Miracle-dz/UniFAR-FTUs huggingface dataset:
The profiles of the 3 to 12 $\mu$m PAH features

We present spectra of the 3.3 µ m and 11.2 µ m PAH features of a large number of stellar sources, planetary nebulae, reﬂection nebulae, H II regions and galaxies, obtained with ISO-SWS. Clear variations are present in the proﬁles of these features. Most of the sources show a symmetric 3.3 µ m feature peaking at ∼ 3.290 µ m, while only very few show an asymmetric 3.3 µ m feature peaking at a slightly longer wavelength. The proﬁles of the 11.2 µ m feature are distinctly asymmetric. The majority of the sources has a 11.2 µ m feature peaking between 11.20 and 11.24 µ m, with a very steep blue rise and a low tail-to-top ratio. A few sources show a 11.2 µ m feature with a peak position of ∼ 11.25 µ m, a less steep blue rise and a high tail-to-top ratio. The sources are classiﬁed independently based on the 3.3 and 11.2 µ m feature proﬁles and peak positions. Correlations between these classes and those based on the 6–9 µ m features (Peeters et al. 2002a) are found. In particular, sources with the most common proﬁles in the 6–9 µ m region also show the most common 3.3 and 11.2 µ m feature proﬁles. However, the uncommon proﬁles do not correlate with each other. Also, these classiﬁcations depend on the type of object. In general, H II regions, non-isolated Herbig AeBe stars and YSO’s show the same proﬁles for all 3-12 µ m features. Many planetary nebulae and Post-AGB stars show uncommon feature proﬁles. The 3 galaxies in our sample show the same proﬁles as the H II regions for all but the 11.2 µ m feature, being similar to that of evolved stars. The observed pronounced contrast in the spectral variations for the CH modes (3.3 and 11.2 µ m bands) versus the CC modes (6.2, 7.7 and 8.6 µ m bands) is striking : the peak wavelengths of the features attributed to CC modes vary by ∼ 15–80 cm − 1 , while for the CH modes the variations are ∼ 4–6.5 cm − 1 . We summarize existing laboratory data and theoretical calculations of the modes emitting in the 3–12 µ m region of PAH molecules and complexes. In contrast to the 6.2 and 7.7 µ m components which are attributed to PAH cations, the 3.3 µ m feature appears to originate in neutral and/or negatively charged PAHs. We attribute the variations in peak position and proﬁle of these IR emission features to the composition of the PAH family. The variations in FWHM of the 3.3 µ m feature remains an enigma while those of the 11.2 µ m can be explained by anharmonicity and molecular structure. The possible origin of the observed contrast in proﬁle variations between the CH modes and the CC modes is highlighted.
Magnetic fields in the Centaurus cluster

We present multifrequency Very Large Array (VLA) observations of the radio galaxy PKS 1246-410 at the centre of the Centaurus cluster, and compare these results with recent Chandra observations. The unusual radio morphology of PKS 1246-410 probably results from interactions with the hot, X-ray-emitting gas. This gas, along with cluster magnetic fields, also produces substantial Faraday rotation measures towards PKS 1246-410. We discuss these observations in the context of a sample of 14 luminous X-ray clusters with embedded radio galaxies and possible cooling flows. A correlation is found between the cooling flow rate and the maximum Faraday rotation measures. Magnetic fields of strength 10-40 μG are found to be common to the centres of clusters with strong cooling flows, and somewhat lower field strengths of 2-10 μG are found in the non cooling-flow clusters.
Extragalactic Results from the Infrared Space Observatory

▪ Abstract More than a decade ago the IRAS satellite opened the realm of external galaxies for studies in the 10 to 100 μm band and discovered emission from tens of thousands of normal and active galaxies. With the 1995–1998 mission of the Infrared Space Observatory1, the next major steps in extragalactic infrared astronomy became possible: detailed imaging, spectroscopy, and spectrophotometry of many galaxies detected by IRAS, as well as deep surveys in the mid- and far-IR. The spectroscopic data reveal a wealth of detail about the nature of the energy source(s) and about the physical conditions in galaxies. ISO's surveys for the first time explore the infrared emission of distant, high-redshift galaxies. ISO's main theme in extragalactic astronomy is the role of star formation in the activity and evolution of galaxies.
A multiplicity survey of the ρ Ophiuchi molecular clouds

We present a volume-limited multiplicity survey with magnitude cutoff (${m}_{K}\leq 10.5\mathrm{\ mag}$) of 158 young stellar objects located within or in the vicinity of the ρ Ophiuchi Dark Cloud. With exception of eleven already well observed objects, all sources have been observed by us in the K-band with 3.5 m telescopes by using speckle techniques. The separation range covered by our survey is $0.13''\leq\theta\leq 6.4''$, where the lower limit is given by the diffraction limit of the telescopes and the upper limit by confusion with background stars. The multiplicity survey is complete for flux ratios $\geq $0.1 ($\Delta{m}_{K}\leq 2.5$) at the diffraction limit. After taking the background density into account the degree of multiplicity is $29.1\%\pm 4.3\%$ and thus only marginally higher than the value $23.5\%\pm 4.8 \%$ derived for the given separation range for the main-sequence solar-like stars in the solar neighbourhood (Duquennoy & Mayor 1991). We discuss the implications of these findings.
A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters

We have determined masses, stellar mass functions, and structural parameters of 112 Milky Way globular clusters by fitting a large set of N-body simulations to their velocity dispersion and surface density profiles. The velocity dispersion profiles were calculated based on a combination of more than 15000 high-precision radial velocities which we derived from archival ESO/VLT and Keck spectra together with similar to 20000 published radial velocities from the literature. Our fits also include the stellar mass functions of the globular clusters, which are available for 47 clusters in our sample, allowing us to self-consistently take the effects of mass segregation and ongoing cluster dissolution into account. We confirm the strong correlation between the global mass functions of globular clusters and their relaxation times recently found by Sollima & Baumgardt (2017). We also find a correlation of the escape velocity from the centre of a globular cluster and the fraction of first generation stars (FG) in the cluster recently derived for 57 globular clusters by Milone et al. (2017), but no correlation between the FG star fraction and the global mass function of a globular cluster. This could indicate that the ability of a globular cluster to keep the wind ejecta from the polluting star(s) is the crucial parameter determining the presence and fraction of second-generation stars and not its later dynamical mass loss.
Changing growth of neurites of sensory ganglion by terahertz radiation

Application of terahertz radiation for the creation of medical equipment and solving of biological problems has become widely spread. From this point of view, the influence of THz radiation on the nerve fibers is of primary concern. In addition, several studies indicated both stimulating and depressive effects on nerve cells. However, the mechanism of this effect has not yet been studied, including the dose and exposure time. Our research was devoted to the impact of broadband pulsed THz radiation in the frequency range of 0.05 to 2 THz on the neurite growth in the sensory ganglia of 10-12-day chicken embryos. Dependence of changes in functional responses of cells on the average output power has been found. An increase in the stimulating effect was observed at the lowest power density used (0.5 μW/cm2). Through non-destructive process and choosing the correct parameters of THz radiation, potential control of neural response becomes possible, which can subsequently lead to new medical treatments.
Modelling Radioactivities and other Observables from OB Associations

Recent observations of the diﬀuse Galactic gamma-ray glow at 1.809 MeV, attributed to the radioactive decay of 26 Al, point towards a massive star origin of this radioactive isotope. Wolf Rayet stars and core-collapse supernovae appear to dominate the production of this isotope. Massive stars are commonly located in clusters and OB associations, regions of recent star formation. We thus discuss the temporal evolution of 26 Al, and 60 Fe within evolving OB associations. The goal of this study is to utilize the associated gamma-ray lines as a diagnostic tool for the study of correlated star formation, and also to provide more detailed models for the interpretation of data obtained with COMPTEL on the Compton Observatory. We investigate the eﬀects of possible aluminum yield enhancements, predicted for some massive close binary systems. In addition to the ejection of chemically processed matter, massive stars also drive strong stellar winds and emit large ﬂuxes of ionizing radiation. This energy and radiation input into the interstellar medium (ISM) is crucial for the dynamical evolution of the gas and subsequent star forming activity in the galactic disk. We discuss population synthesis models for a variety of star formation histories, and compare the predicted gamma-ray line lightcurves to COMPTEL measurements in the Cygnus region. Radioactive tracers such as 26 Al and 60 Fe provide a unique gamma-ray tracer of Galactic star formation activity, complementary to other methods using spectral information in the radio, IR or optical bands.
The Clausius‐Mossotti problem for cubic arrays of spheres

The numerical solution of the Clausius‐Mossotti problem for the permittivity of a suspension of perfectly conducting spheres in a cubic array is presented for sc, fcc, and bcc lattices. The results apply to electrical permittivity, magnetic permeability, electrical and thermal conductivity, and particle diffusivity. The calculations are compared with the Clausius‐Mossotti relation. Rayleigh’s equation is corrected and compared with the numerical results. A simple interpolation formula for the permittivity of a medium of perfectly conducting spheres in a simple cubic lattice is found to give an excellent approximation at all volume ratios.
Boundary conservation from bulk symmetry

The evolution of the black-hole horizon can be effectively captured by a fictitious membrane fluid living on the stretched horizon. We show that the dynamics of this boundary matter arises from the invariance of the bulk action under local symmetries in the presence of the inner boundary. If general covariance is broken in a semi-classical treatment of a quantum field near a black-hole horizon, we argue that it can be restored by the inclusion of a quantum flux into the membrane conservation equation which is exactly equal to the Hawking flux.
The cores of dwarf galaxy haloes

We use N-body simulations to examine the effects of mass outflows on the density profiles of cold dark matter (CDM) halos surrounding dwarf galaxies. In particular, we investigate the consequences of supernova-driven winds that expel a large fraction of the baryonic component from a dwarf galaxy disk after a vigorous episode of star formation. We show that this sudden loss of mass leads to the formation of a core in the dark matter density profile, although the original halo is modeled by a coreless (Hernquist) profile. The core radius thus created is a sensitive function of the mass and radius of the baryonic disk being blown up. The loss of a disk with mass and size consistent with primordial nucleosynthesis constraints and angular momentum considerations imprints a core radius which is only a small fraction of the original scale-length of the halo. These small perturbations are, however, enough to reconcile the rotation curves of dwarf irregulars with the density profiles of haloes formed in the standard CDM scenario.
Cosmic microwave background radiation anisotropy induced by cosmic strings

We report on a current investigation of the anisotropy pattern induced by cosmic strings on the cosmic microwave background radiation (MBR). We have numerically evolved a network of cosmic strings from a redshift of Z = 100 to the present and calculated the anisotropies which they induce. Based on a limited number of realizations, we have compared the results of our simulations with the observations of the COBE-DMR experiment. We have obtained a preliminary estimate of the string mass-per-unit-length µ in the cosmic string scenario.
There are no $Q$-points in Laver’s model for the Borel conjecture

It is shown that it is consistent with ZFC that no nonprincipal ultrafilter on w is a Q-point (also called a rare ultrafilter). All ultrafilters are assumed to be nonprincipal and on w. DEFINITIONS. (1) U is a Q-point (also called rare [C]) iff Vf E oS' if f is finite-to-one then 3X E U, f r X is one-to-one. (2) U is a P-point iff Vf E w, 3X E U, f r X is constant or finite-to-one. (3) U is a semiQ-point (also called rapid [C], iff Vf E o", 3g E o", Vn f(n) n (f(m) (2). Let f(n) = sup( U f(n); then Pn n g". C { g(O), . *, g(n 1)). (3) =X (1). Assume f increasing. Choose no no, IY n f(m)I <Km, since if nk < m <nk+l then Received by the editors April 3, 1978. AMS (MOS) subject classifications (1970). Primary 02K05. O 1980 American Mathematical Society 0002-9939/80/0000-002 3/$02.00 103 This content downloaded from 157.55. 39.17 on Wed, 31 Aug 2016 04:20:06 UTC All use subject to http://about.jstor. org/terms
Exploring the superimposed oscillations parameter space

The space of parameters characterizing an inflationary primordial power spectrum with small superimposed oscillations is explored using Monte Carlo methods. The most interesting region corresponding to high frequency oscillations is included in the analysis. The oscillations originate from some new physics taking place at the beginning of the inflationary phase and characterized by the new energy scale Mc. It is found that the standard slow roll model remains the most probable one given the first-year WMAP data. At the same time, the oscillatory models fit the data better on average, which is consistent with previous works on the subject. This is typical of a situation where volume effects in the parameter space play a significant role. Then, we find the amplitude of the oscillations to be less than 22% of the mean amplitude and the new scale Mc to be such that H/Mc<6.6 × 10−4 at 1σ level, where H is the scale of inflation.
M-type giants as optical counterparts of X-ray sources 4U 1700+24 and 4U 1954+319

We observed with Chandra two peculiar galactic X-ray sources, 4U 1700+24 and 4U 1954+319, which are suspected to have a M-type giant star as optical counterpart, in order to get a high-precision astrometric position for both of them. The peculiarity of these sources lies in the fact that these are the only two cases among low-mass X-ray binaries (LMXBs), besides the confirmed case of GX 1+4, for which the companion can possibly be a M-type giant. We found that in both cases the field M-type giant star is indeed the counterpart of these X-ray sources. We also determined the distance to 4U 1954+319 to be ~1.7 kpc. This result suggests that a number of faint ($L_{\rm X} \sim 10^{32}{-}10^{34}$ erg s -1 ) Galactic X-ray sources are “symbiotic X-ray binaries”, that is, wide-orbit LMXBs composed of a compact object, most likely a neutron star, accreting from the wind of a M-type giant.
First order non-negative integer valued autoregressive processes with power series innovations

In this paper, we introduce a first order non-negative integer valued autoregressive process with power series innovations based on the binomial thinning. This new model contains, as particular cases, several models such as the Poisson INAR(1) model (Al-Osh and Alzaid (J. Time Series Anal. 8 (1987) 261–275)), the geometric INAR(1) model (Jazi, Jones and Lai (J. Iran. Stat. Soc. (JIRSS) 11 (2012) 173–190)) and many others. The main properties of the model are derived, such as mean, variance and the autocorrelation function. Yule–Walker, conditional least squares and conditional maximum likelihood estimators of the model parameters are derived. An extensive Monte Carlo experiment is conducted to evaluate the performances of these estimators in finite samples. Special sub-models are studied in some detail. Applications to two real data sets are given to show the flexibility and potentiality of the new model.
A New Catalog of Radial Velocity Standard Stars from the APOGEE Data

We present a new catalog of 18080 radial velocity (RV) standard stars selected from the APOGEE data. These RV standard stars are observed at least three times and have a median stability (3σRV) around 240 m s−1 over a time baseline longer than 200 days. They are largely distributed in the northern sky and could be extended to the southern sky by the future APOGEE-2 survey. Most of the stars are red giants (J − Ks ≥ 0.5) owing to the APOGEE target selection criteria. Only about 10 per cent of them are main-sequence stars. The H-band magnitude range of the stars is 7–12.5 mag with the faint limit much fainter than the magnitudes of previous RV standard stars. As an application, we show the new set of standard stars to determine the RV zero points of the RAVE, the LAMOST, and the Gaia-RVS Galactic spectroscopic surveys.
HE 1327–2326, an Unevolved Star with [Fe/H] < –5.0. I. A Comprehensive Abundance Analysis

We present the elemental abundances of HE 1327-2326, the most iron-deficient star known, determined from a comprehensive analysis of spectra obtained with the Subaru Telescope High Dispersion Spectrograph. HE 1327-2326 is either in its main-sequence or subgiant phase of evolution. Its non-LTE-corrected iron abundance is [Fe/H] = -5.45, 0.2 dex lower than that of HE 0107-5240, the previously most iron-poor object known, and more than 1 dex lower than those of all other metal-poor stars. Both HE 1327-2326 and HE 0107-5240 exhibit extremely large overabundances of carbon ([C/Fe] ~ +4). The combination of extremely high carbon abundance with outstandingly low iron abundance in these objects clearly distinguishes them from other metal-poor stars. The large carbon excesses in these two stars are not the result of a selection effect. There also exist important differences between HE 1327-2326 and HE 0107-5240. While the former shows remarkable overabundances of the light elements (N, Na, Mg, and Al), the latter shows only relatively small excesses of N and Na. The neutron-capture element Sr is detected in HE 1327-2326, but not in HE 0107-5240; its Sr abundance is significantly higher than the upper limit for HE 0107-5240. The Li I λ6707 line, which is detected in most metal-poor dwarfs and warm subgiants having the same temperature as HE 1327-2326, is not found in this object. The upper limit of its Li abundance [log ϵ < 1.5] is clearly lower than the Spite plateau value. These data provide new constraints on models of nucleosynthesis processes in the first-generation objects that were responsible for metal enrichment at the earliest times. We discuss possible scenarios to explain the observed abundance patterns.
A seismic scaling relation for stellar age

A simple solar scaling relation for estimating the ages of main-sequence stars from asteroseismic and spectroscopic data is developed. New seismic scaling relations for estimating mass and radius are presented as well, including a purely seismic radius scaling relation (i.e., no dependence on temperature). The relations show substantial improvement over the classical scaling relations and perform similarly well to grid-based modeling.
Optical Variability of Narrow-Line Seyfert 1 Galaxies

We present results of a broadband photometric study of the optical variability of six narrow-line Seyfert 1 (NLS1) galaxies observed at 172 epochs. We searched for microvariability on 33 nights. Strong evidence for microvariability was found only for our lowest luminosity object, NGC 4051, on one night. Weaker evidence suggests such variability on a few other nights for two other objects, but the data are not as convincing. Intranight variability in NLS1's is thus concluded to be rare and of low amplitude. We give illustrations of how variable image quality can produce spurious variability. We find that for well-studied non-NLS1's there is a spread in the amplitude of seasonal variability (i.e., in some years an active galactic nucleus [AGN] is more variable than in others). We find that the means of the variability amplitudes of non-NLS1's over several seasons vary from object to object (i.e., some AGNs are, on average, more variable than others). NLS1's also show a spread in seasonal variabilities. The best-studied NLS1, Ark 564, shows a range of amplitudes of variability from season to season that is comparable to the range found in broad-line Seyfert 1 galaxies (BLS1's), and in one season Ark 564 was as variable as the most variable non-NLS1. The seasonal amplitudes of variability for NLS1's are mostly in the lower half of the range of non-BLS1 seasonal amplitudes, but the absence of a suitable control sample makes a precise comparison difficult. However, on long timescales (weeks to years) NLS1's as a class are not more variable than non-NLS1's. The extreme variability seen in the X-rays was not seen in the optical. This has consequences for the models of AGNs in general as well as NLS1's in particular.
Retrieval of two‐dimensional absorption coefficient structure from a scanning radiometer at 23.8 GHz

In this work the retrieval of the structure of the atmospheric specific absorption coefficient through a tomographic acquisition is discussed. Brightness temperatures have been collected daily at 23.8 GHz using a radiometer in tipping curve mode regardless of the sky condition, except for rainy days, for about 60 elevation scans. Each scan has been processed to retrieve the two‐dimensional structure of the underlying atmosphere through the (x‐z) values of the specific absorption coefficient. The forward model is inverted after binning in space and linearization around a reference model. The scanned vertical plan is modeled by allocating M bins spanning in both the vertical and the horizontal direction, whereas the measurements have been collected at 12 elevation angles between 23° and 90°. Singular value decomposition allows identifying an orthogonal basis for the data space (12 elevation angles) and for the model space (M bins). It indicates also that only five eigenvalues are such that the condition number of the matrix representing the linearized problem is acceptable (≈20), so that only five components of the model space may be resolved. A higher number would imply unacceptable noise contamination. In spite of these limitations, the retrieved panel of specific absorption coefficient reveals the horizontal structure of the atmosphere. The scale of the experiment is of the order of kilometers. Therefore, because the vertical structure of the atmosphere dominates over the horizontal, a vertical detrending is needed to reveal horizontal structures. An example shows the typical problems encountered in the inversion and the remedies that have been adopted.