Miracle-dz/UniFAR-FTUs huggingface dataset:
Pulsars as excellent probes for the magnetic structure in our Milky Way

Abstract In this invited talk, I first discuss the advantages and disadvantages of many probes for the magnetic fields of the Milky Way. I conclude that pulsars are the best probes for the magnetic structure in our Galaxy, because magnetic field strength and directions can be derived from their dispersion measures (DMs) and rotation measures (RMs). Using the pulsars as probes, magnetic field structures in the Galactic disk, especially the field reversals between the arms and interarm regions, can be well revealed from the distribution of RM data. The field strengths on large scales and small scales can be derived from RM and DM data. RMs of extragalactic radio sources can be used as the indication of magnetic field directions in the spiral tangential regions, and can be used as probes for the magnetic fields in the regions farther away than pulsars when their median RMs are compared with pulsar RMs.
Millimetre polarization of the protoplanetary nebula OH 231.8+4.2: a follow-up study with CARMA

In order to investigate the characteristics and influence of the magnetic field in evolved stars, we performed a follow-up investigation of our previous submillimeter analysis of the proto-planetary nebula (PPN) OH 231.8+4.2 (Sabin et al. 2014), this time at 1.3 mm with the CARMA facility in polarisation mode for the purpose of a multi-scale analysis. OH 231.8+4.2 was observed at �2.5 ′′ resolution and we detected polarised emission above the 3σ threshold (with a mean polarisation fraction of 3.5%). The polarisation map indicates an overall organised magnetic field within the nebula. The main finding i n this paper is the presence of a structure mostly compatible with an ordered toroidal component that is aligned with the PPN’s dark lane. We also present some alternative magnetic fi eld configuration to explain the structure observed. These data complete our previous SMA submillimeter data for a better investigation and understanding of the magnetic field struc ture in OH 231.8+4.2.
SOME CONSTRAINTS ON THE LOWER MASS LIMIT FOR DOUBLE-DEGENERATE PROGENITORS OF TYPE Ia SUPERNOVAE

Recent theoretical and observational studies both argue that the merging of double carbon-oxygen white dwarfs (WDs) is responsible for at least some Type Ia supernovae (SNe Ia). Previous (standard) studies of the anticipated SN birthrate from this channel have assumed that the merger process is conservative and that the primary criterion for explosion is that the merged mass exceeds the Chandrasekhar mass. Han & Webbink demonstrated that mass transfer and merger in close double WDs will in many cases be non-conservative. Pakmor et al. further suggested that the merger process should be violent in order to initiate an explosion. We have therefore investigated how the SN Ia birthrate from the double-degenerate (DD) channel is affected by these constraints. Using the binary-star population-synthesis method, we have calculated the DD SN Ia birthrate under conservative and non-conservative approximations, and including lower mass and mass-ratio limits indicated by recent smoothed-particle-hydrodynamic calculations. The predicted DD SN Ia rate is significantly reduced by all of these constraints. With dynamical mass loss alone (violent merger) the birthrate is reduced to 56% of the conservative rate. Requiring the mass ratio q > 2/3 further reduces the birthrate to 18% that of the standard assumption. An upper limit of 0.0061 SNuM, or a Galactic rate of 4.6 × 10−4 yr−1, might be realistic.
THE STAR FORMATION RATE OF TURBULENT MAGNETIZED CLOUDS: COMPARING THEORY, SIMULATIONS, AND OBSERVATIONS

The role of turbulence and magnetic fields is studied for star formation in molecular clouds. We derive and compare six theoretical models for the star formation rate (SFR)—the Krumholz & McKee (KM), Padoan & Nordlund (PN), and Hennebelle & Chabrier (HC) models, and three multi-freefall versions of these, suggested by HC—all based on integrals over the log-normal distribution of turbulent gas. We extend all theories to include magnetic fields and show that the SFR depends on four basic parameters: (1) virial parameter αvir; (2) sonic Mach number ; (3) turbulent forcing parameter b, which is a measure for the fraction of energy driven in compressive modes; and (4) plasma with the Alfvén Mach number . We compare all six theories with MHD simulations, covering cloud masses of 300 to 4 × 106 M☉ and Mach numbers –50 and –∞, with solenoidal (b = 1/3), mixed (b = 0.4), and compressive turbulent (b = 1) forcings. We find that the SFR increases by a factor of four between and 50 for compressive turbulent forcing and αvir ∼ 1. Comparing forcing parameters, we see that the SFR is more than 10 times higher with compressive than solenoidal forcing for simulations. The SFR and fragmentation are both reduced by a factor of two in strongly magnetized, trans-Alfvénic turbulence compared to hydrodynamic turbulence. All simulations are fit simultaneously by the multi-freefall KM and multi-freefall PN theories within a factor of two over two orders of magnitude in SFR. The simulated SFRs cover the range and correlation of SFR column density with gas column density observed in Galactic clouds, and agree well for star formation efficiencies SFE = 1%–10% and local efficiencies ϵ = 0.3–0.7 due to feedback. We conclude that the SFR is primarily controlled by interstellar turbulence, with a secondary effect coming from magnetic fields.
FERMI-LAT DETECTION OF PULSED GAMMA-RAYS ABOVE 50 GeV FROM THE VELA PULSAR

The first Fermi-Large Area Telescope (LAT) catalog of sources above 10 GeV reported evidence of pulsed emission above 25 GeV from 12 pulsars, including the Vela pulsar, which showed evidence of pulsation at >37 GeV energy bands. Using 62 months of Fermi-LAT data, we analyzed the gamma-ray emission from the Vela pulsar and searched for pulsed emission above 50 GeV. Having confirmed the significance of the pulsation in 30–50 GeV with the H test (p-value ∼10−77), we extracted its pulse profile using the Bayesian block algorithm and compared it with the distribution of the five observed photons above 50 GeV using the likelihood ratio test. Pulsation was significantly detected for photons above 50 GeV with a p-value of =3 × 10−5 (4.2σ). The detection of pulsation is significant above 4σ at >79 GeV and above 3σ at >90 GeV energy bands, making this the highest energy pulsation significantly detected by the LAT. We explore the non-stationary outer gap scenario of the very high-energy emissions from the Vela pulsar.
EVIDENCE FOR A SYSTEMATIC OFFSET OF −0.25 mas IN THE GAIA DR1 PARALLAXES

We test the parallaxes reported in the Gaia first data release using the sample of eclipsing binaries with accurate, empirical distances from Stassun & Torres. We find an average offset of −0.25 ± 0.05 mas in the sense of the Gaia parallaxes being too small (i.e., the distances too long). The offset does not depend strongly on obvious parameters such as color or brightness. However, we find with high confidence that the offset may depend on ecliptic latitude: the mean offset is −0.38 ± 0.06 mas in the ecliptic north and −0.05 ± 0.09 mas in the ecliptic south. The ecliptic latitude dependence may also be represented by the linear relation, mas (β in degrees). Finally, there is a possible dependence of the parallax offset on distance, with the offset becoming negligible for mas; we discuss whether this could be caused by a systematic error in the eclipsing binary distance scale, and reject this interpretation as unlikely.
The impact of bars and interactions on optically selected AGNs in spiral galaxies

Aims. With the aim of performing a suitable comparison of the internal process of galactic bars with respect to the external effect of interactions on driving gas toward the inner most region of the galaxies, we explored and compared the efficiency of both mechanisms on central nuclear activity in optically selected active galactic nuclei (AGNs) in spiral galaxies. Methods. We selected homogeneous samples of barred AGNs and active objects residing in pair systems, derived from the Sloan Digital Sky Survey (SDSS). In order to carry out a reliable comparison of both samples (AGNs in barred hosts in isolation and in galaxy pairs), we selected spiral AGN galaxies with similar distributions of redshift, magnitude, stellar mass, color and stellar age population from both catalogs. With the goal of providing an appropriate quantification of the influence of strong bars and interactions on nuclear activity, we also constructed a suitable control sample of unbarred spiral AGNs without a companion and with similar host properties to the other two samples. Results. We found that barred optically selected AGNs show an excess of nuclear activity (as derived from the Lum[OIII]) and accretion rate onto a central black hole (ℛ) with respect to AGNs in pairs. In addition, both samples show an excess of high values of Lum[OIII] and ℛ with respect to unbarred AGNs in the control sample. We also found that the fractions of AGNs with powerful nuclear activity and high accretion rates increase toward more massive hosts with bluer colors and younger stellar populations. Moreover, AGNs with bars exhibit a higher fraction of galaxies with powerful Lum[OIII] and efficient ℛ with respect to AGN galaxies inhabiting pair systems, in bins of different galaxy properties. Regarding AGNs belonging to pair systems, we found that the central nuclear activity is remarkably dependent on the galaxy pair companion features. The Lum[OIII] for AGNs in pairs is clearly enhanced when the galaxy companion exhibits a bright and more massive host with high metallicity, blue color, efficient star formation activity and young stellar population. The results of this work reveal an important capacity of both mechanisms, bars and interactions, to transport material towards the galaxy central regions. In this context, it should also be noted that the internal process of the bar is more efficient at improving the central nuclear activity in AGN objects than that corresponding to the external mechanism of the galaxy–galaxy interactions.
Touschek with AdA in Orsay and the first direct observation of electron-positron collisions

We describe how the first direct observation of electron-positron collisions took place in 1963-1964 at the Laboratoire de l'Accelerateur Lineaire d'Orsay, in France, with the storage ring AdA, which had been proposed and constructed in the Italian National Laboratories of Frascati in 1960, under the guidance of Bruno Touschek. The obstacles and successes of the two and a half years during which the feasibility of electron-positron colliders was proved will be illustrated using archival and forgotten documents, in addition to transcripts from interviews with Carlo Bernardini, Peppino Di Giugno, Mario Fascetti, Francois Lacoste, and Jacques Haissinski.
THE SLOAN LENS ACS SURVEY. XII. EXTENDING STRONG LENSING TO LOWER MASSES

We present observational results from a new Hubble Space Telescope (HST) Snapshot program to extend the methods of the Sloan Lens ACS (SLACS) Survey to lower lens-galaxy masses. We discover 40 new galaxy-scale strong lenses, which we supplement with 58 previously discovered SLACS lenses. In addition, we determine the posterior PDFs of the Einstein radius for 33 galaxies (18 new and 15 from legacy SLACS data) based on single lensed images. We find a less-than-unity slope of 0.64 ± 0.06 for the log 10 &sgr; * ? > − log 10 &sgr; SIE ? > relation, which corresponds to a 6σ evidence that the total mass–density profile of early-type galaxies varies systematically in the sense of being shallower at higher lens-galaxy velocity dispersions. The trend is only significant when single-image systems are considered, highlighting the importance of including both “lenses” and “nonlenses” for an unbiased treatment of the lens population when extending to lower mass ranges. By scaling simple stellar-population models to the HST I-band data, we identify a strong trend of increasing dark-matter fraction at higher velocity dispersions, which can be alternatively interpreted as a trend in the stellar initial mass function (IMF) normalization. Consistent with previous findings and the suggestion of a nonuniversal IMF, we find that a Salpeter IMF is ruled out for galaxies with velocity dispersion less than 180 km s−1. Considered together, our mass-profile and dark-matter fraction trends with increasing galaxy mass could both be explained by an increasing relative contribution on kiloparsec scales from a dark-matter halo with a spatial profile more extended than that of the stellar component.
TRACING THE COSMIC METAL EVOLUTION IN THE LOW-REDSHIFT INTERGALACTIC MEDIUM

Using the Cosmic Origins Spectrograph aboard the Hubble Space Telescope, we measured the abundances of six ions (C iii, C iv, Si iii, Si iv, N v, and O vi) in the low-redshift (z ⩽ 0.4) intergalactic medium (IGM). Both C iv and Si iv have increased in abundance by a factor of ∼10 from z ≈ 5.5 to the present. We derive ion mass densities, ρion ≡ Ωionρcr, with Ωion expressed relative to the closure density. Our models of mass-abundance ratios, (Si iii/Si iv) , (C iii/C iv) , and , are consistent with the photoionization parameter log U = −1.5 ± 0.4, hydrogen photoionization rate ΓH = (8 ± 2) × 10−14 s−1 at z < 0.4, and specific intensity I0 = (3 ± 1) × 10−23 erg cm−2 s−1 Hz−1 sr−1 at the Lyman limit. Consistent ionization corrections for C and Si are scaled to an ionizing photon flux Φ0 = 104 cm−2 s−1, baryon overdensity Δb ≈ 200 ± 50, and “alpha-enhancement” (Si/C enhanced to three times its solar ratio). We compare these metal abundances to the expected IGM enrichment and abundances in higher photoionized states of carbon (C v) and silicon (Si v, Si vi, and Si vii). Our ionization modeling infers IGM metal densities of (5.4 ± 0.5) × 105 M☉ Mpc−3 in the photoionized Lyα forest traced by the C and Si ions and (9.1 ± 0.6) × 105 M☉ Mpc−3 in hotter gas traced by O vi. Combining both phases, the heavy elements in the IGM have mass density ρZ = (1.5 ± 0.8) × 106 M☉ Mpc−3 or ΩZ ≈ 10−5. This represents 10% ± 5% of the metals produced by (6 ± 2) × 108 M☉ Mpc−3 of integrated star formation with yield ym = 0.025 ± 0.010. The missing metals at low redshift may reside within galaxies and in undetected ionized gas in galactic halos and circumgalactic medium.
SEARCHING FOR FOSSIL EVIDENCE OF AGN FEEDBACK IN WISE-SELECTED STRIPE-82 GALAXIES BY MEASURING THE THERMAL SUNYAEV–ZEL’DOVICH EFFECT WITH THE ATACAMA COSMOLOGY TELESCOPE

We directly measure the thermal energy of the gas surrounding galaxies through the thermal Sunyaev–Zel’dovich (tSZ) effect. We perform a stacking analysis of microwave background images from the Atacama Cosmology Telescope, around 1179 massive quiescent elliptical galaxies at 0.5 ≤ z ≤ 1.0 (“low-z”) and 3274 galaxies at 1.0 ≤ z ≤ 1.5 (“high-z”), selected using data from the Wide-field Infrared Survey Explorer All-Sky Survey and the Sloan Digital Sky Survey (SDSS) within the SDSS Stripe-82 field. The gas surrounding these galaxies is expected to contain energy from past episodes of active galactic nucleus (AGN) feedback, and after using modeling to subtract undetected contaminants, we detect a tSZ signal at a significance of 0.9 σ for our low-z galaxies and 1.8 σ for our high-z galaxies. We then include data from the high-frequency Planck bands for a subset of 227 low-z galaxies and 529 high-z galaxies and find low-z and high-z tSZ detections of 1.0 σ and 1.5 σ , respectively. These results indicate an average thermal heating around these galaxies of ( 5.6 − 5.6 + 5.9 ) × 10 60 erg for our low-z galaxies and ( 7.0 − 4.4 + 4.7 ) × 10 60 erg for our high-z galaxies. Based on simple heating models, these results are consistent with gravitational heating without additional heating due to AGN feedback.
Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies

Mid-infrared molecular hydrogen (H2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies; it is a potential key tracer of gas evolution and energy dissipation associated with mergers, star formation, and accretion onto supermassive black holes. We detect mid-IR H2 line emission in at least one rotational transition in 91% of the 214 Luminous Infrared Galaxies (LIRGs) observed with Spitzer as part of the Great Observatories All-sky LIRG Survey. We use H2 excitation diagrams to estimate the range of masses and temperatures of warm molecular gas in these galaxies. We find that LIRGs in which the IR emission originates mostly from the Active Galactic Nuclei (AGN) have about 100 K higher H2 mass-averaged excitation temperatures than LIRGs in which the IR emission originates mostly from star formation. Between 10% and 15% of LIRGs have H2 emission lines that are sufficiently broad to be resolved or partially resolved by the high-resolution modules of Spitzer’s Infrared Spectrograph (IRS). Those sources tend to be mergers and contain AGN. This suggests that a significant fraction of the H2 line emission is powered by AGN activity through X-rays, cosmic rays, and turbulence. We find a statistically significant correlation between the kinetic energy in the H2 gas and the H2 to IR luminosity ratio. The sources with the largest warm gas kinetic energies are mergers. We speculate that mergers increase the production of bulk inflows leading to observable broad H2 profiles and possibly denser gas.
SN 2009E: a faint clone of SN 1987A

Context. 1987A-like events form a rare sub-group of hydrogen-rich core-collapse supernovae that are thought to originate from the explosion of blue supergiant stars. Although SN 1987A is the best known supernova, very few objects of this group have been discovered and, hence, studied. Aims. In this paper we investigate the properties of SN 2009E, which exploded in a relatively nearby spiral galaxy (NGC 4141) and that is probably the faintest 1987A-like supernova discovered so far. We also attempt to characterize this subgroup of core-collapse supernovae with the help of the literature and present new data for a few additional objects. Methods. The lack of early-time observations from professional telescopes is compensated by frequent follow-up observations performed by a number of amateur astronomers. This allows us to reconstruct a well-sampled light curve for SN 2009E. Spectroscopic observations which started about 2 months after the supernova explosion, highlight significant differences between SN 2009E and the prototypical SN 1987A. Modelling the data of SN 2009E allows us to constrain the explosion parameters and the properties of the progenitor star, and compare the inferred estimates with those available for the similar SNe 1987A and 1998A. Results. The light curve of SN 2009E is less luminous than that of SN 1987A and the other members of this class, and the maximum light curve
gaming and hostility predict Internet Addiction symptoms in adolescents : An empirical multilevel longitudinal study An

Internet addiction (IA) has become an increasingly researched topic. In the present study, IA symptoms in adolescents were investigated longitudinally with specific focus on the individual’s hostility, gaming use (of Massively Multiplayer Online Role Playing Games [MMORPGs]) and gaming on the classroom level (calculated using the percentage of MMORPG players within classes). The sample comprised 648 Greek adolescents who were assessed over a two-year period (aged 16-18 years). IA symptoms were assessed with the Internet Addiction Test (IAT), and hostility with the relevant subscale of the Symptom Checklist-90 (SCL-90). A three-level hierarchical linear model was used to differentiate individual and classroom-level influences on IA symptoms at age 16 years and over time. MMORPG gamers and more hostile adolescents presented more symptoms of IA. However, being a member of a classroom with a higher percentage of MMORPG gamers appeared to be a protective factor for IA. These longitudinal data emphasize the importance of contextual factors at the level of the classroom in determining differences in IA symptoms during adolescence.
ACCRETION AND OUTFLOW FROM A MAGNETIZED, NEUTRINO COOLED TORUS AROUND THE GAMMA-RAY BURST CENTRAL ENGINE

We calculate the structure and short-term evolution of a gamma-ray burst (GRB) central engine in the form of a turbulent torus accreting onto a stellar mass black hole. Our models apply to the short GRB events, in which a remnant torus forms after the neutron star–black hole or a double neutron star merger and is subsequently accreted. We study the two-dimensional, relativistic models and concentrate on the effects of the black hole and flow parameters as well as the neutrino cooling. We compare the resulting structure and neutrino emission to the results of our previous one-dimensional simulations. We find that the neutrino cooled torus launches a powerful mass outflow, which contributes to the total neutrino luminosity and mass loss from the system. The neutrino luminosity may exceed the Blandford–Znajek luminosity of the polar jets and the subsequent annihilation of neutrino–antineutrino pairs will provide an additional source of power to the GRB emission.
Charged-particle multiplicity in proton–proton collisions

This review summarizes and critically reviews measurements of charged-particle multiplicity distributions and pseudorapidity densities in p + p(P) collisions between √s = 23.6 GeV and √s = 1.8 TeV. Related theoretical concepts are briefly introduced. Moments of multiplicity distributions are presented as a function of √s. Feynman scaling, KNO scaling as well as the description of multiplicity distributions with a single negative binomial distribution and with combinations of two or more negative binomial distributions is discussed. Moreover, similarities between the energy dependence of charged-particle multiplicities in p + p(p) and e + e - collisions are studied. Finally, various predictions for pseudorapidity densities, average multiplicities in full phase space and multiplicity distributions of charged particles in p + p(P) collisions at the LHC energies of √s = 7 TeV, 10 TeV and 14 TeV are summarized and compared.