Miracle-dz/UniFAR-FTUs huggingface dataset:
Neutrino-driven winds from neutron star merger remnants

We present a detailed, three-dimensional hydrodynamic study of the neutrino-driven winds that emerge from the remnant of a neutron star merger. Our simulations are performed with the Newtonian, Eulerian code FISH, augmented by a detailed, spectral neutrino leakage scheme that accounts for heating due to neutrino absorption in optically thin conditions. Consistent with the earlier, two-dimensional study of Dessart et al. (2009), we nd that a strong baryonic wind is blown out along the original binary rotation axis within 100 milliseconds after the merger. We compute a lower limit on the expelled mass of 3:5 10 3 M , large enough to be relevant for heavy element nucleosynthesis. The physical properties vary signicantly between dierent wind regions. For example, due to stronger neutrino irradiation, the polar regions show substantially larger electron fractions than those at lower latitudes. This has its bearings on the nucleosynthesis: the polar ejecta produce interesting r-process contributions from A 80 to about 130, while the more neutron-rich, lower-latitude parts produce in addition also elements up to the third r-process peak near A 195. We also calculate the properties of electromagnetic transients that are powered by the radioactivity in the wind, in addition to the \macronova" transient that stems from the dynamic ejecta. The high-latitude (polar) regions produce UV/optical transients reaching luminosities up to 10 41 erg s 1 , which peak around 1 day in optical and 0.3 days in bolometric luminosity. The lower-latitude regions, due to their contamination with high-opacity heavy elements, produce dimmer and more red signals, peaking after 2 days in optical and infrared. Our numerical experiments indicate that it will be dicult to infer the collapse time-scale of the hypermassive neutron star to a black hole based on the wind electromagnetic transient, at least for collapse time-scales larger than the wind production time-scale.
Magnetic field effects on transport properties of PtSn4

The anisotropic physical properties of single crystals of orthorhombic PtSn{sub 4} are reported for magnetic fields up to 140 kOe, applied parallel and perpendicular to the crystallographic b axis. The magnetic susceptibility has an approximately temperature-independent behavior and reveals an anisotropy between the ac plane and b axis. Clear de Haas-van Alphen oscillations in fields as low as 5 kOe and at temperatures as high as 30 K were detected in magnetization isotherms. The thermoelectric power and resistivity of PtSn{sub 4} show the strong temperature and magnetic field dependencies. A change of the thermoelectric power at H=140 kOe is observed as high as ≃50 μV/K. Single crystals of PtSn{sub 4} exhibit very large transverse magnetoresistance of ≃5×10{sup 5}% for the ac plane and of ≃1.4×10{sup 5}% for the b axis resistivity at 1.8 K and 140 kOe, as well as pronounced Shubnikov de Haas oscillations. The magnetoresistance of PtSn{sub 4} appears to obey Kohler's rule in the temperature and field range measured. The Hall resistivity shows a linear temperature dependence at high temperatures followed by a sign reversal around 25 K which is consistent with thermoelectric power measurements. The observed quantum oscillations and band structure calculations indicate that PtSn{sub 4}more » has three-dimensional Fermi surfaces. « less
Variable accretion rates and fluffy first stars

We combine the output of hydrodynamical simulations of Population III star cluster formation with stellar evolution models, and calculate the evolution of protostars experiencing variable mass accretion rates due to interactions within a massive disc. We find that the primordial protostars are extended ‘fluffy’ objects for the bulk of their pre-main-sequence lifetimes. Accretion luminosity feedback from such objects is high, but, as shown in previous work, it has a minimal effect on the star cluster. The extended radii of the protostars, combined with the observation of close encounters in the simulations, suggest that mergers will occur in such systems. Furthermore, mass transfer between close protostellar binaries with extended radii could lead to massive tight binaries, which are a possible progenitor of gamma-ray bursts.
Probing the anisotropic local Universe and beyond with SNe Ia data

The question of the transition to global isotropy from our anisotropic local universe is studied using the Union 2 catalogue of Type Ia supernovae (SNe Ia). We construct a ‘residual’ statistic sensitive to systematic shifts in their brightness in different directions and use this to search in different redshift slices for a preferred direction on the sky in which the SNe Ia are brighter or fainter relative to the standard Λcold dark matter (ΛCDM) cosmology. At low redshift (z 0.06) so this low-redshift bulk flow will systematically bias any reconstruction of the expansion history of the Universe. At higher redshifts z > 0.15 the agreement between the SNe Ia data and the ΛCDM model does improve, however, the sparseness and low quality of the data mean that the latter cannot be singled out as the preferred cosmological model.
Impact of cosmological satellites on the vertical heating of the Milky Way disc

We present a high resolution study of the impact of realistic satellite galaxies, extracted from cosmological simulations of Milky Way haloes including 6 Aquarius suites and Via Lactea \rom{2}, on the dynamics of the galactic disc. The initial conditions for the multi-component Milky Way galaxy were generated using the GalIC code, to ensure a system in dynamical equilibrium state prior to addition of satellites. Candidate subhaloes that came closer than 25\,kpc to the centre of the host DM haloes with initial mass enclosed within the tidal radius, $M_\textrm{tid}$ $\ge$ 10$^{8} M_{\odot}$\,=\,0.003 $M_\textrm{disc}$, were identified, inserted into our high resolution N-body simulations and evolved for 2 Gyr. We quantified the vertical heating due to such impacts by measuring the disc thickness and squared vertical velocity dispersion $\sigma_{z}^{2}$ across the disc. According to our analysis the strength of heating is strongly dependent on the high mass end of the subhalo distribution from cosmological simulations. The mean increase of the vertical dispersion is $\sim$ 20\,km$^{2}$\,s$^{-2}$\,Gyr$^{-1}$ for R $>$ 4\,kpc with a flat radial profile while, excluding Aq-F2 results, the mean heating is $<$ 12\,km$^{2}$\,s$^{-2}$\,Gyr$^{-1}$, corresponding to 28\% and 17\% of the observed vertical heating rate in the solar neighbourhood. Taking into account the statistical dispersion around the mean we miss the observed heating rate by more than 3$\sigma$. We observed a general flaring of the disc height in the case of all 7 simulations in the outer disc.
THE SECOND ARECIBO SEARCH FOR 5 GHz RADIO FLARES FROM ULTRACOOL DWARFS

We describe our second installment of the 4.75 GHz survey of ultracool dwarfs (UCDs) conducted with the Arecibo radio telescope, which has observed 27 such objects and resulted in the detection of sporadic flaring from the T6 dwarf, WISEPC J112254.73+255021.5. We also present follow-up observations of the first radio-emitting T dwarf, 2MASS J10475385+2124234, a tentatively identified radio-emitting L1 dwarf, 2MASS J1439284+192915, and the known radio-flaring source, 2MASS J13142039+132011 AB. Our new data indicate that 2MASS J1439284+192915 is not a radio-flaring source. The overall detection rate of our unbiased survey for radio-flaring UCDs is ∼5% for new sources, with a detection rate for each spectral class of ∼5%–10%. Evidently, radio luminosity of the UCDs does not appear to monotonically decline with spectral type from M7 dwarfs to giant planets, contradictory to theories of the magnetic field generation and the internal structure of these objects. Along with other, recently published results, our data exemplify the unique value of using radio surveys to reveal and study properties of substellar magnetic activity.
Non-asymptotical sharp exponential estimates for maximum distribution of discontinuous random fields

We offer in this paper the non-asymptotical bilateral sharp exponential estimates for tail of maximum distribution of {\it discontinuous} random fields. Our consideration based on the theory of Prokhorov-Skorokhod spaces of random fields and on the theory of multivariate Banach spaces of random variables with exponential decreasing tails of distributions.
THE LOST DWARFS OF CENTAURUS A AND THE FORMATION OF ITS DARK GLOBULAR CLUSTERS

We present theoretical constraints for the formation of the newly discovered dark star clusters (DSCs) with high mass-to-light ( ) ratios, from Taylor et al. These compact stellar systems photometrically resemble globular clusters (GCs) but have dynamical ratios of ∼10–100, closer to the expectations for dwarf galaxies. The baryonic properties of the DSCs suggest that their host dark matter halos likely virialized at high redshift with . We use a new set of high-resolution N-body simulations of Centaurus A to determine whether there is a set of z = 0 subhalos whose properties are in line with these observations. While we find such a set of subhalos, when we extrapolate the dark matter density profiles into the inner 20 pc, no dark matter halo associated with Centaurus A in our simulations, at any redshift, can replicate the extremely high central mass densities of the DSCs. Among the most likely options for explaining 105– within subhalos of 10 pc diameter is the presence of a central massive black hole (BH). We therefore propose that the DSCs are remnant cusps of stellar systems surrounding the central BHs of dwarf galaxies that have been almost completely destroyed by interactions with Centaurus A.
Constructing monotones for quantum phase references in totally dephasing channels

Restrictions on quantum operations give rise to resource theories. Total lack of a shared reference frame for transformations associated with a group G between two parties is equivalent to having, in effect, an invariant channel between the parties and a corresponding superselection rule. The resource associated with the absence of the reference frame is known as ''frameness'' or ''asymmetry. '' We show that any entanglement monotone for pure bipartite states can be adapted as a pure-state frameness monotone for phase-invariant channels [equivalently U(1) superselection rules] and extended to the case of mixed states via the convex-roof extension. As an application, we construct a family of concurrence monotones for U(1) frameness for general finite-dimensional Hilbert spaces. Furthermore, we study ''frameness of formation'' for mixed states analogous to entanglement of formation. In the case of a qubit, we show that it can be expressed as an analytical function of the concurrence analogously to the Wootters formula for entanglement of formation. Our results highlight deep links between entanglement and frameness resource theories.
TOWARD A BETTER UNDERSTANDING OF THE DISTANCE SCALE FROM RR LYRAE VARIABLE STARS: A CASE STUDY FOR THE INNER HALO GLOBULAR CLUSTER NGC 6723

We present BV photometry for 54 variables in the metal-rich inner halo globular cluster NGC 6723. With the discovery of new RR Lyrae variables (RRLs), we obtain 〈Pab〉 = 0.541 ± 0.066 and 〈Pc〉 = 0.292 ± 0.030 day, n(c)/n(ab+c) = 0.167, and 〈V(RR)〉int = 15.459 ± 0.055. We carry out the Fourier decomposition analysis and obtain [Fe/H]ZW = −1.23 ± 0.11 and E(B − V) = 0.063 ± 0.015 for NGC 6723. By calibrating the zero point from the recent absolute trigonometric parallax measurements for RR Lyr, we derive the revised MV(RR)-[Fe/H] relation, providing MV(RR) = 0.52 at [Fe/H] = −1.50 and (m − M)0 = 18.54 for the Large Magellanic Cloud, in excellent agreement with others. We obtain (m − M)0 = 14.65 ± 0.05, equivalent to a distance from the Sun of 8.47 ± 0.17 kpc, for NGC 6723 from various distance measurement methods using RRLs. We find that RRLs in NGC 6723 do not have magnitude dependency on the radial distance because there is not a severe degree of apparent crowdedness. Finally, we show that a relation exists between the degree of photometric contamination and the apparent crowdedness of the central region of globular cluster systems, . The use of this relation can play a significant role in mitigating the discrepancy in establishing a cosmic distance scale using RRLs in resolved stellar populations in near-field cosmology.
Dark Matter Phase Transition Constrained at O(0.1) eV with LSB Rotation Curves

In order to unravel the nature of the dark matter (DM) we have proposed a particle-physics motivated model called Bound Dark Matter (BDM) that consist in DM massless particles above a threshold energy Ec that acquire mass below it due to nonperturbative methods. Therefore, the BDM model describes DM particles which are relativistic, hot dark matter (HDM) in the denser (inner) regions of galaxies and describes nonrelativistic, cold dark matter (CDM) where halo density is below rho_c = Ec^4. We test this model by fitting rotation curves from Low Surface Brightness (LSB) galaxies from The HI Nearby Galaxy Survey (THINGS). We use a particular DM cored profile that contains three parameters: a typical scale length (rs) and density (rho_0) of the halo, and a core radius (rc) stemming from the relativistic nature of the BDM model. Since the energy Ec parameterizes the phase transition due to the underlying particle physics model, it is independent on the details of galaxy and/or structure formation and therefore the DM profile parameters rs, rc, Ec are constrained, leaving only two free parameters. Through the results we agree with previous ones implying that cored profiles are preferred over the N-body motivated cuspy profiles. We also compute 2D likelihoods of the BDM parameters rc and Ec for the different galaxies and matter contents, and find an average galaxy core radius rc = 1.48kpc and a transition energy between hot and cold dark matter at Ec = 0.06 eV. The phase transition scale Ec is a new fundamental scale for our DM model well motivated theoretical origin from gauge group dynamics.
Study of D+ →k-π+e+νe

We present an analysis of the decay D+→K-π+e+νe based on data collected by the BESIII experiment at the ψ(3770) resonance. Using a nearly background-free sample of 18262 events, we measure the branching fraction B(D+→K-π+e+νe)=(3.77±0.03±0.08)%. For 0.8<mKπ<1.0 GeV/c2, the partial branching fraction is B(D+→K-π+e+νe)[0.8,1.0]=(3.39±0.03±0.08)%. A partial wave analysis shows that the dominant K¯*(892)0 component is accompanied by an S-wave contribution accounting for (6.05±0.22±0.18)% of the total rate and that other components are negligible. The parameters of the K¯*(892)0 resonance and of the form factors based on the spectroscopic pole dominance predictions are also measured. We also present a measurement of the K¯*(892)0 helicity basis form factors in a model-independent way.
Properties of Galactic early-type O-supergiants - A combined FUV-UV and optical analysis

We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from O4 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Using the non-LTE wind code CMFGEN, we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 Msun, while the O5 to O7.5 stars have masses in the range 50 - 40 Msun and are 4 +/- 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 +/- 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.
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Artificial intelligence (AI) enables continuous monitoring of patients’ health, thus improving the quality of their health care. However, prior studies suggest that individuals resist such innovative technology. In contrast to prior studies that investigate individuals’ decisions for themselves, we focus on family members’ rejection of AI monitoring, as family members play a significant role in health care decisions. Our research investigates competing effects of emotions toward the rejection of AI monitoring for health care. Based on two scenario-based experiments, our study reveals that emotions play a decisive role in family members’ decision making on behalf of their parents. We find that anxiety about health care monitoring and anxiety about health outcomes reduce the rejection of AI monitoring, whereas surveillance anxiety and delegation anxiety increase rejection. We also find that for individual-level risks, perceived controllability moderates the relationship between surveillance anxiety and the rejection of AI monitoring. We contribute to the theory of Information System rejection by identifying the competing roles of emotions in AI monitoring decision making. We extend the literature on decision making for others by suggesting the influential role of anxiety. We also contribute to health-care research in Information System by identifying the important role of controllability, a design factor, in AI monitoring rejection.
Climbing NLO and NNLO Summits of Weak Decays

I describe the history of the calculations of NLO and NNLO QCD corrections to weak decays of mesons and particle-antiparticle mixing in the period 1988–2010. Also existing calculations of electroweak and QED corrections to these processes are included in this presentation. These efforts bear some analogies to the climbing of Himalayas and various expeditions by several teams of strongly motivated “climbers”, acting mainly in Germany, Italy, Poland and Switzerland, allowed to move this field from the LO through the NLO to the NNLO level. The material is meant to be a guide to the rich literature on NLO and NNLO corrections in question and includes several anecdotes related to the climbs that I was involved in. While, by no means this presentation should be regarded as a review of the size of NLO and NNLO corrections to weak decays, I hope that some of the comments made in the course of the presentation could turn out to be not only amusing but also instructive.
A multiwavelength study of near- and mid-infrared selected galaxies at high redshift: ERGs, AGN-identification and the contribution from dust

The main focus of this thesis is the IR spectral regime, which since the 70's and 80's has revolutionised our understanding of the Universe. A multi-wavelength analysis on Extremely Red Galaxy populations is first presented in one of the most intensively observed patch of the sky, the Chandra Deep Field South. By adopting a purely statistical methodology, we consider all the photometric and spectroscopic information available on large samples of Extremely Red Objects (EROs, 553 sources), IRAC EROs (IEROs, 259 sources), and Distant Red Galaxies (DRGs, 289 sources). We derive general properties: redshift distributions, AGN host fraction, star-formation rate densities, dust content, morphology, mass functions and mass densities. The results point to the fact that EROs, IEROs, and DRGs all belong to the same population, yet seen at different phases of galaxy evolution. The second part of this thesis is dedicated to the AGN selection in the IR, with particular relevance to the James Webb Space Telescope, to be launched in 2018. We develop an improved IR criterion (using K and IRAC bands) as an alternative to existing IR AGN criteria for the z<2.5 regime, and develop another IR criterion which reliably selects AGN hosts at 0<z<7 (using K, Spitzer-IRAC, and Spitzer-MIPS24um bands, KIM). The ability to track AGN activity since the end of reionization holds great advantages for the study of galaxy evolution. The thesis then focus on the importance of dust. Based on deep IR data on the Cosmological Survey, we derive rest-frame 1.6, 3.3, and 6.2um luminosity functions and their dependency on redshift. We estimate the dust contribution to those wavelengths and show that the hot dust luminosity density evolves since z=1-2 with a much steeper drop than the star-formation history of the Universe. Future prospects are finally discussed in the last chapter.
Three Manifold Mutations Detected by Heegaard Floer Homology

Given a self-diffeomorphism φ of a closed, orientable surface S with genus greater than one and an embedding f of S into a threemanifold M , we construct a mutant manifold by cutting M along f(S) and regluing by fφf−1. We will consider whether there exist nontrivial gluings such that for any embedding, the manifold M and its mutant have isomorphic Heegaard Floer homology. In particular, we will demonstrate that if φ is not isotopic to the identity map, then there exists an embedding of S into a three-manifold M such that the rank of the non-torsion summands of ĤF of M differs from that of its mutant. We will also show that if the gluing map is isotopic to neither the identity nor the genus-two hyperelliptic involution, then there exists an embedding of S into a three-manifold M such that the total rank of ĤF of M differs from that of its mutant.
Improved Cosmic-Ray Injection Models and the Galactic Center Gamma-Ray Excess

Fermi-LAT observations of the Galactic Center (GC) have revealed a spherically- symmetric excess of GeV gamma rays extending to at least 10 deg from the dynamical center of the Galaxy. A critical uncertainty in extracting the intensity, spectrum, and morphology of this excess concerns the accuracy of astrophysical diffuse gamma-ray emission models near the GC. Recently, it has been noted that many diffuse emission models utilize a cosmic-ray injection rate far below that predicted based on the observed star formation rate in the Central Molecular Zone. In this study, we add a cosmic-ray injection component which non-linearly traces the Galactic H2 density determined in three-dimensions, and find that the associated gamma-ray emission is degenerate with many properties of the GC gamma-ray excess. In models that utilize a large sideband (40x40 deg surrounding the GC) to normalize the best-fitting diffuse emission models, the intensity of the GC excess decreases by a factor of 2, and the morphology of the excess becomes less peaked and less spherically symmetric. In models which utilize a smaller region of interest (15x15 deg) the addition of an excess template instead suppresses the intensity of the best-fit astrophysical diffuse emission, and the GC excess is rather resilient to changes in the details of the astrophysical diffuse modeling. In both analyses, the addition of a GC excess template still provides a statistically significant improvement to the overall fit to the gamma-ray data. We also implement advective winds at the GC, and find that the Fermi-LAT data strongly prefer outflows of order several hundred km/s, whose role is to efficiently advect low-energy cosmic rays from the Galactic center. Finally, we perform numerous tests of our models, and conclude that they significantly improve our understanding of multi-wavelength non-thermal emission from the GC.