\hbox{$0.7 \leqslant A_{V} \leqslant 1.2$}0.7 ⩽ AV⩽ 1.2 for the standard ISRF), better shielded from UV photons and where the amount of hydrogen is significantly higher, H-poor carbon can be transformed into H-rich carbon through H atom incorporation, a-C → a-C:H. Similarly, carbon accreted from the gas phase in these transition regions is likely to be and stay H-rich. Then, in the dense molecular clouds, most of the hydrogen is in molecular form and thus not available to produce a-C:H mantles on the grains.


They exploit the maps with different apertures and efficiencies and are applied individually or combined together, even with different weights (see e.g.


The authors used their new results together with


and low-redshift reference data for the Coma cluster


to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2.


According to the theoretical studies, dense cores eventually harbor the first protostellar cores, the first quasi-hydrostatic object during the star formation process (hereafter the first core; e.g.,


which provide the initial condition of star formation.


Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts


or its cessation, bringing the system back onto or even below the main sequence


with the CO properties potentially able to distinguish between these two scenarios.


and the magnetic field can exceed 0.15 T in both the intranetwork and the network quiet region


While the universality of the latter finding is in doubt


it certainly introduces very important subtleties to the old paradigm


The most recent spectroscopic study is from


who reinvestigated the internal rotation measurements and also determined hyperfine coupling parameters due to the nitrogen quadrupole


Gas masses can also be estimated with an empirically calibrated relation between single-band dust continuum flux at the Rayleigh–Jeans (R-J) tail and gas mass (e.g.,


These scaling relations are calibrated with local galaxies or with local galaxies and SMGs up to z ∼ 2. In this method, the gas-to-dust mass ratio is included in the conversion factor, and therefore does not need to be considered.


It remains unclear whether the empirical calibration methods are applicable to galaxies at z > 3 or how much scatter there is in the relationships.


The catalogue explores a wide range of linear diameters and masses, from sub-parsec (≤ 0.1 pc) to parsec scale (1−5 pc) with masses from 1 M⊙ to 105M⊙. These wide ranges mean that we probably mix several types of objects, from single star-forming cores to clumps containing multiple cores, even to entire clouds, depending on the distance of object. Most of these sources, however, fulfil the definition of clump, according to the definition of


Compact BH jets show an LX–LR correlation across ∼eight orders of magnitude in X-ray luminosity


a subset of sources follows a radio-bright correlation with a power-law slope of β ≈ 0.6 (where $L_R \propto L_X^{\beta }$, while others follow a steeper correlation with β ≳ 1 at high X-ray luminosities, before re-joining the other track around LX ≈ 1035 erg s−1 (e.g.


This is not the Kozai–Lidov resonance; in this case, the Kozai–Lidov domain (domain II in


is characterized by libration around $\omega _{\rm r}=0{^\circ }$ (or 180°) which is only briefly observed at the end of the backwards integrations


Out of the recent high-resolution Disk Substructures at High Angular Resolution Project (DSHARP) survey of 20 disks, 3 were found to harbor spirals: Elias 27, WaOph 6, and IM Lup


For example, most existing approaches rely on the adoption of a rigid physical model (e.g. analytic, two-parameter star formation histories combined with a standard dust attenuation curve and the assumption that all stars in a galaxy have the same metallicity) to describe galaxy SEDs (e.g.


this does not allow a physically consistent description of the contributions by stars, gas and dust to the integrated emission from a galaxy, nor the inclusion of a potential AGN component


To illustrate this, we show examples of calibration vectors for SDSS


We also plot the results of previous blank-field surveys


have produced filament catalogues in the SDSS


This ‘funnel’ accretion scenario is also found in other simulations with a spherical-like distribution of rotationally accreting material


At later times, the spectrum depends on the seed photon spectra, but it can roughly be estimated to be a flat spectrum from ∼1 eV to ∼0.1 TeV, while the supernova emission continues, which is expected based on more detailed calculations (e.g.,


This variety can be understood through a detailed radiative transfer calculation, which is analytically solvable only for simple cases (e.g., a static, plane-parallel slab by


Recently, Fernández-Martín et al. (2017) reported a slope of −0.108 ± 0.006 dex kpc−1 using optical spectra for H  ii regions located at RG between 5 and 17 kpc. That value of the slope is considerably much steeper than our determination and other previous estimates from the literature (e.g.


In view of the fact that the limiting magnitude of the follow-up wide-field survey projects is almost ≲21 mag (e.g.,


the maximum detectable distance for BH–NS kilonovae would be ≲200 Mpc, which can hardly cover the horizon of GW-triggered BH–NS merger events that O3 found (as shown in Figure 10).


Therefore, by restricting attention to data in the distribution outskirts, this approach throws away information and reduces the sensitivity to the IGM thermal state significantly


In the classic study, Hernquist & Ostriker (1992) developed a set of basis functions for density and gravitational potential that can reproduce complex morphology of galaxies with a small number of terms (e.g.,


These expansions reproduce the force field of an N-body simulation with a precision of a few percent, so representing the gravitational potential in our model with an expansion of basis functions is tempting. However, a truly realistic solution needs to accurately capture not only the current structure of the Galaxy but also its evolution in time.


This suggests that low-mass stars mostly contribute to carbon around solar metallicity, whereas at super-solar metallicities, massive stars produce carbon together with oxygen, thereby flattening or even decreasing the [C/O] ratio. This trend is in agreement with the metallicity dependent yields from


which provide higher carbon as [Fe/H] increases from massive stars (i.e. also increasing the O production) but lower carbon from low and intermediate mass stars as [Fe/H] increases (i.e. less production of C).


The dispersion relation of strong electromagnetic waves is altered due to the effective electron mass increased by the relativistic effect (e.g.,


Nevertheless, the debris that remains bound eventually contributes to the accretion flow around the SMBH. This part of the debris stream will finally be circularized by energy dissipation, leading to the formation of a small, initially ring-like, accretion disk around the black hole


It is worth noting that the “head-to-tail” scenario seems to support the idea that the filament is supported by sheared arcades


obtained the twin modes of MHD waves in LMXBs (including NS LMXBs and black hole LMXBs), which are considered as the sources of high-frequency QPOs.


The quantitative estimation of the radiated flare energy partition suggested about


and 55%–80% in WL for stellar flares (e.g.,


The nuclear semi-relativistic phase and the galaxy-scale molecular phase have been observed simultaneously in less than a dozen sources, with varied results:


in other cases data suggest momentum driven flows (e.g.


The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.


but there are doubts on the efficiency of accretion at high z, where high dust temperatures due to the CMB (see Section 3.3) keep the desorption time-scale for accreted materials short


Efforts have been made in quantifying mass, star formation rates, gas composition, and kinematics, as well as other LAE properties (e.g.,


This high AGN fraction detected so far, ~23%, makes the overdensity around 7C 1756+6520 similar to the interesting and well-studied cluster around the radio galaxy PKS 1138−262 from this point of view as well


As a result, optical studies have produced the largest number (∼1200) of new extra-Magellanic SNR candidates. Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5


This calibration is relatively insensitive to changes in gas pressure or ionization parameter, and we adopted it as fiducial approach in this paper (see


Of course, care has to be taken to avoid combinations of biosignature molecules which can be generated abiotically together (see e.g.


It is also a great advantage to directly compare the distributions of molecular gas observed by ALMA and positions of massive YSOs identified by Spitzer and Herschel (e.g.,


without any serious contamination in the line of sight.


Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases


and theoretically supported through detailed hydrodynamic simulations (e.g.


Events that took place in the far past are expected to have induced a thickening of the early Galactic disc, first by increasing the in-plane and vertical velocity dispersion of stars


is a good example of such a huge scatter in the FIR luminosity of elliptical galaxies.


The spectral synthesis match was performed using the Stellar Parameters Classification tool (SPC,


It determines effective temperature, surface gravity, metallicity, and line broadening by performing a cross-correlation of the observed spectra with a library of synthetic spectra, and interpolating the correlation peaks to determine the best-matching parameters.


from its interstellar medium and a presumed ${\rm DM}_{\rm Halo}\sim 50 \, {\rm pc \, cm^{-3}}$ from its halo


On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons


For a cosmic void, embedding requires the underdense interior to be “compensated” by an overdense bounding ridge, i.e., a compensated void


Secondly, there are three different KL mechanisms competing, thus the eccentricity of the inner binary of the CO triple can be pumped up by the torque either of the SMBH or the third companion in the CO triple, for which the KL time-scale is shorter (e.g.


A soft excess below 1.5 keV is also present


In all four cases of different initial amplitude, ρIA, the phase speed decreases slighty (consistent with observations; see


In the microquasar Cygnus X-1, radio emission has been measured with a flat spectrum, i.e. α = −0.06 ± 0.05 and α = 0.07 ± 0.04


Larger data sets of star-forming clumps, identified as gaseous protoclusters, also exhibit a mass-size relation.


compiled the observations of Shirley et al. (2003), Faúndez et al. (2004), and Fontani et al. (2005) in their Fig. 1, and found via least-squares regression the relation R ∝ M0.38.


Meanwhile, both studies exhibit mass scatter of about 1 dex and are compatible with constant gas surface density, that is, R ∝ M0.5.


Other examples of AGN with at least two variable phases of the X-ray winds are


magnetic helicity flux from anisotropy of the turbulence produced by differential rotation


USSRH are a prediction of turbulent re-acceleration models


However, about half of our most massive clumps migrate radially outwards.


but requires either large torques or steep surface density gradients


Nevertheless, Swift J1834.9−0846 has some interesting characteristics that are not shared with the entire magnetar population. First, the environment of Swift J1834.9−0846 is extremely crowded, with a Fermi GeV source, an H.E.S.S. TeV source, an SNR, a GMC, and an OH maser in its vicinity


There are two main formation channels that are thought to compete in NSC formation:


or via orbital segregation and merger of massive star clusters that migrate towards the galactic centre via dynamical friction


The explosions, however, leave imprints in the interstellar medium that can remain visible at radio wavelengths for 10 − 100 kyr


thereby allowing the association of pulsars with supernova remnants (SNRs).


It is thus worthwhile to investigate whether new physics might solve or at least alleviate the S8 discrepancy, a possibility that has been investigated in several works.


Models that have been contemplated in this sense include for example


extended or exotic DM and/or dark energy (DE) models and interactions


As a result, two main accretion regimes, super- and subcritical accretion, are expected depending on whether the source luminosity is higher or lower than a “critical luminosity” Lcrit, which strongly depends on the magnetic field of the NS


Unfortunately, in the case of the M 81 Group, this technique appears hardly applicable since the radial velocities of extragalactic and Galactic clouds share a similar LSR (local standard of rest) velocity range


The fast solar winds emanate from coronal holes at higher heliolatitudes


Aside from the histograms, we add a kernel smoothed curve, shown as shaded area, which is derived directly from the data set using an Epanechnikov Kernel Density estimator


with a bandwidth equal to 1.5 times the bin size.


Among the fibers, f1 is clearly tracing the central-densest part of the dust ridge well known from previous dust-continuum observations


For example, in studies of the evolution of MBHBs in circumnuclear discs, a modulated gas inflow from the outer gas distribution periodically fuels the accretion discs within the Hill radii of the individual MBHs (that, being smaller than the surrounding circumbinary disc, are commonly referred to as ‘mini-discs’ in the literature,


as a consequence of the non-axisymmetric and time-dependent potential of the binary.


For instance, it is well known that there is a persistent discrepancy between the Planck CMB measurements of H0 and the local measurements based on distance ladder


The values of the para-H2CO column density were obtained with APEX data (beam size ~30″;


AGNs with predominant radio emission from jet deviate from radio–IR correlation by showing radio-excess


Therefore, we examine if our NLS1s show radio-excess in the radio–IR correlation.


For an analytical expression of the poloidal magnetic field, we follow the practice of


in which poloidal field is given in terms of the vector potential as in (8)\begin{equation} B_{p}=-\frac{\partial A_{t}}{\partial x}\frac{\vec{r}_{\perp}}{r_{\perp}}+\left(\frac{\partial A_t}{\partial r_{\perp}}+\frac{A_t}{r_{\perp}}\right)\vec{x}. \end{equation}Bp=−∂At∂xr⊥r⊥+∂At∂r⊥+Atr⊥x.


Various values of β in MCs have been derived by several authors, ranging from β ∼ 0.38


More interestingly, there are hints suggesting that the impacts of projection effects extend beyond richness misidentification.


Secondly, when More et al. (2016) reported a detection of the so-called ‘splashback’ radius, a physically motivated boundary of cluster haloes, for redMaPPer clusters, the location of the splashback radius was found to be smaller than theoretical expectations (also see


Aperture photometry was performed with the DAOPHOT


that were made to study the impact of global magnetic fields (Lorentz-stress perturbations) on the eigenfrequencies and eigenfunctions of the standard solar model (model S in Christensen-Dalsgaard et al. 1996) focused on the details of the forward problem of frequency shifts induced by an axisymmetric magnetic field not aligned with the rotation axis.


For this work, we used two reference spectra:


an elliptical galaxy showing strong absorptions.


It has been classified as having a cometary-like morphology with an integrated subsolar metallicity of 12 + log(O/H) = 7.73–7.78


Secondly, the propagation of LyC photons within the ISM is favoured by a negligible amount of dust and low column density of HI (N(HI) ≤ 1018 cm-2) in a 10-pc scale region around the emitting star clusters. This could be the case for galaxies embedded in dark-matter halos with masses less than 108 M⊙


measured chemical abundances of six stars in Gaia 1, suggesting an equally high metallicity, but based on their abundance study, the suggestion of an extragalactic origin was revoked.


While a more metal-rich nature found by the latter authors conformed with the results by Simpson et al. (2017), the evolutionary diagrams of both studies are very dissimilar and could not be explained by one simple isochrone fit.


On the other hand, many fewer studies, all recent, were devoted to the full mass spectrum, using optical photometry


The magnetic fields in the low solar atmosphere could be very strong


Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,


It is important to do so because different processes, e.g.


are surely contributing to the same system


Works by other authors seem to support the idea that power-law beam electrons may precipitate throughout the entire flaring atmosphere down to the photosphere


, causing its heating via inelastic collisions with the ambient plasma via a hydrodynamic response


and a comparison with the other EoSs of the BSk family


This is perhaps a much too slow to account for the strong equipartition strength magnetic fields observed in the high-redshift galaxies with z > 1 (e.g.


or even for that in the slowly rotating nearby galaxies. This discrepancy leads one to invoke some additional mechanism such as cosmic rays (CRs) boosting the typical dynamo action.


Since the star-formation histories of galaxies (ETGs included, e.g.


can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs.


Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.


that artificially launch galactic winds, but the results are sensitive to numerical resolution and the exact subgrid model employed


The physical properties of SMGs derived from detailed studies of individual sources and large sky area submillimetre surveys suggest that SMGs represent an early evolutionary phase of all local ellipticals


The high-twist region in our result is also in agreement with the


We scan each trial of data and the on-source window in the 30–1000 Hz frequency band using a predefined bank of waveform templates


Previous studies of intermediate-age star clusters with eMSTOs usually showed tight SGBs throughout


Nevertheless, with the arrival of more powerful supercomputers, other authors have used instead global 3D MHD simulations to model DR and stellar magnetism in the convection zone of solar-like stars


where P0, T0, and Λ values are listed in Table 1, s is the depth from the nucleus surface, $f(s) = 1 - (1 - {s \over R})^4$ for s ≤ R, f(s) = 1 elsewhere, r ≈ 50 nm and R ≈ 5 mm are the radii of the grains of which cometary dust consists


and of the pebbles of which cometary nuclei


Three-dimensional simulations that include all three non-ideal MHD effects are also performed


To also cover lower luminosity galaxies, as the GOALS sample only includes luminous IR galaxies (LIRGs) and ultra-luminous IR galaxies (ULIRGs), we included 38 galaxies from Bernard-Salas et al. (2009) and


to reach the total sample of 196 galaxies with IR line fluxes in the 5.5 − 35 μm interval in which an AGN component is not detected.


It has been shown that shocks at the self-intersection point is the main cause of orbital energy dissipation and the subsequent formation of an accretion disc


While both codes are public, we understand that this approach is not yet ubiquitous in the field of galaxy-scale strong lensing (for instance, it has been difficult thus far to reproduce/check the results of


and Hezaveh et al. 2016), but we hope that our work can help make substructure lensing more reproducible.


In the regions we investigated, the Hapi region displays the lowest spectral slopes 8–11%/100 nm (see also


together with the isolated bright features (IBFs) and the clustered bright features in the Imhotep region.


We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework


Our model consists of four zones; an inner disk (zone 1, as in


Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed


The lack of close-in giant planets may also be explained by the intrinsically different planetary formation for these intermediate-mass stars (see the discussion in


Uncertainties in stellar radius estimates from photometric Kepler observations prevented a detailed assessment of the intrinsic planet size distribution


are the two EoS tables in more widespread use for astrophysical simulations.


varying within an order of magnitude over decades of observations


The [C II]–FIR luminosity ratios of these quasar hosts range from 10−4 to a few ×10−3


following the trend of decreasing [C II]–FIR ratio with increasing FIR luminosities found with the IR luminous star-forming systems


The column density is estimated from the fitted line profile by assuming local thermodynamic equilibrium (LTE)


In Equation (3), ΔE denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction


\hbox{$A_{V} \leqslant 0.7$}AV⩽ 0.7 for the standard ISRF), UV photons are responsible for causing the photo-dissociation of CH bonds, a-C:H → a-C.


However, Lyα emission is known to be extended beyond the continuum


and fluxes based on the TDOSE spectra would therefore be biased.


Methanethiol (or methyl mercaptan, CH3SH) was detected in the Sagittarius B2 (Sgr B2) region of the center of our Galaxy


In some cases, twisted magnetic flux tubes appear close enough to flow vortices, leading to magnetic and kinetic vortex structures closely coexisting in regions with high plasma-β


In the FS (BS), the 2D velocity map between the current and the previous (next) frame is constructed with almost the same method as


In the solar system, superrotation exists in the atmospheres of Venus, Titan, Saturn, and Jupiter, as well as the stratospheric atmosphere of Earth during the westerly phase of the quasi-biennial oscillation (e.g.,


Some of the gas accreting onto a dark matter halo is expected to penetrate surrounding hot gas in a form of filaments of dense and cold infalling gas and directly accrete onto the central galaxy at such high redshift, where the mass accretion rate and matter density tend to be high. Such direct gas supply through the filaments of cold gas could make the gas disk of the central galaxy more turbulent and gravitationally unstable, which leads to thick and clumpy stellar disk and bulge formation/growth in some cases (e.g.,


Moreover, to account for the broad emission line found required by the 2003 data, we added a Gaussian component whose width was kept fixed to σ = 400 eV, in accordance with what literature papers (e.g.


To understand NSC formation, it is therefore critical to be able to disentangle such degeneracies. For example, follow-up spectroscopic observations aiming at decomposing the main stellar populations and the dynamical imprint of a MBH rely on a good mass model to predict the stellar population velocity profile (e.g.


Therefore, methods with more advanced mathematical algorithms were introduced.


Coronal Hole Identification via Multi-thermal Emission Recognition Algorithm (CHIMERA)


have been found to be very effective and are widely used in online solar data visualization tools1$^,$ .2


Narrow-band imaging can efficiently detect LAHs at targeted redshifts through stacking


and narrow-band surveys enable ultradeep, blind samples of LAHs around distant galaxies


Examples of r-process sites that have been proposed and investigated by theoretical studies include (i) neutrino-driven winds from proto-neutron stars (NSs;


In fact, a variety of orientations have previously been observed, and the alignment of filaments and apparent field direction appear to vary between regions and for different gas densities (cf.,


During the past two decades, several Type IIb SNe with such interesting features have been monitored and studied well, e.g.,


Although shown to be too simplistic by the first X-ray studies of clusters


the self-similar relations allow us to investigate if astrophysical processes are less significant in more massive clusters or at higher redshift.


Further observations revealed a transition in average densities at planet sizes ∼1.5 R⊕


with smaller planets having densities consistent with rocky compositions while larger planets having lower densities indicating significant H/He envelopes.


The colour information is considered an important feature to find lenses (see e.g.


The use of colour queries is considered at least an interesting way to make a pre-selection and improve the final deep learning result purity.


At redshifts above z â¼ 1, it is nearly impossible to detect weak auroral lines for directly determining metallicity (but see


Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies


At the same time, gas accretion rates were maximal


Several mechanisms have been suggested that control the efficiency of mass transfer, mass accretion, and mass loss, including the existence of an accretion disk that regulates the amount of mass and angular momentum that can be accreted


In this work, we only focus on the very bright objects, i.e. ${\gt}10^{45}\, \rm erg\,s^{-1}$, avoiding the comparison with lower luminosity given the current limitations on observational and theoretical models. In particular, from an observational standpoint, the covered area and depth of current surveys pose serious challenges when extracting statistical properties of the LF at the faint end


We use a constant SPH artificial viscosity coefficient αSPH ≈ 0.55 such that the corresponding disc viscosity coefficient


These speeds far exceed the few km s−1 planet-frame velocities detected on other planets


The currently accepted distance of NGC 6231 is approximately 1580 pc, and its age is between 2and 8 Myr, with a significant intrinsic spread


and short-duration GRBs (likely caused by the coalescence of two neutron stars or a neutron star and black hole, which lasts for less than 2 s;


More recently, data from the Spectral and Photometric Imaging Receiver (SPIRE) instrument onboard Herschel ESA space observatory and Multiband Imaging Photometer for Spitzer (MIPS) onboard Spitzer allowed the identification of several dust clouds north of the M 81 galaxy with a total hydrogen column density in the range 1.5–5 × 1020 cm-2 and dust temperatures between 13 and 17 K


However, since there is no obvious difference among the individual clouds, there was no way to distinguish between Galactic or extragalactic origin although it is likely that some of the IR emission both toward M 81 and NGC 3077 is of Galactic origin.


98 clusters are identified by the South Pole Telescope (SPT;


but are not included in the Planck PSZ2 catalogue.


The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.


where observations require that $\sigma _T/m_chi \lesssim 1\, {\rm cm^2g^{-1}}$.


This process may provide an explanation for the observed braking indices of young pulsars with n ≠ 3


in contrast to the prediction of a rotating magnetic dipole in vacuum


Observing stellar halos in integrated light is, in principle, more easily scalable to the sample sizes needed to explore the wide variation in the accreted component that is predicted by simulations (e.g.,


One reason why we may not detect many dusty reds as jellyfish galaxies might be due to the fact that these galaxies, despite having relatively high SFRs (only four times lower than that in blue spirals at fixed mass,


However, this does not explain the discrepancy with


The detailed mechanistic route for the interstellar synthesis of MF is a subject of considerable debate


These physical conditions are consistent with what is found for Mrk 231


We then included an absorption component and fixed the photon index to 1.8, as expected for the intrinsic AGN emission (e.g.,


For internal consistency, all EWs in this work have been adjusted to the measurement scale of


If the core does collapse, the explosion proceeds via delayed explosion on short timescales


and 2D simulations suggest the explosion occurs before significant convection has had time to develop


and hence a symmetric explosion results.


While the velocity field is very regular, the velocity dispersion looks more complex. Instead of one peak extended along a southeast-northwest axis (Figs. 10, and 11), we find three (Fig. 13). The central one, elongated along the main axis of the galaxy and not perpendicular to it, is accompanied by two additional regions with wider lines to the northeast and southwest, separated by a total of 5.′′ 9 ± 0.′′2. At these locations we observe the transition between rigid body rotation and steep rotation curve to a flat one (see also


As mentioned before, we conclude that strong bars drive the trends of bar fraction with (g −r) colour, stellar mass, and SFR observed in other studies


A key question that remains unanswered is how BBHs are formed. Viable formation channels include


and dynamical encounters in dense stellar environments, such as globular clusters (e.g.,


The existence of relations between SFR and galaxy stellar mass (SFR–Mass) and specific star formation rate and mass (sSFR = SFR/Mass) have been established from z = 0 out to z > 2


listed in Table 1, are used in this work as fixed values.


A second explanation is related to the stability of H-rich carbon in the ISM, which depends strongly on the radiation field intensity to local density ratio


We followed the implication of this approach described in


and refer the reader to that work for more details.


As for Earth, modeling of exoplanet atmospheres requires as fundamental input the spectral energy distribution of the hosting star, especially UV and shorter wavelengths (e.g.,


The radio to X-ray spectrum of the forward shock afterglow emission of GW170817/GRB 170817A is fν ∝ ν−0.6, which yields a p = 2.2 in the slow-cooling synchrotron radiation scenario


while a portion of the Compton component will escape to reach an observer, the remains (refer as ${\tt{\rm simplc}}$,


will strike back to the disc to generate the reflected component.


When the fastest layers catch up with the slowest, the charged particles contained in the layers are accelerated through mildly relativistic collisionless shocks (internal shocks;


Previous observations show that para-H2CO (3–2) is sensitive to gas temperature at density 105 cm−3


The main conclusion in all these studies is that a [C ii] deficit exists at high redshift, most likely due to the starbursting nature of these galaxies rather than their metallicity, since most of these systems are close to solar (see, e.g.


In principle, an increase in accretion rate would be expected to result in an increase in the scale height of the funnel (e.g.


However, while this must happen over some range of $\dot{M}$ in order for the disc structure to transition from the thin disc expected for standard sub-Eddington accretion to the funnel-like geometry expected for super-Eddington accretion, as discussed by Lasota et al. (2016), once the disc reaches the point of being fully advection-dominated the opening angle of the disc should tend to a constant (H/R ∼ 1, where H is the scale height of the disc at radius R).


and to determine the redshift of galaxies


In the optically thin limit, the emission is significantly polarized


, an effect that has been observed in higher-luminosity AGN sources


To take an even more practical approach, we chose a normalized color parameter based on the Spitzer Infrared Array Camera


as a commonly used photometer for the observation of exoplanets (see, e.g.,


This limit is referred to as the quasi-static approximation to MHD


although recent numerical studies on its turbulent properties and anisotropy have been done as well


Downward field-aligned current is connected to the dawnside ionosphere, and upward field-aligned current is connected to the duskside ionosphere. The pair of field-aligned currents causes magnetic disturbances at mid- and low- latitudes


stars in different evolutionary states in Gaia 1 are progressively being sampled.


This provides a natural route for forming GRBs in low-metallicity environments, as found for most GRB hosts


A detailed theoretical model for gamma-rays from the collision of cosmic ray with the solar atmosphere was presented by


The predicted gamma-ray flux at energies from 10 MeV to 10 GeV has a large uncertainty, being sensitive to the assumptions about the cosmic-ray transport in the magnetic field near the Sun.


Here, τγ, ν is the optical depth of the ejecta to γ-rays and Kγ, ν is the photon inelasticity at a given frequency, where the Klein–Nishina cross section and the cross section for the Bethe–Heitler pair production in the field of a carbon nucleus are taken into account


One possible reaction pathway begins with electron ionization of H2, followed by exothermic proton transfer reactions to form H+MF and subsequent three-body association to generate H+MF-Ln clusters


empirical relations to derive stellar mass in the form of mass-luminosity relations


It has been found that alkali atoms are present in cool brown dwarf atmospheres, indicating that silicate rainout may occur in these objects


There is evidence for radio emission spread over the host galaxy scale for a number of Seyferts when observed with adequate angular resolution and sensitivity


In this case, bodies that formed inward of the snowline (Io) accreted from essentially water-poor building blocks, whereas bodies that formed outward of the snowline (Ganymede, Callisto) formed from a primordial mixture of water ice and silicates (e.g.,


Within this scenario, the low water content of Europa is puzzling.


whereas the more accurate ExoMol POKAZATEL line list


Finally, based on the CASSCF wave functions, the internally contracted multi-reference configuration interaction method with the Davidson correction (icMRCI+Q)


is performed to consider the dynamic correlation and size-consistency error.


This final long-lived stage of disc dispersal gives rise to transition discs which have lifetimes between 105 and 106 yr, but remain optically thick – ‘relic discs’


We recall that, traditionally the loops in the polarization diagram (namely, a plot of Q/I versus U/I for a given wavelength and for a range of magnetic field strength or orientation values) are identified to be due to the level-crossings in the incomplete PBE regime


The main group ureilites represent the mantle residues after the extraction of


We note that the blowout size can be increased with particle porosity and increasing stellar temperature


The goal of these simulations was twofold: (1) to determine how a coronal loop responds to different photospheric velocity patterns, and (2) to investigate how the electric current sheets are formed, as well as the details of the heating that occurs through the dissipation of magnetic energy


related the infrared characteristics to the underlying properties of the stars: objects that present He i features in emission or absorption are B3 or earlier; if the star presents Mg ii in emission but no He i, it is between B2 and b4; objects with Brγ emission but no evidence of He i or Mg ii are B5 or later.


Although SKA might provide number counts at sub-µJy levels


however, one may need to be wary of possible caveats in using radio source number counts at these flux-density levels as one might start seeing at sub-mJy levels, in addition to the powerful distant radio sources, a substantially increasing fraction of very different populations of radio sources, e.g. nearby normal galaxies, starburst galaxies, and even galactic sources


However, the energy balance equations can be expressed in an alternative way by including terms that vanish under spatial averaging and ensure Galilean invariance of all terms


Our result is consistent with that found by


and, according to their classification, it identifies M33 X-8 as a broadened disk source, or in other words, as a source whose spectrum is dominated by emission from a hot disk (see Table 2) and where the additional soft component may be the effect of an unrealistic description of the disk spectrum by the diskbb model.


In color-magnitude space, YSES 2b is very close to the innermost three planets of the HR 8799 multi-planetary system


In recent years, integral field spectroscopic (IFS) surveys


have overcome these problems with the use of instruments with larger FoVs and a fully spectral coverage (e.g


subsequently identified 17 candidate late-M, L, and T dwarfs in 232 arcmin2 of HST/Wide Field Camera 3 (WFC3) imaging of the Great Observatories Origins Deep Survey


using optical and near-infrared color selection, and determined a thin disk vertical scaleheight for these sources of 290 ± 40 pc.


The spatially resolved observations showed that the CND region was a complex dynamical system. For instance, the east and west dots were dominated by a fast shock and a slower shock


Newer, alternate cosmological probes could help alleviate this issue.


H ii starburst galaxy measurements that reach to z ∼ 2.4


Even though there is a lot of scatter in the D − HT diagram caused by variation in f from one comet to the next


This candidate appears to have one of the most compact orbits among the known SMBH binaries and has overcome the ‘final parsec problem’


The simplest of such methods uses a Wiener filtering technique


This approach assumes that the density/velocity field is described as a Gaussian random field and the Wiener filtered reconstruction is the maximum-a-posteriori (MAP) solution for the problem.


Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks


have presented a method for deriving an NLFFF model from sparsely distributed EUV loop observations.


These studies have focused on modeling the field in active regions, where the high density results in bright EUV emission and the limited size of the region allows for a reasonable number of free parameters. Additionally, the complexity of these methods suggests that their primary application would be the detailed study of a specific region of interest, rather than casual production of models for programmatic use. In contrast, the purpose of our study has been to develop a method for the fast production of global coronal magnetic field models based on widely available synoptic magnetograms and coronal images.


and we restricted them to the limiting cases derived in Sect. 3.5 of


rather than allowing them to take arbitrary values.


The radial distance between the centres of the Orion and Sagittarius arms near the Sun is λrad ≈ 2 kpc (cf.


They also can reconnect with the ambient field (e.g.,


However, recent numerical simulations of thermal tides in optically thick atmospheres by


show behaviour of the flow that is in good agreement with a model that uses radiative cooling.


Therefore, in this work we assumeNewtonian cooling as a first model of the action of radiation on atmospheric tides.


The Planck survey provides a large amount of data for polarisation studies at cloud scales


carried out a comparison of the metallicity gradients in the ISM (traced by young SPs) obtained by different numerical and analytical models


Different MHD oscillation modes have been identified to be responsible for QPPs in a single flaring loop


If the evolution proceeds under self-similar, isothermal collapse then the break in the profile will shift to smaller scales, eventually reaching the radius of the protostar


As described in Section 2.4, we find quiescent counterparts in Pan-STARRS and also add in coverage of southerly declinations by using the DeCAPS catalog (


; cross-matching for both catalogs is as explained in Appendix A.3).


However, these trends do not agree with those obtained by fitting the Burkert profile to nearby galaxies in the SPARC dataset and the classical Milky Way dSphs. This poses an issue for SIBEC-DM with Rc ≳ 1 kpc and a largely CDM-like matter power spectrum at late times


as was used in our simulations, although these scenarios are not well-motivated.


Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk


Given the nature of the variability, we measure the period via the reduced χ2 of a sinusoidal fit as a function of frequency (ideally suited to sinusoidal variability, e.g.


MaNGA observed approximately 10 000 galaxies, selected as an unbiased sample in terms of stellar mass (${\it M}_{\star } \gt 10^{9}\, {\rm M}_{\odot }$) and environments


The (μ, σ) pairs allowed in the window relevant for the operational gravitational wave detectors


are mainly constrained by (i) the results from searches for microlensing events on stars in our Galactic neighbourhood and (ii) the effect PBH gas accretion would have on the CMB temperature and ionization history


attribute the bimodality to unusually rapid gas accretion at earlier times, which is also characterized by a short time-scale to convert gas to stars.


The importance of additional processes such as internal waves (e.g.,


Additionally, wide binaries are in principle hard to detect, yielding some uncertainty in identifying them and consequently in drawing any conclusion on the PBH abundance


The high Fe charge states (⟨Fe⟩ ≥ 12) and abnormally high O7+/O6+ ratio (≥1) are the result of flare-related heating in the corona


and therefore they are independently reliable ICME indicators


We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework


which has previously been applied to characterize unresolved point sources in the inner Galaxy


By using the truncating method to neglect the higher-order derivative terms, the approximate correction formulas of parallel or perpendicular diffusion coefficients were obtained (see, e.g.,


For instance, partial ring distributions were frequently observed for solar wind protons at intermediate heliocentric distances, when the spacecraft approached the SWIC


We note that our 1D methods employed for modeling the collapse, core bounce, and initial explosion do not capture the full physics of the central engine (for a discussion, see


and this is a source of uncertainty in our yield calculations.


Some of these events may correspond to gravitationally lensed events with magnification factors ranging from a few tens to a few hundreds


Moreover, most miscentred clusters are merging or disturbed clusters with lower X-ray or SZ surface brightness, which makes them more difficult to be detected. The discrepancy of SZ signal is at a level of 10 per cent in our richness range


Allison, Sadler & Meekin (2014) identified four H i absorbers, including one previously unknown source, with the archival data of the H i Parkes All-Sky Survey (H i PASS; see


In particular, the central question of whether glycine (CH2(NH2)C(O)OH) exists or not in the ISM is one of the most pursued targets in astrochemistry.


However, the masses corresponding to impact flashes recorded on the Moon are several orders of magnitudes larger than mo


This means that the minimum kinetic energy Emin to produce a detectable impact flash on the Moon is much higher than the kinetic energy of a portion of the meteoroids included in the computation of hourly rates on Earth. This means that the velocity and mass distribution of meteoroids must be somehow included in Eq. (11) to take into consideration for the computation of the probability parameter p only those meteoroids with a kinetic energy above the threshold kinetic energy given by Emin


Simulations of this type seem to indicate that although this process is effective in the case of (quasi-)parallel shocks where the magnetic field is aligned with the direction of motion, it becomes ineffective once the angle between the magnetic field and the shock exceeds approximately 50°


Star formation can be triggered by these interactions, within clouds that reach sufficient density (Figs. 9 and 10). However, there is evidence that star formation is possible only within dark-matter encapsulated HVCs such as the Smith Cloud


In contrast, higher localization accuracy would be obtained by networking of 3rd generation GW detectors


Over the last decade, large observational efforts have been devoted to map the molecular gas reservoir of galaxies (e.g.,


These studies are largely based on observations of carbon monoxide (CO) rotational emission lines, used as a tracer of cold molecular hydrogen H2 (the ground-state rotational transition in particular traces the total molecular gas best),


Along decades, results based on this indirect method have indicated Z near or slightly above the solar value in nuclear regions


in consonance with predictions of chemical evolution models


showed that results obtained from this highly correlated approach are close to those deduced using standard coupled cluster techniques extrapolated to the complete basis set (CBS) limit, whereas a strong reduction in CPU time and disc occupancy are observed.


In panel b of Fig. 12, we also superimpose the distribution of [OIII]/[OII] ratio for the GRB sample of


For the majority of the GRBs, this ratio is about two, with seven cases at O32 > 4. GRB 021004 has a high value of O32 > 10 and is the strongest LAE of our golden sample (with fesc(Lyα) of 60%) in agreement with potential high fesc(LyC). Nevertheless, the Lyα profile of GRB 021004 is a single peak with no residual flux at the Lyα line center.


Additionally, CGM observations infer a significant amount of metals (e.g.


The intensity variations in the major and minor volatile species were found to be periodic, and were dependent on both the observing sub-spacecraft latitude and longitude


Given the reported high spin values for these bright AGNs


Thus, we can compare now the new value obtained for Ekin with the mechanical energy deposited in the ISM by the wind of the WR star, Ew = (0.7–2.2) × 1050 erg


The data were recorded in psrfits format and processed using PSRCHIVE tools


determined by ion storage ring experiments,


The expected B values in star forming regions range from ~100 μG, for low-mass objects


, to ~1 mG, as measured in regions hosting high-mass young stars (e.g.,


Numerous mass spectrometric studies have investigated the production of H+MF via various ion–molecule reactions and its fragmentation by metastable decay and collisions


The salmon-coloured points show recent results from other high-resolution spectrographs:


Since mergers are strong drivers of morphological change, this implies that our high-mass galaxies are mostly elliptical, which is in good agreement with observational results for ellipticals and S0 galaxies (e.g.


For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙) (e.g.


have shown that their age histograms contain a large majority of young (1–2 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decline


NGC 419, another young massive cluster with an age of 1.72 Gyr and a mass of ∼104 M⊙, are comparably massive with respect to other star clusters that show clear evidence of MPs


the possibility that they are tidal dwarf galaxies – galaxies formed by strong interactions with recycled material from massive host galaxies, high in metals, and intrinsically born with a lack of dark matter (see e.g.,


A CO spectroscopic redshift of 3.26 was first suggested by Z-spec


observations, then subsequently confirmed by observations by


The Mid-Infrared Spectrograph (MIRS) aboard the Infrared Telescope in Space (IRTS) has also obtained the 4.7–11.7$\, {\rm \mu m}$ spectrum for the diffuse ISM towards l = 44°20′, b = −0°20′


The primary tracer for H2 in current use is the J = (1−0) ground-state rotational transition of 12CO at a wavelength of 3 mm. While this tracer has become widely adopted over the years (see, e.g.,


and has been often defended as a reliable large-scale tracer for molecules in the ISM, it also remains the primary such tracer in common use. There are several reasons to be concerned about this.


It is reasonable to connect the scatter to the stellar rotation rate diversity, considering the fact that there exist noticeable differences in rotation periods between stars of the same temperature in young open clusters (e.g.


Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,


However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.


The pitch angle and the distance at a reference position of the three arms are taken from


These authors used the positions of water masers derived from parallax measurements as part of the Bar and Spiral Structure Legacy (BeSSeL) survey to fit the parameters of the spiral arms.


We found good agreement between the position of the FQS clouds and the modelled position of the Local and the Perseus arms,


Therefore, we can neglect the planet imprint and use this band to measure the stellar pulsations, and most specifically to tune their current phases (see phase shifts in


It is interesting to note that the [Ba/Fe] versus Rgc slope according to this Cepheid sample is also negative, as in our study. [Ba/Fe] is the only n-capture element-to-iron ratio with a negative radial gradient in our sample of stars and in


Dynamical models and N-body simulations (see, e.g.,


and references therein) have shown that, depending on the initial conditions, a bound pair of clusters may either become unbound, because of significant mass-loss in the early phases of stellar evolution, or merge into a single and more massive cluster on a short time-scale (≈60 Myr) due to loss of angular momentum from escaping stars


Inspired by earlier studies from Taylor & Manchester (1977) and


Lorimer et al. (2006) applied the snapshot approach to the canonical3 pulsar population to determine best-fitting probability density functions in Galactocentric radius (R), luminosity (L), height with respect to the Galactic plane (z), and the period P for the currently observed population of pulsars.


For instance, we can use these model-independent measurements


to test natural constants such as the speed of light


Selecting SMGs from observations at longer wavelengths is thought to favor galaxies at higher redshifts (e.g.,


although it is difficult to compare the redshift distributions in an unbiased way


and account for intrinsic variations of galaxy far-IR spectral energy distributions (SEDs).


Possible mechanisms responsible for the energization of particles around RFs have been widely investigated based on both spacecraft observations and numerical simulations during the past decade. The strong convection electric field induced by the strong magnetic field gradient of RFs provides significant adiabatic acceleration of the ambient particles


(simply K in other works) is the conversion factor from the MWO HKP-2 H & K flux (numerator of Equation (1)) to physical flux


We assume a power-law energy distribution of radiating electrons with somewhat shallow index of b = −1.5 that can account for the relatively flat spectrum of the source


The present observational probes that allow us to have a peak in this epoch are the absorption spectra of high-redshift quasars


However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars with metallicities as low as $10^{-4}\, \rm {Z_{\odot }}$


as well as several others with $\rm {[Fe/H]} \lt -5$


Recent relativistic (magneto-) hydrodynamics simulations


have illustrated the importance of the ambient medium in shaping the jet, thereby highlighting the importance of understanding the remnant structure and ejecta properties


It is, however, conceivable that the large grains in this source are not well aligned because the radiative torque mechanism does not operate efficiently on them: this could happen if the characteristic wavelength of the anisotropic component of the local radiation field were much smaller than the mid-plane grain sizes (e.g.


While there is almost unanimous agreement that AGNs of low to moderate luminosity (Lbol ≲ 1045 erg s−1) at z ≈ 0–3 lie on or below the main sequence (e.g.,


, no consensus exists for AGNs with Lbol > 1045 erg s−1.


As the quantity and quality of data available continue to improve over the years, the model parameters derived have become more precise, numerically. Ironically, those numerically more precise results do not converge


The scatters in density law parameters, such as scale lengths, scale heights and local densities of these Galactic components, as reported in the literature, are rather large.


the subhalos also retain their identity for quite some time after accreting a larger halo, so satellites in subhalos less massive than ~1012 M⊙ do not immediately see the effect of the hot gas in the larger halo and accrete in cold mode.


Thus, consistent with the results of Yang et al. (2012) and Béthermin et al. (2013), satellite galaxies continue to accrete gas and convert it to stars over a rather long period,


N-body simulations, combined with either hydrodynamic simulations or analytic prescriptions for migration and eccentricity/inclination damping of planetary growth, have also been used to examine the origins of such systems


It is still difficult to constrain the BH spin parameter from the modelling of the SED of M87 due to some degeneracy in model parameters (wind parameter, s, magnetic parameter ;


The open circle and square are the results from the Arecibo Ultra Deep Survey (AUDS)


we computed 95% upper limits for all the nondetections.


The very fast dissolution of tidally filling models with low King model concentration was already extensively discussed in the literature (e.g.


In 2013 May, the Kepler main mission ended with the failure of a second reaction wheel; however, the first four years of Kepler data have led to a wealth of planetary discoveries with a total of 4706 announced planet candidates


However, a large fraction (${\sim } 28{{\ \rm per\ cent}}$) was found to be inconsistent with the theoretical limit of −2/3 (‘line of death’;


and only specific physical scenarios remain plausible (large emitting radii and Lorentz factors of the flow,


Although our sample is definitely too small to make any strong conclusion in terms of statistical incidence of obscured AGN in dual systems, we note that the fraction of CT AGN in our sample of dual AGN is 25–50 per cent, i.e. higher than the fraction of hard X-ray selected CT AGN in isolated systems in a similar luminosity interval (BAT: 27 ± 4 per cent,


This method has since been used to successfully uncover highly obscured and even Compton-thick AGNs in several other works thus far


In the case of collimated relativistic jets, magnetic fields must play an important role


Optical coordinates, right ascension and declination (epoch 2000.0) for the identified counterpart from Zaritsky et al. (2002), or – when not available there – from


For about 80 yr since the discovery of the extremely hot corona around the late 1930s (Grotian 1939; Edlen 1945), people have worked hard on addressing this issue, and great advances have been made in observation and theoretical studies


The latter model has been invoked as a possible mechanism in the downstream of the CME shock


have established precise initial mass ranges for ECSNe to occur, although these mass ranges are highly sensitive to the adopted convection criteria, overshooting, and mass-loss prescriptions


Other emission lines, however, such as the far-infrared [C ii]λl58 µm line, are strikingly enhanced on global scales in dwarf galaxies (e.g.,


and to use their abundances to estimate the ages of stars, often using neutron capture s-process elements in combination with other elements with opposite behaviours, such as α elements – that we indicate as chemical clocks – and thus maximising the dependence of the relationship with age (see, e.g.,


We assume that polarized BELs are scattered into the line of sight by material that is close to coplanar with the BLR (i.e. the torus). This prediction has been searched for in RQ-NLS1s, but many objects have not been detected in polarized light, and none of the detected show any significant broadening of the BELs (e.g.


Inclusion of mass-loss and/or rotation would produce a similar increase in the Cepheid luminosity level at fixed mass (see


Doing so, we find EX ≈ EU ∼ 2 × 1032 erg for AD Leo


Evidence for offset dust continuum emission relative to the rest-UV has been identified in several high-redshift Lyman-break galaxies (LBGs;


In previous studies, geometrical models based on the assumption of different cone shapes were developed to obtain CME 3D parameters from single spacecraft observations


Analysis of the particle yields produced in relativistic A+A collisions within statistical (thermal) models, i.e., the Hadron Resonance Gas (HRG) model


shows the importance of the particle hard core repulsion.


The dimensionless accretion rate is estimated by $\dot{\mathscr {M}}=20.1\, \ell _{44}^{3/2}M_7^{-2}$ from the Shakura–Sunyaev disc model


where ℓ44 is the 5100 Å luminosity in units of $10^{44}\, {\rm erg\, s^{-1}}$ and $M_7=M_{\bullet }/10^7\, \mathrm{M}_{\odot }$.


showed spectral changes with observed power-law slope varying between 1.0 and 2.0 (see their Fig. 7). For a typical Galactic absorption of 3 × 1020 cm-2 the change from slope of 1.0 to 2.0 would alter our estimated fluxes by −14% (ROSAT), −13% (XMM-Newton), +7% (Swift-XRT), +76% (Suzaku), +25% (Einstein-IPC). The change is large for Suzaku observations since in this case we use the count rate between 2.0–10.0 keV and extrapolate it to the soft band. All other satellites are sensitive in the soft band and hence the fluxes are less dependent upon the assumed spectral index.


They can also shed light on the origins of supermassive black holes and early cosmological reionization and chemical enrichment


A high R-value suggests a small viewing angle to the jet axis, while a low R-value indicates more of an edge-on view to the quasar


, along with the discrepancy between our calculated ratio of Ebp/kBTc = 5.5 ± 0.1 and the prediction of Ebp/kBTc = 7, suggest that the model of Scudder & Olbert (1979) requires a minor update to either the theory or to the input parameters.


With such properties, TOI-849b represents one of the few planets populating the hot Neptune desert, a region on the radius-orbital distance plane characterised by a surprising deficit of Neptune-sized planets on very short orbits (e.g.


In Goswami et al. (2021), we present a detailed analysis and discussion on the classification criteria of CEMP stars, as well as the formation scenarios of CEMP stars put forward by different authors


Recently, we proposed an improved Amati correlation


by using the Gaussian copula, which is a powerful statistical tool capable of describing the dependence structures between multivariate random variables, and has been applied to various fields by the astronomical community


An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH–BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA


Deep Herschel/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects


If 26Al was introduced into the solar system at the earliest stage of the disk evolution (e.g.,


differences in Be–B and Al–Mg systematics between CH–CB and CV CAIs imply that the injection of 26Al have occurred between the evolutionary stages class I and class II of the solar protoplanetary disk.


and displays strong and variable radio polarization (e.g.


A number of theoretical studies predicted that the accretion flow components of hot geometrically thick (RIAF-like) and cold geometrically thin can coexist in either horizontal or vertical stratification (e.g.,


Two-point statistics are central to many of the leading cosmological analyses of the large-scale structure searching for deviations from ΛCDM


and a great deal of effort has gone into accurately modelling the non-linear matter power spectrum in modified gravity and dark energy cosmologies – a theoretical ingredient essential to extract the cosmological information locked in small scales (e.g.


Indeed, Mg ii is known as a good tracer of high column density H i gas in damped Lyman α absorbers (e.g.


on the other hand explored two types of models, with ages being either uniformly distributed between 0 and 1000 Myr, or linearly distributed in log space between 1 and 1000 Myr.


These latter authors found that the uniform-age models efficiently explain the size and luminosity statistics of bright sources observed by LOFAR, while the log-uniform models were a better representation of the faint population.


Modelling by both Shabala et al. (2020) and


confirms the picture in which the remnant lobes fade quickly below the LOFAR detection limit.


This can be mitigated by using integral field spectroscopy (IFS) which is being increasingly used for extragalactic studies (e.g.


although there could still be projection effects with the IFS data.


Recently, it has been demonstrated that its thermal X-ray spectrum is dominated by the colliding-wind region in the close binary, with only a weak/moderate contribution coming from the wind-wind interaction in the wide orbit


It is also well known that the radius R1.4 of canonical NSs is essentially determined by the pressure at densities around ρ0 ∼ 2.5ρ0


while the maximum mass of NSs is determined by the pressure at higher densities reached in the core.


Our findings of bulges and bars suggest a considerable on-going evolution in the local LSB galaxies and the bars might as well be playing a role in the bulge growth


A fraction of the stellar wind is captured and channelled along the strong magnetic field


of the neutron star on to the magnetic poles, producing regular X-ray pulsations caused by the spin period ∼283 s


Recent experiments for key nuclear reactions like 7Be(n,p)7Li and 7Be(d,p)24He allow for a reduction of the 7Li production by about 12%


We shall adopt here the EoS of the BSk21 model


as a representative example of contemporary EoS for the complete NS structure,


Our group is addressing this problem by combining a variety of complementary perspectives:


(iii) by characterizing the three-dimensional (3D) global velocity space through the analysis of the velocity dispersion profile and rotation curve from resolved star spectroscopy


A dust cloud composed by large grains ( ∼ 1 μm) would suppress the scattered intensity even at 1 keV, while it would significantly attenuate X-rays at ≤0.5 keV (e.g.


Previously, we retrieved and cross-matched a large quantity of atomic data from several major atomic databases such as the


and providers within the Virtual Atomic and Molecular Data Centre (VAMDC;


in preparation for quality assessment work


and superluminal motion and high brightness temperature


They may also be aligned in the direction of


or the drift velocity of the grains relative to the ambient gas


In addition to the stellar mass, the spin-filament alignment was shown to depend on other internal properties of galaxies. Blue or rotation-supported galaxies were found to dominate the alignment signal at low stellar mass, while red or dispersion-dominated galaxies tend to show a preferential perpendicular alignment


Instead, the most successful theoretical models link the growth of stellar mass to the growth of the dark matter halos that galaxies inhabit, for example, via subhalo abundance matching (e.g.,


This Tmai is at the low end of the Tmai output by thermal evolution models for multi-Gyr-old sub-Neptunes (e.g.,


Based on weak sources in Chandra deep field images, the threshold for PB adopted based on a balance between reliability and completeness varies from 0.002 to 0.007


Alternatively, the scarcity of detected pulsars might be caused by a more complex scattering structure towards the GC


The upper panel of Figure 4 also shows a strong correlation between [Na/Fe] and the δCN index, which is in good agreement with previous studies


Thus, in clustered DE scenarios, we should consider the contribution of perturbated DE components to the total mass of the haloes


We used total fluxes of 0.2 Jy and 0.55 Jy for the artificial sources; these values ensure that our simulated outflows are sufficiently faint to not violate the constraints given by the known recent brightness evolution of Sgr A* (0.2 Jy from the mean variability of ≈15% from June 2013 to February 2014 at 41 GHz, with 0.55 Jy corresponding to the strongest variation in the same period,


For this reason a subregion of this cloud has been the subject of many previous papers, dealing with different observational aspects of the star formation (SF), such as


According to the pseudo-time-dependent gas-phase astrochemical model under dense cloud conditions (104 cm−3, 10 K, 10 mag) by


the conversion of atomic N into N2 takes an order of Myr, depending on assumed elemental abundances. In the gas-ice model of Daranlot et al. (2012), under the similar physical conditions, the conversion of atomic N to N2 takes ~5 × 105 yr, and it occurs after the significant fraction of nitrogen is frozen out.


In particular, it is known to often display a blue wing (e.g.


generally interpreted as a signature of outflows with dust preferentially hiding one cone behind the stellar disc. For that reason, some studies have excluded the [O iii] blue wing


reported data from the high-resolution Spitzer-IRS spectra.


In this work, we aim to better understand how these considerations affect the observed SZE signals using high-resolution submillimeter and radio imaging of a representative sample of SZE-selected clusters.We present new observations at 345 GHz (19 2 resolution) with the Large APEX Bolometer Camera


on the Atacama Pathfinder EXperiment (APEX


Meanwhile, with the progress of observational studies, two groups of theoretical models, magnetic reconnection models and magnetohydrodynamic wave models, have traditionally attempted to explain coronal heating, but so far no models can address the key mystery perfectly


It has a contribution of at least 15 per cent in the clump at early stages of massive star formation, which is lower than that reported in previous studies


was the first to suggest the existence of an observational signature for the transition between fully and partly convective structures for pre-main sequence stars and predicted that it would result in a HRD gap. This author explored signatures of this transition in young clusters and linked the growth of a radiative core to rapid change in effective temperature caused by changes in the dominant energy transport mechanism and ignition of hydrogen burning.


it is well known that reaction barriers possibly present in gas-phase reactions are not significantly reduced when moving to ice-mediated reactions


spectral models from WM-BASIC for OB-stars


However, considering that little or nothing is known about the LECR fluxes in the Cas A SNR and uncertainties in the generally small cross-sections for the relevant reactions to produce either ${}^{44}_{}\mathrm{Ti}$  or excited ${}^{44}_{}\mathrm{Ca}^{*}$


the validity of such an interpretation of the discrepant measurements of ${}^{44}_{}\mathrm{Ti}$  fluxes at 68 and 78 keV and at 1.157 MeV by different instruments and by the same instrument (SPI) may be doubted.


These triggering processes were numerically studied by Karlický & Jungwirth (1989) and


Additional evolutionary channels for SNIa include


We ignore the pressure term in equation (4), which leads to a set of equations that conserve energy


The peak column densities and total masses of both sources deduced from the 1.3 mm continuum emission are ∼1 × 1024 cm−2, and ∼2 × 102 M⊙, respectively, with an assumption


and a uniform dust temperature of 20 K, which is typically adapted/estimated for galactic high-mass star-forming dust clumps (e.g.,


Dispersions are thought to be driven at least partially by thermal velocities or supernovae


Early work highlighting the issue of the high-redshift offset in the [O iii]λ5007/Hβ vs. [N ii]λ6584/Hα BPT diagram focused on these parameters (e.g.,


In fact, the jet–wind interaction alone can already perturb the jet


other studies describe the formation of both molecules and dust clusters from the shocked gas by assuming a chemical kinetic approach under non-equilibrium conditions and the subsequent coalescence and coagulation of these clusters to form dust grains


The presence of the substructure has been confirmed by Chandra and XMM-Newton


as well as by more recent SZE measurements


Our flared vertical profiles for the thin and thick disks


and are consistent with the number simulations of the chemodynamical evolution in Galactic disks formed in the cosmological context


The upper atmospheres (above optically thick clouds) of giant exoplanets and those of smaller planets around M stars can be probed using spectroscopy during primary and/or secondary transits


The laboratory data most widely used for comparison to observations are those provided by


The first reference gives IR spectra and band strengths of methanol ice at 10 K in the 2.5–20 μm range.


However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature


A statistical study was performed by Richardson & Cane (2011) on more than 300 ICMEs, showing that 80% of them is associated with an FD, detected by the anticoincidence guard data on the International Monitoring Platform (IMP-8;


and that the minimum GCR intensities occur within the MC.


Indeed, the scientific debate about the emission profile of the jet and the subsequent gamma-ray production mechanism of GRB 170817A is still ongoing


For the refractory and main component elements in CC chondrites, we examine the elemental and isotopic compositions of Ti and Cr, respectively, because these are lithophile elements whose isotopic compositions have been measured precisely for a large number of chondrites and their components


GRB 170817A was followed by the discovery of the optical counterpart Swope Supernova Survey 17a [SSS17a (AT 2017gfo)] ∼11 h later in the galaxy NGC 4993


The model of Charbonnel & Lagarde (2010) of thermohaline instability induced mixing and the model by Eggleton et al. (2008) are both based on the ideas of


Cluster number counts from Sunyaev-Z’eldovich surveys are routinely modelled in terms of the signal-to-noise ratio (S/N) or the Compton parameter of the detections, which can be related to the cluster mass via scaling relations from X-ray, lensing, or velocities (e.g.


This result is consistent with previous research within a 1σ error


Here, it is worth noting that the 1σ errors of the γ best fit from previous research are both larger than 0.01.


For the collision term associated with neutrino emission, absorption, and scattering with leptons, nucleons, and nuclei handles, the basic neutrino reactions are adopted


In the optically thin limit, the emission is significantly polarized


an effect that has been observed in higher-luminosity AGN sources


It is also much better at driving winds, because the CRs do not suffer strong energy losses via Alfven wave heating


We repeated the plasma pressure calculation presented by


and Fuselier et al. (2012) for the new ENA energy spectrum.


Such evolutionary behavior is consistent with “strangulation” wherein cold gas that could be used for star formation is depleted as satellites are accreted (e.g.,


has played a workhorse role in a number of previous studies (e.g.


Many of these works have the common goal of determining how GMCs are organized in the stages that precede their collapse and the consequent conversion of gas into stars.


has achieved ∼2% in the inference of H0 from time-delay cosmography under the assumption that the radial-mass distribution of the lens can be described by a power-law mass profile or a composite of a dark-matter halo


, we require multi-temperature components to achieve an adequate description of the observed coronal spectra.


May & Stevenson (2020) claimed that the differences between the retrieved phase offsets is the result of temporal binning which was not used by


and May & Stevenson (2020) but was used by Mendonça et al. (2018), Morello et al. (2019), and this work.


Various observational techniques, such as measuring the Gunn–Peterson optical depth from QSO spectra or the prevalence of Ly α emission in high-redshift galaxies, have placed very tight constraints on the volume filling fraction of neutral hydrogen in the intergalactic medium (IGM) towards the end of reionization at z∼ 6


also investigated the gradients of n-capture element abundance-to-iron ratios with respect to Rgc for a sample of 435 Cepheids.


in the local Universe no ionizing radiation has been detected directly


although some objects show indirect evidence of photon leakage


From the figure, it seems that there is not difference between the SM star and other stars in the remnant of SN 1006 in the aspect of proper motion, i.e. the proper motion of the SM star only slightly deviates from the median value of the proper motions of the stars at the direction of the SNR centre of SN 1006, and such a proper motion disfavours the SM star as the surviving companion of SN 1006


As an example, the analysis of the hyperfine structure of several N-bearing species, such as N-protonated isocyanic acid (H2NCO+,


) which has been detected toward G+0693-0.027


was required for its conclusive line-by-line identification.


The observational constraints of rdt and rdt/rBLR are discussed in estimating tcross for the double-peaked BEL CL-AGN NGC 3516, where rdt is a dust torus radius


In recent years, attention directed towards explosions of sub-MCh WDs triggered by double detonations (primarily related to a DD scenario) has led to promising results (e.g.


found that the deuteration (D/H ratio) of HC(O)NH2 in IRAS 16293 B is similar to that of HNCO, in agreement with the hypothesis that both species are chemically related via grain-surface reactions.


Also, NGC 4490 has a giant H i envelope that probably originated from the star formation


Alternatively, one can compute the bolometric luminosity following


However, there is overwhelming observational evidence that magnetic fields in the ISM have well-defined directions, indicating that turbulence is sub, trans-Alfvénic and hence turbulent properties are highly anisotropic


However, the question of whether galactic bars can significantly affect AGN activity is still under debate


N. E. Raouafi et al. (2015, in preparation) have argued that type II spicules have much more in common with so-called “classical” spicules


than do type I spicules. In particular, type II and classical spicules are both commonly observed in quiet Sun and coronal hole regions, whereas type I spicules appear to be exclusively confined to active regions.


The factor 1.08 is the multiplicative shear calibration bias of the used KSB+ pipeline


to convert from measured to true ellipticity.


Thus, it is possible that disks were massive enough to form the cores of planets at younger ages. This idea has been suggested by


Williams (2012), and Najita & Kenyon (2014), among others. In this scenario, the vast majority of the material composing planets must already be in the form of planetesimals, for rocky planet formation, and of already-formed planetary cores. The latter condition is necessary as gas giant planets need to accrete gas from the gas-rich disk.


The bimodality has now been observed in some simulations


There is also an observed discrepancy between the radial extents of the gas and dust components of protoplanetary discs, with dust discs being significantly more compact


This process can end up as a SN Ia, a highly magnetized WD (MWD), or an accretion-induced collapse


The synchrotron peak usually moves to higher frequencies with increasing flux during outbursts


but no correlation between the break energy and the flux exists when a broken power law is adopted to fit the X-ray spectra


The reason for this discrepancy is not known, but it is likely related to the different redshift ranges probed by the two methods (much more local sources are considered in the second one), and/or—under the assumption of a strong correlation between radio luminosity and environmental density (e.g.,


but see further in this section for different points of view)


To avoid catastrophic suppression of the dynamo action (α-quenching), the magnetic helicity due to the small-scale magnetic field should be removed from the system


Mechanisms suggested to produce these small-scale magnetic helicity fluxes are:


Top right: the r31 brightness temperature ratio of VLASPECS galaxies (green circles) is similar to that of


and z > 2 dusty star-forming galaxies (DSFGs; blue squares; compilation from Sharon et al. 2016; including data from


However, at the corresponding frequency of 138 d−1, the TESS high-cadence data (sector 10) show no signs of such a signal, confirming previous negative reports


The current model of the CGM suggests the presence of a clumpy multiphase medium which extends beyond the virial radius of the host galaxy, with a declining radial density profile, containing a substantial amount of gas and metals (e.g.


Density Functional Theory (DFT) has been used rigorously to calculate the harmonic frequencies and intensities of vibrational modes of PAHs in various forms including size, composition and charge states


The latest Fermi Large Area Telescope (Fermi-LAT) survey data are now providing strong evidence towards an origin mostly due to integrated radiation from blazars and radio galaxies (e.g.


The unprecedented quality of the light curves combined with new curve-shifting algorithms


lead to time delays with typically ∼3 per cent accuracy


The stream interface (S′-F′) is indicated by the vertical line in Fig. 2 and is characterized by a drop of the O7+/O6+ abundance ratio measured with SWICS in the bulk solar wind


For grains surrounded by an ice mantle, the optical properties are derived with the core-mantle Mie theory using the BHCOAT routine given in


The more contentious issue is that of the phase curve’s phase offset and nightside temperature.


initially reported only a 2σ upper limit on the nightside temperature of 650 K, while all subsequent reanalyses (including ours) favour a significantly detectable nightside temperature of ∼800 K.


In this scenario, BHs form in situ in the vicinity of a GN and sink to the inner region due to mass segregation or they are delivered to these regions by infalling globular clusters


then get captured in the disc by hydrodynamic drag as they cross the disc (e.g.


and for one hot Neptunian planet, GJ 435 b


Observations of the Antennae galaxies report only one TDG candidate, at the tip of the southern tail


but the exact nature of this structure is still questioned


Our adopted classification scheme is based on physical properties of a young stellar object, such as envelope and disk masses (e.g.


rather than on observational signatures, such as submillimeter luminosities or effective temperatures


Thus, both survival and replenishment of galaxies should be expected over the time, and two important factors come into play: (i) the accretion rate of galaxies; and (ii) the orbital dependence of galaxy properties (e.g.


The model has been chosen on the basis of a χ2 test and, in every image, the best fit is provided by a Moffat function


Different models for galaxy formation and evolution often make very different assumptions and/or predictions. Among them, semi-analytic galaxy formation models (SAMs; e.g.,


are two powerful tools to trace galaxy formation and evolution in cosmological volumes. SAMs are phenomenological models that use an approximate/empirical formula to describe all baryonic processes relevant to galaxy formation, such as gas accretion, heating and cooling, star formation, feedback from stars and AGN, mergers, and stripping due to tides and ram pressure.


Nevertheless, a recent study of the dynamics of dwarf spheroidals orbiting around the Milky Way has shown some inconsistencies with previous results


The escape fraction is a key parameter in studies of the contribution of the observed galaxy population to reionization


semi-analytic modelling of reionization (e.g.


Since the errors of the LIGO-estimated rates are dominated by Poisson statistics


we approximate the PDF for the expected number of detections $\mathcal {N}=\mathcal {R}VT$ (from the surveyed space–time volume VT) by $\mathrm{d}P/\mathrm{d}\mathcal {N}\propto \mathcal {N}^{k-1/2}\mathrm{e}^{-\mathcal {N}}/k!$, where k = 1 for each of the relevant cases ($\mathcal {R}_{190814}$, $\mathcal {R}_{170817}$, and $\mathcal {R}_{190425}$), and the factor of $\mathcal {N}^{-1/2}$ is from Jeffrey’s prior


The estimated spin-down energy is Ė = 1.36 × 1036 erg s-1 and the surface dipolar magnetic field is 7.4 × 1011 G


The initial perturbation can be compensated or uncompensated, which leads to different void growth scenarios


An accurate determination of the low-energy cutoff to non-thermal electron distributions is crucial for the calculation of power and consequently non-thermal energy in solar flares


Since AGB stars can become C rich and have been confirmed both theoretically and observationally as the main stellar site for the s-process (see, e.g.,


it is natural to interpret these post-AGB observations as the signature of the nucleosynthesis and mixing events that occurred during the preceeding AGB phase.


Previous studies suggested that the early disappearence of circumstellar discs could be related to environmental effects imposed by the presence of massive stars that produce strong UV radiation, stellar winds, and supernova explosions (see e.g.


However, we see no dependency of the spectral index on the position of the stars in our sample and any nearby OB star surrounding the Lupus clouds to support this scenario.


To avoid the redundancy and computational waste of representing the orbits of every single particle in the model, one can use a phase-space distribution function (DF) to represent each population of constituent particles (typically, various stellar populations and dark matter; see e.g.


While the composition of the target surface was different than in


and Higa et al. (1996) (fine granular material vs. solid ice), the similar behavior of the coefficient of restitution supports the fact that particle-surface collisions are very different from particle-particle collisions, and coefficients of restitution are only velocity dependent for collisions with particles with very different sizes (a much larger particle can be approximated as a target surface).


In particular, the “submillimeter-HCN diagram”, first proposed in Izumi et al. (2013) and later expanded upon in


is a very notable example of the use of molecular line ratios as a probe of AGN-galaxies; this diagram makes use of two line ratios, HCN(4−3)/HCO+(4−3) and HCN(4−3)/CS(7−6), where all of the molecules involved are considered tracers of dense gas.


One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500 Myr of Solar system history


This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in this case, today there should be several surviving fragments having diameters around 20 km and above the detection limit.


The CH and CH/CB (hereafter: CH–CB) chondrites and their components are characterized by enrichments in 15N (up to 1,100‰;


Once metallicity starts to increase, low- and intermediate-mass stars release carbon and massive stars start to eject more carbon than oxygen


Unlike LIGO/Virgo, which can only detect merging BHBs in the final inspiral phase before merger, LISA will be able to detect eccentric stellar-mass BHBs for long timescales before they merge in the LIGO/Virgo band (e.g.,


These have led to the discovery of metastable maser lines in 22 different regions


This is confirmed by the blind carbon monoxide (CO J = 1–0) survey of a subsample of the brightest 350 μm peakers (S350 ≥ 115 mJy), which has shown a strikingly similar redshift distribution as 850 μm selected SMGs (zCO = 2.5 ± 0.8;


In order to check the effects of the morphological K-correction, we used publicly available HST/ACS VF606W-band data over a 0.05 deg2 region in the COSMOS field from the CANDELS survey


For instance, a number of measurements have revealed that the stable isotopic compositions of all meteorites fall into two distinct families


Semiminor and semimajor axes of many 2FGL sources are derived with one order of magnitude higher uncertainties than those for Mrk 421 in the 2FGL catalogue


Perhaps a more likely possibility is that, even in this comparatively young source, the grains near the mid-plane, which dominate the total intensity, have already grown to sizes that exceed the maximum size $a_\mathrm{max} = \lambda /2\pi$ for producing polarized emission at wavelength λ (e.g.


It has been shown that for mildly positive surface density gradients or negative entropy gradients, a positive corotation torque can eventually counteract the effect of a negative differential Lindblad torque, which may stall or even reverse migration


Continuum and methanol line maps from Effelsberg observations have also been obtained as part of the GLOSTAR survey


The bar, detected in the NIR by Quillen et al. (1997) and


shows a prominent boxy-shape morphology.


The inferred mass of the galaxy (baryons) in the best model (5.4 × 1010 M⊙) is marginally consistent with the estimated stellar mass derived from the velocity dispersion – stellar mass correlation


These new limits, in conjunction with the inconsistency of isotropic flux interpretations, leave no room for an astrophysical interpretation of AAEs in the context of the standard model for time windows as short as 103 s. However, it has been shown that these events can be explained using physics beyond the standard model, as many models suggest that AAEs lend support for axionic dark matter, sterile neutrinos, supersymmetry, or heavy dark matter


can be constrained by this nonobservation at IceCube.


These simulations were tailored to the BHB system H1743−332, where there is Chandra high-resolution data in both states giving detailed spectral information on the wind or its absence


The slopes solely inferred from the CARS data are consistent with those reported by Greene et al. (2012) and


and are therefore on the shallower side of previous estimates.


and Kitaura et al. (2012) proposed a Gibbs sampling scheme to jointly infer density and velocity fields and corresponding power-spectra.


However, these approaches assume matter density amplitudes to be log-normally distributed. The log-normal distribution reproduces one- and two-point statistics but fails to reproduce higher-order statistics associated with the filamentary dark matter distribution.


Hence, the main idea is to consider the object x as the sum of two components, namely x = xP + xE, where xP represents the point sources and xE the extended source. This approach was proposed for the first time in


assuming that the positions of the point sources are known.


Several ALMA blind surveys have been performed and allowed to detect and characterize the faint SMGs across cosmic times (e.g.,


One can see that the larger the initial amplitude, ρIA, the stronger the decrease of the primary wave’s amplitude, which is consistent with observations


The observed electron cigar distribution and the associated magnetic dip are a strong indication of the betatron cooling effect. This betatron-mediated cigar distribution has been suggested in previous studies


but never clearly observed. These observations, for the first time, show a direct link between the cigar distribution and betatron cooling.


Another model-independent method for distances to PNe are a cluster membership, as studied extensively by Majaess et al. (2007, 2014), and as discussed in


built large-scale, axisymmetric, cycling magnetic fields of somewhat lower amplitude which did not eliminate the star’s differential rotation, reminiscent of the distributed αΩ-type dynamos prevalent in solar-like contexts.


kinetic instabilities such as the Buneman and modified two-stream instability (e.g.,


Lastly, post-AGB stellar evolution models, computed with updated physics in a reduced mass range


show a strong disagreement with the previous grids.


Starting from our completeness limit at 22 μm, after conservatively dereddening it by AV = 20, we assumed a spectral index γ = −2 (see Table 3 for definition) to compute the MIR luminosity from Eq. (6) of


From here on we present all the basic equations in the irreducible basis (see


The optical/near-IR photometry was then complemented with the 24 μm catalog


, built as summarized in Section 2.1 from the Multi-Band Imaging Photometer for Spitzer (MIPS) images


Such a distance would make PSR J2043+2740 a viable target for deep optical observations, never carried out until now, and might be compatible with the debated association


Computing the exact pressure and temperature broadened Voigt profile for each of these lines is computationally extremely demanding. There are several approximate methods for computing Voigt profiles available in the literature (e.g.


Among the latter, Joudaki et al. (2018) recently performed a combined analysis of cosmic shear tomography, galaxy–galaxy lensing tomography, and redshift space multipole power spectra using data from KiDS-450 (∼450 deg2 of cosmic shear data from the KiDS survey) and two overlapping spectroscopic surveys, the 2-degree Field Lensing Survey4 (2dFLenS;


Previous studies have classified light bridges based on their morphological properties. Light bridges separating two umbral regions are called strong light bridges (e.g.,


Their brightness is similar to that of the penumbra, and they typically appear between two regions with the same polarity. Faint light bridges (e.g.,


are elongated bright structures that penetrate the umbra. They are composed of rows of bright grains with sizes comparable to umbral dots.


in their Eq. (2), we plot the relation between the LTE kinetic temperature, TLTE, and the para-H2CO (3–2) line ratio in Fig. 5.


The bulk SW shows a fractionation of elemental abundances correlating with FIP, as previously observed by spacecraft (e.g.,


However, the better accuracy and element coverage of Genesis data compared to in situ measurements allows further insights into this FIP-related fractionation.


Their numerical simulations were performed using the classical version of the Mercury code


which does not include general relativity (GR) effects and tidal interaction with the central star. They studied how the initial number of planets, the spatial separation between them, and the location of the inner planet influence the efficiencies of high-eccentricity mechanisms. As a result, they found that the Kozai–Lidov mechanism plays the most important role in HJ production. The restriction made in the previous study, regarding not including the contribution of GR and realistic initial mass configurations (unequal masses), makes us wonder about the implications of these contributions on the efficiency of each high-eccentricity mechanism in the activation of the HJ production process.


Better agreement with observations can be obtained if freeze-out of O atoms onto dust grains is taken into account in gas-grain chemical models


, with consequence surface production of H2O and O2, which may trap a significant fraction of oxygen, leaving only some atomic O and CO in the gas phase.


To create a single mock light curve, pseudo-random numbers are generated using the Fast Mersenne Twister SFMT19937 generator seeded with hardware-generated random numbers (generated using Intel RDRAND instruction) to ensure that the random number sequences are free of artificial correlations


The submm photometry of HATLAS12-00 at 890 μm acquired with the Submillimeter Array (SMA) as part of this programme


is fully consistent with the 870 μm and 850 μm fluxes derived for this source from the LABOCA and SCUBA2 data to be presented here.


Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on the ionized gas


and the atomic phase – based on the Na D or Mg II lines in absorption (e.g.


Relics trace ICM shock waves with relatively low (M   3) Mach numbers


This assumption is inconsistent with our current understanding of the structure of MCs, which are known to be far from spherically symmetric, and instead consist of an intricate and inhomogeneous network of filaments and clumps within them (e.g.


In recent years, large-area optical surveys have detected candidate TDEs emitting at temperatures of a few ×104 K


However, even with these degrees of freedom, the models still often fail to explain the abundances of certain individual species at the order-of-magnitude level (see, e.g.,


, although they undoubtedly explain many of the observed abundance ratios.


A variety of other studies have reached the same conclusions, placing the combination of RP and photoionization of gas by massive stars as the dominant mechanism for disruption of molecular clouds and internal regulation of the SF process


as well as the best model using a Hernquist component for the stars and an NFW halo for the dark matter with and without adiabatic contraction, also from


More recent numerical and analytic models have continued in this vein (e.g.


rather than address the question of whether CRs represent a significant contribution to the support of the neutral material that dominates the total mass budget and occupies at least $\sim 50{{\ \rm per\ cent}}$ of the volume


Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk


that this ridge structure is governed by the degree of oscillation modes and resembles the predictions made by Ando & Osaki (1975).


found that the number density of massive quiescent and elliptical galaxies with Re 2.5 kpc decreases by about 30% from z~1 to z~0.2 and that their U−V colours are consistent with passive evolution. They concluded that the driving mechanism for the average size-growth of the whole population is the appearance at later epochs of larger quiescent galaxies.


This is not typical for embedded clusters, which have typical half mass radii of ∼0.8 pc


, and therefore would have less frequent interactions between cluster stars and a particular binary.


Previous works have confirmed that H-atmosphere models accurately describe the spectra of qLMXBs, with radii in the range 10–15 km, as expected for NSs, either from single sources (e.g.


Alternatively, BBHs can form dynamically in


the ice was irradiated by VUV photons at the Lyman alpha wavelength, and we now know that methanimine can be efficiently ionized by those photons, we can also argue that ionization of several methanimine molecules can instead trigger the process in cold interstellar ices.


While most systems with exo-Kuiper belts do not have known planetary mass companions, in a few of these it has been possible to directly image one, thus enabling the study of planet–disc interactions in more detail. There are well-known examples such as


and Fomalhaut having a narrow and eccentric planetesimal belt


Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see, e.g.,


NGC 5813 itself has been assumed to be dynamically old


with no evidence of a recent major merger in its history, as indicated by the lack of any significant disturbances to its dusty circumnuclear disc


These values are in the range of those observed towards the molecular clouds in the Galactic centre but lower than in Orion KL


To come to a robust conclusion, independent H0 probes with accuracy better than $2{{\ \rm per\ cent}}$ are crucial


The underlying cause of the split tracks (see


for a clustering analysis into the statistical robustness of this split) for BHXBs is not known


The retrograde x4 (stable) orbit family is also elongated perpendicular to the bar at small radii, but becomes rounder as it extends to larger radii (for detailed description of orbit families and how they are identified see


In the frame of reference rotating with the bar, all of these families are characterized by a 1:2 resonance between the tangential oscillation frequency (Ωϕ) and the radial or epicyclic frequency (ΩR).


The approximate rate of RETs (≥10−6 Mpc−3 yr−1


Such cores can be created within the CDM paradigm by a variety of baryonic processes (e.g.


However, on the other hand, understanding of the formation mechanism of massive stars is still elusive