Search

Strange metals possess highly unconventional electrical properties, such as a linear-in-temperature resistivity1–6, an inverse Hall angle that varies as temperature squared7–9and a linear-in-field magnetoresistance10–13. Identifying the origin of these collective anomalies has proved fundamentally challenging, even in materials such as the hole-doped cuprates that possess a simple bandstructure. The prevailing consensus is that strange metallicity in the cuprates is tied to a quantum critical point at a doping p* inside the superconducting dome14,15. Here we study the high-field in-plane magnetoresistance of two superconducting cuprate families at doping levels beyond p*. At all dopings, the magnetoresistance exhibits quadrature scaling and becomes linear at high values of the ratio of the field and the temperature, indicating that the strange-metal regime extends well beyond p*. Moreover, the magnitude of the magnetoresistance is found to be much larger than predicted by conventional theory and is insensitive to both impurity scattering and magnetic field orientation. These observations, coupled with analysis of the zero-field and Hall resistivities, suggest that despite having a single band, the cuprate strange-metal region hosts two charge sectors, one containing coherent quasiparticles, the other scale-invariant ‘Planckian’ dissipators.

The INBUILD trial investigated the efficacy and safety of nintedanib versus placebo in patients with progressive fibrosing interstitial lung diseases (ILDs) other than idiopathic pulmonary fibrosis (IPF). We aimed to establish the effects of nintedanib in subgroups based on ILD diagnosis.

AbstractWater distillation packed with materials having adsorption ability is proposed for wastewater detritiation, and behavior of HTO depletion or enrichment is experimentally investigated. It is proved that the apparent volatility ratio of H2O-to-HTO is increased by an isotopic effect on adsorption under a steady-state operation. Danckwerts’ surface renewal model is applied to explain the T enrichment process in a lab-scale water distillation column. The effect is estimated in terms of an adsorption enhancement factor included in the T separation factor, εHT,ad,which depends on the kinds of adsorbents and liquid-vapor flow conditions. The value of the enhancement factor is also confirmed εHT,ad = 1.02 in a comparatively large-scale distillation operation packed with Sulzer packing or Raschig ring coated with zeolite adsorbent. A large-scale distillation tower can be designed to detritiate radioactive wastewater generated in Fukushima’s Daiichi NPS based on the present experimental results.

Aims. We want to study the IR (>$8\;\mu$m) emission of galaxies selected on the basis of their rest-frame UV light in a very homogeneous way (wavelength and luminosity) from $z = 0$to $z=1$. We compare their UV and IR rest-frame emission to study the evolution in dust attenuation with zas well as to check if a UV selection is capable of tracking all star formation. This UV selection will also be compared to a sample of Lyman break galaxies selected at $z \simeq 1$.

Aims. We investigate whether the mean star formation activity of star-forming galaxies from $z=0$to $z=0.7$in the GOODS-S field can be reproduced by simple evolution models of these systems. In this case, such models might be used as first-order references for studies at higher zto decipher when and to what extent a secular evolution is sufficient to explain the star formation history in galaxies.

Aims.The total infrared (TIR: 8-1000 μm) and far-ultraviolet (FUV: ~1500 Å) luminosity functions of galaxies and the related luminosity densities $\rho_{\rm TIR}$and $\rho_{\rm FUV}$are known to evolve at differemt rates from $z = 0$to z~1: the galaxy populations appear to be brighter in the past at both wavelengths, but the evolution in the TIR is larger than in the FUV. This leads to an increase of the ratio of TIR to FUV luminosity densities $\rho_{\rm TIR}/\rho_{\rm FUV}$which can be interpreted as a global increase of the dust attenuation from $z = 0$to z~ 1. Our aim is to understand the origin of this increase: is it entirely due to a variation of the dust attenuation with the luminosity of the galaxies as seen as $z = 0$or are properties of galaxies evolving with the redshift?

We investigate the possibility of searching for metal-poor high column density ($\ga$$10^{23}~{\rm cm}^{-2}$) clouds at high redshift (z) by using gamma ray burst afterglows. Such clouds could be related to primeval galaxies that may cause a burst of star formation. We show that a large part of hydrogen is in molecular form in such a high column density environment. Therefore, hydrogen molecules (H2) rather than hydrogen atoms should be searched for. Then we show that infrared H2lines are detectable for metal-poor ($\la$0.01 solar metallicity) high column density ($\log N_{\rm H}~[{\rm cm}^{-2}]\ga 23.5$) systems at high-zwithout suffering dust extinction. The optical properties of dust in infrared could also be constrained by observations of high column density systems. Some possible scenarios for producing high column density systems are finally discussed in the context of galaxy evolution.

Aims.We present the first large, unbiased sample of Lyman Break Galaxies (LBGs) at $z \sim 1$. Far ultraviolet-dropout (1530 Å) galaxies in the Chandra Deep Field South have been selected using GALEXdata. This first large sample in the $z \sim 1$universe provides us with a high quality reference sample of LBGs. Methods.We analyzed the sample from the UV to the IR using GALEX, SPITZER, ESOand HSTdata.Results.The morphology (obtained from GOODS data) of 75% of our LBGs is consistent with a disk. The vast majority of LBGs with an IR detection are also Luminous Infrared Galaxies (LIRGs). As a class, the galaxies not detected at 24 μm are an order of magnitude fainter relative to the UV compared with those detected individually, suggesting that there may be two types of behavior within the sample. For the IR-bright galaxies, there is an apparent upper limit for the UV dust attenuation and this upper limit is anti-correlated with the observed UV luminosity. Previous estimates of dust attenuations based on the ultraviolet slope are compared to new ones based on the FIR/UV ratio (for LBGs detected at 24 μm), which is usually a more reliable estimator. Depending on the calibration we use to estimate the total IR luminosity, β-based attenuations AFUVare larger by 0.2 to 0.6 mag. than the ones estimated from FIR/UV ratio. Finally, for IR-bright LBGs, median estimated β-based SFRs are 2-3 times larger than the total SFRs estimated as ${\it SFR}_{\rm TOT} = {\it SFR}_{\rm UV} + {\it SFR}_{\rm IR}$while IR-based SFRs provide values below ${\it SFR}_{\rm TOT}$by 15-20%. We use a stacking method to statistically constrain the $24~\mu$m flux of LBGs non individually detected. The results suggest that these LBGs do not contain large amounts of dust.

We constructed a local luminosity function (LF) of galaxies using a flux-limited sample ($S_{170} \ge 0.195~\mbox{Jy}$) of 55 galaxies at $z < 0.3$taken from the ISOFIRBACK survey at 170 μm. The overall shape of the 170-μm LF is found to be different from that of the total 60-μm LF (Takeuchi et al. 2003): the bright end of the LF declines more steeply than that of the 60-μm LF. This behavior is quantitatively similar to the LF of the cool subsample of the IRASPSCzgalaxies. We also estimated the strength of the evolution of the LF by assuming the pure luminosity evolution (PLE): $L(z) \propto (1+z)^Q$. We obtained $Q=5.0^{+2.5}_{-0.5}$which is similar to the value obtained by recent Spitzerobservations, in spite of the limited sample size. Then, integrating over the 170-μm LF, we obtained the local luminosity density at $170\;\mu$m, $\rho_L(170\;\mu\mbox{m})$. A direct integration of the LF gives $\rho_L(170\;\mu\mbox{m}) = 1.1 \times 10^8 h \;L_\odot \;\mbox{Mpc}^{-3}$, whilst if we assume a strong PLE with $Q=5$, the value is $5.2 \times 10^{7} h \; L_\odot \;\mbox{Mpc}^{-3}$. This is a considerable contribution to the local FIR luminosity density. By summing up with other available infrared data, we obtained the total dust luminosity density in the Local Universe, $\rho_L(\mbox{dust})=1.1 \times 10^{8}h\;L_\odot \;\mbox{Mpc}^{-3}$. Using this value, we estimated the cosmic star formation rate (SFR) density hidden by dust in the Local Universe. We obtained $\rho_{\rm SFR}(\mbox{dust}) \simeq 1.1\mbox{--}1.2\, h \times 10^{-2} \; M_\odot \,\mbox{yr}^{-1}\, \mbox{Mpc}^{-3}$, which means that 59% of the star formation is obscured by dust in the Local Universe.

The ratio between far-ultraviolet (FUV) and infrared (IR) luminosity densities from $z=0$to $z=1$is discussed by using the luminosity functions (LFs) of both wavelengths. The FUV LF ($z=0\mbox{--}1$) based on GALEXhas been reported by (Arnouts et al. (2005, ApJ, 619, L43), whilst for the IR LF, we used the IRASPSCz60-μm LF for the local universe and the Spitzer15-μm LF at higher-zas used by Le Floc'h et al. (2005, ApJ, in press). Both luminosity densities show a significant evolutionary trend, but the IR evolves much faster than the FUV. Consequently, the ratio $\rho_{\rm dust}/\rho_{\rm FUV}$increases toward higher-z, from ∼4 (local) to ∼15 ($z\simeq 1$). It is also shown that more than $70\%$of the star formation activity in the universe is obscured by dust at $0.5 \la z \la 1.2$.

The infrared (IR) emission plays a crucial role in understanding the star formation in galaxies hidden by dust. We first examined four estimators of the IR luminosity of galaxies, LFIR[CITE], LTIR[CITE], revised version of LTIR[CITE] (we denote LTIR2), and LIR[CITE] by using the observed SEDs of well-known galaxies. We found that LIRprovides excellent estimates of the total IR luminosity for a variety of galaxy SEDs. The performance of LTIR2was also found to be very good. Using LIR, we then statistically analyzed the IRASPSCzgalaxy sample [CITE] and found useful formulae relating the MIR monochromatic luminosities [ $L(12\,\mu\mbox{m})$and $L(25\,\mu\mbox{m})$] and LIR. For this purpose we constructed a subsample of 1420 galaxies with all four IRASband (12, 25, 60, and $100\,\mu$m) flux densities. We found linear relations between LIRand MIR luminosities, $L(12\,\mu\mbox{m})$and $L(25\,\mu\mbox{m})$. The prediction error with a 95% confidence level is a factor of 4–5. Hence, these formulae are useful for the estimation of the total IR luminosity only from $12\,\mu$m or $25\,\mu$m observations. We further tried to make an “interpolation” formula for galaxies at $0

Lyman-break galaxies (LBGs) contain a non-negligible amount of dust. Takeuchi (2003a, MNRAS, 343, 839) (T03) constructed a model of the infrared spectral energy distribution (SED) for very young galaxies by taking into account the dust size distribution in the early stage of galaxy evolution, which can be different from that of present-day evolved galaxies. We applied the T03 model to LBGs and constructed their expected SED. In order to examine the grain size distribution of dust, we calculated the SEDs based on two distinct types of the distribution models: a single-sized distribution and a power-law distribution with a slope of ${\rm d}N/{\rm d}a \propto a^{-3.5}$. We found that the single-sized and power-law dust size distributions yield a very similar detectability of LBGs at submillimetres (submm). We also found that galaxies with a power-law dust distribution have much less flux in the mid-infrared (MIR) than the other type. By making use of this fact we will be able to explore the dust grain size distribution in high-redshift galaxies through (observer-frame) FIR observations in future observations. We then applied the model to a gravitationally lensed LBG MS 1512-cB58(cB58), a unique probe of the dust emission from LBGs. Observations by SCUBA suggest that the galaxy has hot dust. Our model well reproduced the hot dust temperature under natural physical assumptions for the star formation rate (SFR), starburst age, and the radius of the star forming region in this galaxy. We also examined the detectability of LBGs at submm wavelengths in an eight-hour deep survey by ALMA. The LBG population with an age ${\ga} 10^8\,{\rm yr}$and a ${\rm SFR} \ga 10\,M_\odot ~{\rm yr}^{-1}$can be detected in such a survey. By integrating over their redshifted SEDs with the observed luminosity functions, we obtained the contribution of LBGs to the cosmic infrared background radiation (CIRB). Although they have a non-negligible amount of dust, their contribution was found to be small, especially in the ${\rm FIR} \sim 200\,\mu$m. Thus, we need a strongly obscured population of galaxies which contains a large amount of star formation, at some epoch in the history of the universe.

Effects of magnetic field on martensitic transformations have been examined in order to know a magnetic field-induced martensitic transformation by using Fe3Pt and Fe-Ni-Co-Ti shape memory alloys and an Fe-Ni alloy polycrystals, and control of variants by magnetic field by using Fe-Pd, Ni2MnGa and Fe3Pt shape memory alloy single crystals. Following results were obtained: (i) The effects of magnetic field on the martensitic transformation start temperature is explained by the equation proposed by our group. (ii) Magnetoelastic martensitic transformation (maretensites are induced only while a magnetic field is applied and are transformed back to the parent phase when the magnetic field is removed) appears in an ausaged Fe-Ni-Co-Ti shape memory alloy. (iii) In Fe-31.2Pd(at.%), whose easy axis is the a-axis in martensite state, a large expansion of about 3% appears in [OOl]p(P is the symbol of the parent phase) direction at 77 K by applying a magnetic field along [001]pdirection. In Ni2MnGa, whose easy axis is the c-axis in martensite state, a large contraction of about 3.8% appears in [001]pdirection at 77 K by applying a magnetic field along [001]pdirection. These strains are nearly the same as those expected from perfect conversion to the preferred variants under magnetic field. In Fe3Pt, whose easy axis is the c-axis in martensite state, a large contraction of about 2.3% appears in [001]pdirection at 4.2 K by applying a magnetic field along [001]pdirection, and a part of this contraction (0.6%) recovers as the field is removed. Considering results of (iii), the mechanism of conversion of variants by magnetic field is discussed.

Objective.To evaluate the longterm safety and efficacy of subcutaneous tocilizumab (TCZ-SC) as monotherapy in patients with rheumatoid arthritis (RA).Methods.Of 346 patients who received 24 weeks of double-blind treatment with either TCZ-SC monotherapy, 162 mg every 2 weeks (q2w); or intravenous TCZ (TCZ-IV) monotherapy, 8 mg/kg every 4 weeks; 319 patients continued to receive TCZ-SC q2w in the 84-week open-label extension (OLE) of the MUSASHI study (JAPICCTI-101117). Efficacy, safety, and immunogenicity were evaluated for all patients treated with TCZ during 108 weeks.Results.The proportions of patients who achieved American College of Rheumatology 20/50/70 responses, low disease activity [28-joint Disease Activity Score (DAS28) ≤ 3.2], or remission (DAS28 < 2.6) at Week 24 were maintained until Week 108. The incidences of adverse events and serious adverse events were 498.3 and 16.9 per 100 patient-years (PY), respectively. The overall safety of TCZ-SC monotherapy was similar to that of TCZ-IV monotherapy. Rates of injection site reactions (ISR) through 108 weeks remained similar to rates through 24 weeks. ISR were mild and did not cause any patient withdrawals. No serious hypersensitivity events (including anaphylactic reactions) occurred. Anti-TCZ antibodies were present in 2.1% of patients treated with TCZ-SC monotherapy.Conclusion.TCZ-SC monotherapy maintained a favorable safety profile and consistent efficacy throughout the 108-week study. Like TCZ-IV, TCZ-SC could provide an additional treatment option for patients with RA.

We present the results of the analysis of multiwavelength Spectral Energy Distributions (SEDs) of far-infrared galaxies detected in the AKARI Deep Field-South (ADF-S) Survey. The analysis uses a carefully selected sample of 186 sources detected at the 90 μm AKARI band, identified as galaxies with cross-identification in public catalogues. For sources without known spectroscopic redshifts, we estimate photometric redshifts after a test of two independent methods: one based on using mainly the optical—mid infrared range, and one based on the whole range of ultraviolet—far infrared data. We observe a vast improvement in the estimation of photometric redshifts when far infrared data are included, compared with an approach based mainly on the optical—mid infrared range. We discuss the physical properties of our far-infrared-selected sample. We conclude that this sample consists mostly of rich in dust and young stars nearby galaxies, and, furthermore, that almost 25% of these sources are (Ultra)Luminous Infrared Galaxies. Average SEDs normalized at 90 μm for normal galaxies (138 sources), LIRGs (30 sources), and ULIRGs (18 galaxies) show a significant shift in the peak wavelength of the dust emission, and an increasing ratio between their bolometric and dust luminosities which varies from 0.39 to 0.73.

We present the measurements of the angular two-point correlation function for AKARI 90-μm point sources, detected outside the Milky Way plane and other regions characterized by high Galactic extinction in the northern Galactic hemisphere, and categorized as extragalactic sources according to our far-infrared-color based criterion. Together with our previous work (Pollo et al., 2013) this is the first measurement of the large-scale angular clustering of galaxies selected in the far-infrared after IRAS. We present the first attempt to estimate the spatial clustering properties of AKARI All-Sky galaxies and we conclude that they are mostly a very nearby (z≤ 0.1) population of moderately clustered galaxies. We measure their correlation length r0~ 4.5 h−1Mpc, which is consistent with the assumption that the FIS AKARI All-Sky surveys observes mostly a nearby star-forming population of galaxies.

An accurate estimation of the star formation-related properties of galaxies is crucial for understanding the evolution of galaxies. In galaxies, ultraviolet (UV) light emitted by recently formed massive stars is attenuated by dust, which is also produced by star formation (SF) activity, and is re-emitted at mid- and far- infrared (IR) wavelengths. In this study, we investigate the star formation rate (SFR) and dust extinction using UV and IR data. We selected local galaxies which are detected at AKARI FIS 90 μm and matched the IRAS IIFSCz60 μm select catalog. We measured FUV and NUV flux densities from GALEX images. We examined the SF and extinction of Local galaxies using four bands of AKARI. Then, we calculated FUV and total IR luminosities, and obtained the SF luminosity, LSF, the total luminosity related to star formation activity, and the SFR. We find that in most galaxies, LSFis dominated by Ldust. We also find that galaxies with higher SF activity have a higher fraction of their SF hidden by dust. In fact, the SF of galaxies with SFRs > 20 M⊙yr−1is almost completely hidden by dust. Our results boast a significantly higher precision with respect to previously published works, due to the use of much larger object samples from the AKARI and GALEX all sky surveys.

Diamagnetic anisotropy Δχdiawas detected on a submillimeter-sized calcite crystal by observing the rotational oscillation of its magnetically stable axis with respect to the magnetic field direction. The crystal was released in an area of microgravity generated by a 1.5-m-long drop shaft. When the oscillations are observable, the present method can measure Δχdiaof crystal grains irrespective of how small they are without measuring the sample mass. In conventional Δ χmeasurements, the background signal from the sample holder and the difficulty in measuring the sample mass prevent measurement of Δχdiafor small samples. The present technique of observing Δχdiaof a submillimeter-sized single crystal is a step toward realizing Δχdiameasurements of micron-sized grains. The Δχdiavalues of single micron-sized grains can be used to assess the validity of a dust alignment model based on magnetic torque that originates from the Δχdiaof individual dust particles.

The evolution of galaxies and the history of star formation in the Universe are among the most important topics in today’s astrophysics. Especially, the role of small, irregular galaxies in the star-formation history of the Universe is not yet clear. Using the data from the AKARI IRC survey of the Large Magellanic Cloud at 3.2, 7, 11, 15, and 24 μm wavelengths, i.e., at the mid- and near-infrared, we have constructed a multiwavelength catalog containing data from a cross-correlation with a number of other databases at different wavelengths. We present the separation of different classes of stars in the LMC in color-color, and color-magnitude, diagrams, and analyze their contribution to the total LMC flux, related to point sources at different infrared wavelengths.

Post-irradiation annealing (PIA) behavior of irradiation-induced microstructural changes and hardening of two kind of A533B (first generation (1stGENS: 0.16 wt.% Cu) and second generation (2ndGENS: 0.04 wt.% Cu)) steels after neutron-irradiation of 3.9 × 1019 n cm–2 at 290 °C has been studied by positron annihilation spectroscopy, atom probe tomography and Vickers microhardness measurements. In the 1stGENS, clear two recovery stages are observed: (i) as-irradiated state to 450 °C and (ii) 450 to 600 °C. The first stage is due to annealing out of the most of irradiation-induced vacancy-related defects (VRDs), and the second stage corresponds to dissolving irradiation-induced Cu-rich solute nano-clusters (CRSCs). The experimental hardening is almost twice of the hardening due to the CRSCs estimated by Russell-Brown model below 350 °C, but almost the same as the estimation from 400 to 550 °C. In the 2ndGENS, the VRDs and non-Cu-rich solute nano-clusters (NCRSCs) recover at 450 °C. No CRSC has been formed even in all the annealing process. The experimental hardening is almost twice of the hardening estimated due to the NCRSCs by Russell-Brown model below 400 °C.