Miracle-dz/UniFAR-FTUs huggingface dataset:
The nature of the ISM in galaxies during the star-formation activity peak of the Universe

We combine a semi-analytic model of galaxy formation, tracking atomic and molecular phases of cold gas, with a three-dimensional radiative-transfer and line tracing code to study the sub-mm emission from atomic and molecular species (CO, HCN, [C I], [C II], [O I]) in galaxies. We compare the physics that drives the formation of stars at the epoch of peak star formation (SF) in the Universe (z = 2.0) with that in local galaxies. We find that normal star-forming galaxies at high redshift have much higher CO-excitation peaks than their local counterparts and that CO cooling takes place at higher excitation levels. CO line ratios increase with redshift as a function of galaxy star-formation rate, but are well correlated with H2 surface density independent of redshift. We find an increase in the [O I]/[C II] line ratio in typical star-forming galaxies at z = 1.2 and z = 2.0 with respect to counterparts at z = 0. Our model results suggest that typical star-forming galaxies at high redshift consist of much denser and warmer star-forming clouds than their local counterparts. Galaxies belonging to the tail of the SF activity peak at z = 1.2 are already less dense and cooler than counterparts during the actual peak of SF activity (z = 2.0). We use our results to discuss how future ALMA surveys can best confront our predictions and constrain models of galaxy formation.
A survey of carbon monoxide emission in dark clouds. [cosmic dust

Results are reported of a CO and $sup 13$CO survey of 68 dark clouds from the Lynds catalog. CO was detected in 63 of the 64 sources in which it was searched for, and the $sup 13$CO line was seen in 52 of 55 clouds. There is a rather narrow distribution of CO peak line radiation temperatures about a mean of approx.6 K; this may reflect the presence of a roughly uniform kinetic temperature of about a mean of approx.9. 5 K in the sources. Despite the probably subthermal excitation temperature of the $sup 13$CO transition observed, derived $sup 13$CO column densities are most likely good to within a factor of 2. Typical CO column densities for the clouds surveyed are N/sub co/approx. =5times10$sup 17$ cm$sup -2$, assuming a terrestrial carbon isotope ratio. All 68 clouds have previously been studied by Dieter in 6-cm H$sub 2$CO absorption; a comparison of line widths shows the $sup 13$CO lines to generally be wider than their formaldehyde counterparts. Possible explanations of this fact in terms of internal cloud motions are discussed. (AIP)
Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

Context. SMM J04542-0301 is an extended (similar to 1') submm source located near the core of the cluster MS0451.6-0305. It has been suggested that part of its emission arises from the interaction between a LBG and two EROs at z similar to 2.9 that are multiply-imaged in the optical/NIR observations. However, the dramatic resolution difference between the sub-mm map and the optical/NIR images make it di. cult to confirm this hypothesis. Aims. In a previous paper, we reported the detection of 1.4 GHz continuum radio emission coincident with this sub-mm source using VLA archival data. To fully understand the relation between this radio emission, the sub-mm emission, and the optical/IR multiplyimaged sources, we have re-observed the cluster with the VLA at higher resolution. Methods. The previous archival data has been re-reduced and combined with the new observations to produced a deep (similar to 10 mu Jy beam(-1)), high resolution (similar to 2 '') map centred on the cluster core. The strong lensing effect in the radio data has been quantified by constructing a new lens model of the cluster. Results. From the high resolution map we have robustly identified six radio sources located within SMM J 04542-0301. The brightest and most extended of these sources (RJ) is located in the middle of the sub-mm emission, and has no obvious counterpart in the optical/NIR. Three other detections (E1, E2 and E3) seem to be associated with the images of one of the EROs (B), although the NIR and radio emission appear to originate at slightly different positions in the source plane. The last two detections (CR1 and CR2), for which no optical/ NIR counterpart have been found, seem to constitute two relatively compact emitting regions embedded in a similar to 5 '' extended radio source located at the position of the sub-mm peak. The presence of this extended component (which contributes 38% of the total radio flux in this region) can only be explained if it is being produced by a lensed region of dust obscured star formation in the center of the merger. A comparison between the radio and sub-mm data at the same resolution suggests that E1, E2, E3, CR1 and CR2 are associated with the sub-mm emission. Conclusions. The radio observations presented in this paper provide strong observational evidence in favour of the merger hypothesis. However, the question if RJ is also contributing to the observed sub-mm emission remains open. These results illustrate the promising prospects for radio interferometry and strong gravitational lensing to study the internal structure of SMGs.
Erroneous use of Statistics behind Claims of a Major Solar Role in Recent Warming

In a study that attempted to relate solar and human activity to Earth's recent temperature change, Connolly et al. committed a basic error in the choice of statistical methods and so overreported the effect of the Sun. A major theme of their study was that there are many data sets of past solar activity, and some of these allegedly provide statistical evidence of “most of the recent global warming being due to changes in solar activity. ” We avoid methods that are known to give inaccurate results and show that for 1970–2005 Northern Hemisphere land the corrected solar attribution fraction is −7% to +5%, compared with values of up to 64% reported in Connolly et al. Their higher values are entirely due to mistaken application of statistics. Unfortunately, we cannot test truly “recent” global warming since most of their solar data sets end before 2015, and two finish in the 1990s, but all tested post-1970 periods show similarly small solar contributions. The solar-climate linkage is an area of fascinating and ongoing research with rigorous technical discussion. We argue that instead of repeating errors, they should be acknowledged and corrected so that the debate can focus on areas of legitimate scientific uncertainty.
Scientific Temper among Junior High School Students of Balasore District, Odisha

Scientific temper is an essential skill of 21st century youth. The New Education Policy (NEP 2020) in its recommendation clearly mentioned Specific skills and abilities, such as scientific temper, creativity, communication, fitness and wellness, teamwork, problem-solving, digital literacy, ethics, and so on, will be emphasized in school. In this context each and every individual should process scientific temper for holistic development. Recently it was conducted to find out the scientific temper of high school students in relation to their gender and locality. The current study used a descriptive survey method. The sample for the present study consisted of 112 students of 10th standard studying in government schools of Sadar block and Remuna block of Balasore District of Odisha were got as the example through stratified random sampling method. Data was collected by using scientific temper test constructed by Elizabeth Joshua of Mahatma Gandhi University Kottayam. Statistical techniques like Mean, Median, S.D. and t-test to examine the data. The results of the study stated that Girls have high level of Scientific Temper compared to that of Boys, and students studying in school urban area are having high level of Scientific Temper compared to the students studying in rural area.
DRESDYN - A new facility for MHD experiments with liquid sodium

The DREsden Sodium facility for DYNamo and thermohydraulic studies (DRESDYN) is intended as a platform both for large scale experiments related to geo- and astrophysics as well as for experiments related to thermohydraulic and safety aspects of liquid metal batteries and liquid metal fast reactors. The most ambitious projects in the framework of DRESDYN are a homogeneous hydromagnetic dynamo driven solely by precession and a large Taylor-Couette type experiment for the combined investigation of the magnetorotational instability and the Tayler instability. In this paper we give a short summary about the ongoing preparations and delineate the next steps for the realization of DRESDYN.
Comparisons and Connections between Mean Field Dynamo Theory and Accretion Disc Theory

The origin of large scale magnetic fields in astrophysical rotators, and the conversion of gravitational energy into radiation near stars and compact objects via accretion have been subjects of active research for a half century. Magnetohydrodynamic turbulence makes both problems highly nonlinear, so both subjects have benefitted from numerical simulations.However, understanding the key principles and practical modeling of observations warrants testable semi-analytic mean field theories that distill the essential physics. Mean field dynamo (MFD) theory and alpha-viscosity accretion disc theory exemplify this pursuit. That the latter is a mean field theory is not always made explicit but the combination of turbulence and global symmetry imply such. The more commonly explicit presentation of assumptions in 20th century textbook MFDT has exposed it to arguably more widespread criticism than incurred by 20th century alpha-accretion theory despite complementary weaknesses. In the 21st century however, MFDT has experienced a breakthrough with a dynamical saturation theory that consistently agrees with simulations. Such has not yet occurred in accretion disc theory, though progress is emerging. Ironically however, for accretion engines, MFDT and accretion theory are presently two artificially uncoupled pieces of what should be a single coupled theory. Large scale fields and accretion flows are dynamically intertwined because large scale fields likely play a key role in angular momentum transport. I discuss and synthesize aspects of recent progress in MFDT and accretion disc theory to suggest why the two likely conspire in a unified theory (© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
THE C14N/C15N RATIO IN DIFFUSE MOLECULAR CLOUDS

We report the first detection of C15N in diffuse molecular gas from a detailed examination of CN absorption lines in archival spectra, obtained with the Ultraviolet and Visual Echelle Spectrograph of the Very Large Telescope of stars probing local diffuse clouds. Absorption from the C15N isotopologue is confidently detected (at ≳ 4 &sgr; ? > ) in three out of the four directions studied and appears as a very weak feature between the main 12CN and 13CN absorption components. Column densities for each CN isotopologue are determined through profile fitting, after accounting for weak additional line-of-sight components of 12CN, which are seen in the absorption profiles of CH and CH+ as well. The weighted mean value of C14N/C15N for the three sight lines with detections of C15N is 274 ± 18. Since the diffuse molecular clouds toward our target stars have relatively high gas kinetic temperatures and relatively low visual extinctions, their C14N/C15N ratios should not be affected by chemical fractionation. The mean C14N/C15N ratio that we obtain should therefore be representative of the ambient 14N/15N ratio in the local interstellar medium. Indeed, our mean value agrees well with that derived from millimeter-wave observations of CN, HCN, and HNC in local molecular clouds.
Exoplanet science with the LBTI: instrument status and plans

The Large Binocular Telescope Interferometer (LBTI) is a strategic instrument of the LBT designed for highsensitivity, high-contrast, and high-resolution infrared (1.5-13 μm) imaging of nearby planetary systems. To carry out a wide range of high-spatial resolution observations, it can combine the two AO-corrected 8.4-m apertures of the LBT in various ways including direct (non-interferometric) imaging, coronagraphy (APP and AGPM), Fizeau imaging, non-redundant aperture masking, and nulling interferometry. It also has broadband, narrowband, and spectrally dispersed capabilities. In this paper, we review the performance of these modes in terms of exoplanet science capabilities and describe recent instrumental milestones such as first-light Fizeau images (with the angular resolution of an equivalent 22.8-m telescope) and deep interferometric nulling observations.
Effects of Free Amino Acids, Metallothionein, and Chemical Forms of Heavy Metals on the Accumulation and Detoxification of Cadmium and Chromium in Chinese Goldthread (Coptis chinensis Franch.)

Chinese goldthread (Coptis chinensis Franch.) is an important medicinal plant worldwide. However, its clinical safety is negatively impacted by high cadmium (Cd) and chromium (Cr) levels. Understanding the accumulation pattern and detoxification mechanism of heavy metals, such as Cd and Cr, is important for regulating their transportation and reducing their accumulation in plants. Free amino acids (FAAs), metallothioneins, and chemical forms of heavy metals are closely associated with heavy metal accumulation and detoxification mechanisms. In the present study, we evaluated the uptake of Cd and Cr in Chinese goldthread and characterized the changes in FAA levels, CcMT2, a metallothionein gene, expression under Cd and Cr stress, and Cr chemical forms in various tissues of Chinese goldthread. The majority of Cd and Cr was retained in the roots; this might be the tolerance strategy utilized by Chinese goldthread to protect the aboveground photosynthetic tissues. A chemical continuous extraction method was utilized to analyze the chemical forms of Cr, and the results suggested that Cr was primarily fixed by oxalate in all tissues, and after Cr treatment, Cr tended to combine with phosphate to form an insoluble complex that reduced the toxicity and bioavailability of Cr in Chinese goldthread. The accumulation of Cd and Cr was significantly positively correlated with valine, histidine, threonine, tyrosine, and serine levels and significantly negatively correlated with glutamic acid and alanine levels. The variation in proline levels under Cd stress was different than that under Cr stress. FAAs might affect the accumulation of and resistance to Cd and Cr through various detoxification strategies, such as chelation with heavy metals ions and conversion into the required products. Furthermore, CcMT2 was isolated for the first time and found to be dominantly expressed in leaves. CcMT2 was induced under Cd and Cr stress in all plant tissues, indicating its role in the accumulation of and tolerance to Cd and Cr.
Dynamical evolution of primordial dark matter haloes through mergers

Primordial darkmatter (DM) haloes are the smallest gravitationally bound DM structures from which the first stars, black holes and galaxies form and grow in the early universe. However, their structures are sensitive to the free streaming scale of DM, which in turn depends on the nature of DM particles. In this work, we test the hypothesis that the slope of the central cusps in primordial DM haloes near the free streaming scale depends on the nature of merging process. By combining and analysing data from a cosmological simulation with the cutoff in the small-scale matter power spectrum as well as a suite of controlled, high-resolution simulations of binary mergers, we find that (1) the primordial DM haloes form preferentially through major mergers in radial orbits;(2) their central DM density profile is more susceptible to a merging process compared to that of galaxy-and cluster-sized DM haloes;(3) consecutive major mergers drive the central density slope to approach the universal form characterized by the Navarro-Frenk-White profile, which is shown to be robust to the impacts of mergers and serves an attractor solution for the density structure of DM haloes. Our work highlights the importance of dynamical processes on the structure formation during the Dark Ages.
SUPPRESSION OF STAR FORMATION IN THE HOSTS OF LOW-EXCITATION RADIO GALAXIES

The feedback from radio-loud active galactic nuclei (R-AGNs) may help maintain low star-formation (SF) rates in their early-type hosts, but the observational evidence for this mechanism has been inconclusive. We study systematic differences of aggregate spectral energy distributions (SEDs) of various subsets of ∼4000 low-redshift R-AGNs from Best & Heckman with respect to (currently) inactive control samples selected to have matching redshift, stellar mass, population age, axis ratio, and environment. Aggregate SEDs, ranging from the ultraviolet (UV) through mid-infrared (mid-IR, 22 μm), were constructed using a Bayesian method that eliminates biases from non-detections in Galaxy Evolution Explorer and Wide-field Infrared Survey Explorer. We study rare high-excitation sources separately from low-excitation ones, which we split by environment and host properties. We find that both the UV and mid-IR emission of non-cluster R-AGNs (80% of sample) are suppressed by ∼0.2 dex relative to that of the control group, especially for moderately massive galaxies (log M* ≲ 11). The difference disappears for high-mass R-AGNs and for R-AGNs in clusters, where other, non-AGN quenching/maintenance mechanisms may dominate, or where the suppression of SF due to AGNs may persist between active phases of the central engine, perhaps because of the presence of a hot gaseous halo storing AGN energy. High-excitation (high accretion rate) sources, which make up 2% of the R-AGN sample, do not show any evidence of SF suppression (their UV is the same as in controls), but they exhibit a strong mid-IR excess due to AGN dust heating.
Mortality trend of heart diseases in China, 2013–2020

Background and purpose: Heart diseases are the leading cause of death in China. Understanding of the secular trend of different subcategories of heart disease is important for policy making. The purpose of this study is to analyze the mortality trend of heart diseases in China from 2013 to 2020. Methods: A population-based longitudinal analysis was conducted using the China National Mortality Surveillance System to examine heart disease mortality change during a period from 2013 to 2020. The causes of death were coded using the International Classification of Diseases-10th Revision. The number of deaths and mortality rate were calculated based on sex, subcategories of heart disease, urban versus rural setting, and across different geographic locations. Data from the sixth census in China in 2010 was used as the standard population, and the mortality rates were adjusted based on the under-reporting rate. Results: Ischemic heart disease (IHD), hypertensive heart disease (HHD), and rheumatic heart disease (RHD) are the three leading causes of heart disease deaths during 2013–2020. There was a trend for increased age-standardized mortality rate (ASMR) of cardiac arrest, aortic aneurysm (AA), and nonrheumatic valvular heart diseases (NRVHDs) during the study period. In comparison to men, women had higher ASMR of RHD, and lower ASMR of IHD, HHD, cardiac arrest, AA, and NRVHDs. In comparison to rural areas, urban areas had lower ASMR of IHD, HHD, and RHD, and higher ASMR of cardiac arrest, AA, and NRVHDs. The spectrum of heart diseases differed significantly across age groups. In 2020, the percentages of IHD and HHD in the ≥65-year age group were higher than in other age groups. Significant differences in ASMR were noted across different geographic locations, with the highest in Xinjiang (198.14/100,000) and the lowest in Shanghai (62.19/100,000) in 2020. Conclusions: The mortality rate decreased for IHD, HHD, and RHD during the study period, but remained the leading causes of heart disease death in China. There was a trend for increasing mortality of cardiac arrest, AA, and NRVHDs, and significant difference across different geographic locations.
The Effect of Parental Attention on Learning Outcomes in Elementary School Students

This study aims to determine the positive and significant influence and the magnitude of the effective contribution of parental attention on mathematics learning outcomes in elementary school students. This quantitative research employed the correlation method. The research samples were 260 public elementary school students in the Central Java, taken by cluster random sampling. Research data were collected by distributing questionnaires and test instruments. The data were then analyzed utilizing the SPSS version 25 application. From the regression analysis performed, the t-count value was 8.909 ≥ t-table of 1.969, and the Sig. was 0.000 ≤ 0.05. It indicates that parental attention had a positive and significant effect on students' mathematics learning outcomes. In addition, the correlation analysis results obtained r-count = 0.485 > r-table (df = 260) = 0.121, with an effective contribution value of 23.5%. Thus, it is concluded that there was a significant influence and effective contribution of parental attention on the learning outcomes of public elementary school students in the Gebang Sub-district, Purworejo Regency.
CONSTRAINING THE DYNAMICAL IMPORTANCE OF HOT GAS AND RADIATION PRESSURE IN QUASAR OUTFLOWS USING EMISSION LINE RATIOS

Quasar feedback models often predict an expanding hot gas bubble that drives a galaxy-scale outflow. In many circumstances this hot gas radiates inefficiently and is therefore difficult to observe directly. We present an indirect method to detect the presence of a hot bubble using hydrostatic photoionization calculations of the cold ( ∼ 10 4 K ? > ) line-emitting gas. We compare our calculations with observations of the broad line region, the inner face of the torus, the narrow line region (NLR), and the extended NLR, and thus constrain the hot gas pressure at distances 0.1 pc – 10 kpc ? > from the center. We find that emission line ratios observed in the average quasar spectrum are consistent with radiation-pressure-dominated models on all scales. On scales < 40 pc ? > a dynamically significant hot gas pressure is ruled out, while on larger scales the hot gas pressure cannot exceed six times the local radiation pressure. In individual quasars, ≈25% of quasars exhibit NLR ratios that are inconsistent with radiation-pressure-dominated models, although in these objects the hot gas pressure is also unlikely to exceed the radiation pressure by an order of magnitude or more. The derived upper limits on the hot gas pressure imply that the instantaneous gas pressure force acting on galaxy-scale outflows falls short of the time-averaged force needed to explain the large momentum fluxes p ˙ ≫ L AGN / c ? > inferred for galaxy-scale outflows. This apparent discrepancy can be reconciled if optical quasars previously experienced a buried, fully obscured phase during which the hot gas bubble was more effectively confined and during which galactic wind acceleration occurred.