Miracle-dz/UniFAR-FTUs huggingface dataset:
The SFR-M ∗ main sequence archetypal star-formation history and analytical models

We derive the SFH of MS galaxies showing how the SFH peak of a galaxy depends on its seed mass at e.g. z=5. Following the MS, galaxies undergo a drastic slow down of their stellar mass growth after reaching the peak of their SFH. According to abundance matching, these masses correspond to hot and massive DM halos which state could results in less efficient gas inflows on the galaxies and thus could be at the origin of the limited stellar mass growth. As a result, galaxies on the MS can enter the passive region of the UVJ diagram while still forming stars. The ability of the classical analytical SFHs to retrieve the SFR of galaxies from SED fitting is studied. Due to mathematical limitations, the exp-declining and delayed SFH struggle to model high SFR which starts to be problematic at z>2. The exp-rising and log-normal SFHs exhibit the opposite behavior with the ability to reach very high SFR, and thus model starburst galaxies, but not low values such as those expected at low redshift for massive galaxies. We show that these four analytical forms recover the SFR of MS galaxies with an error dependent on the model and the redshift. They are, however, sensitive enough to probe small variations of SFR within the MS but all the four fail to recover the SFR of rapidly quenched galaxies. However, these SFHs lead to an artificial gradient of age, parallel to the MS which is not exhibited by a simulated sample. This gradient is also produced on real data, using a sample of GOODS-South galaxies at 1.5<z<1.2. We propose a SFH composed of a delayed form to model the bulk of stellar population plus a flexibility in the recent SFH. This SFH provides very good estimates of the SFR of MS, starbursts, and rapidly quenched galaxies at all z. Furthermore, used on the GOODS-South sample, the age gradient disappears, showing its dependency on the SFH assumption made to perform the SED fitting.
A polarization study of three blazars using uGMRT at ∼ 600 MHz

We present results from our radio polarimetric study with the upgraded giant metrewave radio telescope (uGMRT) at band 4 (550–850 MHz) of three blazars: radio-loud quasars 3C390.3, 4C71.07 and BL Lac object 1ES 2344 + 514. The aim of this study was (i) to carry out a feasibility study for band 4 polarization with the uGMRT and (ii) to compare and contrast the kpc-scale polarization properties between the blazar sub-classes. We have detected linear polarization in all the three sources. The degree of linear polarization in the cores of the two quasars is higher than the BL Lac object, consistent with similar differences observed on parsec-scales in blazars. The highest fractional polarization of ≈ 15% is observed in the hotspot region of 3C390.3, which also shows extended polarized lobe structures. 1ES 2344 + 514 shows a core–halo structure, whereas 4C71.07 remains unresolved. A rotation of polarization electric vectors along the northern hotspot of 3C390.3 and the core of 1ES 2344 + 514, suggest jet bending. Greater depolarization in the southern lobe of 3C390.3 compared to the northern lobe indicates the presence of Laing–Garrington effect. Multi-frequency uGMRT polarimetric data are underway to study the kpc-scale rotation measures across these sources to ﬁnd differences in the surrounding media.
X-ray source populations in the Galactic Plane

We present the first results from the XMM-Newton Galactic Plane Survey (XGPS). In the first phase of the programme, 22 pointings were used to cover a region of approximately 3 deg 2 between 19° and 22° in Galactic longitude and ±0.6° in latitude. In total we have resolved over 400 point X-ray sources, at ≥ 5σ significance, down to a flux limit of ∼2 x 10 -14 erg s -1 cm -2 (2-10 keV). The sources exhibit a very wide range of spectral hardness, with interstellar absorption identified as a major influence. The source populations detected in the soft (0.4-2 keV) band and hard (2-6 keV) band show surprisingly little overlap. The majority of the soft sources appear to be associated with relatively nearby stars with active stellar coronae, judging from their high coincidence with bright stellar counterparts. The combination of the XGPS measurements in the hard X-ray band with the results from earlier surveys carried out by ASCA and Chandra reveals the form of the low-latitude X-ray source counts over 4 decades of flux. It appears that extragalactic sources dominate below ∼10 -13 erg s -1 cm -2 (2-10 keV), with a predominantly Galactic source population present above this flux threshold. The nature of the faint Galactic population observed by XMM-Newton remains uncertain, although cataclysmic variables and RS CVn systems may contribute substantially. XMM-Newton observes an enhanced surface brightness in the Galactic plane in the 2-6 keV band associated with Galactic ridge X-ray emission (GRXE). The integrated contribution of Galactic sources plus the breakthrough of extragalactic signal accounts for up to 20 per cent of the observed surface brightness. The XGPS results are consistent with the picture suggested from a deep Chandra observation in the Galactic plane, namely that the bulk of the GRXE is truly diffuse.
V- and R-band Galaxy Luminosity Functions and Low Surface Brightness Galaxies in the Century Survey

We use 64 deg2 of deep V and R CCD images to measure the local V- and R-band luminosity functions of galaxies. The V0 < 16.7 and R0 < 16.2 redshift samples contain 1255 and 1251 galaxies and are 98.1% and 98.2% complete, respectively. We apply k-corrections before the magnitude selection so that the completeness is to the same depth for all spectral types. The V and R faint-end slopes are surprisingly identical: α = -1.07 ± 0.09. Representative Schechter function parameters for H0 = 100 are: M = -20.88 ± 0.09, ϕ = 0.016 ± 0.003 Mpc-3 and M = -20.23 ± 0.09, ϕ = 0.020 ± 0.003 Mpc-3. The V and R local luminosity densities, jR = (1.9 ± 0.6) × 108 L⊙ and jV = (2.2 ± 0.7) × 108 L⊙, are in essential agreement with the recent 2 Degree Field Galaxy Redshift Survey and Sloan Digital Sky Survey determinations. All low surface brightness (LSB) galaxies fall in the large-scale structure delineated by high surface brightness galaxies. The properties and surface number density of our LSB galaxies are consistent with the LSB galaxy catalog of O'Neil, Bothun & Cornell, suggesting that our samples are complete for LSB galaxies to the magnitude limits. We measure colors, surface brightnesses, and luminosities for our samples, and find strong correlations among these galaxy properties. The color–surface brightness relation is (V - R)0 = (-0.11 ± 0.05)μR, 0 + (2.6 ± 0.9).
A Long, Hard Look at the Low/Hard State in Accreting Black Holes

We present the first results of coordinated multiwavelength observations of the Galactic black hole GX 339-4 in a canonical low/hard state, obtained during its 2004 outburst. XMM-Newton observed the source for two revolutions, or approximately 280 ks; RXTE monitored the source throughout this long stare. The resulting data offer the best view yet obtained of the inner accretion flow geometry in the low/hard state, which is thought to be analogous to the geometry in low-luminosity active galactic nuclei. The XMM-Newton spectra clearly reveal the presence of a cool accretion disk component and a relativistic Fe K emission line. The results of fits made to both components strongly suggest that a standard thin disk remains at or near to the innermost stable circular orbit, at least in bright phases of the low/hard state. These findings indicate that potential links between the inner disk radius and the onset of a steady compact jet, and the paradigm of a radially recessed disk in the low/hard state, do not hold universally. The results of our observations can best be explained if a standard thin accretion disk fuels a corona that is closely related to, or consistent with, the base of a compact jet. In a brief examination of archival data, we show that Cygnus X-1 supports this picture of the low/hard state. We discuss our results within the context of disk-jet connections and prevailing models for accretion onto black holes.
128 : of Intensive Studies on Language, Literature, Art, and Culture ABSURDITY IN MADURESE AND ENGLISH DRAMA: A COMPARATIVE STUDY : Language, Art, and

Comedies from different countries have their absurdities. Absurdity is something that humans often experience for searching for the meaning of life. Therefore, a comparative study of literature is used in this study to compare absurdities in the comedy originating from Madura and England. The objective of this study is to find out how the absurdities are shown in the Madurese and English comedy. Then, the method of this study is the qualitative method. The sources of the data of this study are Juragan Hadroh and Gara-Gara Tukang Cukur EDAN ! by Sukur, CS was performed in 2021 and is compared to George Bernard Shaw’s Too True To Be Good which was performed in 1949. This study uses the theory of absurdity that can be called “the philosophy of the absurd” by Albert Camus. The data of this study are in the form of character utterances, and gestures. This study found that both of Madurese and English comedies exist as the form of searching for the meaning of life. Absurdities that are shown by Madurese and English comedies start from the names of characters, utterances, and acts of the characters.
An empirical investigation of the impact of social media tool usage on employees work performance among Ghana Commercial Bank Workers

Goal: The motivation of this paper is to forge and foster an insightful and comprehensive understanding of social media potential and its possible impact on Ghana Commercial Bank employees’ performance. Design / Methodology / Approach: Five cities were strategically sampled using convenient sampling technique to represent the various diversifications in corporate compositions. Data was collected from 249 workers of the Ghana Commercial Bank. The study utilized the structural equation modeling technique to construct and evaluate the proposed research model. Results: Social media usage had a significant positive relationship with employee engagement and knowledge transfer. Knowledge transfer had no significant relationship with work performance and employee engagement had a significant positive relationship with work performance. Experience with social media had a significant moderating effect on relationship between knowledge transfer and work performance. Research limitations/implications: The study covered employees from one bank and this has implications on generalization. The study used cross sectional data and employed quantitative analysis. Mixed methods would have added some insights and longitudinal data could further unravel causal relationships among overtime. Practical implications: Social media platform managers and policy makers within the banking sector should proactively harness social media platform and utilize to benefit corporate bodies. Banking authorities and allied stakeholders should train workers to ensure positive inclination to social media usage. Originality/Value: Contributes to theory by validating and establishing the theoretical model. The findings provide insights with respect to development and subsequent deployment of practical guidelines for successful integration of social media in enterprise activities.
Thermal Visualization and Performance Analysis in a Channel Installing Transverse Baffles with Square Wings

The experimental examination of local heat transfer, thermal intensification, friction factors, and thermal performance factors (TPF) in a rectangular channel with square-winged transverse baffles (SW-TB) are presented in this paper. The purpose of this study is to modify the typical transverse baffles (TB) into square-winged transverse baffles (SW-TB) in order to improve the thermal performance and heat transfer rate of the channel. The effects of SW-TBs with various wing attack angles and Reynolds numbers on the heat transfer performance characteristics were examined using a thermochromic liquid crystal sheet. In the experiments, the SW-TBs were attached to the bottom wall of the channel, which had an aspect ratio (W:H) of 3.75:1. The SW-TBs had a width (w) of 150 mm, a square perforated cross-sectional area (a × b) of 8 × 8 mm2, and attack angles (θ) of 0° (solid transverse-baffle), 22.5°, 45°, 67.5°, and 90°. The bottom wall of the channel was evenly heated, while the other walls were insulated. The temperature contours on the heated surface were plotted using temperatures obtained through using the thermochromic liquid crystal (TLC) image-processing method. Experimental results revealed that the SW-TBs created multiple impinging jets, apart from the recirculation. At the proper attack angles (θ = 22.5° and 45°), the SW-TBs offered greater heat transfer rates and caused lower friction losses, resulting in higher TPFs than the solid transverse baffles. In the current work, channels where the SW-TBs display a θ = 45° presented the greatest TPF, as high as 1.26. The multiple impinging jets issuing by the SW-TBs suppressed the size of the recirculation flow and allowed better contact between the fluid flow and channel wall.
Testing a model for subphotospheric dissipation in GRBs: fits to Fermi data constrain the dissipation scenario

It has been suggested that the prompt emission in gamma-ray bursts (GRBs) could be described by radiation from the photosphere in a hot fireball. Such models must be tested by directly fitting them to data. In this work we use data from the Fermi Gamma-ray Space Telescope and consider a specific photospheric model, in which the kinetic energy of a low-magnetization outflow is dissipated locally by internal shocks below the photosphere. We construct a table model with a physically motivated parameter space and fit it to time-resolved spectra of the 36 brightest Fermi GRBs with a known redshift. We find that about two-thirds of the examined spectra cannot be described by the model, as it typically underpredicts the observed flux. However, since the sample is strongly biased towards bright GRBs, we argue that this fraction will be significantly lowered when considering the full population. From the successful fits we find that the model can reproduce the full range of spectral slopes present in the sample. For these cases we also find that the dissipation consistently occurs at a radius of ∼1012 cm and that only a few per cent efficiency is required. Furthermore, we find a positive correlation between the fireball luminosity and the Lorentz factor. Such a correlation has been previously reported by independent methods. We conclude that if GRB spectra are due to photospheric emission, the dissipation cannot only be the specific scenario we consider here.
Impact of COVID-19 Vaccination on Seroprevalence of SARS-CoV-2 among the Health Care Workers in a Tertiary Care Centre, South India

Global vaccine development efforts have been accelerated in response to the devastating COVID-19 pandemic. The study aims to determine the seroprevalence of SARS-CoV-2 IgG antibodies among vaccine-naïve healthcare workers and to describe the impact of vaccination roll-out on COVID-19 antibody prevalence among the health care centers in tertiary care centers in South India. Serum samples collected from vaccinated and unvaccinated health care workers between January 2021 and April 2021were subjected to COVID-19 IgG ELISA, and adverse effects after the first and second dose of receiving the Covishield vaccine were recorded. The vaccinated group was followed for a COVID-19 breakthrough infection for a period of 6 months. Among the recruited HCW, 156 and 157 participants were from the vaccinated and unvaccinated group, respectively. The seroprevalence (COVID-19 IgG ELISA) among the vaccinated and unvaccinated Health Care Workers (HCW) was 91.7% and 38.2%, respectively, which is statistically significant. Systemic and local side-effects after Covishield vaccination occur at lower frequencies than reported in phase 3 trials. Since the COVID-19 vaccine rollout has commenced in our tertiary care hospital, seropositivity for COVID-19 IgG has risen dramatically and clearly shows trends in vaccine-induced antibodies among the health care workers.
Ownership Structure and Corporate Risk Taking: Evidence from an Emerging Market

We investigate the impact of ownership structure on corporate risk-taking across Chinese firms between 1999 to 2008. We find a U-shape relationship between the largest shareholder’ ownership and corporate risk taking. Specifically, when the largest shareholder’s ownership is low, the largest shareholder discourages corporate risk taking due to the dominance of the management entrenchment effect, but if the largest shareholding rises past a threshold, it encourages corporate risk taking instead, due to the dominance of the incentive alignment effect. We also find government ownership deters corporate risk-taking, while foreign ownership encourages corporate risk-taking.
The linear-size evolution of classical double radio sources

Recent investigations of how the median size of extragalactic radio sources change with redshift have produced inconsistent results. In a previous investigation Eales compared the radio and optical properties of a bright 3C and a faint 6C sample and concluded that for a universe with Ω0 = 0Dmed ∝ (1 + z)-1.1±0.5, with Dmed being the median size of the radio sources at a given epoch and z the redshift. Oort, Katgert, & Windhorst, on the other hand, from a comparison of the properties of a number of radio samples, found a much stronger evolution, with Dmed ∝ (1 + z)-3.3±0.5 forΩ0 = 0. In this paper we attempt to resolve the difference. We have repeated the analysis of Eales using the much improved data, in particular, the virtually complete redshift information that now exists for the 6C sample. Confining our analysis to FR 2 sources, or "classical doubles," which we argue is the best understood class of radio sources and the least likely to be affected by selection effects, we find Dmed ∝ (1 + z)-1.2±0.5 for = ω0 and Dmed ∝ (1 + z)1.7±0.4 for Ω0 = 1. Moreover, in contrast to earlier studies, we find no intrinsic correlation between size and radio luminosity. We show that there is a selection effect that affects studies of this kind, the magnitude of which has not previously been realized and has likely led to an overestimate in the strength of the size evolution found in previous investigations. Our complete redshift information allows us to gain insight into our result by plotting a radio luminosity- size (P-D) diagram for the 6C sample, the first time this has been possible for a faint radio sample. The most obvious difference between the 3C and 6C P-D diagrams (i.e., the radio astronomers' H-R diagram) is the clump of sources in the 6C diagram at D ˜ 100 kpc, P151 1027-1028 W Hz-1 sr-1. These clump sources have similar sizes to the emission-line regions found around high-redshift radio galaxies, suggesting that the presence of dense line-emitting gas around high-redshift radio galaxies is responsible for the size evolution. We show that this explanation can quantitatively explain the observed size evolution, as long as either there is little X-ray emitting gas around these objects or, if there is, it is distributed in a way similar to the distribution of the emission-line gas, namely, highly anisotropic and inhomogeneous.
On smoothness-asymmetric null infinities

We discuss the existence of asymptotically Euclidean initial data sets for the vacuum Einstein field equations which would give rise (modulo an existence result for the evolution equations near spatial infinity) to developments with a past and a future null infinity of different smoothness. For simplicity, the analysis is restricted to the class of conformally flat, axially symmetric initial data sets. It is shown how the free parameters in the second fundamental form of the data can be used to satisfy certain obstructions to the smoothness of null infinity. The resulting initial data sets could be interpreted as those of some sort of (nonlinearly) distorted Schwarzschild black hole. Their developments would be that they admit a peeling future null infinity, but at the same time have a polyhomogeneous (non-peeling) past null infinity.
Optical and GeV-TeV Flashes from Gamma-Ray Bursts

The synchrotron optical flash caught in GRB 990123 overlaps with the MeV radiation front. Therefore, the optical-emitting electrons must also produce GeV-TeV emission by inverse Compton scattering of MeV photons. The ultra-high-energy flash can be much stronger than its optical counterpart. We also note that Compton cooling by MeV photons immediately terminates the optical emission unless the fireball Lorentz factor exceeds 103. Severe Compton losses may explain the nondetections of optical flashes in several long GRBs. Such failed optical flashes should be especially efficient GeV producers and likely to develop e± cascades. This probably happened in GRB 941017, and its mysterious high-energy component is well explained by Compton upscattering of GRB photons at the fireball deceleration radius. The proposed mechanism of GeV emission should not work for short GRBs that early decouple from the fireball and avoid interaction with the electrons in the deceleration flash. Observations by Swift and the Gamma-Ray Large Area Telescope will provide an opportunity to test these expectations. The existing data for GRB 990123 already impose interesting constraints on the explosion.
Compensation goals and firm performance

Using a large dataset of performance goals employed in executive incentive contracts, we find that a disproportionately large number of firms exceed their goals by a small margin as compared to the number that fall short of the goal by a similar margin. This asymmetry is particularly acute for earnings goals, when compensation is contingent on a single goal, when the discontinuity around the goal is concave-shaped and for grants with non-equity-based payouts. Firms that exceed their compensation target by a small margin are more likely to beat the target the next period and CEOs of firms that miss their targets are more likely to experience a forced turnover. Firms that just exceed their EPS goals have higher abnormal accruals and lower Research and Development (R&D) expenditures, and firms that just exceed their profit goals have lower SG&A expenditures. Overall, our results highlight some of the costs of linking managerial compensation to specific compensation targets. JEL Classification: G30, J33
Controlled ion-beam transformation of electrical, magnetic, and optical materials properties

The key condition for radical progress in technology in the 21th century is the availability of a technique for the controlled production in a solid of 3D patterns incorporating regions of desired physical and chemical properties, with the possibility of downsizing pattern elements to the nanometer scale being a crucial requirement. In this paper, a method for changing the electrical, magnetic, optical and other key physical properties in a direct and deliberate manner by radically modifying the solid's atomic composition is proposed for the first time. The physical foundation of the new nonlithography technology is the observation — thoroughly investigated and well verified in our numerous experiments — that accelerated particle beams can be used to selectively remove atoms from thin films of di- or polyatomic compounds. It is shown, in particular, that by selectively removing atoms of a given sort, dielectrics can be transformed into metals or semiconductors, nonmagnetic materials into magnetic ones, and the optical and other properties of materials can be changed radically. The selective removal of atoms of a specified sort from a material is of great interest for future technologies, especially for those relevant to nanoelectronics and, more broadly, to the numerous 'nanoproblems' ahead in the third millennium.