As seen in Fig. 8 there are no Bullet cluster analogues (structures of approximate mass and dissociation) in L210N1024NR, this is unsurprising as a simulation requires a significantly larger volume than that of L210N1024NR ((210cMpc h−1)3) to expect such an object (e.g.


This phenomenon is observed to start at higher frequencies (where the emission is produced closer to the compact object) and terminates as the jet break evolves through the radio band


There are two primary causes for darkness in GRBs: attenuation by dust, or rest frame ultraviolet H i absorption at high redshift


The number density of the ambient medium is assumed to be


In absorption, bands at 3.4, 6.85, and 7.25 μm are also observed in the diffuse interstellar medium (ISM) of our Galaxy, as well as in extragalactic ISM, and can be well represented by a material with a significant amount of aliphatic character, also called HAC or a-C:H, which is a family of hydrogenated amorphous carbons (e.g.


but its location is actually outside the structure


The origin of hard lag is not clearly known. One possible explanation is provided by the propagation fluctuation model in which fluctuations associated with accretion flow propagate inwards in an accretion disc and thus resulting in the emission of the soft photons from relatively outer regions earlier than the hard photons from the innermost regions


The Sun is situated at the inner edge of the Orion arm


Also for dSphs, for which the determination of the dark matter density distribution is more difficult, there are indications that cored dark matter density profiles may be favoured with respect to cuspy profiles


The discrepancy can be calculated using a statistic like χ2


but here we will work with the Freeman–Tukey discrepancy since it is weight independent


We assume ages between about 100 yr, for the most compact sources, and 105 yr for sources with LS of several kpc, as derived from radiative and kinematic ages of sources (e.g.


These values were computed by an analysis of the differences between the Portsmouth stellar masses of our galaxies


Previous studies have considered the implications of structure models on the true energetics and rates of GRBs


while the Σnl parameter encodes the smoothing of the BAO peak due to non-linear effects


Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions and micro- and nano-flares—all of these small-scale magnetic activities contribute greatly to coronal heating


In this case, the multiple bright blobs are plasmoids formed by bursty reconnection in this current sheet, another phenomenon commonly found in high-Lundquist-number reconnection simulations (e.g.,


Our estimate of the stellar mass fraction agrees


and with the estimates from strong lensing studies (see for example


which produced stellar mass fractions in the range 30%â70% integrated inside the Einstein radius of the lenses.


In particular, solar wind samples containing more Alfvénic fluctuations are typically associated with less developed turbulence, as inferred from both shallower spectra and reduced intermittency (see


Conversely, for LINERs, that are powered by RIAF discs, the relation between bolometric AGN and jet power is difficult to model because jet emission can dominate their entire SED


The foregrounds, system noise, and calibration errors together keep the current observations at bay from directly detecting the EoR 21-cm signal. As a consequence, the first detection is likely to be statistical in nature. These observations plan to measure the power spectrum (PS) of the EoR 21-cm signal (e.g.


Therefore, during our fitting procedure we use the frequencies determined in


as starting values plus their derived errors as Gaussian priors


Magnetic braking of the system is a possible explanation for the measured $\dot{P}$, but other explanations, such as resonant interactions between the binary and the possible circumbinary disc, have been proposed


while ‘achromatic’ flux variability (no colour evolution,


Even though arguments (e.g. variability,


exist that favour a compact corona, we used extended coronae.


To obtain the structural parameters of the LSBG candidates, the detected sources are usually fitted with a Sérsic model


are used to obtain accurate morphological and structural parameters. However, the computational cost of these is very high, becoming a bottleneck in LSBG analysis pipelines. For this reason, it is advisable to minimize the number of LSBG candidates prior to their Sérsic fitting to save computational time. This is not trivial because structural parameters from automated segmentation catalogs are much less accurate than Sérsic fit modeling, making correct screening of the sample challenging. As a last step, a “supervision” of all the objects matching the criteria of the sample is necessary in order to discard the frequent presence of false positives. These are sources that, although meeting the imposed criteria, are clearly not LSBGs. Examples of false positives are clumped sources that have been considered as a single source, faint reflections due to the optics of the instrumentation, or artifacts present in the images. Depending on the data volume analyzed, the number of objects to be supervised can become very high.


Other single-dish samples of SMGs have also been obtained at 1.1–1.3 mm using


A few years later the authors searched with a larger field systematically around many nebulae for extended emission features without detecting the very low surface brightness halo we investigate here


The model uses the hybrid approximation where electrons are considered as a massless, charge-neutralizing fluid and ions are described by a particle-in-cell model


It has been shown elsewhere that these models produce similar results to those of numerical cosmological simulations and other SAMs


and that they are also in agreement with higher redshift observations of galaxy populations


We also show the Spitzer Infrared Nearby Galaxy Sample


analyzed in da Cunha et al. (2008) as purple stars for comparison.


But why is there such a wide range of radial gradient slopes measured? There are several possibilities. (1) Measurement uncertainty. Measurement errors will cause some variations, but it is unlikely to produce a factor of 3 difference in slope. Homogeneity in observing procedures and data analysis may be more important given the variations in abundance that can be derived for the same source (for further discussion see


The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes


Following the results shown in Fig. 2 of


we roughly estimated that XO-2N could have ingested an amount of iron slightly higher than 5 M⊕ to increase its photospheric iron content by ~0.05 dex, given its Teff ~ 5300 K.


The Albedos, A1 and A2, and gravity darkening coefficients, g1 and g2, were set to generally adopted values for the given spectral types of the components


Marks etÂ al. (2014, in preparation) show that random pairing with subsequent dynamical processing does indeed reproduce at least the observed low-mass stellar population (see also


This initial binary population is then altered by dynamical evolution. Close binaries with orbital periods below about 10Â days undergo eigenevolution


and tend to equalize the companion masses. Note that this eigenevolution term alters the very-low-mass end of the star-like IMF. For the purpose of this work, however, these effects only play a negligible role.


Strong non-potential field arcades have been observed in


micro-sigmoids in soft X-ray imaging on scales of ∼50″


and now at EUV temperatures in QS-like mixed network fields with lengths down to ∼10″. This range of lengths over a range of temperatures and magnetic field topologies points directly to self-similar mechanisms influencing plasma and magnetic field dynamics at a range of scales.


A number of detailed studies suggest that the radio emission beam consists of a central core emission surrounded by conal emission arranged in nested rings


Surveys of radio bursts in decimetric wavelengths is presented in papers by Isliker & Benz (1994) and


within 1–3 GHz and 0.8–2.0 GHz frequency ranges, respectively.


FDs caused by high-speed streams (HSS) from coronal holes (CHs) have a recurrent character


Let us stress that implementing nulling in weak-lensing analysis is central in order to avoid extracting biased information from the small scales that lack a full theoretical understanding (including due to the effect of baryon physics that needs to be modelled in weak-lensing surveys


This magnetic structure would also be consistent with polarised radio synchrotron emission above and below the planes of galaxies known to host outflows in the nearby Universe, with the polarisation direction aligned with the orientation of the outflow cone (see, e.g.


Also, we consider $Q^{+}_{{\rm diss}}-Q^{-}_{{\rm rad}}=fQ^{+}_{{\rm diss}}$ in ADAFs (where f, the advection parameter, is defined by


The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g.


For more details, we refer the readers to


While we know that very massive stars (VMS) above 100  M⊙ exist


this mass is significantly diminished via stellar winds already during core hydrogen (H) burning


have found very high reddening and densities associated with ionised outflows in local objects


Perhaps a more likely mechanism is convective overshooting, which was first studied by Freytag et al. (1996) in a white dwarf context and more recently by Tremblay et al. (2015) and


High-mass star forming regions (HMSFRs) also present a rich chemical diversity. One of the best known examples is provided by Orion-KL. This source harbours: (i) a dichotomy between the spatial distribution of complex O-bearing and complex N-bearing species, with the latter species probing the hotter gas (see,


photometric follow-up started in August, 2010, and ended in October, 2012, coinciding with these LBT data.


The discrepancy is even larger in the case of the low-mass models of


After combining with the existing NB2071 data (186 min integration), we reconstructed all the data using the reduction pipeline mcsred2


Using the diagonal elements of the 14N quadrupole coupling tensor in NEFA


we have computed the expected hyperfine splitting of all lines in the W band.


From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc


Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars


These galaxies hereafter referred to as LyC leakers, possess many properties similar to those of high-redshift galaxies both at z ∼ 2–3 and z$\gtrsim$ 6 such as compact morphology with similar galaxy radii (e.g.


Later on, Gomes et al. (2005), Gallardo et al. (2012), and


showed that the Lidov–Kozai mechanism raised by the giantplanets inside a mean-motion resonance with Neptune is able to raise the perihelion of small bodies beyond 60 au in a few thousands of million years.


Since these characteristics are somewhat consistent with model predictions for drift mode of MTSI


, we do not rule out the possibility of some waves at certain frequencies and during some intervals being generated by the slow drift mode of MTSI.


We used data for two clusters observed by Kaluzny and his collaborators with the highest number of CBs (except for ω Centauri).


detected nine CBs with one BS among them


show a gap at around 36 au, with an outer ring at a separation >40 au from the star.


In this concern, a large family of dynamical DE models with time-varying EoS parameters has been proposed in the literature (for some earlier attemts, see


However, there is an important caveat; PAHs are destroyed by ionizing radiation from newly formed stars


leading to a deficit in the 8 μm luminosity in galaxies with low metallicity, whereas PAHs are less well shielded by metals


Extreme mass ratio systems are prone to unstable mass transfer and thus to CEE, and although the exact value of the boundary is not well-constrained, we assume that this occurs for evolved donors in systems with q ≲ 0.4, following previous works such as Wellstein et al. (2001), Hurley et al. (2002) and


In Fig. 5 we compare the distributions of the core radii (Rcore) constrained by the V06 model and the concentration parameter (cSB) between these two samples.


The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500


Intuitively, the expectation is that the smaller the core radius, the more compact the cluster.


The left panel of Fig. 5 clearly shows that the clusters in the point source sample have relatively smaller core radii, hence the emission is more concentrated in a smaller area. Consistently, the concentration of the point source sample shows a clear excess in higher values than the extent-selected sample, indicating that a significantly larger fraction of cool-core clusters and clusters host a central AGN.


assuming a mean beam efficiency ηMB = 0.49


In space, an analogous process to carbon soot formation occurring on Earth can be initiated through the completion of that first aromatic ring and may also lead to the synthesis of PAHs


This has led to significant theoretical development, focused on the resonant interaction of electrons with the whistler and fast-magnetosonic whistler (FM/W) modes (e.g.


Observations have struggled to confirm these theories.


Moreover, the degree of central concentration of a halo depends on its formation epoch and hence on its total mass (e.g.,


This is consistent with the magnetic field measured by Hubrig et al. (2009), 89 ± 26 G, although non detections have also been reported


In our long-term project aimed at reconstructing the past magnetic activity on the Sun


we also use indirect measurements of magnetic fields obtained, in particular, from chromospheric spectroheliograms.


, the maximum of the field strength was found to be 0.15 T. The magnetic field could be even stronger in the active region near the sunspot. Therefore, we set b0 = 0.05 T in Case I and Case II, and b0 = 0.15 T in Case IIa.


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


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


Moreover, it is observed that this relationship does not apply to radio-loud magnetars, which in general show larger duty cycles than what one would expect from the extrapolation of this tentative relation for radio pulsars to magnetars (see, e.g.,


To allow fast calculations, we make the major assumption that the grains are spherical and compute their optical properties using the Mie theory


with the Fortran 90 version of the BHMIE routine given in


The oxygen line ratio [O III]λ 5007 Å/[O II] λλ3726, 3728 Å (O32) proposed by Jaskot & Oey (2013) and


was successfully used to select LyC-leaking candidates


From the theoretical point of view, it is believed that low-mass main-sequence stars synthesize 3He through the p–p chains with peak abundances of few 10−3 by number


We note that the measured values must be corrected for instrumental effects, in particular for the signal convolution with the instrumental PSF, which can introduce significant cancellation of the disk signal


first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙.


It was only in 1928 that Baade first classified it as a GC owing to its high latitude, richness in faint stars and presence of variable stars


First, ultra-hot Jupiters are accessible objects to observe. Their short orbital periods (1–2 d) and hot, extended atmospheres make them perfect targets for transmission spectroscopy


Based on a radial velocity of $-13\pm 17\, {\rm km^{\rm -1}}$ and a distance of 2.07 ± 0.18 kpc


, we can calculate the UVW velocities of the SM star, i. e. $U=-5.2\pm 14\, {\rm km^{\rm -1}}$, $V=197\pm 10\, {\rm km^{\rm -1}}$, and $W=3.1\pm 5\, {\rm km^{\rm -1}}$.


From the application of Comptonization models, such high-energy data allow to constrain the plasma temperature, which is commonly found to range from 50 to 100 keV


Each of the new detrended light curves, jointly with the nominal PDC-SAP flux, is then processed through the transit least squares (TLS) package


In contrast to the classical box least-squares (BLS) algorithm


the TLS algorithm uses an analytical transit model that takes the stellar parameters into account.


For the case of β Pictoris and HD 169142, also having giant planets at long distances, CA models seem to be favored


The exact value of the interferometer’s modulation efficiency (ME), which acts essentially as an additional throughput loss, is the major source of uncertainty on the absolute flux calibration


We also show as a gray band the best fit for the stellar fraction in the form of stars determined by


in a study of a large sample of lens galaxies using strong lensing and photometry,


In the past decade, owing to the rise of large spectroscopic surveys of galaxies with well-determined physical properties (e.g. SDSS), all sky UV surveys (e.g. GALEX), and improved sensitivity of UV spectrographs (e.g. COS), studies of the gaseous haloes of galaxies could systematically connect gas absorption properties to galaxy properties in statistically meaningful samples (e.g.


the number of known SMGs is now of the order of a few thousand (e.g.,


and intensive observational efforts have been devoted to understanding their physical properties.


Dissipative effects such as shear and bulk viscosities work towards suppressing GR driven instabilities and has been studied by various authors over the past few years


We recall that in these models (see also


the dense clouds can be either self-gravitating virialised clouds, which implies that their internal velocity dispersion (Δvsg) is locked to their mass (Mvir) and size (R) through Δvsg = (GMvir/G)1/2, or unbound clouds, for which Δv ≫ Δvsg.


We approximate the PSR body as a perfect sphere. However, due to the spin of the PSR the true shape is more oblate. This will ultimately influence the pitch angle of the ray with the neutron star surface. This effect is considered to be minor, but the method could easily be extended to account for this oblateness (see


of the sample of bayerite prepared at 1273 K suggests only θ-alumina was present, and their infrared and NMR spectroscopy confirms this.


From the convective flux as presented in


one also would expect a similar temperature gradient in the overshooting zone.


Of course, the recent report of an absorption signal in the sky-averaged spectrum at z ∼ 17 from EDGES (Bowman et al. 2018)


than models in ΛCDM cosmologies generally predict.


Subsequent observations have led to the detection of new metastable ammonia masers, including


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


with the theoretical expectation that the IMF should vary as the star-forming environment alters


the observed IMFs of star clusters in the local Universe are consistent with no variation


In this case, the mass of the white dwarf is also calculated from the IMFR of


computed mode line profiles in both the velocity and the intensity power spectrum alternatively at mean unity optical depth and instantaneous unity optical depth. Their results indeed show that the modulation of the “observed” intensity fluctuations due to radiative transfer could be significant enough to reverse the sense of mode asymmetry.


For the lowest 41 energy levels, we see that our calculated energies and previous fac energies


belonging to the n = 3 complex in Ni xiv agree well with each other and both set of calculation are of the same accuracy.


However, our calculated ground state configuration levels show better agreement with measured energies in comparison to those of fac calculations (7.2 per cent).


As predicted by asymptotic theory, the pulsation periods for γ Dor and SPB stars were observed to form period spacing patterns (e.g.


On the other hand, the stellar rotation leads to shifts in the observed pulsation mode frequencies


Indeed, the ultraviolet and X-ray variability detected for many of these LINERs


is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM).


This is consistent with the fact that most of the [O III] morphologies found for LINERs are spheroids, if we assume that the [O III] traces the NLR.


These objects spend most of their time in quiescence at very low accretion rates, but occasionally, they produce outbursts that last from a few months to a year. Their flux then rises by several orders of magnitude across the whole electromagnetic spectrum (see, e.g.,


WDS 02499+0856 turned out to be a quadruple system, when the northern component was found to be a double-lined (SB2) binary from the DDO spectroscopic observations


Typically about a dozen events occur during each solar cycle, although only two GLEs were reported in cycle 24, probably due to the change in the state of the heliosphere


SEP events with gigaelectronvolt components are accompanied by type II radio bursts from meter (m) wavelengths to kilometer (km) wavelengths


Many important results were noticed based on the spectral fitting of RXTE data of this source. The mass accretion rate was found to be constant along with the Z phase in Sco-like variation and different mechanisms were proposed to explain the spectral and timing variations during the Z phase variations


he RWI can be triggered at steep radial density gradients


such a gradient may be generated at the viscosity transition between regions in which the magnetorotational instability can operate (e.g.


the four candidate HVSs from the LAMOST survey


Numerous studies have been performed using chemical models


For comet 8P/Tuttle, it is however not possible to distinguish the solution of a binary nucleus that formed in the first billion years of our Solar System


from a more recent origin following its injection into the inner Solar System (e.g.,


Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 ± 1.7 K, which is consistent with the mean value of 11 ± 1 K found by


This seems to suggest that its presence closely traces star formation sites, resulting in a linear relation, as found by De Looze et al. (2014) and Herrera-Camus et al. (2015). While at low-redshift and close to solar metallicity such a relation is well established, as shown by several observations


and also numerical simulations (see, e.g.


significant deviations can arise in different ISM conditions, like at lower metallicity or in presence of a strong ionizations field, that are more typically found in the high-redshift Universe.


Improvements in cosmological measurement in recent years have been said to hail an era of “precision cosmology,” with observations of


luminosity distance–redshift relation of Type Ia supernovae (SNIa;


providing constraints on cosmological model parameters at percent, or subpercent, level precision.


Possible compact-object merger pathways include isolated binary evolution


These parameters are entirely consistent with those found in preliminary studies


Here, we present a new approach to derive the VDF based on the lens redshift distribution


and to constrain its evolution out to z ∼ 1, given its strong dependency on the dynamical properties of galaxies (i.e. stellar velocity dispersion) and the number density of gravitational lenses (i.e. galaxy evolution).


Beyond this redshift, matters are complicated by uncertainties about the density evolution and the build-up of high black hole masses in the early universe


These conclusions have been strengthened by recent observations by Siana et al. (2015), who found no convincing detection in their deep HST imaging with WFC3-UVIS of five LyC emitters extracted from the sample of Nestor et al. (2011), or by Mostardi et al. (2015), who only found one robust LyC emitter after a reanalysis of a sample of 16 galaxies by


reported that there is no correlation between the turbulent and outflow energies.


Robust lens models of galaxy clusters are built thanks to the identification of large numbers of multiply lensed sources, which can span a large redshift range


The existence of a shock is also indicated by orbital-phase- and frequency-dependent radio eclipses of the MSP (since plasma structures at the shock attenuates the radio), where in RBs the eclipse fraction can be >50% (e.g.


of the orbital phase (while the MSP remains largely uneclipsed at inferior conjunction of the pulsar).


M15 show, via use of covariance spectra (see


for a review of the technique), that the ULX continuum emission originates from at least two components that cross at ∼1 keV.


Recent observations during the STEREO era, however, question this simple picture, especially since the nature of events showing wide longitudinal SEP spreads appears to be more complicated. It was found that 3He-rich events extend over more than 130° in longitude


and that near-relativistic electron events can spread up to almost all around the Sun.


For these reasons, detections in emission at high-redshifts are currently limited to deep fields


while detections at z1 are now becoming available


Many studies of the outburst evolution of these sources have been reported in the literature (e.g.


the various outbursts observed do not have any detectable recurrence period and, in addition, show a complex behaviour in both soft and hard energy ranges and very different luminosities.


The angular expansion rate of 0.64 arcsec yr−1 obtained from comparing X-ray images from 2007 and 2009


gives an upper limit for the age of about 160 yr, less if (as is almost certainly the case) deceleration has occurred;


This boils down to quantifying the relation between molecular gas and star formation rate (SFR), which appears nearly linear in nearby discs


In precision cosmology, Bayesian inference is the main tool for setting constraints on cosmological parameters


Both the correlation of VHE emission with the CMZ and the lack of a cutoff in the diffuse spectrum support a hadronic scenario, capable of explaining both VER J1745–290 and the diffuse emission


The three transitions of singly ionized Sulfur (Sii; upper ionization potential 23.3 eV) at λλ1250.58, 1253.81, 1259.52Å represent important tracers for neutral and weakly ionized gas in the local interstellar and intergalactic medium and in distant galaxies (e.g.


In addition, the apparent speed and length of these network jets are positively correlated, which is very similar to what has already been reported in previous works


with the sole exception of cluster ESO121-3 and very recently also KMHK1592, as reported by


Later, indirect evidence of the existence of intracluster magnetic fields has been given by several statistical studies on the effect of the Faraday rotation on the radio signal from background galaxies or galaxies embedded in galaxy clusters


The nonlinear PT for MG was developed initially in


and has been further studied in several other works


Observations on smaller, sub galactic scales, have proven more problematic for ΛCDM, with suggestions that the low abundance (e.g.


inferred for haloes hosting Milky Way satellites are inconsistent with the numerous substructures with cuspy density profiles that form in Milky Way-like CDM haloes.


EoSs were constructed using the Skyrme effective nuclear forces Ska and SLy4, respectively.


The collision effect can become important in the case of higher density medium where the collision rate $\tau _c^{-1}$ (either inelastic collision rate or Van der Waals collision rate) dominates over optical pumping rate $B_{lu}\bar{J}^0_0$ (see


First, thermodynamic calculations of conditions in photodissociation regions (PDRs) have been coupled with self-consistent equations for the thermally driven disc wind


The confirmation of their cosmological origin allows them to be widely proposed as promising tools for studying the universe and fundamental physics, e.g., the distribution of baryons in the intergalactic medium (IGM) or diffuse gas


As a result, magnetars have been suggested as the central engines for some GRBs, including both long and short events


This problem might be alleviated in future simulations by introducing more realistic top boundary conditions like that used in


These vortices tend to have a long lifetime and are widely observed in space, laboratory, and numerical simulation of plasma


It was argued that magnetic flux ropes in the solar wind can be viewed to first order as being quasi-two-dimensional (quasi-2D) helical contracting and merging flux-rope structures based on three-dimensional (3D) simulations of compressible MHD turbulence that included a strong guide magnetic field


Following the approach of Nguyen et al. (2010), we have inferred a GCE relationship between δ29Si and initial 18O/16O, which is based on a tight correlation between 29Si/28Si and 46Ti/48Ti ratios in SiC mainstream grains (Figure 11, left; data from


Such non-evolving VDF has been extensively applied in the previous studies on lensing statistics


n these regions, CRs have a wide variety of effects, one of the most important is being a producer of atomic hydrogen through the dissociation of H2


Secondly, the total metal flux into the disc across the outer boundary cannot exceed that supplied by advection of gas with metallicity $\mathcal {Z}_{\rm CGM}$ into the disc, since otherwise this would imply the presence of a metal reservoir external to the disc that is supplying metals to it, which is true only in special circumstances, e.g. during or after a merger


(and, by extension, the z ∼ 3 semi-constraints) assume a gas-to-dust ratio (G/D).


We recall a few salient features obtained in those papers and reproduced here: in the initial stages (two leftmost panels), the rising portion of the flux tube has a mushroom shape, akin to an air bubble rising in water (e.g.,


We speculate that some stars of the Hyades stream might be remnants of the Hyades cluster, while others may be the dynamical effect of non-axisymmetric components


The RVs were measured using the two-dimensional cross-correlation algorithm TODCOR


The captured material can form a quasi-spherical shell


The standard internal shock model of blazars considers that the discrete ejecta with higher speeds (with Lorentz factor Γf) catch up with the preceding slower ejecta (with Lorentz factor Γs), and the collision leads to the nonthermal emission (e.g.,


Indeed, some misaligned circumbinary discs have already been reported


The two panels show model spectra at times t = 0, 1, 3, 5, and 7âMyr after a coeval burst of star formation, using evolutionary tracks with rotation, at solar metallicity (Z = 0.014 from


a number of dedicated facilities have been conducted to search FRBs, such as


and the Five-hundred-meter Aperture Spherical radio Telescope (FAST;


All these efforts result in an increasing rate of new FRB detections. Among them, more than 20 repeating FRBs have been reported.


If Tr 24 is also slightly younger than NGC 6231, as we argue below, our M-stars in Tr 24 will reach down to lower masses than in NGC 6231, with a steep increase in the detected M-star population: adopting the IMF from


the predicted number of cluster M stars doubles considering the mass interval 0.25–0.5 M⊙ rather than 0.35–0.5 M⊙.


The second scenario involves mass transfer episodes and the evolution of the binary is obtained following the prescriptions of the bse package


following the parameter assumptions detailed in Camacho et al. (2014).


The covariance of the 3PCF, on the other hand, is not diagonal, even for Gaussian fluctuations, which makes the modelling more difficult


In the last 20 years, disc-oscillation and resonance models and wave models have been proposed (e.g.


Temporal variability studies during the 2012 September–October multi-band flaring period found a near-simultaneous γ-ray and optical flaring behavior, inferring a co-spatial origin


this interval is characterized by two different spectral scalings: a typical inertial range ∼ τ5/3 is found at large scales (i.e., τ > τb), while a steeper scaling ∼ τ7/3 is found at small scales (i.e., τ τb), with τb ∼ 2.4 s


For a galaxy of halo mass Mh, the relation between the halo mass and the velocity dispersion is simply Mh = 2σ2R/G; while the velocity dispersion can be directly related to the black hole mass using the MBH–σ relation


The most basic result, already mentioned in Sect. 4.4.1, is that initial conditions which have a finite nonzero flux integral (called ‘the mass’ in the mathematical literature for the PME) converge toward the ZKBP solution with the same flux integral (‘mass’) asymptotically in time


Theorem 18.2); here, allowance is made for either a positive or negative flux integral by globally changing the sign of the ZKBP solution


However, systems in a state of high mass accretion often do not show an optically thick soft X-ray component; instead, many exhibit optically thin hard X-ray emission


with an X-ray luminosity much smaller than expected, i.e., much smaller than the disk luminosity.


A significant contribution to the stack SED comes from a few sources, the most important one is RMC143. This was already identified as a massive nebula


Signatures of past mergers take the form of faint extended tidal features such as tails (e.g.


– which are typically produced by major mergers


Several studies of lower-luminosity AGN host morphologies with inactive control samples have been conducted in HST extragalactic survey fields (e.g.,


[C ii] 158-μm luminosity, L[C II], has been discussed as an indicator of SFR (e.g.


One important thing to note, that is particularly relevant here, is that most of those coherent emitters for which we know the properties of the radio spectrum have quite steep spectra, typically going as ν−2 or even ν−3 (see e.g.


, in contrast with a typical ν−0.8 for optically thin synchrotron emission. This means that low-frequency instruments such as LOFAR may be intrinsically at an advantage to find coherent emitters (in addition to having larger fields of view).


the farthest blazar detected so far is at z = 5.47,


From 2008–2009 INTEGRAL data, Beckmann & Do Cao (2010) report a cut-off of ∼80 keV with a hard photon index, but these results are not confirmed by NuSTAR


Studies of orbit composition of B/PS bulges and X-structures in different numerical and analytical models


showed that an X-shape is observed in these models due to a tendency of a star to spend more time near turning points of its trajectory.


This is indeed the case for the realistic bar potential


In contrast to the Lempo system, all other known triples in the Solar system have their orbits almost regularly spaced, with one component much smaller than the others, with the most distant component being the largest


With the goal of identifying new exotic pulsar systems or highly stable MSPs suitable for PTA studies, the SPAN512 pulsar survey


was conducted between 2012 and 2018 at the NRT.


CS approaches based on constrained optimization problems, solved via convex optimization techniques, have been applied broadly in RI imaging


These techniques have shown promising results, with improvements in terms of image fidelity and flexibility compared to traditional approaches such as clean-based methods and MEM.


This approximation works well, even for evolved density fields, while deviations from Gaussianity can also be taken into account


and possible alternative explanations of the changing-look behaviour are


transient events, e.g. tidal disruption of a star by the central black hole (e.g.


Stripping and star formation consume the available gas and galaxies first appear as truncated disks


Optical ionised gas has been observed by


next to the black hole in a field of view1 of 5′′ × 3.5′′, but this emission is weak.


Initially the core size of a galaxy was determined by fitting the so-called ‘Nuker-profile’


to the surface brightness profile, a method that however depends sensitively on the radial fitting range and yields unreliable results when fit to surface brightness profiles with a large radial extent (e.g.


In these radiative envelopes, the transport of chemical elements on a macroscopic scale is ascribed to


The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.


More recently, the emission-line OMEGA-OSIRIS survey provided similar results


Many simulations consider either an intermediate-mass BH (e.g.


Accordingly, it is informative to investigate the shape of the probability distribution of the matter density field and its evolution


However, it is worth noting that the gA-values obtained by the latter authors were deduced from the combination of branching ratio measurements with available experimental lifetimes for the 3d74p z5F, z5D, z5G levels


but also with estimated lifetimes for the z3G, z3F and z3D levels from the measurement of total intensity of all lines of each of these levels under the assumption of almost equal population.


In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,


The reason that high-velocity features are interesting to investigate in connection with blueshifted Na i D features is that there are suggestions that the high-velocity Ca ii features may be at least partially due to ejecta–CSM interaction (e.g.


Therefore, if a link between these quantities was identified, it would provide evidence that blueshifted Na i D features are due to CSM also rather than contamination.


CMEs have been observed to occur often having spatial and temporal relation with solar flares, eruptive prominences


In order to produce a steep gravitational potential at low |z|, there could be a breathing mode in the stellar disk


which is currently in its most compressed state.


Indeed, other studies confirm that abiotic buildup of ozone is possible (e.g.,


The input of dust from the inner disc triggers a streaming instability in the outer disc


lasting ≈0.1 Myr and concentrating pebbles and fractals sticking to pebbles into filaments where the comet nucleus collapses by gravity at speeds 1 m s−1 into a randomly packed


aggregate of cm-sized pebbles, with the fractals stored in the voids among the pebbles


In addition to morphological disturbances, galaxy mergers can trigger vigorous galactic outflows associated with feedback from the enhanced star formation (e.g.


Similar conclusions can be reached for the


sample where they adopt the same analysis as in Nestor et al. (2013).


For example, star count observations in the solar neighbourhood


followed by its characterization as the old α-enhanced population in the double sequence exhibited by the solar neighbourhood stars in the [α/Fe] versus [Fe/H] plane


Following Paper I, we have also adopted a 0.2 dex difference in metallicity between G2 and G1, and assumed 12 and 10 Gyrs for the ages of G1 and G2, respectively, with the same population ratio for the two RCs


Each deformable mirror uses 672 actuators that routinely correct 400 modes and provide Strehl ratios exceeding 80%, 95%, and 99% at 1.6âÎ¼m, 3.8âÎ¼m, and 10âÎ¼m, respectively


S19 hereafter), we used a complementary approach and looked for evidence of the lack of star formation as seen in the sub-millimetre regime to confirm the passive classification of the high-z candidates selected in GOODS-S.


At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity


This matter replenishment may be channeled from within the cloud itself through molecular filaments


Dry minor or intermediate mergers contribute little to the mass growth but promote substantial size growth (the accreted stars tend to be deposited mostly in the external regions), making spheroidal galaxies less compact and likely also less concentrated


Theoretical models have found that CO should be the dominant carbon-bearing molecule for hydrogen-dominated atmospheres above 1000 K


and CO has been detected at high resolution in hot Jupiter atmospheres (e.g.


In addition, technical development offers a new and barely explored perspective: a panchromatic, more detailed view of the universe through the use of narrowband filter systems, such as those from the J-PLUS and J-PAS surveys


The discovery of snail shells in the phase-space distribution of MW disk stars


has inspired debates about their origin:


Another model for their formation is by increasing their spin rates due to incident and remitted solar photons, known as the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. The YORP effect on contact binary asteroids has been studied


A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations


has become an effective standard ruler, which have been extensively applied to test cosmological models


In the last decades, KAWs have received considerable attention due to their possible role in a normal mode description of turbulence. Indeed, theoretical studies (e.g.,


have shown that the turbulent cascade in magnetized plasma tends to develop mainly in directions perpendicular to B0.


The linear stability analysis of these idealized configurations


as well as the corresponding non-linear solutions (e.g.


These properties can also be explained by the locations of resonances


Varying star densities can affect the results (e.g.


In this section we therefore explore the sensitivity of the shear measurement bias to various assumptions and simplifications made in the simulations.


Most DSFGs are discovered in wide-area observations using single-dish far-IR (FIR)/millimeter instruments such as


In addition, we also included fgas estimates derived from the (median) stacked FIR spectral energy distributions of ETGs at


z ∼ 1.2, z ∼ 0.8, and z ∼ 0.5 (1394, 1536, and 563 galaxies, respectively;


Increasing numbers of LAEs are being observed by surveys including narrow-band imaging (e.g.,


Recent work also finds that transient spiral structure


may lead to the formation of moving groups, as well as perturbations due to spiral arms in the MW


As a consequence, only large or massive planets are detected around the classical evolved stars


The atmosphere above the Canary Islands, and especially the western islands Tenerife and La Palma, has been extensively characterized over the past 50 yr


(54 509) was the first asteroid for which the effect of YORP has been observed


There is indeed evidence for a potentially large population of heavily obscured, possibly Compton-thick AGN, among the WISE population (e.g.


Alternatively, the jet could be (ii) structured, with a fast and energetic inner core surrounded by a slower, less energetic layer/sheath/cocoon (first proposed for long GRBs


In particular, there are two intermittent quasi-periodicities for both NGC 5408 X-1 and M81 X-6, suggesting that the quasi-periods are changing or evolving. They resemble some Galactic X-ray binaries that show similar behaviour (e.g. Cyg X–2 and SMC X–1;


These characteristics resemble closest the behavior often observed in (luminous) red novae


a modern category of eruptive stars known from our and other galaxies (e.g.


chose the propagating direction averaged over the whole CME derived by the polarization ratio technique to correct the radial speed in the 2D maps, but the key information along the LOS is still lacking.


Some recent investigations showed that the mass-transfer process in the lobe-filling BH binaries is more stable than previously expected (e.g.,


; the maximal mass ratio of the donor star to the BH for stable mass transfer can reach as high as ∼6. Hence only a few BH–He XRBs with orbital periods of ≲1 day are produced in our calculations.


However, their emissivities can be computed based on specific energy absorbed in each grid cell and assuming that the emissivity is the function of the mean intensity of the radiation field, which approximates the spectral shape to the first order


In this context we promoted the ESO-VLT Multi-Instrument Kinematic Survey (hereafter the MIKiS survey;


a project specifically designed to characterize the kinematical properties of a sample of GGCs in different dynamical evolutionary stages from the radial velocities (RVs) of hundreds of individual stars distributed over the entire radial range of each stellar system.


observed a clear trend that AGNs, including the Seyfert composite galaxy NGC 1068, tend to show higher HCN/HCO+ and/or HCN/CS than in SB galaxies as long as the observations were at high enough spatial resolutions to separate energetically discrete regions.


The luminosity in these FIR lines generally exhibits a deficit in the most FIR luminous galaxies compared to the trend expected from lower luminosity galaxies (e.g.


The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500


Note that there is some degeneracy between broken power-law break frequency


and extinction, which could lead to inference of grey dust for some instances


The reason is probably that the asteroids classified by Bus & Binzel (2002) as members of this taxonomic class include objects that belong to the old F-class, originally proposed by


and included in the Tholen taxonomy, due to its flat spectrum and low albedo;


Although it appears that small-scale flux ropes tend to contract or merge predominantly incompressibly in discussions of particle simulations (e.g.,


In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,


However, the measured solar disk emission flux was about a factor of seven higher than that predicted about this disk component by a “nominal” model


In the past, the limited observations showed that precursor activities of solar eruptions can come in various forms,


as well as nonthermal processes in microwave or hard X-ray wavelength


Moreover, these disc-sources are confirmed to be binaries and show orbital periods between 100 and 2000 d


The literature on indirect evidence of the presence of planets is now becoming very rich, and nearby young stars surrounded by gas-rich disks are intensively studied for this purpose. In most cases, available data cannot fully eliminate alternative hypotheses, or the data have ambiguous interpretations (see, e.g.,


The hole-like structure may result from the expansion of a large-scale supershell produced by a supernova in the Per OB2 association that compresses the Taurus cloud from the far side


The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLGC; or one of its variants; see, e.g.,


The majority of extremely metal-poor stars shows overabundances of carbon, [C/Fe] > 0.7, and it appears that carbon-enhanced metal-poor (CEMP) stars split into two groups, with dramatically different carbon abundances (see, e.g.,


Based on this behaviour, it becomes possible to form hot Jupiters on retrograde orbits by combining the eccentric ZLK effect and tidal friction


Those blended emission lines can be easily detected at the position of the flare ribbon, including known and unknown emission lines, such as the C i line at 1354.29 Å, the Fe ii lines at 1353.02 Å, 1354.01 Å, and 1354.75 Å, the Si ii lines at 1352.64 Å and 1353.72 Å, and the unidentified lines at 1353.32 Å and 1353.39 Å (e.g.,


The timing of the coronal-hole-originated solar wind observation aligned well with the PSP orbit. PSP started passing through the leading edge of the high-speed stream, continued as the high-speed stream corotates over the spacecraft, and ended passing the trailing edge of the stream as seen in Figure 3, standing as a perfect classic CIR/SIR event


Furthermore, in galactic nuclei with a high X-ray flux we would expect to see an increase in the dust temperature and infrared luminosity


Therefore in galactic nuclei, and in particular in AGNs, we expect a reduction in [C ii] emission relative to FIR/IR emission depending on the relative contribution of different ISM components to the [C ii] luminosity.


The conversion factor depends on the physical conditions of the gas in the ISM (temperature, surface density, dynamics, and metallicity), as well as the star formation and associated feedback


For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions


These explanations can be very roughly divided into two main categories:


and mergers due to dynamical interactions (e.g.,


Adam optimization, compared to other gradient-based optimization, is very suitable for noisy and sparse gradients, and for simulated data that show very large scatter with respect to a given quantity of parameter


The Rayleigh–Jeans dust continuum emission has been used to estimate dust and gas masses, assuming an average emissivity and dust temperature for the dominant cold dust component and a constant dust-to-gas ratio


In the regime of stability, the normal modes are undamped oscillation modes in absence of lateral streaming


If the particle is too small to be detected by the GDS system, it may be detected by the IS sensor only (IS particles): in this case the particle momentum is converted to the mass assuming the mean value of the velocities of the GDS+IS particles in the same momentum bin, or assuming the velocities predicted by tail models


as well as the power spectrum of H i distribution in nearby galaxies


These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in the power spectrum estimates.


Observational calibrations of the virial factor also tend to support this conclusion (e.g.,


according to diffusive shock acceleration (DSA; e.g.,


The radial variation of the stellar surface density of the high $\mathrm{[ \alpha \mathrm{/Fe]}}$ mono-age populations is found to have insignificant breaks, and they are better fit by a single exponential in this disc region. As these populations are the oldest, this may be a sign of the disc evolution washing out the density peak over time, or may point to a different formation scenario for high $\mathrm{[ \alpha \mathrm{/Fe]}}$ stars, where no density peak ever existed. These findings are in good agreement with earlier studies of MAPs


The origin of this large scatter is usually explained as a combination of the time variability of the SFR during the course of cloud evolution and intrinsic scatter of SFEs due to the diversity of GMC properties


To estimate the positions of the snow lines in observed disks, the temperature profile is often assumed to be a simple power law


which is broken if the disk has shadows on the disk surface


The last column in Table 1 reports the number of OB stars minus the “diffuse” population estimated from their density in the Reference field (22.5 stars per square degree): as is immediately seen, the M-star statistics is much larger than the OB star statistics. This can hardly be considered surprising, if an ordinary IMF (e.g., that from


is assumed for the star-formation region.


The spectrum of He seems harder than that of H as indicated by many spectral studies, implying, e.g. time-dependent particle acceleration


or more efficient He injection in the shock acceleration process


The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of


This observed behaviour of [C/O] is in contrast to the steady increase of [C/O] up to [Fe/H] ~ 0.3 dex found, for example, by Franchini et al. (2021).


In the simulations, hydrodynamics and neutrino transfer in general relativity are solved simultaneously


Alone, the energy released by jetted outflows appears to be on the same order as the energy needed to offset cooling (e.g.


therefore suggesting that AGN feedback is a good candidate for solving the cooling flow problem.


or through dynamical feedback driven by starbursts or active galactic nuclei


For example, GRBs that are highly offset from their hosts may have afterglows with much lower luminosities, making precise localization (and therefore host identification) difficult


The starting point is the “hybrid Vlasov–Maxwell” (HVM) code


which is already equipped with a fluid model in which electrons are described as an isotropic, isothermal fluid with finite inertia. The HVM code has recently been upgraded in order to implement a more sophisticated model for the electron fluid. This includes evolution equations for the anisotropic (gyrotropic) electron pressures, p∥, e and p⊥, e (where ∥ and ⊥ refer to the local magnetic-field direction, b = B/|B|), and a Landau-fluid (LF) closure for the parallel transport of the gyrotropic electron thermal energy along field lines (i.e., parallel heat fluxes, q∥, e and q⊥, e).


We showed that molecular gas is falling in and slowly rotating with sub-Keplerian velocities down to radii of 500 au from the central star, where we measured a mass infall rate of 6 × 10−4 M⊙ yr−1


while short GRBs are consistent with null or negligible intrinsic spectral lag and are therefore an ideal tool to measure the LIV effect


Similarly, stronger-than-expected 21-cm signals can arise if the cosmic radio background has contributions other than the CMB


The existence of MPs in Pal 13 supports the statement that this phenomenon is not unique in Galactic GCs formed in situ (e.g.,


More generally, in the case of strong shocks, the velocity u is identified as the velocity of the shock, as it is precisely the velocity jump at the shock discontinuity which drives the acceleration of the particles via the DSA mechanism (e.g.


After convolving our models with a 10″ FWHM Gaussian kernel to simulate the data analysis presented in Lefèvre et al. (2014) and following the


prescription to take into account the part of the ISRF+CM light that can be transmitted through the cloud3, we compute the synthetic photometry for each pixel along a radial cut through our model clouds. The results are shown in Figs. 10a and b, which present the coreshine ratio as a function of the 3.6 μm intensity for the 21 starless cores of Lefèvre et al. (2014) and in Fig. 10c and d, which displays the near- to mid-IR ratio as a function of the coreshine ratio for the Taurus-Perseus and L183/L134 regions.


Inspired by the new observations of this GW event at 3.3 yr after the initial merger


in this paper, we extend the synchrotron model presented in Fraija et al. (2021a), including the continuous energy injection from the central engine (either a spinning magnetized NS or BH remnant) into the blast wave through a numerical approach and analytic arguments.


We primarily used the OGLE catalogues for RR Lyrae stars


These cross-matches returned a list of 88 578 known RR Lyrae stars in our sample of 140 784 stars.


This up-gradient transport into the jet can result from Rossby waves, coupled Rossby–Kelvin waves, mixed Rossby–gravity waves, wave–jet resonance, barotropic instability, or baroclinic instability


This property enables the creation of steep phase ramps that efficiently diffract light into a single order without scattering


The problem of the balance between driving and decay for magnetized turbulence is most acute in molecular clouds. Since these have linewidths indicating the presence of supersonic flow, the fast dissipation of turbulence found by these simulations necessitates a mechanism to reinject the energy equally quickly. A number of candidates have been proposed, including


Despite this only six radio pulsars have been discovered within half a degree of Sgr A*


For MR Del, we revised the absolute parameters using its full light curve and the published radial velocities, which are similar to those published previously


Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature


which was suggested as an absorption feature of XCN ice.


, the Poisson noise is 200 e− for a typical detector with a gain of a few e− ADU−1 and the flat illumination level is of 20 000 ADU pixel−1 = 40 000 e− pixel−1. Thus, a typical photometric aperture with a radius of 3 pixels contributes ∼1 mmag photon noise.


This complex environment is multiphase and has been observed in numerous surveys


Hence, to reduce the number of 24 free parameters and the values they can take, we use prior knowledge about the pulsation spectrum of the star that was acquired during


For a collision at a velocity ∼108 cm s−1, which is a typical velocity scale for young SNR shocks, the cross-section is ∼10−13 cm2, giving a reaction rate ∼10−5 cm3 s−1 (e.g.


Thus, if the density is ∼106 cm−3, the collisional depopulation becomes important.


In OMC-1, the low- and high-velocity outflows from BN/KL plunge into the ambient molecular cloud


producing hot (from Tk ≃ 200–2000 K) and dense (up to n(H2) ≃ 106–107 cm−3) post-shocked gas in H2 Peaks 1 and 2


Theoretical work suggests major mergers can provide the torque to displace such an overwhelming fraction of the angular momentum of the gas, allowing for the highest accretion rates on to the central black hole whilst transforming the galaxy morphology


As already noted, the companions are generally significantly fainter than the exploding star, although this is frequently not the case for stripped SN progenitors – for Type Ibc SNe, it should not be surprising to find that the binary companion is more visually luminous than the SN progenitor. This point is of considerable importance for the one candidate Type Ib progenitor iPTF13bvn


In order to estimate a temperature for the dust, we have fitted a modified blackbody to the available photometry at wavelengths longer than 10 µm (AKARI, WISE, IRAS, Herschel)3 and the new ALMA photometry using the emcee Affine Invariant Markov chain Monte Carlo Ensemble sampler implementation


Graham (2001) analysed a sample of 86 face-on disc-dominated galaxies previously selected by


hus, 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 disk of an AGN provides a natural environment for stars and compact objects to accrete materials and to migrate within it (e.g.,


claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009)


although the lower mass limit is estimated as 5.4 M⊙ by Corral-Santana et al. (2011).


Also shown in Fig. 12 (with a black [gray] solid line for the low [high] dust content) is the proposed analytic solution for fesc by


(18)\begin{equation} f_{\rm esc}^{\rm HO06} = 1/{\rm cosh}(\!\sqrt{2 N_{\cl}\epsilon}), \label{eq:fescHO06} \end{equation}fescHO06=1/cosh(2Nclϵ),where for Ncl we used Eq. (8)(with (a1,b1) = (3/2, 2) as found in Sect. 4.1) and for the clump albedo (i.e., the fraction of incoming photons that are reflected) ϵ, we adopted a value of c1(1−e− τd,cl) with c1 = 1.6 [c1 = 0.06] to match the NHI,cl = 1022 cm-2 data points for τd,cl = 10-4 [τd,cl = 1].


Early studies concentrated on measurements of higher order correlation hierarchy in the angular space due to small survey size


On the other hand, the Minkowski functionals (MFs) are extremely useful tools in quantitatively describing the morphology because, in principle, they contain information on all the higher-order moments.


Since then they have been extensively employed to study the morphology of the large-scale structure of the universe and the cosmic web


Next, we adopt the position of 3FGL J1640.4-4634c provisionally provided by the 3FGL catalog


This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by


Kerszberg et al. (2017), Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.


Other global 21-cm experiments, including the Large-Aperture Experiment to Detect the Dark Ages


provide upper limits on the signal from Cosmic Dawn and the Epoch of Reionization (EoR), ruling out some extreme astrophysical scenarios.


It was soon realized that these frequencies are probably related to oscillations of the neutron star, and several groups tried to identify them as


The data were manually calibrated by the EA ARC node using the Common Astronomy Software Applications (CASA) of the version 5.1.1


Recent measurements of the LMC abundances based on the X-ray spectral analysis of SNRs


suggest ∼50% lower LMC abundance values for O, Ne, Mg, and Fe than the previously estimated values


Our derived shock parameters are consistent (within statistical uncertainties), assuming either set of these LMC abundances in tbnew.


The B/T ratio is an important indicator of galaxy structure and is well correlated with several other physical quantities of interest in studies of galaxy evolution, such as


In this scenario SMBHs have to begin growing even earlier than the very first stars are assumed to have appeared (see discussion in


Studies based on both observations and simulations have shown that galaxy collisions and mergers can dramatically affect the galaxies undergoing the interaction, by, e.g.


A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques,


and high resolution spectroscopic techniques (e.g.


To date, several candidate jet–ISM interaction sites have been identified;


From these past works, it is clear that finding and confirming interaction sites can be incredibly difficult and often observationally expensive (e.g. requiring deep, wide-field radio continuum observations).


However, the depth of the feature is ΔT21 ∼ 0.5 K ($99{{\ \rm per\ cent}}$ confidence level), which is two to three times stronger and considerably wider (Δν ∼ 19 MHz) than that predicted by the most optimistic astrophysical models (e.g.


Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones


Moreover, in massive galaxies, the role of AGNs in influencing galaxy evolution and quenching SF is supported by several observations


On the other side, we have the tidal (gravitational) mechanisms occurring


In fact, homologous jets, continuing for hours at a time, have been commonly observed (e.g.,


More evolved disks do not show a degree of linear polarization larger than 0.5%


and a similar phenomenon has also been observed in the case of


Since cool core clusters have short radiative cooling time-scales on the order of 108 yr in their centres (e.g.


starbursts are expected to be common at the centre of such clusters.


Comparison of 1D marginal posterior distributions over the parameters S8 ≡ σ8(Ωm/0.3)0.5, σ8 and Ωm, from DES Y3 data as well as other experiments, and consistency tests for this work (in blue).


Constraints from other weak lensing surveys, namely HSC Y1


They have shown that the ionised phase appears to be an ideal tracer of stripped gas in dense regions: approximately 50% of late-type galaxies show extended (~50 kpc) tails of ionised gas with surface brightness Σ(Hα) of approximately a few 10−18 erg s−1 cm−2 arcsec−2


while only a handful of galaxies have extended cold or hot gaseous tails


Since relxillDCp considers the thermal Comptonization model nthComp


as the irradiating (primary) continuum, we replaced the zpowerlw continuum with nthComp.


For this paper, κ is taken to be equal to 1, in agreement with numerical simulations of decaying turbulence


Observationally, the bulk Lorentz factor of the jet in the low/hard state of X-ray binaries can be restricted in a relatively narrow range and the velocity of the jet is mildly relativistic, i.e. Γjet ≲ 2. More strictly, the bulk Lorentz factor is restricted to be as Γjet ≲ 1.67


A similar effect is also found in measurements of the propagation velocity of travelling waves


In particular, it has been demonstrated repeatedly that the power spectral density (PSD) of blazar light curves is, in general, of a power-law form


This kind of weak anti-correlation between the activity cycle and the meridional flow has been found in solar observations


The reasons for studying the dynamic properties of small-scale magnetic fields in the quiet photosphere are manifold. Firstly, magnetic fields provide an opportunity to probe


and energy propagation to the upper atmospheric layers (see, e.g.


that cannot be addressed otherwise from an observational point of view.


In particular, the analysis of CMB data, most notably from the Wilkinson Microwave Anisotropy Probe


experiments, has not yet provided conclusive evidence for the hypothesis of Cosmological Isotropy


Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst has occurred


giving the neutral material time to propagate out to the impact parameters probed by COS-AGN


Stars with brighter K-band absolute magnitudes tend to have higher [N/Fe] and lower [C/Fe] (middle and bottom panels of Figure 8), which is consistent with extra-mixing theory and observation


Higher angular resolution observations of the (3, 3) NH3 absorption line (0\hbox{$\farcs$}.̋3 beamsize) showed signatures of rotation within 2000 AU based on a position-velocity (pv) diagram


Here, for instance, the presence of a magnetic field leads to the formation of early outflows. These reduce the radiation pressure, which allows the protostar mass to grow further


Here we adopted an intermediate value between the solar and supersolar G/Ds used in


and we increased the error bars of these points to include both the solar and supersolar confidence estimates.


Although hotspots located at the foot of accretion streams can affect RV measurements mimicking the signal of an orbiting body


Johns-Krull et al. (2016) specifically looked for these signals and found no evidence that hotspots produced the RV signals seen in photospheric absorption lines.


As for the density profile, simulations of the FHSC stage show a flat inner region, corresponding to the FHSC structure and extending up to ∼10 au


Some of the recent observations and studies


indicate that the CGM can account for a good fraction of the baryons in these galaxies.


From power spectrum analysis, significant periodicities ranging from about 1.4 to 10 yr were found in PSR B1540−06, PSR B1642−03, PSR B1818−04, PSR B1826−17, PSR B1828−11, and PSR B2148+63


In all cases, we consider a solar metallicity for the main SF episode and, according to the results of


a subsolar metallicity (Z = 0.004) for the later one.


If the carbene is formed in its first excited singlet state (a1A1), the insertion is barrierless


Using these indicators, a number of studies have found that the color or SFR transition of galaxies is associated with the consumption of their gas content (e.g.,


As shown by comparisons to dark moon observations only particle events are recorded in the stow position


The cool molecular envelope exhibits ice and dust absorption bands


Sagittarius A* (Sgr A*) is inferred to be accreting at a rate of 10−3 to $10^{-2}\ \dot{M}_{\rm B}$ (e.g.


In more detail, the existence of a “blue” and possibly also a “purple” component in the AT 2017gfo emission further indicated that the merger product of the GW170817 event is very likely to be a hypermassive NS, which lasted for at least a few hundred milliseconds, as an immediately formed black hole can only be associated with a “red” kilonova1


The origin of this correlation is puzzling, as stellar clustering is expected to affect mostly the outer part of planetary systems in very dense environments


which is one of the commonly used methods of mass determination in galaxy clusters (see e.g.


This new estimate is consistent with the ratio expected between the aGg′ and gGg′ conformers under thermal equilibrium conditions at 300 K, the excitation temperature of glycolaldehyde derived in IRAS 16293


these are based on the vector eccentricity and the vector inclination.


The initial condition is the Orszag–Tang vortex (OTV) (e.g.,


also, ‘convergence’ is meant in the sense that the Lp norm of the difference between the actual solution and the ZKBP function tends to zero as t → ∞ faster than a negative power of the time with an exponent which is a function of n, m, and p (e.g. −1/3 for n = 2 and m = 3 in the L2 norm; see details in the book by


The CO photodesorption yield reaches its highest value when this ice is deposited at low temperatures (down to 7 K, the lowest temperature studied experimentally) and decreases gradually at higher deposition temperatures


The explanation for this phenomenon motivated further research.


On the other hand, if the torus is made of a collection of clouds, each cloud is heated to ∼300 K to emit MIR emission while absorbing the background light when the foreground cloud is cooler than the one behind. The radiation transfer effect among the clouds significantly reduces the net silicate absorption even when the torus is seen edge-on


The first three LoTSS Deep Fields are the European Large-Area ISO Survey-North 1 (ELAIS-N1


these were chosen to have extensive multi-wavelength coverage from past and ongoing deep, wide-area surveys sampling the X-ray


Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g.


This proved to be a useful distinction and an excellent predictor of several trends


but recent results, including our present and previous analysis


show that the demarcation between starburst and main-sequence galaxies is more blurred that we previously considered.


Metallicity gradients in units of dex kpc-1 determine tight correlations with the global properties of galaxies such as the stellar mass or the size, which are erased when normalised by a characteristics radius such as the half-mass radius (e.g.


For example, it was observed that a single emission line at around 14 keV can fit two features around 10 and 20 keV for


In the case of GRO J2058+42, an introduction of a single Gaussian emission line in this range of energies could not appropriately fit the spectrum.


In this context ‘scale-free’ cosmological models, in which both the expansion law and the power spectrum characterizing the initial fluctuations are simple power laws, have the advantage of relative simplicity, and they have for this reason been studied quite extensively in the literature (see e.g.


Extreme geomagnetic storms can cause widespread interference and damage to technological systems


and then lead to significant economic loss (e.g.,


Our upper limit on the Fopt/Fx for the PSR J0633+0632 PWN is above the values obtained for the other PWNe, which are typically ∼ 0.02–0.04, apart from the Crab PWN which has an Fopt/Fx ∼ 2


This is also the case for the PSR J1124−5916 PWN


Also the dependence of the IMF on the SFR is nowadays observationally well established


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


The fact that simulations usually produce anti-solar differential rotation for the solar rotation rate could indicate that the Sun is in a transitional regime (e.g.,


or could also mean that simulations still cannot fully capture the true rotational influence on turbulent convection in the Sun.


But there is no well-resolved system that matches the theoretical expectations (see, e.g.,


Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are


for dwarf galaxies, the tightness of the baryonic Tully–Fisher relation


The comparison sample is compiled from the literature up to z ∼ 3


There have been searches for a periodic signal in the prompt emission of GRBs with a number of instruments with no success, for example:


At certain geocentric velocities the cometary [O i] 6300 Å emission sits on top of a strong telluric absorption, and at high airmass inaccurate removal of this feature can result in a decrease in the measured flux and therefore production rate. This was observed for C/2012 S1 (ISON)


Several observations have shown that properties of galaxies such as star formation, gas content, and colour are affected by the cluster environment at large clustercentric distances (e.g.


Here, Ai,j are the entropic functions of the particles


A cold-phase of the CGM at ≈104 K has also been observed, but its origins are less clear


It was the first source identified as a hot corino


based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies


Turbulence on scales less than the scale height of the warm–cold ISM likely originates primarily due to the feedback from young stars


To model mechanical feedback, we adopt a phenomenological model proposed by Ostriker et al. (2010), while radiative feedback is treated by adopting the standard and slim disc model


, the intensity of H2O in the coma dominated the overall signal, with maxima in the H2O signal every ~6 h, about twice during a rotation.


Interestingly, however, CO2 and CO displayed a separate additional maximum when the H2O signal was near its minimum. This independent maximum in CO2 and CO only occurred at negative observing latitudes that are associated with a particular “view” of Rosetta at 67P, with the larger lobe blocking out the neck and head.


found that the disc thermal emission (∼0.3–0.7 keV, soft band) leads the power-law variations (∼0.7–1.5 keV, hard band) on long timescales (> 1s).


The propeller regime has been investigated both analytically


In this paper, we adopt Mpi = 20 M⊕ and Mpf = 10 M⊕ nominally (close to the standard model adopted in


Negative radial metallicity gradients have been widely observed in the low-redshift galaxy population (e.g.


Gravitational interactions in the perturbed disc drive turbulence causing the disc to self-regulate in a marginally stable state with Q ≲ 1


that can last for more than a Gyr so long as the accretion is not interrupted.


Apart from cosmological simulations, dedicated zoom-in simulations


have revealed that dry mergers that dominate the passive evolution of ETGs below z ≈ 2 could make the total density profile shallower than isothermal


We calculate the GW amplitudes A(f) of NS–WD binaries using the phenomenological (PhenomA) waveform model in the Fourier domain


According to the review of the leptonic model (see, e.g.,


the electrons injected into PWNe are accelerated by the pulsar magnetosphere and the termination shock. Therefore, the relativistic particles injected into the PWNe are also assumed as two different power-law components from the pulsar magnetosphere and shock acceleration, respectively.


and a comparison with the other EoSs of the BSk family


Intermittency is related to the scale-dependent shape of the probability distribution function of the increments Δϕ


This, additionally, implies the existence of nonvanishing odd moments.


whereas radio relics are apparently associated with localized, post-merger shock-fronts


an apparent link is seen between radio galaxies and radio relics.


concluded that WR 130 could have alone created the observed structure, it is important to note that they did not take into account the molecular mass present in the shell, which considerably increases the kinetic shell energy.


Linking purely gravitational interactions to symmetries such as defined in equation (3) suggests deeper physics and constitutes a motivation for viewing MOND as much more than a mere phenomenological description of galactic dynamics


Although period-folding improves performance


Becker et al. (2020)’s time-space RNN does not require the period to be calculated, and is thus less computationally expensive in terms of preprocessing.


This representative value for our AGN is in line but not as low as previous work targeting extremely powerful sources (e.g., Mgas, mol/M*  0.05 in


As a result, when the power spectrum is observed as a function of (k∥, k⊥), the foreground emission remains concentrated near the low k∥, inside the ‘wedge’


Another problem is the use of time-dependent mixing-length formalisms


to account for modal surface effects (e.g.,


Strong gravitational lensing systems are a powerful tool for cosmology. They have been used to study how dark matter is distributed in galaxies and clusters


and are uniquely suited to probe the low end of the dark matter mass function and test the prediction of the cold dark matter (CDM) model beyond the local universe (e.g.,


A way to possibly explain this polarization change is to view it as a mode-coupling phenomenon, the process by which the rays reverse their original sense of polarization while passing through a quasi-transverse field region along the line of sight from the radiation source to the observer, depending on the degree of mode coupling there


In addition, we argue that the Galaxy is the azimuthally asymmetric spiral system (cf.


The charge transfer inefficiency (CTE) correction for the ACS data was performed by the pipeline, whereas CTE losses in WFC3/UVIS


were treated manually using the tools supplied by STScI.


t is worth pointing out that clumpy galaxy fractions are highly sensitive to methodology and clump definition and vary widely in the literature (e.g.,


so we should not expect complete agreement.


Here, we use the new formalism presented in


who showed that the Newtonian potential is exactly reproduced by using an intermediate scalar function ℋ, namely \hbox{$\Phi = \partial_{xy}^2 {\cal H}$}Φ=∂xy2ℋ. In 3D, this hyperpotential is written as (12)\begin{equation} {\cal H}(x,y,z) = -G \iiint_{\Omega'}{\rho(x',y',z')} \kappa^{xy}(X,Y,Z){\rm d}x'{\rm d}y'{\rm d}z' , \end{equation}ℋ(x,y,z)=−G$Ω′ρ(x′,y′,z′)κxy(X,Y,Z)dx′dy′dz′,with X = x−x′, Y = y−y′ and Z = z−z′.


However, the repulsive nature of lensing by a large and deep underdense region (i.e., cosmic voids) as described by the rigorously derived but simply implemented embedded lens formalism did not appear until


Indeed, other studies confirm that abiotic buildup of ozone is possible


however, detectable levels are unlikely if liquid water is abundant, as e.g. rainout of oxidized species would keep atmospheric O2 and O3 low


, unless the CO2 concentration is high and both H2 and CH4 emissions are low


and RFs are associated with energy conversion from electromagnetic fields to particles


This accounts for the bias due to contaminating galaxies that are physically associated with the centrals but are not satellites (i.e., the 2-halo term of the correlation function; see


have long been recognized as one way to produce significant changes in the flux and polarization


Vacuum birefringence dramatically increases the linear polarization of the observed radiation, from a level of a few  per cent up to even ∼100 per cent, depending on the viewing geometry and the surface emission mechanism


recalled several issues that should be taken into account when considering the Si iv/O iv density diagnostic. The main ones were: (1) O iv and Si iv ions are formed at quite different temperatures in equilibrium and hence a change in the O iv/Si iv ratio could imply a change in the temperature rather than in the plasma density (2) the chemical abundances of O and Si are not known with any great accuracy and could be varying during the observed events (3) density effects on the ion populations could increase the Si iv/O iv relative intensities by a factor of roughly three to four.


are believed to originate from the inner accretion flow/corona that is associated with the Comptonized power-law component of the X-ray spectrum, as this component shows a much larger variability amplitude than the blackbody disc component


This latter assumption does not perfectly reflect spacecraft observations of the same


, but leads to relatively simple, tractable expressions for the parallel and perpendicular MFPs.


Non-chondrite meteorites (including achondrites) also originate from differentiated asteroids and planets, e.g. from Moon, Mars, and Vesta, and the angrite and ureilite parent bodies


This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments


Here, $\widetilde{v}_r$ and $\widetilde{v}_\varphi$ are the amplitudes of the radial and tangential wave motions that depend weakly on the Galactocentric distance r, and ϕ is the phase of the wave


Indeed, Terzan 5 hosts the largest population of MSPs among all Galactic GCs


Still, in four dimensions, hairy BHs have been described in different theories of gravity, such as Einstein–Yang–Mills


Originally it was proposed that due to mutual gravitational interactions that all black holes would have been ejected from globular clusters


do not seem to be related to unaccounted variation in the CO-to-H2 conversion factor


but has been interpreted as evidence that SiO disappears from the gas phase at high densities to be incorporated into dust grains


This method has been intensively implemented with updated observations


To limit the ISGRI calibration uncertainties


This is within the range of the equipartition magnetic fields of 17 HFP radio sources


and 5 HFPs at 0.084   z   1.887 (18–160 mG


These values are in very good agreement with those measured from the average long-term Swift/BAT (Burst Alert Telescope) spectrum


As shown in greater detail in Stritzinger et al. (2020, hereafter Paper I), the ILRT subtype is well represented by NGC 300-2008-OT and SN 2008S, and has been linked to asymptotic giant branch (S-AGB) stars


In this paper, the data from DC to 2 MHz are discussed. These measurements are obtained from the potentials of the four antennas, V1 through V4, that are located in the plane perpendicular to the Sun–satellite line. They produce E12 = (V1−V2)/3.5 and E34 = (V3−V4)/3.5, which are then rotated into the spacecraft coordinate system to produce EX and EY. The direction, X, is perpendicular to the Sun–spacecraft line, in the ecliptic plane, and pointing in the direction of solar rotation (against the ram direction), Y is perpendicular to the ecliptic plane, pointing southward, and Z points toward the Sun. The numerical factor, 3.5, is the effective antenna length


No Compton reflection hump has been detected with


despite the presence of a complex Fe Kα line.


The initial dispersion of the LUV − LX relation is relatively large (δ ∼ 0.35−0.4,


but after a detailed study, Lusso & Risaliti (2016) suggest that most of the observed dispersion is not intrinsic, but it is rather due to observational effects.


We use an α approximation for the turbulent viscosity


when the (rφ) component of the stress tensor trφ is written as (5)\begin{equation} t_{r\phi}=\alpha\, P, \label{trphi} \end{equation}trφ=α P,where the phenomenological non-dimensional parameter α ≤ 1.


Early on, the MUSE Guaranteed Time Observations (GTO) team established surveys including MUSE-QuBES


to relate gas traced by absorbers to galaxies.


Topological estimators such as the Minkowski functionals (MFs) are also important diagnostics in this direction as they carry information at all orders. The MFs have been extensively developed as a statistical tool in a cosmological setting for both two-dimensional (2D; projected) and 3D (redshift) surveys. The MFs have analytically known results for a Gaussian random field, making them suitable for studies of non-Gaussianity. Examples of such studies include CMB data


These microlensing magnification estimates are calculated after subtracting the emission line flux ratios, which are little affected by microlensing (see, e.g.,


from the continuum flux ratios, and are therefore virtually free from extinction, substructure, and macro model effects (as these affect the line and continuum flux ratios equally).


Furthermore, well-defined large samples of white dwarfs are an extremely useful starting point for identifying rare white dwarf types like


or white dwarfs with dusty or gaseous planetary debris discs


Observations have shown that the AGN fraction does increase with decreasing distance between two merging galaxies


but this has not been well tested at the very centers of merger-remnant galaxies because of the observational difficulty of detecting and resolving two AGNs with separations 10 kpc.


Moreover, c-C3HD and c-C3D2 have been surveyed in a sample of low-mass prestellar and protostellar cores


finding that the corresponding isotopic ratios are relatively uniform, within a factor of a few, and similar to those in L1544 and L483.


However, differences in the yields produced in the He detonation can in part be attributed to the slightly different setups of Model M2a (and therefore Model M2a_pp) and Model M10_05_1 at the beginning of the relaxation simulation, with the differences in the total and shell masses being less than 1% (see


This results in different spatial distributions in which tiny grains are present at the disk surfaces


and in the cavity or gaps from which the pebbles are missing (e.g.


We expect the centroid of a blended source to be determined with poor accuracy (see e.g.


For this reason as a further test we plotted the distribution of distances in arcsec of the VMC sources cross-matched with the OGLE IV RRLs.


In some cases, the mergers eventually devoid their entire neighbourhood, leaving behind a single elliptical galaxy of group-scale mass, called a fossil group galaxy


Using their spectroscopic catalog with radial velocities measured with an external accuracy of 7–10 km s-1 and applying photometric parallax relations, the SDSS teams have traced K–M dwarfs in the distance range up to ~2 kpc, thus providing valuable information on the spatial, velocity, and metallicity distributions with respect to vertical distance from the Galactic plane


as well as on the luminosity and mass functions of low-mass dwarfs in the Galactic disk


Second, our calculations neglect the effects of binary star systems. Mass transfers and mergers between binary companions can extend the period over which ionizing photons are produced by the stellar population, which would harden the time-integrated spectrum


Then, as this polarization propagates, it is further modified by Faraday effects, important for depolarizing accretion flows down to observed levels and generating the observed rotation measure


Following OSO-7, a series of spacecraft (Skylab, Helios, P78-1 Solwind, SOHO, Coriolis, and STEREO, etc.) have observed thousands of CMEs leading to a vast literature


detected INV during three nights out of three using C- and F-tests (a total monitoring duration of 16 h in the R-band).


Fornasier et al. (2015) obtained results for the 67P nucleus surface reflectivity applying a HG-type phase function


with a best-fitting G of −0.13. Fig. 5 shows the phase angle-corrected afρ values of 67P for the various phase function solutions.


Asymmetric inflow reconnection has also been investigated in


The LMC star cluster formation history is believed to be three-staged, including a period of rapid cluster star formation in the early universe (τ ≳ 10 Gyr), followed by a long quiescent period between ∼10 and ∼2–4 Gyr ago and then by a period of rapid star cluster formation extending to the present day, potentially due to the interaction between the LMC and SMC


Hydrodynamic simulations using the code HYADES


developed a classification scheme based on a disk+power law fit, to be applied to ULX spectra, according to which the spectral state of an ULX source can be defined by the disk temperature, the power-law slope, and the ratio between the flux contribution of the two spectral components in the 0.3−1 keV band.


The X-ray luminosity of GRBs is given by the energy input from the electromagnetic and gravitational waves into the surrounding medium


Therefore, in order to standardize GRBs as standard candles through the Dainotti relation, it is recommended that X-ray plateaus caused by the same physical mechanism are used (electromagnetic dipole radiation or gravitational waves).


For the three first cases, we assumed ISM[M/H](R⊙) = 0.0 to estimate Rbirth from the stellar metallicity. However,


have their own zero point, defined as: [Fe/H] = −0.06 * Rg + 0.57, with a clear shift in the relation compared to the other ones assumed in this work.


Single-case studies reported some EIT waves covering a whole solar hemisphere


and the GOALS samples, we excluded all the composite starburst-AGN objects identified as those with a detection of [NeV] either at 14.3 or 24.3 μm.


A cool spot at a higher latitude would reduce the amplitude of the NIR wide-band flux modulations; a quenching of the convective shifts or the Zeeman effect also do not appear to be viable explanations because they increase the effect of a cool spot on the RV at NIR wavelengths


The most rapid changes of surface temperature occur early,


and then when the temperature drops below the critical temperature for core neutrons to become superfluid, which activates the efficient neutrino emission process of Cooper pair formation and breaking


For PN in O-rich AGB atmospheres, the disagreement between the observed abundances, (1–2) × 10−8


and the calculated maximum chemical equilibrium abundance is almost three orders of magnitude.


Compact starbursts containing hot O stars offer an alternative explanation for the relative intensities of LINER emission lines


, but have difficulty explaining the broad Balmer emission wings often seen in LINER spectra


, since this would require long-lived supernova remnants.


The Hα line of V410 Tau can grow much stronger and broader during a flare, and also show asymmetries; however, the observed asymmetries seen during flares do not show excess emission with apparent peaks shifted out to greater than ±200 km s−1


was used to clear the image of cosmic rays to produce the final Hα and final R image.


Several attempts have been made to infer clusters dynamical state, using both observational data and simulations, by analysing the images of the emission in optical


A relaxed, dynamically old group or cluster should be characterized by a central galaxy which is the brightest (most massive) member by a significant margin (e.g.


Different column densities of para-H2CO only weakly affect derived kinetic temperatures (see Fig. 3 in


as long as all lines are optically thin.


The spectra of the AGNs to be compared are taken from those of the IR galaxies observed by Spitzer/IRS


As mentioned previously, magnetars have been identified in many studies as promising candidates for the acceleration of cosmic rays and the production of secondary high-energy neutrinos, for instance Blasi et al. (2000), Fang et al. (2012, 2013), Lemoine et al. (2015),


We estimated the optical depths of the AGNs of Stierwalt et al. (2013), Wu et al. (2010), and Roussel et al. (2006) by ourselves in the same manner as was performed for LEDA 1712304 with the method defined by


and continue to attract much attention in the quest for unraveling quantum effects such as the geometric phase (GP) in chemical reactions


Using Bayesian analysis to fit a distribution function to full 6D phase-space data (globular clusters, satellites, and halo stars) has been a recent popular choice among many works


The ascending of a filament can go on high into the corona (successful eruptions) and gives rise to a coronal mass ejection (CME) or can stop at some greater height in the corona (confined or failed eruptions)


Accounting for the ramp up of the driver and scaling the values, this corresponds to an energy injection rate of ≈5.6 × 1023 erg s−1 at the maximum driving speed. During the quasi-steady phase, this injection is balanced by losses to numerical diffusion and equates to roughly the free energy available for heating the plasma. Even after accounting for the unrealistically fast driving speed (see below), this energy release rate compares well with the observed values of 1023–1024 erg s−1 for bright points


A possible fix of this proposal is to introduce rapidly spinning magnetars born from binary neutron star (BNS) mergers


Recently, several works have attempted to estimate the expected coalescence time for binary BHs by post-processing cosmological simulations, finding time-scales on the order of 100s of Myr to Gyr for the binary coalescence time (e.g.


For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed


Generally, the spectrum hardens when the flux increases


but photon indices can saturate at higher fluxes


It is not yet clear which process is the dominant source of the elements in the early Universe (see discussions by, e.g.,


As a consequence, mergers are also expected to play a significant role in driving the evolution of galaxy properties, for example,


star formation in the host galaxy or by driving its morphological evolution (e.g.


At the centre of the debate is the strength of the surface dipole field and any multipolar component. Should the dipole field strength be similar to that of Galactic HMXBs (1012 G – e.g.


then it is quite plausible that the flow will be supercritical ($\dot{m}/\dot{m}_{\rm Edd} \gt $ 1 where $\dot{m}_{\rm Edd}$ is the Eddington accretion rate) at radii greater than the magnetospheric truncation radius (rM).


We have now access to the size evolution up to z ~ 10 from the deepest HST imaging data


There is a debate about the extent to which DIG affects measurements of gas-phase metallicity and its radial slope


as some observations indicate lower metallicity (up to 1 dex) in DIG compared to nearby H ii regions.


For example, if G1.75-0.08 follows the line width–size relation in the central molecular zone, or CMZ, which for HCN is found to be σ ∝ R0.62


, the aforementioned HCN(1 – 0) line width would be expected to be only ~2.5 km s−1 on the ~0.1 pc scale, which is a typical inner width (FWHM) of filamentary molecular clouds


In particular, classification by ML (e.g.,


can avoid time-consuming visual inspections and will be helpful for the visual classification of galaxy−galaxy interactions from the forthcoming large surveys.


We stress that our SOFIA/FORCAST images do not detect the outer polar rings seen in Spitzer IRAC images


For the sake of simplicity, the specific heat capacity c was assumed constant, c = 560 J kg−1 K−1, and the regolith grain density obtained for C-type meteorites was used, ρ = 3.11 g cm−3 (both from


We collect the total radio flux density from literature


We estimate the fluxes Fx (see Table 1) of LHS and HIMS of the 1999 outburst of the source


There are examples of merging clusters that show presence of X-ray–SZ offsets, such as


For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed


A novel aspect of the search here presented is the inclusion in the data analysis chain of the uncertainty that possible unknown parameters, related to the characteristic activity of the central engine, can introduce in the neutrino flux evaluation. This is crucial in order to correctly interpret the validity of model-dependent results, in terms of upper limits set by non-detections of neutrinos in coincidence with GRBs


Analogously to previous ANTARES searches


MC simulations of the signal predicted by NeuCosmA were performed, while the respective background was estimated directly from off-source data collected by ANTARES.


Following Rosdahl et al. (2018), we have calibrated the SN feedback in order to reproduce the high-redshift stellar mass–halo mass relation from abundance matching


The same source was followed up and consistently localized at other wavelengths (e.g.,


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


in order to lower its Fermi energy (starting at about two times the saturation density).


Such studies are dependent on the observations of a handful of storms that have approached or rivalled the Carrington geomagnetic storm in observed/inferred intensity and/or auroral extent. These include great storms in


For consistency, we adopt the translation of this to the absolute velocities of cluster galaxies normalized by their respective galaxy cluster velocity dispersions into the range $0.3 \lt |\Delta \mathrm{V}|/\sigma _{r_{200}} \lt 0.5$ as deduced by


With ALMA and NOEMA, ground-based observations of the [C II] 158 μm line in high redshift galaxies have come into reach and such data are routinely used to infer SFRs


based upon validations of this relationship in the nearby Universe


A common interpretation of the MS is that the location of galaxies relative to the MS follows a different time evolution of SFR


Several studies have already measured the distance ratios (e.g.


though they are afflicted by several systematics such as, uncertainties in modelling cluster profiles and cosmic variance in the case of multiple strong lens systems, and photometric redshift uncertainties as well as imaging systematics that cause a redshift-dependent shear calibration in the case of weak lensing.


was conceived during its preliminary design phases with the goal of maximizing operational efficiency, flexibility, and scientific output while complying with the standard Paranal Observatory operational scheme.