Miracle-dz/UniFAR-FTUs huggingface dataset:
Potential Carbon Storage In The Forest Area Of Mount Merbabu National Park (MMbNP) Resort Selo Central Java

Forests play a very large function in the solution of climate problems. Trees are capable of absorbing carbon dioxide (CO2) in the photosynthesis process and store it in the form of biomass, thereby reducing the concentration of carbon in the atmosphere. The forest area of Mount Merbabu National Park (MMbNP) has great potential to absorb carbon emissions and mitigate climate. The purpose of this study was to determine the potential for carbon storage in MMbNP. The research method used is quantitative descriptive and analyzed by allometric method adapted to tree species at low, medium, and high densities. The estimated carbon storage refers to the Indonesian National Standard (SNI) 7724 of 2011. The potential for total carbon storage in the forest area is 129.357,71 tons. In detail, the total carbon storage in low density land cover types is 10.201,87 tons, medium density is 23.729. 66 tons, and high density is 95.426,18 tons. This type of land cover with high density has the highest carbon absorption capacity; this is relevant to the presence of the number of trees that are able to absorb more carbon and have a larger area than other types of land cover.
Developing a Visual Counting Method to Quantify Riverine Plastic Litter: A Case Study of Rivers in Semarang City, Indonesia

Indonesia has established a national action plan on marine plastic debris to tackle the issue of marine plastic debris. Because most of the marine plastic debris in Indonesia is likely due to mismanaged plastic waste, it is important to address the problem of riverine plastic river problem in Indonesia. The objectives of this study are to visually observe the condition of the river in terms of plastic pollution, to quantify plastic litter in the river, and to develop a visual counting model of plastic litter quantification. The visual counting of plastic debris (> 2.5 cm) method based on the European standard method was applied to a river in Indonesia. The main challenge was the high turbidity of the water that obstructed visual observation. The deployment of the fishing net was also not appropriate to collect debris. Most of the plastic debris was stranded on the riverbanks, indicating that the plastic flow was likely elevated due to runoff during the rainy season. Four types of plastic litter polymers were obtained, i.e., polyethylene terephthalate (PET), low-density polyethylene (LDPE), polypropylene (PP), and polystyrene (PS). The highest percentage of macroplastics is LDPE, which usually used as daily packaging (90%).
Emission-line studies of young stars. I - The T Tauri stars. II - The Herbig Ae/Be stars

High-resolution optical (CCD) spectra of 53 T Tauri stars are presented as part of a program to study the emission-line properties of young stars. The permitted lines are interpreted in terms of active stellar chromospheres, which emit narrow (≤ 40 km/s) lines (e.g., of Si I, Ca I and II, Mg I and II, and Fe I and II), and extended envelopes, which produce the usual broad (≥ 100 km/s) line profiles. A weak correlation between the Hα and narrow-line strenghts suggests that these two regions are somehow interacting
Relativistic models of two low‐luminosity radio jets: B2 0326+39and B2 1553+24

We apply the intrinsically symmetrical, decelerating relativistic jet model developed by Laing & Bridle for 3C 31 to deep, full-synthesis 8.4-GHz VLA imaging of the two low-luminosity radio galaxies B2 0326+39 and B2 1553+24. After some modifications to the functional forms used to describe the geometry, velocity, emissivity and magnetic-field structure, these models can accurately fit our data in both total intensity and linear polarization. We conclude that the jets in B2 0326+39 and B2 1553+24 are at angles of 64° ± 5° and 7. °7 ± 1. °3 to the line of sight, respectively. In both objects, we find that the jets decelerate from 0.7-0.8c to < 0.2c over a distance of approximately 10 kpc, although in B2 1553+24 this transition occurs much further from the nucleus than in B2 0326+39 or 3C 31. The longitudinal emissivity profiles can be divided into sections, each fitted accurately by a power law; the indices of these power laws decrease with distance from the nucleus. B2 0326+39 also requires a discontinuity in emissivity to in order to fit a region with several bright knots of emission. In B2 1553+24, the sudden brightening of the jet can be explained by a combination of rapid expansion of the jet and a continuous variation of emissivity. The magnetic fields in both objects are dominated by the longitudinal component in the high-velocity regions close to the nucleus and by the toroidal component further out, but B2 0326+39 also has a significant radial component at large distances, whereas B2 1553+24 does not. Simple adiabatic models fail to fit the emissivity variations in the regions of high velocity but provide good descriptions of the emissivity after the jets have decelerated. Given the small angle to the line of sight inferred for B2 1553+24, there should be a significant population of similar sources at less extreme orientations. Such objects should have long (? 200 kpc), straight, faint jets and we show that their true sizes are likely to have been underestimated in existing images.
Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions

Collisionless shocks channel the energy of the directed plasma flow into the heating of the plasma species and magnetic field enhancement. The kinetic processes at the shock transition cause the ion distributions just behind the shock to be nongyrotropic. Gyrotropization and subsequent isotropization occur at different spatial scales. Accordingly, for a given upstream plasma and magnetic field state, there would be different downstream states corresponding to the anisotropic and isotropic regions. Thus, at least two sets of Rankine–Hugoniot relations are needed, in general, to describe the connection of the downstream measurable parameters to the upstream ones. We establish the relation between the two sets.
On Minisuperspace Models of S-branes

In this note we reconsider the minisuperspace toy models for rolling and bouncing tachyons. We show that the theories require to choose boundary conditions at infinity since particles in an exponentially unbounded potential fall to infinity in finite world-sheet time. Using standard techniques from operator theory, we determine the possible boundary conditions and we compute the corresponding energy spectra and minisuperspace 3-point functions. Based on this analysis we argue in particular that world-sheet models of S-branes possess a discrete spectrum of conformal weights containing both positive and negative values. Finally, some suggestions are made for possible relations with previous studies of the minisuperspace theory.
Constraining Theories of Polarized SiO Maser Transport: Multi-epoch Analysis of a π/2 Electric Vector Rotation Feature

The detailed polarization mechanisms of SiO masers originating from the near-circumstellar environment of asymptotic giant branch stars are not yet definitively known. Prevailing theories are broadly classified as either Zeeman or non-Zeeman in origin, the latter including effects such as anisotropic pumping or anisotropic resonant scattering. The predicted behavior of the linear and circular polarization fractions and the electric vector position angle (EVPA) vary by theory. In particular, individual maser features that exhibit a rotation in linear polarization of ∼π/2 as a function of frequency over their extent can be utilized as a test of several maser polarization transport theories. In this paper, we analyze one SiO (ν = 1, J = 1 − 0) maser feature toward the Mira variable, TX Cam, that exhibits this internal polarization rotation and persists across five epochs (spanning ∼3 months). We compare our results to the predictions by several maser polarization theories and find that the linear polarization across the feature is consistent with a geometric effect for a saturated maser originating when the angle between the projected magnetic field and the line of sight (θ) crosses the Van Vleck angle θF ∼ 55°. However, the EVPA exhibits a smooth rotation across the spatial extent of the feature rather than the expected abrupt π/2 flip. We discuss possible explanations for this discrepancy and alternative theories. Circular polarization across the feature is also analyzed, and it is most accurately described by Zeeman effects giving rise to a circular polarization fraction of the form .
The FMOS-COSMOS Survey of Star-forming Galaxies at z ∼ 1.6. VI. Redshift and Emission-line Catalog and Basic Properties of Star-forming Galaxies

We present a new data release from the Fiber Multi-Object Spectrograph (FMOS)-COSMOS survey that contains the measurements of the spectroscopic redshift and flux of rest-frame optical emission lines (Hα, [N ii], [S ii], Hβ, [O iii]) for 1931 galaxies out of a total of 5484 objects observed over the 1.7 deg2 COSMOS field. We obtained H- and J-band medium-resolution (R ∼ 3000) spectra with FMOS mounted on the Subaru telescope, which offers an in-fiber line flux sensitivity limit of for an on-source exposure time of 5 hr. The full sample contains the main population of star-forming galaxies at z ∼ 1.6 over the stellar mass range , as well as other subsamples of infrared-luminous galaxies detected by Spitzer and Herschel at the same and lower (z ∼ 0.9) redshifts and X-ray-emitting galaxies detected by Chandra. This paper presents an overview of our spectral analyses, a description of the sample characteristics, and a summary of the basic properties of emission-line galaxies. We use the larger sample to redefine the stellar mass–star formation rate relation based on the dust-corrected Hα luminosity and find that the individual galaxies are better fit with a parameterization including a bending feature at M* ≈ 1010.2 M⊙, and that the intrinsic scatter increases with M* from 0.19 to 0.37 dex. We also confirm with higher confidence that the massive (M* ≳ 1010.5 M⊙) galaxies are chemically mature as much as local galaxies with the same stellar masses, and that the massive galaxies have lower [S ii]/Hα ratios for their [O iii]/Hβ as compared to local galaxies, which is indicative of enhancement in the ionization parameter.
Rational Decisions in Large Worlds.

This paper argues that we need to look beyond Bayesian decision the, for an answer to the general problem of making national decision under uncertainty. The view that Bayesian decision theory is only genuinely valid in a small world was asserted very firmly by SAVAGE [1951] when laying down the principles of the theory in his path - breaking Foundations of Statistics. He makes the distinction between small and large worlds in a folksy way by quoting the proverbs "Look before you leap" and "Cross that bridge when you corne to it". You are in a small world if it is feasible always to look before you leap. You are in a large world if there are some bridges that you cannot cross before you corne to them.
Galaxy rotation and supermassive black hole binary evolution

Supermassive black hole (SMBH) binaries residing at the core of merging galaxies are recently found to be strongly affected by the rotation of their host galaxies. The highly eccentric orbits that form when the host is counterrotating emit strong bursts of gravitational waves that propel rapid SMBH binary coalescence. Prior work investigated planar orbits and a uniform rotation profile, an unlikely interaction configuration. However, the coupling between rotation and SMBH binary evolution appears to be such a strong dynamical process that it warrants further investigation. This study uses direct N-body simulations to isolate the effect of galaxy rotation in more realistic interactions. In particular, we systematically vary the SMBH orbital plane with respect to the galaxy rotation axis, the radial extent of the rotating component, and the initial eccentricity of the SMBH binary orbit. We find that the initial orbital plane orientation and eccentricity alone can change the inspiral time by an order of magnitude. Because SMBH binary inspiral and merger is such a loud gravitational wave source, these studies are critical for the future gravitational wave detector, LISA, an ESA/NASA mission currently set to launch by 2034.
The Dual superconformal theory for L**pqr manifolds

We present the superconformal gauge theory living on the world-volume of D3 branes probing the toric singularities with horizon the recently discovered Sasaki-Einstein manifolds Lp,q,r. Various checks of the identification are made by comparing the central charge and the R-charges of the chiral fields with the information that can be extracted from toric geometry. Fractional branes are also introduced and the physics of the associated duality cascade discussed.
On-shell recurrence relations for one-loop QCD amplitudes

We present examples of on-shell recurrence relations for determining rational functions appearing in one-loop QCD amplitudes. In particular, we give relations for one-loop QCD amplitudes with all legs of positive helicity, or with one leg of negative helicity and the rest of positive helicity. Our recurrence relations are similar to the tree-level ones described by Britto, Cachazo, Feng and Witten. A number of new features arise for loop amplitudes in non-supersymmetric theories like QCD, including boundary terms and double poles. We show how to eliminate the boundary terms, which would interfere with obtaining useful relations. Using the relations we give compact explicit expressions for the n-gluon amplitudes with one negative-helicity gluon, up through n = 7.
Tidal Interaction of M32 and NGC 205 with M31: Surface Photometry and Numerical Simulations

We investigate the interaction history of the M31 subgroup by comparing surface photometry of two of its satellites, M32 and NGC 205, with N-body simulations of satellite destruction. The recent discovery of a giant stream in the outer halo of M31, apparently pointed in the direction of M32 and NGC 205, makes such an investigation particularly relevant. The observational component of this study is based on 1. °7 × 5° B- and I-band CCD mosaic images centered on M31 and covering both satellites. Standard ellipse-fitting techniques are used to model and remove M31 disk light and to perform surface photometry on the satellites to limiting brightness levels of (μB, μI) = (27, 25) mag arcsec-2, corresponding to isophotal semimajor axis lengths of r = 420″ (1.6 kpc) and r = 720″ (2.7 kpc). A hint of excess light in the outer parts of M32 noted in earlier studies is confirmed; in particular, clear evidence is seen for a sharp (upward) break in the surface brightness profile at r = 150″ relative to a r1/4 law that fits the inner region of M32. This break is accompanied by a steep increase in isophotal ellipticity ϵ, as well as position angle ϕ′ twisting. In addition to this excess, evidence is seen for an inner downward break in the surface brightness profile at r = 50″. The robustness of the M32 isophotal features is demonstrated through their (1) insensitivity to the details of background subtraction, (2) symmetry about M32's center, and (3) narrow range of B-I color that is consistent with the interior regions of M32 but not with M31 residual spiral arm/dust lane features. The study of NGC 205 reveals pronounced isophote twisting at r ∼ 300″ that is coincident with a subtle downward break in the surface brightness profile, relative to an exponential law fitted to the inner region. The simulation component of this project is based on the analysis of single-component, spherical satellites that are being tidally disrupted through interactions with their parent galaxy. Generic features of the simulations include an excess in the surface brightness profile at large radii, a depletion zone at intermediate radii, and isophotal elongation and twists that are coincident with breaks in the brightness profile. The two satellites, M32 and NGC 205, display most of these features consistently across the B and I bands, which is strongly suggestive of tidal interaction and probable stripping by M31. We discuss what these observed features can tell us about the satellites' orbital parameters and histories. Specifically, M32 is found to be on a highly eccentric orbit and away from pericenter. Investigating M32's unusual combination of high surface brightness and low luminosity (the hallmark of compact ellipticals), we make empirical estimates of the galaxy's intrinsic properties and conclude that it is not likely to be the residual core of a tidally stripped normal elliptical galaxy, as has been suggested, but rather that its precursor was intrinsically compact.
Long-term sequelae of COVID-19 (myalgic encephalomyelitis): An international cross-sectional study

Background: As a result of prolonged effects on multiple organs, recovery from COVID-19 caused by SARS-CoV-2 cannot be verified. This study seeks to understand chronic and acute long-term symptoms of COVID-19 lasting from a few weeks after diagnosis. The study also aims to gain insight into prevalence of chronic fatigue syndrome/myalgic encephalomyelitis, a potentially comorbid condition for several months after the infection, in addition to taking a broad perspective on rare symptoms that may have developed during or after the infection. Study design: Cross-sectional questionnaire\descriptive study. Methods: The questionnaire was developed to assess the long-term effects of the global pandemic of COVID-19 using DePaul Symptom Questionnaire-2. The DePaul Symptom Questionnaire, Patient Health Questionnaire, and other symptoms that have been introduced by literature review. Discussion: A large cohort of people from all over the world will be examined to understand the differential effects of people who have experienced COVID-19, as well as the potential occurrence of ME. In total, 20,000 COVID patients are expected to be included in the study by Sep 1, 2022. Patients who have experienced COVID-19 will be asked about their persistent symptoms from 1 week up to more than 6 months after catching or recovery from the infection.
Boundary inflation and the WMAP data

Inflation in a five-dimensional brane world model with two boundary branes is studied. We make use of the moduli space approximation whereby the low energy theory reduces to a four-dimensional biscalar-tensor gravity plus a minimally coupled scalar field. After a detailed analysis of the inflationary solutions, we derive the evolution equations of the linear perturbations separating the adiabatic mode from two entropy modes. We then examine the primordial scalar and tensor power spectra and show that their tilt depends on the scalar-tensor coupling constant. Finally, the induced cosmic microwave background (CMB) anisotropies are computed and we present a Monte Carlo Markov chains exploration of the parameter space using the first year WMAP data. We find a marginalized probability bound for the associated Eddington parameter at the end of inflation 1-γ<2×10-3, at 95% confidence level. This suggests that future CMB data could provide crucial information helping to distinguish scalar-tensor and standard inflationary scenarios.
Vacuum polarization on the spinning circle

Vacuum polarization of a massive scalar field in the background of a two-dimensional version of a spinning cosmic string is investigated. It is shown that when the `radius of the universe' is such that spacetime is globally hyperbolic the vacuum fluctuations are well behaved, diverging though on the `chronology horizon'. Naive use of the formulae when spacetime is nonglobally hyperbolic leads to unphysical results. It is also pointed out that the set of normal modes used previously in the literature to address the problem gives rise to two-point functions which do not have a Hadamard form, and therefore are not physically acceptable. Such normal modes correspond to a locally (but not globally) Minkowski time, which appears to be at first sight a natural choice of time to implement quantization.
The “Planckonions”

We consider a spherically symmetric stellar configuration with a density profile [Formula: see text]. This configuration satisfies the Schwarzchild black hole condition [Formula: see text] for every [Formula: see text]. We refer to it as “Planckonion”. The interesting thing about the Planckonion is that it has an onion-like structure. The central sphere with radius of the Planck-length [Formula: see text] has one unit of the Planck-mass [Formula: see text]. Subsequent spherical shells of radial width [Formula: see text] contain exactly one unit of [Formula: see text]. We study this stellar configuration using Tolman–Oppenheimer–Volkoff equation and show that the equation is satisfied if pressure [Formula: see text]. On the geometrical side, the space component of the metric blows up at every point. The time component of the metric is zero inside the star but only in the sense of a distribution (generalized function). The Planckonions mimic some features of black holes but avoid appearance of central singularity because of the violation of null energy conditions.
Overview of Information Theory, Computer Science Theory, and Stochastic Thermodynamics for Thermodynamics of Computation

I give a quick overview of some of the theoretical background necessary for using modern non-equilibrium statistical physics to investigate the thermodynamics of computation. I first present some of the necessary concepts from information theory, and then introduce some of the most important types of computational machine considered in computer science theory. After this I present a central result from modern non-equilibrium statistical physics: an exact expression for the entropy flow out of a system undergoing a given dynamics with a given initial distribution over states. This central expression is crucial for analyzing how the total entropy flow out of a computer depends on its global structure, since that global structure determines the initial distributions into all of the computer's subsystems, and therefore (via the central expression) the entropy flows generated by all of those subsystems. I illustrate these results by analyzing some of the subtleties concerning the benefits that are sometimes claimed for implementing an irreversible computation with a reversible circuit constructed out of Fredkin gates.
Feeding ecology of invasive lionfish in the Punta Frances MPA, Cuba: insight into morphological features, diet and management

Cuba’s shelf has been invaded by lionfish (Pterois volitans/Pterois miles), which have become established over the archipelago, including areas of natural importance. The present study aims to evaluate morphometric features of lionfish and to explore the relationship between lionfish size and diet composition in different habitats in the Punta Frances National Park, Cuba. In total 620 lionfish were captured at 29 sites between 2013 and 2016. Lionfish stomachs were removed and their contents were analyzed using frequency and numerical methods. The length-weight allomentric relationship was obtained, and a decrease in lionfish sizes was shown over time, likely due to the extractions carried out. The diet was composed by fishes, crustaceans, mollusks and phytobenthos, with a predominance of fishes. Lionfish caught in seagrass beds tended to be smaller in size and consumed fewer fishes and more crustaceans than those captured in coral reefs. A positive correlation was observed between lionfish body size and gape size; however, no significant correlation was detected between lionfish body size and prey size. Larger lionfish tended to consume more fishes, while crustaceans were more significant in the diet of juvenile lionfish. This is the first study that examines the feeding habits of lionfish in the Punta Frances MPA, and provides valuable information on lionfish inhabiting this MPA across four years of sampling. Furthermore, this research may serve as a baseline for subsequent evaluations of lionfish impact and management actions in the area.