Miracle-dz/UniFAR-FTUs huggingface dataset:
Spikes in the SED and ripples in the outskirts of galaxies

Abstract We describe a new method that allows us to quantitatively characterize galactic satellites from analysis of disturbances in outer gas disks, without requiring knowledge of their optical light. We have demonstrated the validity of this method, which we call Tidal Analysis, by applying it to local spirals with known optical companions, including M51 and NGC 1512. These galaxies span the range from having a low mass companion (~ one-hundredth the mass of the primary galaxy) to a fairly massive companion (~ one-third the mass of the primary galaxy). This approach has broad implications for many areas of astrophysics – for the indirect detection of dark matter (or dark matter-dominated dwarf galaxies), and for galaxy evolution in its use as a decipher of the dynamical impact of satellites on galactic disks. Here, we present some preliminary results on the emergent SEDs and images, calculated along the time sequence of these dynamical simulations using the 3-D self-consistent Monte Carlo radiative transfer code RADISHE. We explore star formation prescriptions and how they affect the emergent SEDs and images. Our goal is to identify SED colors that are primarily affected by the galaxy's interaction history, and are not significantly affected by the choice of star formation prescription. If successful, we may be able to utilize the emergent UV-IR SED of the primary galaxy to understand its recent interaction history.
The metallicity distribution of bulge clump giants in Baade’s window

Aims. We seek to constrain the formation of the Galactic bulge by analysing the detailed chemical composition of a large sample of red clump stars in Baade’s window. These stars were selected to minimise the contamination by other Galactic components, so they are good tracers of the bulge metallicity distribution in Baade’s window, at least for stars more metal-rich than ∼−1.5. Methods. We used an automatic procedure to measure [Fe/H] differentially with respect to the metal-rich star μLeo in a sample of 219 bulge red clump stars from R = 20 000 resolution spectra obtained with FLAMES/GIRAFFE at the VLT. For a subsample of 162 stars, we also derived [Mg/H] from spectral synthesis around the Mg i triplet at λ 6319 A. Results. The Fe and Mg metallicity distributions are both asymmetric with median values of +0.16 and +0.21, respectively. They show only a small proportion of stars at low metallicities, extending down to [Fe/H] = −1. 1o r [Mg/H] = −0.7. The iron distribution is clearly bimodal, as revealed both by a deconvolution (from observational errors) and a Gaussian decomposition. The decomposition of the observed Fe and Mg metallicity distributions into Gaussian components yields two populations of equal sizes (50% each): a metal-poor component centred on [Fe/H] = −0.30 and [Mg/H] = −0.06 with a large dispersion and a narrow metal-rich component centred on [Fe/H] =+ 0.32 and [Mg/H] =+ 0.35. The metal-poor component shows high [Mg/Fe] ratios (around 0.3), while stars in the metal-rich component are found to have nearly solar ratios. Kinematical differences between the two components have also been found: the metal-poor component shows kinematics compatible with an old spheroid, while the metal-rich component is consistent with a population supporting a bar. In view of their chemical and kinematical properties, we suggest different formation scenarii for the two populations: a rapid formation time scale as an old spheroid for the metal-poor component (old bulge) and for the metal-rich component, a formation on a longer time scale driven by the evolution of the bar (pseudo-bulge). The observations are described well by a simple model consisting of two components: a simple closed box model to predict the metal-poor population contribution and a local thin disc metallicity distribution, shifted in metallicity, to represent the metal-rich population. The pseudo-bulge is compatible with its being formed from the inner thin disc, assuming high (but plausible) values of the gradients in the early Galactic disc.
Relativistic mechanical–thermodynamical formalism—description of inelastic collisions

We present a relativistic formalism inspired by the Minkowski four-vectors that also includes conservation laws such as the first law of thermodynamics. It remains close to the relativistic four-vector formalism developed for a single particle, but is also related to the classical treatment of problems that require both Newton's second law and the energy conservation law. We apply the developed formalism to inelastic collisions to better show how it works.
Constraint on pulsar wind properties from induced Compton scattering off radio pulses

Constraint on pulsar wind properties from induced Compton scattering off radio pulses Shuta J. Tanaka1,∗ and Fumio Takahara2 1Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa City, Chiba 277-8582, Japan 2Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka, Osaka 560-0043, Japan ∗E-mail: sjtanaka@icrr.u-tokyo.ac. jp
Interpretation of HINODE SOT/SP asymmetric Stokes profiles observed in the quiet Sun network and internetwork

Aims. Stokes profiles emerging from the magnetized solar photosphere and observed by SOT/SP aboard the HINODE satellite present a variety of complex shapes. These are indicative of unresolved magnetic structures that have been overlooked in the inversion analyses performed so far. Here we present the first interpretation of the Stokes profile asymmetries measured in the Fei 630 nm lines by SOT/SP, in both quiet Sun internetwork (IN) and network regions. Methods. The inversion is carried out under the hypothesis of MIcro-Structured Magnetized Atmosphere (MISMA), where the unresolved structure is assumed to be optically thin. We analyze a 29.52 00 � 31.70 00 subfield carefully selected to be representative of the properties of a 302 00 � 162 00 quiet Sun field-of-view at disk center. Results. The inversion code is able to reproduce the observed asymmetries in a very satisfactory way, including the 35 % of inverted profiles presenting large asymmetries. The inversion code interprets 25 % of inverted profiles as emerging from pixels in which both positive and negative polarities coexist. These pixels are located either in frontiers between opposite polarity patches or in very quiet regions. kG field strengths are found at the base of the photosphere in both network and IN; in the case of the latter, both kG fields and hG fields are admixed. When considering the magnetic properties at the mid photosphere most kG fields are gone, and the statistics is dominated by hG fields. According to the magnetic filling factors derived from the inversion, we constrain the magnetic field of only 4.5 % of the analyzed photosphere (and this percentage reduces to 1.3 % when referred to all pixels, including those with low polarization not analyzed). The rest of the plasma is consistent with the presence of weak fields not contributing to the detected polarization signals. The average flux densities derived in the full subfield and in IN regions are higher than the ones derived from the same dataset by Milne-Eddington inversion. Conclusions. The existence of large asymmetries in HINODE SOT/SP polarization profiles is uncovered. These are not negligible in quiet Sun data. The MISMA inversion code reproduces them in a satisfactory way, and provides a statistical description of the magnetized IN and network which partly differs and complements the results obtained so far. From this it follows the importance of having a complete interpretation of the line profile shapes.
Hot gas in groups: NGC 5328 and the intriguing case of NGC 4756 with XMM-Newton

Context. Environment appears to have a strong influence on the fundamental properties of galaxies, modifying both their morphologies and their star formation histories. Similarly, galaxies play a role in determining the properties of the hot intergalactic medium in groups, heating and enriching it through a variety of mechanisms. NGC 5238 and NGC 4756 are the brightest unperturbed elliptical galaxies in their respective loose groups, but the analysis of their environment suggests that they may be at different evolutionary stages. Aims. We aim to characterize the properties of the hot gas in both the halos of the brightest galaxy members and in the environment. In NGC 4756, we are also interested in the properties of a substructure identified to the southwest and the region connecting the two structures, to search for a physical connection between the two. However, we have to take into account that the group is projected against the bright, X-ray emitting cluster A1361, which heavily contaminates and confuses the emission from the foreground structure. Methods. We present XMM-Newton observations of the groups and a careful analysis to separate different components. We examine the X-ray morphology, hot gas distribution, and spectral characteristics of both NGC 4756 and NGC 5328 and their companion galaxies. To better characterize the environment, we also present a re-evaluation of the dynamical properties of the systems. Smoothed particle hydrodynamical simulations are used to interpret the results. Results. We find that the X-ray source associated with NGC 4756 indeed sits on top of extended emission from the background cluster A1361, but can be distinguished relatively well from it as a significant excess out to r ∼ 150 �� (∼40 kpc). NGC 4756 has an X-ray luminosity of Lx ∼ 10 41 erg s −1 due to hot gas, with an average temperature of kT ∼ 0.7 keV. We measure a faint diffuse emission in the region of the subclump to the SW, but more interestingly, we detect gas between the two structures, indicating a possible physical connection. The X-ray emission from NGC 5328 is clearly peaked on the galaxy, has Lx ∼ 10 41 erg s −1 , and extends to r ∼ 110 kpc. Simulations provide an excellent reproduction of the spectral energy distribution and the global properties of both galaxies, which are caught at two different epochs of the same evolutionary process, with NGC 5328 ∼ 2.5 Gyr younger than NGC 4756.
Measuring and using non-Markovianity

We construct measures for the non-Markovianity of quantum evolution with a physically meaningful interpretation. We first provide a general setting in the framework of channel capacities and propose two families of meaningful quantitative measures, based on the largest revival of a channel capacity, avoiding some drawbacks of other non-Markovianity measures. We relate the proposed measures to the task of information screening. This shows that the non-Markovianity of a quantum process may be used as a resource. Under these considerations, we analyze two paradigmatic examples, a qubit in a quantum environment with classically mixed dynamics and the Jaynes-Cummings model.
COMMON ORIGIN OF TWO RR LYRAE POPULATIONS AND THE DOUBLE RED CLUMP IN THE MILKY WAY BULGE

A recent survey looking toward the Milky Way bulge has discovered two sequences of RR Lyrae stars on the period–amplitude diagram with a maximum period-shift of P ≈ 0.015 between the two populations. Here we show, from our synthetic horizontal-branch models, that this period-shift is most likely due to the small difference in helium abundance (ΔY = 0.012) between the first- and second-generation stars (G1 and G2), as is the case in our models for the inner halo globular clusters with similar metallicity ([Fe/H] ≈ −1.1). We further show that the observed double red clump (RC) in the bulge is naturally reproduced when these models are extended to solar metallicity following ΔY/ΔZ ≈ 6 for G2, as would be expected from the chemical evolution models. Therefore, the two populations of RR Lyrae stars and the double RC observed in the bulge appear to be different manifestations of the same multiple population phenomenon in the metal-poor and metal-rich regimes, respectively.
Wide binaries in Tycho-Gaia II: metallicities, abundances and prospects for chemical tagging

From our recent catalog based on the first Gaia data release (TGAS), we select wide binaries in which both stars have been observed by the Radial Velocity Experiment (RAVE) or the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST). Using RAVE and LAMOST metallicities and RAVE Mg, Al, Si, Ti, and Fe abundances, we find that the differences in the metallicities and elemental abundances of components of wide binaries are consistent with being due to observational uncertainties, in agreement with previous results for smaller and more restricted samples. The metallicity and elemental abundance consistency between wide binary components presented in this work confirms their common origin and bolsters the status of wide binaries as "mini-open clusters. " Furthermore, this is evidence that wide binaries are effectively co-eval and co-chemical, supporting their use for e.g., constraining age-activity-rotation relations, the initial-final mass relation for white dwarfs, and M-dwarf metallicity indicators. Additionally, we demonstrate that the common proper motion, common parallax pairs in TGAS with the most extreme separations (s $\gtrsim$ 0.1 pc) typically have inconsistent metallicities, radial velocities or both and are therefore likely to be predominantly comprised of random alignments of unassociated stars with similar astrometry, in agreement with our previous results. Finally, we propose that wide binaries form an ideal data set with which to test chemical tagging as a method to identify stars of common origin, particularly because the stars in wide binaries span a wide range of metallicities, much wider than that spanned by nearby open clusters.
THE SLOAN LENS ACS SURVEY. X. STELLAR, DYNAMICAL, AND TOTAL MASS CORRELATIONS OF MASSIVE EARLY-TYPE GALAXIES

We use stellar masses, surface photometry, strong-lensing masses, and stellar velocity dispersions (σe/2) to investigate empirical correlations for the definitive sample of 73 early-type galaxies (ETGs) that are strong gravitational lenses from the SLACS survey. The traditional correlations (fundamental plane (FP) and its projections) are consistent with those found for non-lens galaxies, supporting the thesis that SLACS lens galaxies are representative of massive ETGs (dimensional mass Mdim = 1011–1012 M☉). The addition of high-precision strong-lensing estimates of the total mass allows us to gain further insights into their internal structure: (1) the average slope of the total mass-density profile ( ) is 〈γ′〉 = 2.078 ± 0.027 with an intrinsic scatter of 0.16 ± 0.02; (2) γ′ correlates with effective radius (re) and central mass density, in the sense that denser galaxies have steeper profiles; (3) the dark matter (DM) fraction within re/2 is a monotonically increasing function of galaxy mass and size (due to a mass-dependent central cold DM distribution or due to baryonic DM—stellar remnants or low-mass stars—if the initial mass function is non-universal and its normalization increases with mass); (4) the dimensional mass Mdim ≡ 5reσ2e/2/G is proportional to the total (lensing) mass M , and both increase more rapidly than stellar mass M* (M ); (5) the mass plane (MP), obtained by replacing surface brightness with surface mass density in the FP, is found to be tighter and closer to the virial relation than the FP and the M*P, indicating that the scatter of those relations is dominated by stellar population effects; (6) we construct the fundamental hyper-plane by adding stellar masses to the MP and find the M* coefficient to be consistent with zero and no residual intrinsic scatter. Our results demonstrate that the dynamical structure of ETGs is not scale invariant and that it is fully specified by M , re, and σe/2. Although the basic trends can be explained qualitatively in terms of varying star formation efficiency as a function of halo mass and as the result of dry and wet mergers, reproducing quantitatively the observed correlations and their tightness may be a significant challenge for galaxy formation models.
GIANT MOLECULAR CLOUD FORMATION IN DISK GALAXIES: CHARACTERIZING SIMULATED VERSUS OBSERVED CLOUD CATALOGS

We present the results of a study of simulated giant molecular clouds (GMCs) formed in a Milky Way–type galactic disk with a flat rotation curve. This simulation, which does not include star formation or feedback, produces clouds with masses ranging between 104 M☉ and 107 M☉. We compare our simulated cloud population to two observational surveys: the Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey and the BIMA All-Disk Survey of M33. An analysis of the global cloud properties as well as a comparison of Larson's scaling relations is carried out. We find that simulated cloud properties agree well with the observed cloud properties, with the closest agreement occurring between the clouds at comparable resolution in M33. Our clouds are highly filamentary—a property that derives both from their formation due to gravitational instability in the sheared galactic environment, as well as to cloud–cloud gravitational encounters. We also find that the rate at which potentially star-forming gas accumulates within dense regions—wherein nthresh ⩾ 104 cm−3—is 3% per 10 Myr, in clouds of roughly 106 M☉. This suggests that star formation rates in observed clouds are related to the rates at which gas can be accumulated into dense subregions within GMCs via filamentary flows. The most internally well-resolved clouds are chosen for listing in a catalog of simulated GMCs—the first of its kind. The cataloged clouds are available as an extracted data set from the global simulation.
MOLECULAR GAS HEATING MECHANISMS, AND STAR FORMATION FEEDBACK IN MERGER/STARBURSTS: NGC 6240 AND Arp 193 AS CASE STUDIES

We used the SPIRE/FTS instrument aboard the Herschel Space Observatory to obtain the Spectral Line Energy Distributions (SLEDs) of CO from J = 4–3 to J = 13–12 of Arp 193 and NGC 6240, two classical merger/starbursts selected from our molecular line survey of local Luminous Infrared Galaxies (LIR ⩾ 1011 L☉). The high-J CO SLEDs are then combined with ground-based low-J CO, 13CO, HCN, HCO+, CS line data and used to probe the thermal and dynamical states of their large molecular gas reservoirs. We find the two CO SLEDs strongly diverging from J = 4–3 onward, with NGC 6240 having a much higher CO line excitation than Arp 193, despite their similar low-J CO SLEDs and LFIR/LCO, 1 − 0, LHCN/LCO (J = 1–0) ratios (proxies of star formation efficiency and dense gas mass fraction). In Arp 193, one of the three most extreme starbursts in the local universe, the molecular SLEDs indicate a small amount (∼5%–15%) of dense gas (n ⩾ 104 cm−3) unlike NGC 6240 where most of the molecular gas (∼60%–70%) is dense (n ∼ (104–105) cm−3). Strong star-formation feedback can drive this disparity in their dense gas mass fractions, and also induce extreme thermal and dynamical states for the molecular gas. In NGC 6240, and to a lesser degree in Arp 193, we find large molecular gas masses whose thermal states cannot be maintained by FUV photons from Photon-Dominated Regions. We argue that this may happen often in metal-rich merger/starbursts, strongly altering the initial conditions of star formation. ALMA can now directly probe these conditions across cosmic epoch, and even probe their deeply dust-enshrouded outcome, the stellar initial mass function averaged over galactic evolution.
TRACING THE PECULIAR DARK MATTER STRUCTURE IN THE GALAXY CLUSTER Cl 0024+17 WITH INTRACLUSTER STARS AND GAS

Intracluster light (ICL) is believed to originate from the stars stripped from cluster galaxies. They are no longer gravitationally bound to individual galaxies, but to the cluster, and their smooth distribution potentially makes them serve as much denser tracers of the cluster dark matter than the sparsely distributed cluster galaxies. We present our study of the ICL in the galaxy cluster Cl 0024+17 using both Advanced Camera for Surveys (ACS) and Subaru data, where we previously reported the discovery of a ring-like dark matter structure with gravitational lensing. The ACS images provide much lower sky levels than ground-based data, and enable us to measure relative variation of surface brightness reliably. This analysis is repeated with the Subaru images to examine if consistent features are recovered despite a different reduction scheme and different instrumental characteristics. We find that the ICL profile clearly resembles the peculiar mass profile, which stops decreasing at r ∼ 50″ (∼265 kpc) and slowly increases until it turns over at r ∼ 75″ (∼397 kpc). This feature is seen in both ACS and Subaru images for nearly all available passband images while the features are in general stronger in red filters. The consistency across different filters and instruments strongly rules out the possibility that the feature might come from any residual, uncorrected calibration errors. In addition, our re-analysis of the cluster X-ray data shows that the peculiar mass structure is also indicated by a non-negligible (3.7σ in Chandra and 2.4σ in XMM-Newton) bump in the intracluster gas profile when the geometric center of the dark matter ring, not the peak of the X-ray emission, is chosen as the center of the radial bin. The location of the gas ring is closer to the center by ∼15″ (∼80 kpc), raising an interesting possibility that the ring-like structure is expanding and the gas ring is lagging behind perhaps because of the ram pressure if both features in mass and gas share the same dynamical origin.
The non-local thermodynamic equilibrium barium abundance in dwarf stars in the metallicity range of −1 < [Fe/H] < +0.3

We present the results of determination of the barium abundance considering the non-local thermodynamic equilibrium (NLTE) effects in 172 dwarf stars in the metallicity range of −1 < [Fe/H] < +0.3, assigned to different Galactic substructures by kinematic criteria. We used a model of the Ba atom with 31 levels of Ba i and 101 levels of Ba ii. The atmosphere models for the investigated stars were computed using the atlas9 code modified by new opacity distribution functions by Castelli & Kurucz. The NLTE profiles of the unblended Ba ii (4554, 5853, 6496 A) were computed and then compared to those observed. The line 6141 A was also used, but with an allowance for its correlation with the iron line. The average barium abundances in the thin and thick discs are 0.01 ± 0.08 and −0.03 ± 0.07, respectively. The comparison to the calculations of the Galactic chemical evolution by Serminato et al. was conducted. The trend obtained for the Ba abundance versus [Fe/H] suggests a complex barium production process in the thin and thick discs.
“I feel the mind enlarging itself”: Anne Lister’s gendered reading practices

Abstract This article argues for the usefulness of deploying a trans lens to examine the diaries of Anne Lister (1791-1840). The author contends that a trans reading may expand possibilities for critical analysis of Lister’s gender practices within the context of early-nineteenth-century white, upper-class Halifax society, in addition to existing labels such as “lesbian” and “queer. ” Examples to illustrate these possibilities are drawn from Lister’s reading habits, facilitated by some initial quantitative analysis of Lister’s own indexing practices. The article concludes that Lister structures their literary life to enable them to trans certain gender practices, and to fashion a livable gendered existence amidst the competing pressures of class, nationhood, financial security, self-determination, and sexual desire.