Miracle-dz/UniFAR-FTUs huggingface dataset:
Interaction and gas outflows in radio-loud AGN - Disruptive and constructive effects of radio jets

In the last years, Active Galactic Nuclei (AGN) have become more popular than ever. The possibility of using them to produce feedback effects that would help solving some of the still open questions connected to the hierarchical scenario of galaxy formation and evolution, has made them particularly popular among theorists. AGN-driven outflows can have different origin. Here, I will concentrate on the role that the radio-loud phase of nuclear activity (and the presence of radio plasma jets) can play in the evolution of a galaxy. I will focus on two aspects in which radio activity could be important. The first is exploring whether relativistic plasma jet associated with radio-loud galaxies could provide an effective way to produce gas outflows with characteristics that can be relevant in the evolution of the host galaxy. The second, is to investigate whether they can provide a mechanism for the triggering of star formation.
OBSCURED STARBURST ACTIVITY IN HIGH-REDSHIFT CLUSTERS AND GROUPS

Using Spitzer-Multiband Imaging Photometer 24 μm imaging and extensive Keck spectroscopy, we examine the nature of the obscured star-forming population in three clusters and three groups at z ∼ 0.9. These six systems are the primary components of the Cl1604 supercluster, the largest structure imaged by Spitzer at redshifts approaching unity. We find that the average density of 24 μm detected galaxies within the Cl1604 clusters is nearly twice that of the surrounding field and that this overdensity scales with the cluster's dynamical state. The 24 μm bright members often appear optically unremarkable and exhibit only moderate [O ii] line emission due to severe obscuration. Their spatial distribution suggests that they are an infalling population, but an examination of their spectral properties, morphologies, and optical colors indicates that they are not simply analogs of the field population that have yet to be quenched. Using stacked composite spectra, we find that the 24 μm detected cluster and group galaxies exhibit elevated levels of Balmer absorption compared with galaxies undergoing normal, continuous star formation. A similar excess is not observed in field galaxies with equivalent infrared luminosities, indicating a greater fraction of the detected cluster and group members have experienced a burst of star formation in the recent past compared to their counterparts in the field. Our results suggest that gas-rich galaxies at high redshift experience a temporary increase in their star formation activity as they assemble into denser environments. Using Hubble Space Telescope Advanced Camera for Surveys imaging, we find that disturbed morphologies are common among the 24 μm detected cluster and group members and become more prevalent in regions of higher galaxy density. We conclude that mergers are the dominant triggering mechanism responsible for the enhanced star formation found in the Cl1604 groups, while a mix of harassment and mergers are likely driving the activity of the cluster galaxies.
Intraparenchymal metastases as a cause for local recurrence of pancreatic cancer

Sir: Pancreatic ductal adenocarcinoma (PDAC) is one of the most lethal forms of cancer, with a dismal 5year survival rate of 11%. Of the one in five patients fortunate enough to qualify for surgery, approximately 80% will develop a recurrence, with 24% of recurrences involving the remnant pancreas. Although PDAC is known to be highly invasive along ductal, neural and vascular networks, limitations in the resolution of diagnostic imaging (such as computed tomography) have hindered our ability to identify the microscopic processes that produce recurrences. Here, using serial tissue sectioning and deep learning, we report unique identification of a microscopic, intraparenchymal metastasis, providing evidence for one mechanism by which PDAC can recur in the remnant pancreas. An elderly male was diagnosed with a 2.5-cm poorly differentiated pancreatic ductal adenocarcinoma. A Whipple procedure was performed and all surgical margins were pronounced microscopically negative for tumour. CODA, a recently developed tool for three-dimensional (3D) reconstruction of tissues, was applied to resected grossly uninvolved pancreatic tissue from the elderly male patient. Briefly, grossly normal pancreatic parenchyma was formalin-fixed, paraffin-embedded (FFPE) and serially sectioned to a depth of 6.4 mm. Every third section was stained with haematoxylin and eosin (H&E) and digitised, while intervening sections were left unstained (Figure 1A). Scanned H&E sections were registered to create a digital volume using a non-linear histological image registration approach. A semantic segmentation algorithm was used to label seven pancreatic components in the tissue: islets of Langerhans, normal ductal epithelium, vasculature, fat, acini,
HerMES: THE REST-FRAME UV EMISSION AND A LENSING MODEL FOR THE z = 6.34 LUMINOUS DUSTY STARBURST GALAXY HFLS3

We discuss the rest-frame ultraviolet emission from the starbursting galaxy HFLS3 at a redshift of 6.34. The galaxy was discovered in Herschel/SPIRE data due to its red color in the submillimeter wavelengths from 250 to 500 μm. Keck/NIRC2 Ks-band adaptive optics imaging data showed two potential near-IR counterparts near HFLS3. Previously, the northern galaxy was taken to be in the foreground at z = 2.1, while the southern galaxy was assumed to be HFLS3's near-IR counterpart. The recently acquired Hubble/WFC3 and Advanced Camera for Surveys (ACS) imaging data show conclusively that both optically bright galaxies are in the foreground at z < 6. A new lensing model based on the Hubble imaging data and the millimeter-wave continuum emission yields a magnification factor of 2.2 ± 0.3, with a 95% confidence upper limit on the magnification of 3.5. When corrected for lensing, the instantaneous star formation rate is 1320 M☉ yr−1, with the 95% confidence lower limit around 830 M☉ yr−1. The dust and stellar masses of HFLS3 from the same spectral energy distribution (SED) models are at the level of 3 × 108 M☉ and ∼5 × 1010 M☉, respectively, with large systematic uncertainties on assumptions related to the SED model. With Hubble/WFC3 images, we also find diffuse near-IR emission about 0.5 arcsec (∼3 kpc) to the southwest of HFLS3 that remains undetected in the ACS imaging data. The emission has a photometric redshift consistent with either z ∼ 6 or a dusty galaxy template at z ∼ 2.
Radio galaxies in the Sloan Digital Sky Survey: spectral index–environment correlations

ABSTRACT We analyze optical and radio properties of radiogalaxies detected in the Sloan DigitalSky Survey (SDSS). The sample of radio sources are selected from the catalogue ofKimball & Ivezi´c (2008) with ﬂux densities at 325, 1400 and 4850 MHz, using WENSS,NVSS and GB6 radio surveys and from ﬂux measurements at 74 MHz taken from VLALow-frequency Sky Survey (Cohen et al. 2006). We study radiogalaxy spectral prop-erties using radio colour-colour diagrams and ﬁnd that our sample follows a singlepower law from 74 to 4850 MHz. The spectral index vs. spectroscopic redshift relation(α − z) is not signiﬁcant for our sample of radio sources. We analyze a subsample ofradio sources associated with clusters of galaxies identiﬁed from the maxBCG cata-logue and ﬁnd that about 40% of radio sources with ultra steep spectra (USS, α < −1,where S ν ∝ ν α ) are associated with galaxy clusters or groups of galaxies. We constructa Hubble diagram of USS radio sources in the optical r band up to z ∼ 0.8 and com-pare our results with those for normal galaxies selected from diﬀerent optical surveysand ﬁnd that USS radio sources are around as luminous as the central galaxies in themaxBCG cluster sample and typically more than 4 magnitudes brighter than normalgalaxies at z ∼ 0.3. We study correlations between spectral index, richness and luminosity of clustersassociated with radio sources. We ﬁnd that USS at low redshift are rare, most of themreside in regions of unusually high ambient density, such of those found in rich clusterof galaxies. Our results also suggest that clusters of galaxies associated with steeperthan the average spectra have higher richness counts and are populated by luminousgalaxiesin comparison with those environments associated to radiosources with ﬂatterthan the average spectra. A plausible explanation for our results is that radio emissionis more pressure conﬁned in higher gas density environments such as those found inrich clusters of galaxies and as a consequence radio lobes in rich galaxy clusters willexpand adiabatically and lose energy via synchrotron and inverse Compton losses,resulting in a steeper radio spectra.Keywords: surveys – radio continuum: general – radio continuum: galaxies – galax-ies: high-redshift
A candidate reference method and multiple commutable control materials for serum 25‐hydroxyvitamin D measurement

The aim of the current study was to establish a reliable candidate reference method for serum 25‐hydroxyvitamin D [25(OH)D] measurement and to assess the commutability of multiple control materials among liquid chromatography–tandem mass spectrometry (LC–MS/MS) methods.
Exploring extra dimensions with scalar waves

This paper provides a pedagogical introduction to the physics of extra dimensions focussing on the ADD, Randall-Sundrum and DGP models. In each of these models, the familiar particles and fields of the standard model are assumed to be confined to a four dimensional space-time called the brane; the brane is a slice through a higher dimensional space-time called the bulk. The geometry of the ADD, Randall-Sundrum and DGP space-times is described and the relation between Randall-Sundrum and Anti-de-Sitter space-time is explained. The necessary differential geometry background is introduced in an appendix that presumes no greater mathematical preparation than multivariable calculus. The ordinary wave equation and the Klein-Gordon equation are briefly reviewed followed by an analysis of the propagation of scalar waves in the bulk in all three extra-dimensional models. We also calculate the scalar field produced by a static point source located on the brane for all three models. For the ADD and Randall-Sundrum models at large distances the field looks like that of a point source in four space-time dimensions but at short distances it crosses over to a form appropriate to the higher dimensional space-time. For the DGP model the field has the higher dimensional form at long distances rather than short. The scalar field results provide qualitative insights into the corresponding behavior of gravitational fields. In particular the explanation within the ADD and Randall-Sundrum model of the weakness of gravity compared to other forces is discussed as are the implications of the two models for colliders and other experiments.
HSC Niche Dynamics in Regeneration, Pre-malignancy, and Cancer: Insights From Mathematical Modeling

Abstract The hematopoietic stem cell (HSC) niche is a crucial driver of regeneration and malignancy. Its interaction with hematopoietic and malignant stem cells is highly complex and direct experimental observations are challenging. We here develop a mathematical model which helps relate processes in the niche to measurable changes of stem and non-stem cell counts. HSC attached to the niche are assumed to be quiescent. After detachment HSC become activated and divide or differentiate. To maintain their stemness, the progeny originating from division must reattach to the niche. We use mouse data from literature to parametrize the model. By combining mathematical analysis and computer simulations, we systematically investigate the impact of stem cell proliferation, differentiation, niche attachment, and detachment on clinically relevant scenarios. These include bone marrow transplantation, clonal competition, and eradication of malignant cells. According to our model, sampling of blood or bulk marrow provides only limited information about cellular interactions in the niche and the clonal composition of the stem cell population. Furthermore, we investigate how interference with processes in the stem cell niche could help to increase the effect of low-dose chemotherapy or to improve the homing of genetically engineered cells.
A UNIFIED EMPIRICAL MODEL FOR INFRARED GALAXY COUNTS BASED ON THE OBSERVED PHYSICAL EVOLUTION OF DISTANT GALAXIES

We reproduce the mid-infrared to radio galaxy counts with a new empirical model based on our current understanding of the evolution of main-sequence (MS) and starburst (SB) galaxies. We rely on a simple spectral energy distribution (SED) library based on Herschel observations: a single SED for the MS and another one for SB, getting warmer with redshift. Our model is able to reproduce recent measurements of galaxy counts performed with Herschel, including counts per redshift slice. This agreement demonstrates the power of our 2-Star-Formation Modes (2SFM) decomposition in describing the statistical properties of infrared sources and their evolution with cosmic time. We discuss the relative contribution of MS and SB galaxies to the number counts at various wavelengths and flux densities. We also show that MS galaxies are responsible for a bump in the 1.4 GHz radio counts around 50 μJy. Material of the model (predictions, SED library, mock catalogs, etc.) is available online.
A DISTINCTIVE DISK–JET COUPLING IN THE LOWEST-MASS SEYFERT, NGC 4395

Simultaneous observations of X-rays and radio luminosities have been well studied in accreting stellar-mass black holes. These observations are performed in order to understand how mass accretion rates and jetted outflows are linked in these individual systems. Such contemporaneous studies in supermassive black holes (SMBH) are harder to perform, as viscous times scale linearly with mass. However, as NGC 4395 is the lowest known mass Seyfert galaxy, we have used it to examine the simultaneous X-ray (Swift) and radio (Very Large Array) correlation in a SMBH in a reasonably timed observing campaign. We find that the intrinsic X-ray variability is stronger than the radio variability, and that the fluxes are only weakly or tentatively coupled, similar to prior results obtained in NGC 4051. If the corona and the base of the jet are one and the same, this may suggest that the corona in radio-quiet active galactic nucleus filters disk variations, only transferring the strongest and/or most sustained variations into the jet. Further, when both NGC 4395 and NGC 4051 are placed on the stellar-mass LX–LR plane, they appear to reside on the steeper LX–LR track. This suggests that SMBHs also follow two distinct tracks just as stellar-mass black holes do, and supports the idea that the same physical disk–jet mechanisms are at play across the mass scale.
Bacterial culture time to detection in platelet components: An evidence synthesis and estimation of detection failures

Non‐pathogen reduction platelet bacterial risk control strategies in the US FDA guidance include at least one culture. Almost all of these strategies have a culture hold time of ≥12 h. Studies have reported time to detection (TTD) of bacterial cultures inoculated with bacteria from contaminated platelets, but these data and estimates of risk associated with detection failures have not been synthesized.
A weak lensing detection of the cosmological distance–redshift relation behind three massive clusters

The amplitude of weak lensing should increase with source distance, rising steeply behind a lens and saturating at high redshift, providing a model-independent means of measuring cosmic geometry. We measure the amplitude of weak lensing with redshift for three massive clusters, A370 (z = 0.375), ZwCl0024+17 (z = 0.395) and RXJ1347−11 (z = 0.451), using deep, three-colour Subaru imaging. We define the depth of lensed populations with reference to the COSMOS and GOODS fields, providing a consistency check of photo-z estimates over a wide range of redshift and magnitude. The predicted distance–redshift relation is followed well for the deepest data set, A370, for a wide range of cosmologies, and is consistent with less accurate data for the other two clusters. Scaling this result to a new survey of ∼25 massive clusters should provide a useful cosmological constraint on w, complementing existing techniques, with distance measurements covering the untested redshift range, 1 < z < 5.
Tomography from the next generation of cosmic shear experiments for viable f(R) models

We present the cosmic shear signal predicted by two viable cosmological models in the framework of modified-action f(R) theories. We use f(R) models where the current accelerated expansion of the Universe is a direct consequence of the modified gravitational Lagrangian rather than Dark Energy (DE), either in the form of vacuum energy/cosmological constant or of a dynamical scalar field (e.g. quintessence). We choose Starobinsky's (St) and Hu & Sawicki's (HS) f(R) models, which are carefully designed to pass the Solar System gravity tests. In order to further support ? or rule out ? f(R) theories as alternative candidates to the DE hypothesis, we exploit the power of weak gravitational lensing, specifically of cosmic shear. We calculate the tomographic shear matrix as it would be measured by the upcoming ESA Cosmic Vision Euclid satellite. We find that in the St model the cosmic shear signal is almost completely degenerate with ? CDM, but it is easily distinguishable in the HS model. Moreover, we compute the corresponding Fisher matrix for both the St and HS models, thus obtaining forecasts for their cosmological parameters. Finally, we show that the Bayes factor for cosmic shear will definitely favour the HS model over ? CDM if Euclid measures a value larger than ~ 0.02 for the extra HS parameter nHS.
Symbolic Verification and Strategy Synthesis for Turn-based Stochastic Games

Stochastic games are a convenient formalism for modelling systems that comprise rational agents competing or collaborating within uncertain environments. Probabilistic model checking techniques for this class of models allow us to formally specify quantitative specifications of either collective or individual behaviour and then automatically synthesise strategies for the agents under which these specifications are guaranteed to be satisfied. Although good progress has been made on algorithms and tool support, efficiency and scalability remain a challenge. In this paper, we investigate a symbolic implementation based on multi-terminal binary decision diagrams. We describe how to build and verify turn-based stochastic games against either zero-sum or Nash equilibrium based temporal logic specifications. We collate a set of benchmarks for this class of games, and evaluate the performance of our approach, showing that it is superior in a number of cases and that strategies synthesised in a symbolic fashion can be considerably more compact.
Online Signal Recovery via Heavy Ball Kaczmarz

Recovering a signal $x^{\ast}\in \mathbb{R}^{n}$ from a sequence of linear measurements is an important problem in areas such as computerized tomography and compressed sensing. In this work, we consider an online setting in which measurements are sampled one-by-one from some source distribution. We propose solving this problem with a variant of the Kaczmarz method with an additional heavy ball momentum term. A popular technique for solving systems of linear equations, recent work has shown that the Kaczmarz method also enjoys linear convergence when applied to random measurement models, however convergence may be slowed when successive measurements are highly coherent. We demonstrate that the addition of heavy ball momentum may accelerate the convergence of the Kaczmarz method when data is coherent, and provide a theoretical analysis of the method culminating in a linear convergence guarantee for a wide class of source distributions.
The neutron skin thickness from the measured electric dipole polarizability in 68Ni, 120Sn, and 208Pb

The information on the symmetry energy and its density dependence is deduced by comparing the available data on the electric dipole polarizability αD of 68Ni, 120Sn, and 208Pb with the predictions of the random-phase approximation, using a representative set of nuclear energy density functionals. The calculated values of αD are used to validate different correlations involving αD, the symmetry energy at the saturation density J , the corresponding slope parameter L, and the neutron skin thickness rnp, as suggested by the droplet model. A subset of models that reproduce simultaneously the measured polarizabilities in 68Ni, 120Sn, and 208Pb are employed to predict the values of the symmetry energy parameters at saturation density and rnp. The resulting intervals are J =30-35 MeV, L=20-66 MeV; and the values for rnp in 68Ni, 120Sn, and 208Pb are in the ranges 0.15-0.19, 0.12-0.16, and 0.13-0.19 fm, respectively. The strong correlation between the electric dipole polarizabilities of two nuclei is instrumental to predict the values of electric dipole polarizabilities in other nuclei.
Optimal regularity and fine asymptotics for the porous medium equation in bounded domains

We prove the optimal global regularity of nonnegative solutions to the porous medium equation in smooth bounded domains with the zero Dirichlet boundary condition after certain waiting time $T^*$. More precisely, we show that solutions are $C^{2,\alpha}(\overline\Omega)$ in space, with $\alpha=\frac1m$, and $C^\infty$ in time (uniformly in $x\in \overline\Omega$), for $t>T^*$. Furthermore, this allows us to refine the asymptotics of solutions for large times, improving the best known results so far in two ways: we establish a faster rate of convergence $O(t^{-1-\gamma})$, and we prove that the convergence holds in the $C^{1,\alpha}(\overline\Omega)$ topology.
Field line subdiffusion and cosmic ray perpendicular transport in isotropic turbulence

The transport of high-energy particles in the presence of small-scale, turbulent magnetic fields is a long-standing issue in astrophysics. Analytical theories disagree with numerical simulations at rigidities where the particles' gyroradii are slightly smaller than the correlation length of turbulence. At the same time, extending the numerical simulations to lower rigidities has proven computationally prohibitive. In this letter, we provide a solution to the problem of perpendicular transport in isotropic turbulence at both, high and low rigidities. We also clarify the relation between the perpendicular diffusion of particles and the transport of magnetic field lines. To this end, we have run a large suite of test particle simulations at unprecedentedly low rigidites, making extensive use of graphical processing units (GPUs). We have also developed an analytical model, based on (1) initial particle transport along field lines, (2) the transport of field lines and (3) the eventual decorrelation of particles from field lines. Our numerical results exhibit a non-standard rigidity-dependence for the perpendicular diffusion coefficient at intermediate rigidites. At the lowest rigidities, the standard rigidity-dependence is recovered. The simulated diffusion coefficients are nicely reproduced by our analytical model. We have traced the non-standard rigidity-dependence to a subdiffusive phase in the field line transport. Our study has important implications for the transport of Galactic cosmic rays, acceleration at perpendicular shocks and for high-energy particles in the heliosphere.