Miracle-dz/UniFAR-FTUs huggingface dataset:
Simulating gyrokinetic microinstabilities in stellarator geometry with GS2

The nonlinear gyrokinetic code GS2 has been extended to treat non-axisymmetric stellarator geometry. Electromagnetic perturbations and multiple trapped particle regions are allowed. Here, linear, collisionless, electrostatic simulations of the quasi-axisymmetric, three-field period national compact stellarator experiment (NCSX) design QAS3-C82 have been successfully benchmarked against the eigenvalue code FULL. Quantitatively, the linear stability calculations of GS2 and FULL agree to within ∼10%.
Multi-frequency VLBA Polarimetry of the high-redshift GPS Quasar OQ172

Multi-frequency Very Long Baseline Array (VLBA) polarimetry observation of the GHz-Peaked Spectrum (GPS) quasar OQ172 (J1445+0958) has been performed at 1.6, 2.2, 4.8, 8.3 and 15.3 GHz in 2005. Core-jet structures are detected in all bands with the jet strongly bent at about 3 mas from the core. The radio emission of the source is polarised at all five bands. We study the Faraday Rotation in the core and jet components at all five bands, and find good linear fits of Faraday Rotation in the core and jet components at 4.8 and 8.3 GHz. At these two frequencies, the Rotation Measure (RM) is $\sim 2000~\rm rad~m^{-2}$ in the core and $\sim 700~\rm rad~m^{-2}$ in the inner jet components and continues to decrease at the outer jet parts. We find that the depolarisation at 4.8 and 8.3 GHz might be caused by the internal medium in the source. We investigate consistency of the turnover spectra of VLBI components with the Synchrotron Self-Absorption (SSA) and Free-Free Absorption (FFA) models. Although these two models can not be easily distinguished due to the lack of low-frequency data, the physical parameters can be constrained for each model. We find that the large width of the $\rm [OIII]_{5007}$ line is likely caused by a jet interaction with a Narrow Line Region (NLR) medium. The jet bending, significant RM variations, Faraday depolarisation, spectral turnover, and broad line width of $\rm [OIII]_{5007}$ could be closely related, likely caused by the same nucleus medium, presumably NLR.
FIRST SPECTROSCOPIC MEASUREMENTS OF [O iii] EMISSION FROM Lyα SELECTED FIELD GALAXIES AT z ∼ 3.1,

We present the first spectroscopic measurements of the [O iii] 5007 Å line in two z ∼ 3.1 Lyα emitting galaxies (LAEs) using the new near-infrared instrument LUCIFER1 on the 8.4 m Large Binocular Telescope. We also describe the optical imaging and spectroscopic observations used to identify these LAEs. Using the [O iii] line we have measured accurate systemic redshifts for these two galaxies, and discovered a velocity offset between the [O iii] and Lyα lines in both, with the Lyα line peaking 342 and 125 km s-1 redward of the systemic velocity. These velocity offsets imply that there are powerful outflows in high-redshift LAEs. They also ease the transmission of Lyα photons through the interstellar medium and intergalactic medium around the galaxies. By measuring these offsets directly, we can refine both Lyα-based tests for reionization, and Lyα luminosity function measurements where the Lyα forest affects the blue wing of the line. Our work also provides the first direct constraints on the strength of the [O iii] line in high-redshift LAEs. We find [O iii] fluxes of 7 and 36 ×10−17 erg s−1 cm−2 in two z ∼ 3.1 LAEs. These lines are strong enough to dominate broadband flux measurements that include the line (in this case, Ks-band photometry). Spectral energy distribution fits that do not account for the lines would therefore overestimate the 4000 Å (and/or Balmer) break strength in such galaxies, and hence also the ages and stellar masses of such high-z galaxies.
The first Galaxy scale hunt for the youngest high-mass protostars

The origin of massive stars is a fundamental open issue in modern astrophysics. Pre-ALMA interferometric studies reveal precursors to early B to late O type stars with collapsing envelopes of 15-20 M$_\odot$ on 1000-3000 AU size-scales. To search for more massive envelopes we selected the most massive nearby young clumps from the ATLASGAL survey to study their protostellar content with ALMA. Our first results using the intermediate scales revealed by the ALMA ACA array providing 3-5" angular resolution, corresponding to $\sim$0.05-0.1 pc size-scales, reveals a sample of compact objects. These massive dense cores are on average two-times more massive than previous studies of similar types of objects. We expect that once the full survey is completed, it will provide a comprehensive view on the origin of the most massive stars.
Mass and concentration estimates from weak and strong gravitational lensing: a systematic study

We study how well halo properties of galaxy clusters, like mass and concentration, are recovered using lensing data. In order to generate a large sample of systems at dierent redshifts we use the code MOKA. We measure halo mass and concentration using weak lensing data alone (WL), best fitting with a NFW profile the reduced tangential shear profile, or combining it with strong lensing data, by using the information about the size of the Einstein ring (WL+SL). For dierent redshifts, we measure the mass and the concentration bias finding that these are mainly caused by the random orientation of the halo ellipsoid with respect to the line-of-sight. Since our simulations account for the presence of a bright central galaxy, we perform mass and concentration measurements using a generalized NFW profile which allows for a free inner slope. This reduces both the mass and the concentration biases but introduces an additional free parameter. We discuss how the mass function and the concentration mass relation change when using WL and WL+SL estimates. Finally, we investigate how selection eects impact the measured concentration-mass relation showing that strong lens clusters may have a concentration 20 30% higher than the average, at fixed mass, considering also the particular case of strong lensing selected samples of relaxed clusters.
The PAH Emission Characteristics of the Reflection Nebula NGC 2023

We present 5–20 μm spectral maps of the reflection nebula NGC 2023 obtained with the Infrared Spectrograph SL and SH modes on board the Spitzer Space Telescope, which reveal emission from polycyclic aromatic hydrocarbons (PAHs), C60, and H2 superposed on a dust continuum. We show that several PAH emission bands correlate with each other and exhibit distinct spatial distributions that reveal a spatial sequence with distance from the illuminating star. We explore the distinct morphology of the 6.2, 7.7, and 8.6 μm PAH bands and find that at least two spatially distinct components contribute to the 7–9 μm PAH emission in NGC 2023. We report that the PAH features behave independently of the underlying plateaus. We present spectra of compact, oval PAHs ranging in size from C66 to C210, determined computationally using density functional theory, and we investigate trends in the band positions and relative intensities as a function of PAH size, charge, and geometry. Based on the NASA Ames PAH database, we discuss the 7–9 μm components in terms of band assignments and relative intensities. We assign the plateau emission to very small grains with possible contributions from PAH clusters and identify components in the 7–9 μm emission that likely originate in these structures. Based on the assignments and the observed spatial sequence, we discuss the photochemical evolution of the interstellar PAH family as the PAHs are more and more exposed to the radiation field of the central star in the evaporative flows associated with the Photo-Dissociation Regions in NGC 2023.
Ratio of black hole to galaxy mass of an extremely red dust-obscured galaxy at z = 2.52

We present a near-infrared (NIR) spectrum of WISE J104222.11+164115.3, an extremely red dust-obscured galaxy (DOG), which has been observed with the Long-slit Intermediate Resolution Infrared Spectrograph (LIRIS) on the 4.2m William Hershel Telescope. This object was selected as a hyper-luminous DOG candidate at z ∼ 2 by combining the optical and IR photometric data based on the Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE), although its redshift had not yet been confirmed. Based on the LIRIS observation, we confirmed its redshift of 2.521 and total IR luminosity of log(LIR/L⊙) = 14.57, which satisfies the criterion for an extremely luminous IR galaxy (ELIRG). Moreover, we indicate that this object seems to have an extremely massive black hole with MBH = 1010.92 M⊙ based on the broad Hα line: the host stellar mass is derived as M⋆ = 1013.55 M⊙ by a fit of the spectral energy distribution. Very recently, it has been reported that this object is an anomalous gravitationally lensed quasar based on near-IR high-resolution imaging data obtained with the Hubble Space Telescope. Its magnification factor has also been estimated with some uncertainty (i.e., μ = 53−122). We investigate the ratio of the black hole to galaxy mass, which is less strongly affected by a lensing magnification factor, instead of the absolute values of the luminosities and masses. We find that the MBH/M⋆ ratio (i.e., 0.0140–0.0204) is significantly higher than the local relation, following a sequence of unobscured quasars instead of obscured objects (e.g., submillimeter galaxies) at the same redshift. Moreover, the LIRIS spectrum shows strongly blueshifted oxygen lines with an outflowing velocity of ∼1100 km s−1, and our Swift X-ray observation also supports that this source is an absorbed AGN with an intrinsic column density of NHint = 4.9 × 1023 cm−2. These results imply that WISE J104222.11+164115.3 is in a blow-out phase at the end of the buried rapid black hole growth.
NEUTRINO TRANSFER IN THREE DIMENSIONS FOR CORE-COLLAPSE SUPERNOVAE. I. STATIC CONFIGURATIONS

We develop a numerical code to calculate the neutrino transfer with multi-energy and multi-angle in three dimensions (3D) for the study of core-collapse supernovae. The numerical code solves the Boltzmann equations for neutrino distributions by the discrete-ordinate (Sn) method with a fully implicit differencing for time advance. The Boltzmann equations are formulated in the inertial frame with collision terms being evaluated to the zeroth order of v/c. A basic set of neutrino reactions for three neutrino species is implemented together with a realistic equation of state of dense matter. The pair process is included approximately in order to keep the system linear. We present numerical results for a set of test problems to demonstrate the ability of the code. The numerical treatments of advection and collision terms are validated first in the diffusion and free-streaming limits. Then we compute steady neutrino distributions for a background extracted from a spherically symmetric, general relativistic simulation of a 15 M☉ star and compare them with the results in the latter computation. We also demonstrate multi-dimensional capabilities of the 3D code solving neutrino transfers for artificially deformed supernova cores in 2D and 3D. Formal solutions along neutrino paths are utilized as exact solutions. We plan to apply this code to the 3D neutrino-radiation hydrodynamics simulations of supernovae. This is the first article in a series of reports on the development.
Nucleon electromagnetic form factors at high $Q^2$ from Wilson-clover fermions

We present results on the nucleon electromagnetic form factors from Lattice QCD at momentum transfer up to about $12$~GeV$^2$. We analyze two gauge ensembles with the Wilson-clover fermion action, a lattice spacing of $a\approx 0.09$~fm and pion masses $m_\pi\approx 170$~MeV and $m_\pi\approx 280$~MeV. In our analysis we employ momentum smearing as well as a set of techniques to investigate excited state effects. Good agreement with experiment and phenomenology is found for the ratios $G_E/G_M$ and $F_2/F_1$, whereas discrepancies are observed for the individual form factors $F_1$ and $F_2$. We discuss various systematics that may affect our calculation.
An XMM-Newton spatially-resolved study of metal abundance evolution in distant galaxy clusters

Context. We present an XMM-Newton analysis of the X-ray spectra of 39 clusters of galaxies at 0.4 2�) abundance evolution with redshift. The most significant de viation from no evolution (at a 90% confidence level) is observed by consid ering the emission from the whole cluster (r < 0.6r500), which can be parametrized as Z ∝ (1 + z) −0.8±0.5 . Dividing the emission into three radial bins, no significan t evidence of abundance evolution is observed when fitting the data with a power law. We find close agreement with measurements presented in previous studies. Computing the error-weighted mean of the spatially resolved abundances into three redshift bins, we find that it is consi stent with being constant with redshift. Although the large error bars in the measurement of the weighted-mean abundance prevent us from claiming any statistically significant spatially resolved evolution, the trend with z in the 0.15-0.4r500 radial bin complements nicely the measures of Maughan et al., and broadly agrees with theoretical predictions. We also find that the data points derived from the spatially resolved analysis are well-fitted by the relation Z(r, z) = Z0(1 + (r/0.15r500) 2 ) −a ((1 + z)/1.6) − , where Z0 = 0.36± 0.03, a = 0.32± 0.07, and = 0.25± 0.57, which represents a significant negative trend of Z with radius and no significant evolution with redshift. Conclusions. We present the first attempt to determine the evolution of abu ndance at different positions in the clusters and with redshift. However, the sample size and the low-quality data statistics associated with most of the clusters studied pre vents us from drawing any statistically significant conclusion about the different evolutionary path that the different regions of t he clusters may have traversed.
The star-forming progenitors of massive red galaxies

The link between massive red galaxies in the local Universe and star-forming galaxies at high redshift is investigated with a semi-analytic model that has proven successful in many ways, e.g. explaining the galaxy colour-magnitude bimodality and the stellar mass-age relation for red-sequence galaxies. The model is used to explore the processes that drive star formation in different types of galaxies as a function of stellar mass and redshift. We find that most z = 2 4 star-forming galaxies with M∗ > 10 10 M⊙ evolve into red-sequence galaxies. Also, most of the massive galaxies on the red-sequence today have passed through a phase of intense star formation at z > 2. Specifically, � 90% of today’s red galaxies with M∗ > 10 11 M⊙ were fed during this phase by cold streams including minor mergers. Gas-rich major mergers are rare and the effects of merger-driven starbursts are ephemeral. On the other hand, major mergers are important in powering the most extreme starbursts. Gas-rich mergers also explain the tail of intermediate-mass red galaxies that form relatively late, after the epoch of peak star formation. In two thirds of the currently red galaxies that had an intense star formation event at z < 1, this event was triggered by a merger.
2004 TT357: A Potential Contact Binary in the Trans-Neptunian Belt

We report photometric observations of the trans-Neptunian object 2004 TT357 obtained in 2015 and 2017 using the 4.3 m Lowell’s Discovery Channel Telescope. We derive a rotational period of 7.79 ± 0.01 hr and a peak-to-peak lightcurve amplitude of 0.76 ± 0.03 mag. 2004 TT357 displays a large variability that can be explained by a very elongated single object or can be due to a contact/close binary. The most likely scenario is that 2004 TT357 is a contact binary. If it is in hydrostatic equilibrium, we find that the lightcurve can be explained by a system with a mass ratio qmin = 0.45 ± 0.05, and a density of ρmin = 2 g cm−3, or less likely a system with qmax = 0.8 ± 0.05, and ρmax = 5 g cm−3. Considering a single triaxial ellipsoid in hydrostatic equilibrium, we derive a lower limit to the density of 0.78 g cm−3, and an elongation (a/b) of 2.01 assuming an equatorial view. From Hubble Space Telescope data, we report no resolved companion orbiting 2004 TT357. Despite an expected high fraction of contact binaries in the trans-Neptunian belt, 2001 QG298 is the unique confirmed contact binary in the trans-Neptunian belt, and 2004 TT357 is only the second candidate to this class of systems, with 2003 SQ317.
Self tuning scalar tensor black holes

Studying a certain sub class of higher order Horndeski (scalar-tensor) theories we discuss a method discovered recently permitting analytic black hole solutions with a non trivial and regular scalar field. One of the solutions found has de Sitter asymptotics and self tunes the bulk cosmological constant. Using the aforementioned method we find and analyse new black hole solutions which can also have de Sitter asymptotics. By looking at small deviations of the integration constant responsible for self tuning we discuss the robustness of the self tuning mechanism. We find that neighboring solutions to the one previously found present also self tuning properties with unaltered effective cosmological constant.
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT

We present numerical results on three-dimensional (3D) hydrodynamic core-collapse simulations of an 11.2 M☉ star. By comparing one-dimensional (1D) and two-dimensional (2D) results with those of 3D, we study how the increasing spacial multi-dimensionality affects the postbounce supernova dynamics. The calculations were performed with an energy-dependent treatment of the neutrino transport that is solved by the isotropic diffusion source approximation scheme. In agreement with previous study, our 1D model does not produce explosions for the 11.2 M☉ star, while the neutrino-driven revival of the stalled bounce shock is obtained in both the 2D and 3D models. The standing accretion-shock instability (SASI) is observed in the 3D models, in which the dominant mode of the SASI is bipolar (ℓ = 2) with its saturation amplitudes being slightly smaller than 2D. By performing a tracer-particle analysis, we show that the maximum residency time of material in the gain region becomes longer in 3D than in 2D due to non-axisymmetric flow motions, which is one of advantageous aspects of 3D models to obtain neutrino-driven explosions. Our results show that convective matter motions below the gain radius become much more violent in 3D than in 2D, making the neutrino luminosity larger for 3D. Nevertheless, the emitted neutrino energies are made smaller due to the enhanced cooling. Our results indicate whether these advantages for driving 3D explosions could or could not overwhelm the disadvantages is sensitive to the employed numerical resolutions. An encouraging finding is that the shock expansion tends to become more energetic for models with finer resolutions. To draw a robust conclusion, 3D simulations with much higher numerical resolutions and with more advanced treatment of neutrino transport and of gravity are needed, which could be practicable by utilizing forthcoming Petaflops-class supercomputers.
THE HARD X-RAY CONTINUUM OF CEN A OBSERVED WITH INTEGRAL SPI

We revisit the average hard X-ray spectrum from the active galactic nucleus (AGN) of Centaurus A (Cen A) using 10 yr worth of observations with INTEGRAL SPI. This source has the highest flux observed from any AGNs in the SPI bandpass (23 keV–8 MeV). The 10 year light curve of Cen A is presented, and hardness ratios confirm that the spectral shape changes very little despite the luminosity varying by a factor of a few. Primarily, we establish the presence of a reflection component in the average spectrum by demonstrating an excess between 20 and 60 keV, from extending the spectral shape observed at low energy to the SPI regime. The excess in Chandra HETGS and INTEGRAL SPI data is well described by reflection of the dominant power-law spectrum from a neutral, optically thick atmosphere. We find that the reprocessed emission contributes 20%–25% of the 23–100 keV flux. The existence of a cutoff at tens to hundreds of kiloelectron volts remains controversial. Using simulated spectra, we demonstrate that a high energy cutoff reproduces the observed spectral properties of Cen A more readily than a simple power law. However, we also show that such a cutoff is probably underestimated when neglecting (even modest) reflection, and for Cen A would be at energies >700 keV, with a confidence of >95%. This is atypically high for thermal Comptonizing plasmas observed in AGNs, and we propose that we are in fact modeling the more gradual change in spectral shape expected of synchrotron self-Compton spectra.
THE GROWTH RATE OF COSMIC STRUCTURE FROM PECULIAR VELOCITIES AT LOW AND HIGH REDSHIFTS

Peculiar velocities are an important probe of the growth rate of mass density fluctuations in the universe. Most previous studies have focused exclusively on measuring peculiar velocities at intermediate (0.2 < z < 1) redshifts using statistical redshift-space distortions. Here, we emphasize the power of peculiar velocities obtained directly from distance measurements at low redshift (z ≲ 0.05), and show that these data break the usual degeneracies in the Ωm, 0– σ8, 0 parameter space. Using only peculiar velocity data, we find and σ8, 0 = 0.748 ± 0.035. Fixing the amplitude of fluctuations at very high redshift using observations of the cosmic microwave background, the same data can be used to constrain the growth index γ, with the strongest constraints coming from peculiar velocity measurements in the nearby universe. We find γ = 0.619 ± 0.054, consistent with ΛCDM. Current peculiar velocity data already strongly constrain modified gravity models and will be a powerful test as data accumulate.
ULTRA-LUMINOUS INFRARED GALAXIES IN SLOAN DIGITAL SKY SURVEY DATA RELEASE 6

Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH–host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z < 0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study. We found that the BH masses of Type I ULIRGs are typically smaller than those of Palomar–Green QSOs, and most Type I ULIRGs follow the MBH–σ relation. However, some ULIRGs with a larger Eddington ratio deviate from this relation, even though the line width of the [O iii] narrow-line (NL) core or the [S ii] line was used as the surrogate of velocity dispersion. This implies that at least some ULIRGs are probably still in the early evolution stage toward QSOs. The anti-correlation between the mass deviation from the MBH–σ relation and the Eddington ratio supports that the evolution of Type I ULIRGs is probably followed by the building up of the MBH–σ relation and the evolution to the QSO phase.