Miracle-dz/UniFAR-FTUs huggingface dataset:
THE ACS FORNAX CLUSTER SURVEY. IX. THE COLOR–MAGNITUDE RELATION OF GLOBULAR CLUSTER SYSTEMS

We investigate the color–magnitude relation for globular clusters (GCs)—the so-called blue tilt—detected in the Advanced Camera for Surveys (ACS) Fornax Cluster Survey and using the combined sample of GCs from the ACS Fornax and Virgo Cluster Surveys. We find a tilt of γz ≡ d(g − z)/dz = −0.0257 ± 0.0050 for the full GC sample of the Fornax Cluster Survey (≈5800 GCs). This is slightly shallower than the value γz = −0.0459 ± 0.0048 found for the Virgo Cluster Survey GC sample (≈11,100 GCs). The slope for the merged Fornax and Virgo data sets (≈16,900 GCs) is γz = −0.0293 ± 0.0085, corresponding to a mass–metallicity relation of Z ∝ M0.43±0.12. We find that the blue tilt sets in at masses in excess of M ∼ 2 × 105 M☉. The tilt is stronger for GCs belonging to high-mass galaxies (M* ≳ 5 × 1010 M☉) than for those in low-mass galaxies (M* ≲ 5 × 1010 M☉). It is also more pronounced for GCs with smaller galactocentric distances. Our findings suggest a range of mass–metallicity relations ZGC ∝ M0.3–0.7GC which vary as a function of host galaxy mass/luminosity, a scaling similar to that observed for dwarf spheroidal galaxies. We compare our observations to a recent model of star cluster self-enrichment with generally favorable results. We suggest that, within the context of this model, the protocluster clouds out of which the GCs formed may have had density profiles slightly steeper than isothermal and/or star formation efficiencies somewhat below 0.3. We caution, however, that the significantly different appearance of the color–magnitude diagrams (CMDs) defined by the GC systems associated with galaxies of similar mass and morphological type poses a challenge to any single mechanism, including self-enrichment, that seeks to explain generically the observed GC color–magnitude relations. We therefore suggest that the detailed (and stochastic) merger/accretion histories of individual galaxies have likely played a non-negligible role determining the distribution of GCs in the CMDs of individual GC systems.
A simple and robust method for automated photometric classification of supernovae using neural networks

A method is presented for automated photometric classificat ion of supernovae (SNe) as TypeIa or non-Ia. A two-step approach is adopted in which: (i) the SN lightcurve flux measurements in each observing filter are fitted separately to an anal ytical parameterised function that is sufficiently flexible to accommodate vitrually all types o f SNe; and (ii) the fitted function parameters and their associated uncertainties, along with the number of flux measurements, the maximum-likelihood value of the fit and Bayesian evidenc e for the model, are used as the input feature vector to a classification neural network ( NN) that outputs the probability that the SN under consideration is of Type-Ia. The method is trained and tested using data released following the SuperNova Photometric Classificati on Challenge (SNPCC), consisting of lightcurves for 21,319 SNe in total. We consider several r andom divisions of the data into training and testing sets: for instance, for our sample D1 (D4), a total of 10 (40) per cent of the data are involved in training the algorithm and the remai nder used for blind testing of the resulting classifier; we make no selection cuts. Assigning a canonical threshold probability of pth = 0.5 on the network output to class a SN as Type-Ia, for the sample D1 (D4) we obtain a completeness of 0.78 (0.82), purity of 0.77 (0.82), an d SNPCC figure-of-merit of 0.41 (0.50). Including the SN host-galaxy redshift and its uncer tainty as additional inputs to the classification network results in a modest 5‐10 per cent incr ease in these values. We find that the quality of the classification does not vary significantly with SN redshift. Moreover, our probabilistic classification method allows one to calculat e the expected completeness, purity and figure-of-merit (or other measures of classification qua lity) as a function of the threshold probability pth, without knowing the true classes of the SNe in the testing sample, as is the case in the classification of real SNe data. The method may thus be improved further by optimising pth and can easily be extended to divide non-Ia SNe into their different classes.
THE SPITZER VIEW OF LOW-METALLICITY STAR FORMATION. III. FINE-STRUCTURE LINES, AROMATIC FEATURES, AND MOLECULES

We present low- and high-resolution Spitzer/IRS spectra, supplemented by Infrared Array Camera and Multiband Imaging Photometer for Spitzer measurements, of 22 blue compact dwarf (BCD) galaxies. The BCD sample spans a wide range in oxygen abundance (12+log(O/H) between 7.4 and 8.3), and hardness of the interstellar radiation field (ISRF). The Infrared Spectrograph (IRS) spectra provide us with a rich set of diagnostics to probe the physics of star and dust formation in very low metallicity environments. We find that metal-poor BCDs have harder ionizing radiation than metal-rich galaxies: [O iv] emission is ≳4 times as common as [Fe ii] emission. They also have a more intense ISRF, as indicated by the 71 to 160 μm luminosity ratio. Two-thirds of the sample (15 BCDs) show polycyclic aromatic hydrocarbon (PAH) features, although the fraction of PAH emission normalized to the total infrared (IR) luminosity is considerably smaller in metal-poor BCDs (∼0.5%) than in metal-rich star-forming galaxies (∼10%). We find several lines of evidence for a deficit of small PAH carriers at low metallicity, and attribute this to destruction by a hard, intense ISRF, only indirectly linked to metal abundance. Our IRS spectra reveal a variety of H2 rotational lines, and more than a third of the objects in our sample (eight BCDs) have ≳3σ detections in one or more of the four lowest-order transitions. The warm gas masses in the BCDs range from 103 M☉ to 108 M☉, and can be comparable to the neutral hydrogen gas mass; relative to their total IR luminosities, some BCDs contain more H2 than Spitzer Nearby Galaxy Survey galaxies.
Detecting Gaussian entanglement via extractable work

We show how the presence of entanglement in a bipartite Gaussian state can be detected by the amount of work extracted by a continuos variable Szilard-like device, where the bipartite state serves as the working medium of the engine. We provide an expression for the work extracted in such a process and specialize it to the case of Gaussian states. The extractable work provides a sufficient condition to witness entanglement in generic two-mode states, becoming also necessary for squeezed thermal states. We extend the protocol to tripartite Gaussian states, and show that the full structure of inseparability classes cannot be discriminated based on the extractable work. This suggests that bipartite entanglement is the fundamental resource underpinning work extraction.
The strength and detectability of the YORP effect in near-Earth asteroids: a statistical approach

In addition to collisions and gravitational forces, it is now becoming widely acknowledged that photon recoil forces and torques from the asymmetric reflection and thermal re-radiation of sunlight are primary mechanisms that govern the rotational evolution of an asteroid. The Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect causes changes in the rotation rate and pole direction of an irregularly shaped asteroid. We present a simple Monte Carlo method to estimate the range of YORP rotational accelerations acting on a near-Earth asteroid (NEA) without knowledge of its detailed shape, and to estimate its detectability using light-curve observations. The method requires knowledge of an asteroid's orbital properties and size, and assumes that the future observational circumstances of an asteroid have already been thought through. It is verified by application to the observational circumstances of the seven YORP-investigated asteroids, and is then applied to 540 NEAs with NEOWISE and/or other diameter measurements, and to all NEAs using Minor Planet Center Orbit absolute magnitudes. The YORP detectability is found to be a strong function of the combined asteroid orbital and diameter properties, and is independent of the rotation period for NEAs that do not have very fast or slow rotation rates. The median and 1σ spread of YORP rotational acceleration expected to be acting on a particular NEA (dω/d t in rad yr −2 ) can be estimated from its semimajor axis ( a in au), eccentricity ( e ) and diameter ( D in km) by using |dω/d t |=1.20 +1.66 −0.86 ×10 −2 ( a 2 √1− e 2 D 2 ) −1 and/or by using |dω/d t |=1.00 +3.07 −0.81 ×10 −2 ( a 2 √1− e 2 D 2 ) −1 if the diameter is instead estimated from the absolute magnitude by assuming a geometric albedo of 0.1. The length of a light-curve observational campaign required to achieve a 50 per cent probability of detecting the YORP effect in a particular NEA ( T CAM_50 in yr) can be estimated by using T CAM_50 =12.5( a 2 √1− e 2 D 2 ) 1/2 and/or by using T CAM_50 =13.7( a 2 √1− e 2 D 2 ) 1/2 for an absolute-magnitude-estimated diameter. To achieve a 95 per cent YORP-detection probability, these last two relations need to be multiplied by factors of ~3.4 and ~4.5, respectively. This method and approximate relations will be useful for astronomers who plan to look for YORP rotational acceleration in specific NEAs, and for all-sky surveys that may serendipitously observe NEA light curves.
PARSEC-SCALE RADIO EMISSION FROM THE LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE DWARF STARBURST GALAXY HENIZE 2-10

A candidate accreting massive black hole (BH) with MBH ∼ 106 M☉ has recently been identified at the center of the dwarf starburst galaxy Henize 2-10 (He 2-10). This discovery offers the first possibility of studying a growing BH in a nearby galaxy resembling those in the earlier universe, and opens up a new class of host galaxies to search for the smallest supermassive BHs. Here we present very long baseline interferometry observations of He 2-10 taken with the Long Baseline Array (LBA) at 1.4 GHz with an angular resolution of ∼0. ″1 × 0. ″03. A single compact radio source is detected at the precise location of the putative low-luminosity active galactic nucleus. The physical size of the nuclear radio emission is ≲3 pc × 1 pc, an order of magnitude smaller than previous constraints from the Very Large Array (VLA), and the brightness temperature of TB > 3 × 105 K confirms a non-thermal origin. These LBA observations indicate that the nuclear radio emission originates from a single object, and exclude the possibility of multiple supernova remnants as the origin of the nuclear radio emission previously detected with the VLA at lower resolution. A weaker, more extended, off-nuclear source is also detected with the LBA and a comparison with multi-wavelength ancillary data indicate that, unlike the nuclear source, the off-nuclear source is co-spatial with a super star cluster, lacks a detectable X-ray point-source counterpart, and is almost certainly due to a supernova remnant in the host star cluster.
Physical properties of galactic winds using background quasars

Background quasars are potentially sensitive probes of galactic outflows provided that one can determine the origin of the absorbing material since both gaseous disks and strong bipolar outflows can contribute to the absorption cross-section. Using a dozen quasars passing near spectroscopically identified galaxies at z 0:1, we find that the azimuthal orientation of the quasar sight-lines with strong Mg II absorption (withW 2796 r > 0:3 ˚ A) is bi-modal: about half the Mg II sight-lines are aligned with the major axis and the other half are within = 30 of the minor axis, suggesting that bipolar outflows can contribute to the Mg II cross-section. This bi-modality is also present in the instantaneous star-formation rates (SFRs) of the hosts. For the sight-lines aligned along the minor axis, a simple bi-conical wind model is indeed able to reproduce the observed Mg II kinematics and the Mg II dependence with impact parameter b, (W 2796 r / b 1 ). Using our wind model, we can directly extract key wind properties such as the de-projected outflow speed Vout of the cool material traced by Mg II and the outflow rates _ Mout. The outflow speeds Vout are found to be 150-300 kms 1 , i.e. of the order of the circular velocity, and smaller than the escape velocity by a factor of 2. The outflow rates _ Mout are typically two to three times the instantaneous SFRs. Our results demonstrate how background quasars can be used to measure wind properties with high precision.
Search for Ultra-High-Energy Neutrinos with AMANDA-II

A search for diffuse neutrinos with energies in excess of 105 GeV is conducted with AMANDA-II data recorded between 2000 and 2002. Above 107 GeV, the Earth is essentially opaque to neutrinos. This fact, combined with the limited overburden of the AMANDA-II detector (roughly 1.5 km), concentrates these ultra-high-energy neutrinos at the horizon. The primary background for this analysis is bundles of downgoing, high-energy muons from the interaction of cosmic rays in the atmosphere. No statistically significant excess above the expected background is seen in the data, and an upper limit is set on the diffuse all-flavor neutrino flux of E2Φ90% CL < 2.7 × 10−7 GeV cm−2 s−1 sr−1 valid over the energy range of 2 × 105 to 109 GeV. A number of models that predict neutrino fluxes from active galactic nuclei are excluded at the 90% confidence level.
THE PROGENITOR OF SN 2011ja: CLUES FROM CIRCUMSTELLAR INTERACTION

Massive stars, possibly red supergiants, which retain extended hydrogen envelopes until core collapse, produce Type II plateau (IIP) supernovae. The ejecta from these explosions shocks the circumstellar matter originating from the mass loss of the progenitor during the final phases of its life. This interaction accelerates particles to relativistic energies which then lose energy via synchrotron radiation in the shock-amplified magnetic fields and inverse Compton scattering against optical photons from the supernova. These processes produce different signatures in the radio and X-ray parts of the electromagnetic spectrum. Observed together, they allow us to break the degeneracy between shock acceleration and magnetic field amplification. In this work, we use X-rays observations from the Chandra and radio observations from the Australia Telescope Compact Array to study the relative importance of processes which accelerate particles and those which amplify magnetic fields in producing the non-thermal radiation from SN 2011ja. We use radio observations to constrain the explosion date. Multiple Chandra observations allow us to probe the history of variable mass loss from the progenitor. The ejecta expands into a low-density bubble followed by interaction with a higher density wind from a red supergiant consistent with MZAMS ≳ 12 M☉. Our results suggest that a fraction of Type IIP supernovae may interact with circumstellar media set up by non-steady winds.
Preconscious categorization impacts how interracial same-sex couples are perceived by others: Implications for counseling and supervision

Abstract Introduction In order to understand implicit biases, we examined participants’ preconscious neural activity when viewing photos of differing racial combinations of same-sex male couples. Method P200 amplitudes measured preconscious neural activity while viewing photo stimuli. Result Participants engaged in preconscious categorization of all three types of photo stimuli. The largest P200 amplitudes appeared when viewing photos of Black gay couples, followed by White-Black gay couples, then White gay couples. Conclusion Individuals begin to categorize same-sex couples by their racial makeup as early as 200 milliseconds. Evidence of preconscious categorization may be helpful in dispelling inaccuracies of using a colorblindness approach to counseling and supervision.
REVISITING THE SOLAR TACHOCLINE: AVERAGE PROPERTIES AND TEMPORAL VARIATIONS

The tachocline is believed to be the region where the solar dynamo operates. With over a solar cycle's worth of data available from the Michelson Doppler Imager and Global Oscillation Network Group instruments, we are in a position to investigate not merely the average structure of the solar tachocline, but also its time variations. We determine the properties of the tachocline as a function of time by fitting a two-dimensional model that takes latitudinal variations of the tachocline properties into account. We confirm that if we consider the central position of the tachocline, it is prolate. Our results show that the tachocline is thicker at latitudes higher than the equator, making the overall shape of the tachocline more complex. Of the tachocline properties examined, the transition of the rotation rate across the tachocline, and to some extent the position of the tachocline, show some temporal variations.
A SEARCH FOR INFALL EVIDENCE IN EGOs. I. THE NORTHERN SAMPLE

We report the first systematic survey of molecular lines (including HCO+ (1–0) and 12CO, 13CO, C18O (1–0) lines at the 3 mm band) toward a new sample of 88 massive young stellar object (MYSO) candidates associated with ongoing outflows (known as extended green objects or EGOs) identified from the Spitzer GLIMPSE survey in the northern hemisphere with the Purple Mountain Observatory 13.7 m radio telescope. By analyzing the asymmetries of the optically thick line HCO+ for 69 of 72 EGOs with HCO+ detection, we found 29 sources with “blue asymmetric profiles” and 19 sources with “red asymmetric profiles. ” This results in a blue excess of 0.14, seen as a signature of collapsing cores in the observed EGO sample. We found that the sources not associated with infrared dark clouds (IRDCs) show a higher blue excess (0.41) than those associated with IRDCs (−0.08), and “possible” outflow candidates show a higher blue excess (0.29) than “likely” outflow candidates (0.05). A higher blue excess (0.19) and a lower blue excess (0.07) were also measured in ultracompact H ii regions and 6.7 GHz class II methanol maser sources, respectively. These suggest that the relatively small blue excess (0.14) in our full sample is due to the fact that the observed EGOs are mostly dominated by outflows and at an earlier evolutionary phase associated with IRDCs and 6.7 GHz methanol masers. The physical properties of clouds surrounding EGOs derived from CO lines are similar to those of massive clumps wherein the massive star-forming cores associated with EGOs possibly embedded. The infall velocities and mass infall rates derived for 20 infall candidates are also consistent with the typical values found in MYSOs. Thus, our observations further support the speculation of Cyganowski et al. that EGOs trace a population with ongoing outflow activity and at the active rapid accretion stage of massive protostellar evolution from a statistical view, although there may be limitations due to a single-pointing survey with a large beam.
ILLUMINATING THE PRIMEVAL UNIVERSE WITH TYPE IIn SUPERNOVAE

The detection of Population III (Pop III) supernovae (SNe) could directly probe the primordial initial mass function for the first time, unveiling the properties of the first galaxies, early chemical enrichment and reionization, and the seeds of supermassive black holes. Growing evidence that some Pop III stars were less massive than 100 M☉ may complicate prospects for their detection, because even though they would have been more plentiful, they would have died as core-collapse SNe, with far less luminosity than pair-instability explosions. This picture greatly improves if the SN shock collides with a dense circumstellar shell ejected during a prior violent luminous blue variable type eruption. Such collisions can turn even dim SNe into extremely bright ones whose luminosities can rival those of pair-instability SNe. We present simulations of Pop III Type IIn SN light curves and spectra performed with the Los Alamos RAGE and SPECTRUM codes. Taking into account Lyα absorption in the early universe and cosmological redshifting, we find that 40 M☉ Pop III Type IIn SNe will be visible out to z ∼ 20 with the James Webb Space Telescope and out to z ∼ 7 with WFIRST. Thus, even low mass Pop III SNe can be used to probe the primeval universe.
IN SITU AND EX SITU FORMATION MODELS OF KEPLER 11 PLANETS

We present formation simulations of the six Kepler 11 planets. Models assume either in situ or ex situ assembly, the latter with migration, and are evolved to the estimated age of the system, . Models combine detailed calculations of both the gaseous envelope and the condensed core structures, including accretion of gas and solids, of the disk’s viscous and thermal evolution, including photo-evaporation and disk-planet interactions, and of the planet’s evaporative mass loss after disk dispersal. Planet–planet interactions are neglected. Both sets of simulations successfully reproduce measured radii, masses, and orbital distances of the planets, except for the radius of Kepler 11b, which loses its entire gaseous envelope shortly after formation. Gaseous (H+He) envelopes account for % of the planet masses, and between and % of the planet radii. In situ models predict a very massive inner disk, whose solid surface density ( ) varies from over 104 to at stellocentric distances . Initial gas densities would be in excess of if solids formed locally. Given the high disk temperatures ( ), planetary interiors can only be composed of metals and highly refractory materials. Sequestration of hydrogen by the core and subsequent outgassing is required to account for the observed radius of Kepler 11b. Ex situ models predict a relatively low-mass disk, whose initial varies from to at and whose initial gas density ranges from to . All planetary interiors are expected to be rich in H2O, as core assembly mostly occurs exterior to the ice condensation front. Kepler 11b is expected to have a steam atmosphere, and H2O is likely mixed with H+He in the envelopes of the other planets. Results indicate that Kepler 11g may not be more massive than Kepler 11e.
Chemical Analysis of Five Red Giants in the Globular Cluster M10 (NGC 6254)

We have determined Al, α, Fe-peak, and neutron capture elemental abundances for five red-giant branch (RGB) stars in the Galactic globular cluster M10. Abundances were determined using equivalent width analyses of moderate-resolution (R ∼ 15,000) spectra obtained with the Hydra multifiber positioner and bench spectrograph on the WIYN telescope. The data sample the upper RGB from the luminosity level near the horizontal branch to about 0.5 mag below the RGB tip. We find, in agreement with previous studies, that M10 is moderately metal-poor with [Fe/H] = -1.45 (σ = 0.04). All stars appear enhanced in Al with 〈[Al/Fe]〉 = +0.33 (σ = 0.19), but no stars have [Al/Fe] ≳ +0.55. We find the α elements to be enhanced by +0.20 to +0.40 dex and the Fe-peak elements to have [el/Fe] ∼ 0, which are consistent with predictions from type II SNe ejecta. Additionally, the cluster appears to be r-process rich with 〈[Eu/La]〉 = +0.41.
Municipal solid waste charging based on residents’ preference, a case of Harbin City, China

ABSTRACT Municipal solid waste management (MSWM) has been an increasing challenge for cities in China. Effective and sensible charging mechanism of municipal solid waste (MSW) needs to be designed to abate rapid generation of MSW from its source. This paper investigates four aspects related to public preference on MSW charging, including cleanliness, frequency, time, and cost. A case study was conducted in Harbin, which is a megacity in China and one of the first pilot cities for MSW classification. This study adopted stratified sampling approach in surveying Harbin residents, which generated a final sample of 280 residents for empirical investigation. Conjoint analysis was employed to analyze residents’ preference for MSW charging. The results demonstrate that the preference varies with the level of income. High-income and middle-income residents are more favourable to cleanliness, while the low-income group is more concerned about the cost of MSWM. To a large extent, this difference may be related to differences in personal needs and consumption patterns.