crosses the supernova remnant (SNR)

We estimate the magnetic field in the jets of the recently discovered 7 Mpc long Porphyrion system. We used nondetection of the system in gamma-rays to derive a lower bound on the co-moving magnetic field strength at the level of ∼10 nG (comoving). This value is consistent with recent estimates of magnetic fields in the filaments of the large-scale structure. We discuss the possibility that, instead

Context. Low-mass stellar and substellar companions are indispensable objects for verifying evolutionary models that transition from low-mass stars to planets. Their formation is likely also affected by the surrounding stellar environment. The Fornax-Horologium (FH) association is a recently classified young association in the solar neighbourhood with a dissolving open cluster in its centre. It has

Context. A long-standing enigma in observational astronomy is the identification of the so-called 21 µm feature in a subset of envelopes of post-asymptotic giant branch (post-AGB) stars. Identifying this transient feature is important for understanding the chemical processes during the brief post-AGB phase and the enrichment of the interstellar medium. Understanding the structures and chemical environments

Understanding the creation of relativistic jets originating from active galactic nuclei (AGNs) requires a thorough understanding of the accompanying plasma instabilities. Our high-sensitivity, high-resolution, global, very-long-baseline-interferometry observations of the jet in the radio galaxy 3C 84 have enabled us to study its inner morphology. We find that its thread-like pattern can be described

Aims. The James Webb Space Telescope now enables the spectral study of ices with unprecedented sensitivity and angular resolution. Water ice plays a crucial role in the growth of grains and in planetary formation but its spatial distribution in protoplanetary disks is poorly constrained. To aid the interpretation of future observations, we study here for the first time how the water ice band depends

Aims. Previous estimates of planet occurrence rates in the CARMENES survey indicated increased numbers of planets on short orbits for M dwarfs with masses below 0.34M⊙. Here we focused on the lowest-mass stars in the survey, comprising 15 inactive targets with masses under 0.16 M⊙.Methods. To correct for detection biases, we determined detection sensitivity maps for individual targets and the entire

Aims. There is evidence that stars and browns dwarfs grow through episodic rather than continuous gas accretion. However, the role of episodic accretion in the formation of brown dwarfs remains mostly unexplored. We investigate the role of episodic accretion, triggered by the magnetorotational instability in the inner disk regions, resulting in episodic outbursts during the formation of brown dwarfs