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Background: Cardiopulmonary exercise testing (CPET) variables represent central and peripheral factors and combined factors in the pathology of patients with cardiac disease. The difference in end‐tidal oxygen partial pressure from resting to anaerobic threshold (ΔPETO2) may represent predominantly peripheral factors. This study aimed to verify the prognostic significance of ΔPETO2 for major adverse cardiac and cerebrovascular events (MACCE) in cardiac patients, including comparison with the minute ventilation–carbon dioxide production relationship (VE/VCO2 slope), and peak oxygen uptake (VO2). Methods: In total, 185 patients with cardiac disease who underwent CPET were consecutively enroled in this retrospective study. The primary endpoint was 3‐year MACCE. The ability of ΔPETO2, VE/VCO2 slope, and peak VO2 to predict MACCE was examined. Results: Optimal cut‐off values for predicting MACCE were 2.0 mmHg for ΔPETO2 (area under the curve [AUC]: 0.829), 29.8 for VE/VCO2 slope (AUC: 0.734), and 19.0 mL/min/kg for peak VO2 (AUC: 0.755). The AUC of ΔPETO2 was higher than those of VE/VCO2 slope and peak VO2. The MACCE‐free survival rate was significantly lower in the ΔPETO2 ≤ 2.0 group versus the ΔPETO2 > 2.0 group (44.4% vs. 91.2%, p < 0.001). ΔPETO2 ≤ 2.0 was an independent predictor of MACCE after adjustment for age and VE/VCO2 slope (hazard ratio [HR], 7.28; p < 0.001) and after adjustment for age and peak VO2 (HR, 6.52; p < 0.001). Conclusion: ΔPETO2 was a strong predictor of MACCE independent of and superior to VE/VCO2 slope and peak VO2 in patients with cardiac disease. [ABSTRACT FROM AUTHOR]

Context Adrenocorticotropin (ACTH) loading is used to increase the success rate of adrenal vein sampling (AVS). Objective We aimed to determine the effect of intraprocedural cortisol measurement (ICM) on ACTH-stimulated AVS (AS-AVS) owing to a lack of reliable data on this topic. Methods This multicenter, retrospective, observational study took place in 28 tertiary centers in Japan. Among 4057 patients enrolled, 2396 received both basal AVS (B-AVS) and AS-AVS and were divided into 2 groups according to whether ICM was used. The effect of ICM on AS-AVS was measured. Results In patients who underwent both AVS procedures, the ICM group had significantly higher success rates for both B-AVS and AS-AVS than the non-ICM group did. However, the probability of failure of AS-AVS after a successful B-AVS and the probability of success of AS-AVS after a failed B-AVS were not significantly different in the 2 groups. For subtype diagnosis, propensity-score matching revealed no significant difference between the 2 groups, and the discrepancy rate between B-AVS and AS-AVS for subtype diagnosis was also not significantly different. Conclusion ICM significantly increased the success rate of B-AVS and AS-AVS in protocols in which both AVS procedures were performed and had no effect on subtype diagnosis. However, in protocols in which both AVS procedures were performed, the results suggest ICM may not be necessary when performing AS-AVS if ICM is used only when B-AVS is performed. Our study suggests that ICM during AVS plays an important role and should be recommended. [ABSTRACT FROM AUTHOR]

We present new spectroscopic observations of Ly α (Ly α) Blob 2 (z ∼ 3.1). We observed extended Ly α emission in three distinct regions, where the highest Ly α surface brightness (SB) centre is far away from the known continuum sources. We searched through the MOSFIRE slits that cover the high Ly α SB regions, but were unable to detect any significant nebular emission near the highest SB centre. We further mapped the flux ratio of the blue peak to the red peak and found it is anticorrelated with Ly α SB with a power-law index of ∼ –0.4. We used radiative transfer models with both multiphase, clumpy, and shell geometries and successfully reproduced the diverse Ly α morphologies. We found that most spectra suggest outflow-dominated kinematics, while 4/15 spectra imply inflows. A significant correlation exists between parameter pairs, and the multiphase, clumpy model may alleviate previously reported discrepancies. We also modelled Ly α spectra at different positions simultaneously and found that the variation of the inferred clump outflow velocities can be approximately explained by line-of-sight projection effects. Our results support the 'central powering  + scattering' scenario, i.e. the Ly α photons are generated by a central powering source and then scatter with outflowing, multiphase H   i gas while propagating outwards. The infalling of cool gas near the blob outskirts shapes the observed blue-dominated Ly α profiles, but its energy contribution to the total Ly α luminosity is less than 10 per cent, i.e. minor compared to the photoionization by star-forming galaxies and/or AGNs. [ABSTRACT FROM AUTHOR]

We present observations of [N  ii ] 205 μm, [O  iii ] 88 μm, and dust emission in a strongly-lensed, submillimeter galaxy (SMG) at z = 6.0, G09.83808, with the Atacama Large Millimeter/submillimeter Array (ALMA). Both [N  ii ] and [O  iii ] line emissions are detected at >12σ in the |${0{^{\prime \prime}_{.}}8}$| -resolution maps. Lens modeling indicates that the spatial distribution of the dust continuum emission is well characterized by a compact disk with an effective radius of 0.64 ± 0.02 kpc and a high infrared surface brightness of ΣIR = (1.8 ± 0.3) × 1012  L ⊙ kpc−2. This result supports that G09.83808 is the progenitor of compact quiescent galaxies at z ∼ 4, where the majority of its stars are expected to be formed through a strong and short burst of star formation. G09.83808 and other lensed SMGs show a decreasing trend in the [N  ii ] line to infrared luminosity ratio with increasing continuum flux density ratio between 63 and 158 μm, as seen in local luminous infrared galaxies (LIRGs). The decreasing trend can be reproduced by photoionization models with increasing ionization parameters. Furthermore, by combining the [N  ii ]/[O  iii ] luminosity ratio with far-infrared continuum flux density ratio in G09.83808, we infer that the gas phase metallicity is already Z ≈ 0.5–0.7  Z ⊙. G09.83808 is likely one of the earliest galaxies that has been chemically enriched at the end of reionization. [ABSTRACT FROM AUTHOR]

This study aimed to clarify the effects of gardening on hemodynamic response, rating of perceived exertion (RPE) during exercise, and body weight in patients in whom phase 2 cardiac rehabilitation (CR) was interrupted due to the Coronavirus disease 2019 (COVID-19) pandemic. Among 76 outpatients participating in consecutive phase 2 CR in both periods from March to April and June to July 2020, which were before and after CR interruption, respectively, at Sanda City Hospital were enrolled. The inclusion criterion was outpatients whose CR was interrupted due to COVID-19. Patients under the age of 65 were excluded. We compared the data of hemodynamic response and RPE during exercise on the last day before interruption and the first day after interruption when aerobic exercise was performed at the same exercise intensity in the gardener group and the non-gardener group. Forty-one patients were enrolled in the final analysis. After CR interruption, the gardener group did not show any significant difference in all items, whereas the non-gardener group experienced significant increase in HR (Peak) (p = 0.004) and worsening of the Borg scale scores for both dyspnea and lower extremity fatigue (p = 0.039 and p = 0.009, respectively). Older phase 2 CR patients engaged in gardening did not show any deterioration in hemodynamic response or RPE during exercise, despite CR interruption and refraining from going outside. Gardening may be recommended as one of the activities that can maintain or improve physical function in older phase 2 CR patients during the COVID-19 pandemic. [ABSTRACT FROM AUTHOR]

The anaerobic threshold (AT), obtained during cardiopulmonary exercise testing (CPET), is an important prognostic measure and can be used to develop an exercise prescription in patients after a myocardial infarction (post-MI). The purpose of this study was to examine the central and peripheral determinants of AT in post-MI patients end-tidal oxygen partial pressure (PETO2) measures. We performed cardiopulmonary exercise testing (CPET) on 148 consecutively enrolled post-MI patients to determine PETO2 measured at the AT (AT PETO2) and ΔPETO2 (difference between resting PETO2 and AT PETO2). We subsequently investigated the relationship between these measures of PETO2 and the individual AT for each patient. Multivariate linear regression analysis indicated that AT PETO2 and ΔPETO2 were independently and significantly associated with the AT (β = −0.344, p < 0.001 and β = 0.228, p < 0.001, respectively). Furthermore, the independent factors of AT PETO2 were left ventricular ejection fraction (p = 0.005), resting ventilatory equivalent for carbon dioxide (p = 0.002), and resting dead-space gas volume to tidal volume ratio (p < 0.001). However, the independent factors for ΔPETO2 were history of diabetes (p = 0.047), estimated glomerular filtration rate (p = 0.001), and resting systolic blood pressure (p = 0.017). These findings suggested that AT PETO2 was associated with central determinants; whereas, and ΔPETO2 was associated with peripheral determinants, The AT PETO2 and ΔPETO2 provide variable insight regarding the cause of exercise intolerance and can be used to determine appropriate therapies. [ABSTRACT FROM AUTHOR]

We report a massive quiescent galaxy at spectroscopically confirmed at a protocluster in the SSA22 field by detecting the Balmer and Ca ii absorption features with the multi-object spectrometer for infrared exploration on the Keck I telescope. This is the most distant quiescent galaxy confirmed in a protocluster to date. We fit the optical to mid-infrared photometry and spectrum simultaneously with spectral energy distribution (SED) models of parametric and nonparametric star formation histories (SFHs). Both models fit the observed SED well and confirm that this object is a massive quiescent galaxy with a stellar mass of and , and a star formation rate of SFR/M⊙ yr−1 < 0.3 and for parametric and nonparametric models, respectively. The SFH from the former modeling is described as an instantaneous starburst whereas that of the latter modeling is longer-lived, but both models agree with a sudden quenching of the star formation at ∼0.6 Gyr ago. This massive quiescent galaxy is confirmed in an extremely dense group of galaxies predicted as a progenitor of a brightest cluster galaxy formed via multiple mergers in cosmological numerical simulations. We discover three new plausible [O iii ]λ5007 emitters at 3.0791 ≤ zspec ≤ 3.0833 serendipitously detected around the target. Two of them just between the target and its nearest massive galaxy are possible evidence of their interactions. They suggest the future great size and stellar mass evolution of this massive quiescent galaxy via mergers. [ABSTRACT FROM AUTHOR]

We present observations of a giant Lyα blob (LAB) in the SSA22 protocluster at z = 3.1, SSA22-LAB1, taken with the Atacama Large Millimeter/submillimeter Array. Dust continuum, along with [C ii ] 158 μm and CO(4–3) line emission have been detected in LAB1, showing complex morphology and kinematics across a ∼100 kpc central region. Seven galaxies at z = 3.0987–3.1016 in the surroundings are identified in [C ii ] and dust continuum emission, with two of them potential companions or tidal structures associated with the most massive galaxies. Spatially resolved [C ii ] and infrared luminosity ratios for the widely distributed media (L[Cɪɪ]/LIR ≈ 10−2−10−3) suggest that the observed extended interstellar media are likely to have originated from star formation activity and the contribution from shocked gas is probably not dominant. LAB1 is found to harbor a total molecular gas mass Mmol = (8.7 ± 2.0) × 1010M⊙, concentrated in the core region of the Lyα-emitting area. While (primarily obscured) star formation activity in the LAB1 core is one of the most plausible power sources for the Lyα emission, multiple major mergers found in the core may also play a role in making LAB1 exceptionally bright and extended in Lyα as a result of cooling radiation induced by gravitational interactions. [ABSTRACT FROM AUTHOR]

We present a detailed investigation of millimeter-wave line emitters ALMA J010748.3-173028 (ALMA-J0107a) and ALMA J010747.0-173010 (ALMA-J0107b), which were serendipitously uncovered in the background of the nearby galaxy VV 114 with spectral scan observations at λ = 2–3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA) detection of CO(4–3), CO(3–2), and [C i ](1–0) lines for both sources, their spectroscopic redshifts are unambiguously determined to be z = 2.4666 ± 0.0002 and z = 2.3100 ± 0.0002, respectively. We obtain the apparent molecular gas masses Mgas of these two line emitters from [C i ] line fluxes as (11.2 ± 3.1) × 1010M⊙ and (4.2 ± 1.2) × 1010M⊙, respectively. The observed CO(4–3) velocity field of ALMA-J0107a exhibits a clear velocity gradient across the CO disk, and we find that ALMA-J0107a is characterized by an inclined rotating disk with a significant turbulence, that is, a deprojected maximum rotation velocity to velocity dispersion ratio of 1.3 ± 0.3. We find that the dynamical mass of ALMA-J0107a within the CO-emitting disk computed from the derived kinetic parameters, (1.1 ± 0.2) × 1010M⊙, is an order of magnitude smaller than the molecular gas mass derived from dust continuum emission, (3.2 ± 1.6) × 1011M⊙. We suggest this source is magnified by a gravitational lens with a magnification of μ ≳ 10, which is consistent with the measured offset from the empirical correlation between CO-line luminosity and width. [ABSTRACT FROM AUTHOR]

This study aimed to clarify the effects of the interruption of cardiac rehabilitation (CR) and refraining from going outside due to the COVID-19 pandemic on hemodynamic response and rating of perceived exertion (RPE) during exercise including differences by age in phase 2 CR outpatients. Among 76 outpatients participating in consecutive phase 2 CR in both periods from March to April and June to July 2020, which were before and after CR interruption, respectively, at Sanda City Hospital were enrolled. The inclusion criterion was outpatients whose CR was interrupted due to COVID-19. We compared the data of hemodynamic response and RPE during exercise on the last day before interruption and the first day after interruption when aerobic exercise was performed at the same exercise intensity in the < 75 years group and ≥ 75 years group. Fifty-three patients were enrolled in the final analysis. Post-CR interruption, peak heart rate increased significantly (p = 0.009) in the < 75 years group, whereas in the ≥ 75 years group, weight and body mass index decreased significantly (p = 0.009, 0.011, respectively) and Borg scale scores for both dyspnea and lower extremities fatigue worsened significantly (both, p < 0.001). CR interruption and refraining from going outside due to the COVID-19 pandemic affected the hemodynamic response, RPE during exercise and body weight in phase 2 CR outpatients. In particular, patients aged ≥ 75 years appeared to be placed at an increased risk of frailty. [ABSTRACT FROM AUTHOR]

We present results of the cross-correlation Lyα intensity mapping with Subaru/Hyper Suprime-Cam (HSC) ultra-deep narrowband images and Lyα emitters (LAEs) at z = 5.7 and 6.6 in a total area of 4 deg2. Although an overwhelming amount of data quality controls have been performed for the narrowband images, we further conduct extensive analyses evaluating systematics of large-scale point-spread function wings, sky subtractions, and unknown errors based on physically uncorrelated signals and sources found in real HSC images and object catalogs, respectively. Removing the systematics, we carefully calculate cross-correlations between Lyα intensity of the narrowband images and the LAEs. We tentatively identify very diffuse Lyα emission with the ≃3σ (≃2σ) significance at ≳100 comoving kiloparsecs (ckpc) far from the LAEs at z = 5.7 (6.6), around and probably even beyond a virial radius of star-forming galaxies with Mh ∼ 1011M⊙. The diffuse Lyα emission possibly extends up to 1000 ckpc with the surface brightness of 10−20–10−19 erg s−1 cm−2 arcsec−2. We confirm that the small-scale (<150 ckpc) Lyα radial profiles of LAEs are consistent with those obtained by recent Multi-Unit Spectroscopic Explorer observations. Comparisons with numerical simulations suggest that the large-scale (∼150–1000 ckpc) Lyα emission are not explained by unresolved faint neighboring galaxies including satellites, but by a combination of Lyα photons emitted from the central LAE and other unknown sources, such as cold-gas streams and galactic outflow. We find no evolution in the Lyα radial profiles of our LAEs from z = 5.7 to 6.6, where theoretical models predict a flattening of the profile slope made by cosmic reionization, albeit with our moderately large observational errors. [ABSTRACT FROM AUTHOR]

Aim: Worsening renal function (WRF) induced by acute myocardial infarction (AMI) is a strong predictor of cardiovascular events and mortality. Peak oxygen uptake may contribute to prognosis in AMI patients with WRF, however, the impact of WRF on peak oxygen uptake is unclear. Methods: Among 154 patients with AMI who underwent emergency percutaneous coronary intervention and participated in phase II cardiac rehabilitation, those who underwent cardiopulmonary exercise testing were consecutively enrolled. WRF was defined as a ≥20% decrease in estimated glomerular filtration rate (eGFR [ml/min/1.73 m2]) from admission to that at cardiopulmonary exercise testing. The association of WRF with peak oxygen uptake was evaluated by multivariate regression analysis. The non‐WRF group was divided into two subgroups according to eGFR <60/≥60 at cardiopulmonary exercise testing, and eGFR at cardiopulmonary exercise testing and peak oxygen uptake of all three groups were compared. Results: Ninety‐four patients were enrolled in the final analysis. Multiple linear regression analysis showed that WRF was associated with peak oxygen uptake (p =.003). Comparing the non‐WRF group with eGFR at cardiopulmonary exercise testing <60 and the WRF group, although eGFR at cardiopulmonary exercise testing was similar (p = 1.000), peak oxygen uptake in the WRF group was significantly lower (p =.026). Conclusion: WRF, not eGFR at cardiopulmonary exercise testing was significantly associated with peak oxygen uptake in patients with AMI. This result suggests that when considering the relationship between renal function and peak oxygen uptake, WRF must be taken into account. SUMMARY AT A GLANCE: This is a retrospective cohort study on 94 patients followed for up to 6 months in Japan showing that worsening of kidney function after acute myocardial infarction (MI) is associated with peak oxygen uptake on exercise test, and this association is independent of baseline kidney function. Thus a decline is kidney function post MI may have implications for worse outcomes than the absolute level of kidney function. [ABSTRACT FROM AUTHOR]

We present the results of CO(1–0) observations of the host galaxy of a Type I superluminous supernova (SLSN-I), SN 2017egm, one of the closest SLSNe-I at z = 0.03063, by using the Atacama Large Millimeter/submillimeter Array. The molecular gas mass of the host galaxy is M gas = (4.8 ± 0.3) × 109  M ⊙, placing it on the sequence of normal star-forming galaxies in an M gas–star-formation rate (SFR) plane. The molecular hydrogen column density at the location of SN 2017egm is higher than that of the Type II SN PTF10bgl, which is also located in the same host galaxy, and those of other Type II and Ia SNe located in different galaxies, suggesting that SLSNe-I have a preference for a dense molecular gas environment. On the other hand, the column density at the location of SN 2017egm is comparable to those of Type Ibc SNe. The surface densities of molecular gas and the SFR at the location of SN 2017egm are consistent with those of spatially resolved local star-forming galaxies and follow the Schmidt–Kennicutt relation. These facts suggest that SLSNe-I can occur in environments with the same star-formation mechanism as in normal star-forming galaxies. [ABSTRACT FROM AUTHOR]

We present our new Atacama Large Millimeter/Submillimeter Array (ALMA) observations targeting [O iii ]88 μm, [C ii ]158 μm, [N ii ]122 μm, and dust-continuum emission for three Lyman break galaxies at z = 6.0293–6.2037, identified in the Subaru/Hyper Suprime-Cam survey. We clearly detect [O iii ] and [C ii ] lines from all of the galaxies at 4.3–11.8σ levels, and identify multi-band dust-continuum emission in two of the three galaxies, allowing us to estimate infrared luminosities and dust temperatures simultaneously. In conjunction with previous ALMA observations for six galaxies at z > 6, we confirm that all the nine z = 6–9 galaxies have high [O iii ]/[C ii ] ratios of , ∼10 times higher than z ∼ 0 galaxies. We also find a positive correlation between the [O iii ]/[C ii ] ratio and the Lyα equivalent width (EW) at the ∼90% significance level. We carefully investigate physical origins of the high [O iii ]/[C ii ] ratios at z = 6–9 using Cloudy, and find that high density of the interstellar medium, low C/O abundance ratio, and the cosmic microwave background attenuation are responsible to only a part of the z = 6–9 galaxies. Instead, the observed high [O iii ]/[C ii ] ratios are explained by 10–100 times higher ionization parameters or low photodissociation region (PDR) covering fractions of 0%–10%, both of which are consistent with our [N ii ] observations. The latter scenario can be reproduced with a density-bounded nebula with PDR deficit, which would enhance the Lyα, Lyman continuum, and ionizing photons escape from galaxies, consistent with the [O iii ]/[C ii ]-Lyα EW correlation we find. [ABSTRACT FROM AUTHOR]

We present an IGM H i tomographic map in a survey volume of (cMpc3) centered at MAMMOTH-1 nebula and three neighboring quasars at z = 2.3. The MAMMOTH-1 nebula is an enormous Lyα nebula (ELAN), hosted by a type-II quasar dubbed MAMMOTH1-QSO, that extends over cMpc with no clear physical origin. Here we investigate the H i -gas distribution around MAMMOTH1-QSO with the ELAN and three neighboring type-I quasars, making the IGM H i tomographic map with a spatial resolution of 2.6 h−1 cMpc. Our H i tomographic map is reconstructed with H i Lyα forest absorption of bright background objects at z = 2.4–2.9: one eBOSS quasar and 16 Keck/LRIS galaxy spectra. We estimate the radial profile of H i overdensity for MAMMOTH1-QSO, and find that MAMMOTH1-QSO resides in a volume with fairly weak H i absorption. This suggests that MAMMOTH1-QSO may have a proximity zone where quasar illuminates and photoionizes the surrounding H i gas and suppresses H i absorption, and that the ELAN is probably a photoionized cloud embedded in the cosmic web. The H i radial profile of MAMMOTH1-QSO is very similar to those of three neighboring type-I quasars at z = 2.3, which is compatible with the AGN unification model. We compare the distributions of the H i absorption and star-forming galaxies in our survey volume, and identify a spatial offset between density peaks of star-forming galaxies and H i gas. This segregation may suggest anisotropic UV background radiation created by star-forming galaxy density fluctuations. [ABSTRACT FROM AUTHOR]

We report on the detection of the [C  ii ] 157.7 μ m emission from the Lyman break galaxy (LBG) MACS0416_Y1 at z  = 8.3113, by using the Atacama Large Millimeter/submillimeter Array (ALMA). The luminosity ratio of [O  iii ] 88 μ m (from previous campaigns) to [C  ii ] is 9.3 ± 2.6, indicative of hard interstellar radiation fields and/or a low covering fraction of photodissociation regions. The emission of [C  ii ] is cospatial to the 850 μ m dust emission (90 μ m rest frame, from previous campaigns), however the peak [C  ii ] emission does not agree with the peak [O  iii ] emission, suggesting that the lines originate from different conditions in the interstellar medium. We fail to detect continuum emission at 1.5 mm (160 μ m rest frame) down to 18 μ Jy (3σ). This non-detection places a strong limits on the dust spectrum, considering the 137 ± 26 μ Jy continuum emission at 850 μ m. This suggests an unusually warm dust component (T > 80 K, 90 per cent confidence limit), and/or a steep dust-emissivity index (βdust > 2), compared to galaxy-wide dust emission found at lower redshifts (typically T ∼ 30–50 K, βdust ∼ 1–2). If such temperatures are common, this would reduce the required dust mass and relax the dust production problem at the highest redshifts. We therefore warn against the use of only single-wavelength information to derive physical properties, recommend a more thorough examination of dust temperatures in the early Universe, and stress the need for instrumentation that probes the peak of warm dust in the Epoch of Reionization. [ABSTRACT FROM AUTHOR]

Objectives: We investigated the clinical significance of ACTH stimulation d uring adrenal venous sampling (AVS) by surgical outcome of primary aldosteronism (PA). Design: Multicenter retrospective study by Japan PA study. Method: We allocated 314 patients with both basal and ACTH-stimulated AVS data who underwent adrenalectomy to three groups: basal lateralization index (LI) =2 with ACTH-stimulated LI =4 on the ipsilateral side (Unilateral (U) to U group, n = 245); basal LI <2 with ACTH-stimulated LI =4 (Bilateral (B) to U group, n = 15); and basal LI =2 with ACTH-stimulated LI <4 (U to B group, n = 54). We compared surgical outcomes among the groups using the Primary Aldosteronism Surgical Outcome (PASO) criteria. Results: Compared with U to U group, U to B group had poor clinical and biochemical outcomes and low rates of adrenal adenoma as pathological findings (P = 0.044, 0.006, and 0.048, respectively), although there were no significant differences between U to U and B to U groups. All patients in U to B group with clinical and biochemical benefits, however, had adrenal adenoma as pathological findings and could be well differentiated from those with poor surgical outcomes via basal LI (>8.3), but not ACTH-stimulated LI. These results were similar ev en when we defined each group based on a cut-off value of 4 for basal LI. Conclusions: Although PA patients in U to B group had worse surgical outcom es than did those in U to U group, basal LI could discriminate among patients with better surgical outcomes in U to B group. [ABSTRACT FROM AUTHOR]

Context Aldosterone-producing adenomas are a curable subtype of primary aldosteronism (PA); however, hypertension persists in some patients after adrenalectomy. Objective To identify factors associated with, and develop prediction models for, blood pressure (BP) normalization or improvement after adrenalectomy. Design Retrospective analysis of patients treated between 2006 and 2018, with a 6-month follow-up. Setting A nationwide, 29-center Japanese registry encompassing 15 university hospitals and 14 city hospitals. Patients We categorized 574 participants in the Japan Primary Aldosteronism Study, who were diagnosed with PA and underwent adrenalectomy, as BP normalized or improved, on the basis of their presentations at 6 months postsurgery. Main Outcome Measure The rate of complete, partial, and absent clinical success. Predictive factors related to BP outcomes after PA surgery were also evaluated. Results Complete clinical success was achieved in 32.6% and partial clinical success was achieved in 53.0% of the patients at 6 months postsurgery. The following five variables were independent predictors for BP normalization: ≤7 years of hypertension, body mass index ≤25 kg/m2, no more than one antihypertensive medication, absence of medical history of diabetes, and female sex. The area under the receiver operator characteristic curve was 0.797 in the BP normalization model. Conclusion We established models that predicted postoperative BP normalization in patients with PA. These should be useful for shared decision-making regarding adrenalectomy for PA. [ABSTRACT FROM AUTHOR]

We report results of a search for galaxies at z > 3 with Lyman continuum (LyC) emission using a narrow-band filter NB359   with Subaru/Suprime-Cam in an ∼800 arcmin2 blank field around the GOODS-N. We use 103 star-forming galaxies (SFGs) and 8 active galactic nuclei (AGNs) with spectroscopic redshifts in a range between 3.06 and 3.5 and 157 photometrically selected z  = 3.1 Lyman α emitter (LAE) candidates as the targets. After removing galaxies spectroscopically confirmed to be contaminated by foreground sources, we found two SFGs and one AGN as candidate LyC-emitting sources among the targets with spectroscopic redshifts. Among LAE candidates, five sources are detected in the NB359 image, and three among them may be contaminated by foreground sources. We compare the sample galaxies in the GOODS-N with those in the SSA22, where a prominent protocluster at z  = 3.1 is known and an LyC search using the same NB359 filter has been made. The frequency of galaxies with LyC leakage in the SSA22 field may be about two times higher than that of galaxies in the GOODS-N with the sample ultraviolet (UV) magnitude range, although the numbers of LyC detections in these fields are too small to make a statistically significant conclusion. By combining the sample galaxies in these fields, we place the 3σ upper limits of the observed LyC-to-UV flux density ratio and LyC escape fraction for galaxies at z  = 3.1 with absolute UV magnitude M UV < −18.8 as (f LyC/ f UV)obs < 0.036 and |$f_\mathrm{esc}^\mathrm{abs}\,\lt\, 8$|  per cent, respectively. [ABSTRACT FROM AUTHOR]

Context In patients with primary aldosteronism (PA), it remains unclear whether aldosterone-producing adenomas are likely to develop in the left or right adrenal gland. Objective To investigate left-right differences of PA laterality diagnoses via CT imaging and adrenal vein sampling (AVS). Design Retrospective, observational study. Patients From the Japan Primary Aldosteronism Study, 1493 patients with PA were enrolled who underwent CT and ACTH-stimulated AVS. Measurements Left or right adrenal nodular lesion distribution and laterality observed on CT scans and from AVS were noted. Results Both on CT scans and AVS, unilateral results were observed more frequently on the left side than on the right side (25.1% vs 15.4% and 17.3% vs 13.5%, respectively; P < 0.01for both diagnostic techniques). There was no significant difference in the concordance rate for CT and AVS between patients with left and right unilateral nodular lesions observed on CT scans (44.1% and 50.9%, respectively; P = 0.15). In patients with nodules <20 mm, the concordance rate was significantly greater on the right side than the left side (45.8% vs 56.4%; P = 0.03). In patients with bilateral results of AVS, unilateral nodular lesions were detected more frequently on the left side than the right side (17.8% vs 9.4%; P < 0.01). Conclusion These results suggest aldosterone-producing adenomas and nonfunctioning tumors are more likely to develop on the left side in patients with PA and that misdiagnosis of CT-based lateralization may occur more frequently on the left side. [ABSTRACT FROM AUTHOR]

A primary goal of the Submillimetre Common User Bolometer Array-2 web survey is to perform tomography of the early intergalactic medium by studying systems containing some of the brightest quasi-stellar objects (QSOs; 2.5 |$\, {\lt }\, z\, {\lt }\,$| 3.0) and nearby submillimetre galaxies (SMGs). As a first step, this paper aims to characterize the galaxies that host the QSOs. To achieve this, a sample of 13 hyper-luminous (⁠|$L_{\rm AGN}\, {\gt }\, 10^{14}\, {\rm L}_{\odot }$|⁠) QSOs with previous submillimetre continuum detections were followed up with CO(3–2) observations using the NOrthern Extended Millimeter Array interferometer. All but two of the QSOs are detected in CO(3–2); for one non-detection, our observations show a tentative 2σ line at the expected position and redshift, and for the other non-detection we find only continuum flux density an order of magnitude brighter than the other sources. In three of the fields, a companion potentially suitable for tomography is detected in CO line emission within 25 arcsec of the QSO. We derive gas masses, dynamical masses, and far-infrared luminosities, and show that the QSOs in our sample have similar properties compared to less luminous QSOs and SMGs in the literature, despite the fact that their black hole masses (which are proportional to L AGN) are 1–2 orders of magnitude larger. We discuss two interpretations of these observations: this is due to selection effects, such as preferential face-on viewing angles and picking out objects in the tail ends of the scatter in host-galaxy mass and black hole mass relationships; or the black hole masses have been overestimated because the accretion rates are super-Eddington. [ABSTRACT FROM AUTHOR]

We present the VIMOS Spectroscopic Survey of a Supercluster in the COSMOS field (VIS3COS) at z ∼ 0.84. We use VIMOS high-resolution spectra (GG475 filter) to spectroscopically select 490 galaxies in and around the superstructure and an additional 481 galaxies in the line of sight. We present the redshift distribution, the catalogue to be made public, and the first results on the properties of individual galaxies and stacked spectra (3500 Å < λ <  4200 Å rest-frame). We probe a wide range of densities and environments (from low-density field to clusters and rich groups). We find a decrease in the median star formation rate from low- to high-density environments in all bins of stellar mass and a sharp rise of the quenched fraction (from ∼10% to ∼40 − 60%) of intermediate-stellar-mass galaxies (10 <  log10 (M⋆/M⊙) <  10.75) from filaments to clusters. The quenched fraction for massive galaxies shows little dependence on environment, being constant at ∼30 − 40%. We find a break in the strength of the [O II] emission, with nearly constant line equivalent widths at lower densities (∼ − 11 Å) and then a drop to ∼ − 2.5 Å towards higher densities. The break in the [OII] line strength happens at similar densities (log10(1 + δ) ∼ 0.0 − 0.5) as the observed rise in the quenched fraction. Our results may provide further clues regarding the different environmental processes affecting galaxies with different stellar masses and highlight the advantages of a single dataset in the COSMOS field probing a wide range of stellar masses and environments. We hypothesise that quenching mechanisms are enhanced in high-density regions. [ABSTRACT FROM AUTHOR]

Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [O  iii ] |$88\,\mu \mathrm{ m}$| line from galaxies at z ∼ 7−9. We use a cosmological simulation of galaxy formation to study the physical properties of [O  iii ] |$88\,\mu \mathrm{ m}$| emitters. In a comoving volume of 50  h −1 Mpc on a side, we locate 34 galaxies with stellar masses greater than |$10^8\ \rm M_{\odot }$| at z = 9, and more than 270 such galaxies at z = 7. We calculate the [O  iii ] |$88\,\mu \mathrm{ m}$| luminosities (⁠|$L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$|⁠) by combining a physical model of H  ii regions with emission line calculations using the photoionization code cloudy. We show that the resulting |$L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$|⁠, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7–9. Bright [O  iii ] emitters with |$L_{{\rm O\,{{\rm {\small{III}}}, 88}}}\gt 10^8\, \rm L_{\odot }$| have star formation rates higher than |$3\,\rm M_{\odot }\,{\rm yr}^{-1}$|⁠, and the typical metallicity is |${\sim } 0.1\, \rm Z_{\odot }$|⁠. The galaxies are hosted by dark matter haloes with masses greater than |$10^{11}\, \rm M_{\odot }$|⁠. We propose to use the [O  iii ] 5007 Å line, to be detected by James Webb Space Telescope, to study the properties of galaxies whose [O  iii ] |$88\,\mu \mathrm{ m}$| line emission has been already detected with ALMA. [ABSTRACT FROM AUTHOR]

Summary: Context: The current Endocrine Society Guideline suggests that patients aged <35 years with marked primary aldosteronism (PA) and unilateral adrenal lesions on adrenal computed tomography (CT) scan may not need adrenal vein sampling (AVS) before proceeding to unilateral adrenalectomy. This suggestion is, however, based on the data from only one report in the literature. Objective: We sought to determine the accuracy of CT findings in young PA patients who had unilateral adrenal disease on CT with hypokalaemia and elevation of aldosterone. Design and patients: We retrospectively studied 358 PA patients (n = 30, aged <35 years; n = 39, aged 35‐40 years; n = 289, aged ≥40 years) with hypokalaemia and elevation of aldosterone and unilateral disease on CT who had successful AVS. Main outcome measure: Accuracy of CT findings is determined by AVS findings and/or surgical outcomes in patients aged <35 years. Results: Concordance of the diagnosis between CT and AVS was 90% (27/30) in patients aged <35 years, 79% (31/39) in patients aged 35‐40 years and 69% (198/289) in those aged ≥40 years (trend for P < .01). Surgical benefit was confirmed in three patients aged <35 years and in three patients aged 35‐40 years with the available surgical data who had discordance between CT and AVS findings. Collectively, the diagnostic accuracy of CT findings was 100% (30/30) if aged <35 years and 87% (34/39) if aged 35‐40 years. Conclusion: Primary aldosteronism patients aged <35 years with hypokalaemia and elevation of aldosterone and unilateral disease on adrenal CT could be spared AVS. [ABSTRACT FROM AUTHOR]

Objective Although corticotropin is a representative secretagogue of aldosterone, the utility of the cosyntropin stimulation test (C- ST) in diagnosing primary aldosteronism ( PA) has not been elucidated. Aim of the study was to evaluate the clinical utility of C- ST for confirmatory testing and subtype classification of PA. Design, Setting and Patients In this retrospective study, we identified patients with hypertension and positive case-detection results for PA who underwent C- ST and saline infusion testing ( SIT) between 2006 and 2013 at eight referral centres in Japan. PA and essential hypertension ( EH) were distinguished based on SIT results. PA subtype classification was determined by adrenal venous sampling ( AVS). Plasma aldosterone concentration ( PAC) was measured before and 30 and 60 min after intravenous cosyntropin administration. The ability of C- ST to distinguish PA from EH and to distinguish unilateral from bilateral disease was assessed by the area under the receiver operating characteristic curve. Results Of 205 patients with hypertension and positive case-detection results, 139 (68%) had PA based on SIT results. Eighteen patients in whom AVS was unsuccessful were excluded from analysis. The baseline PAC before C- ST was significantly higher ( P < 0·01) in patients with PA than in those with EH. However, the degree of difference in PAC between patients with PA and EH was not enhanced by the administration of cosyntropin. In addition, the administration of cosyntropin did not improve the distinction between bilateral and unilateral PA subtypes. Conclusions C- ST has no utility as a confirmatory and subtype testing of PA when the diagnosis of PA is based on the positive results in SIT. [ABSTRACT FROM AUTHOR]

Context In adrenal vein sampling (AVS) for patients with primary aldosteronism, the contralateral ratio of aldosterone/cortisol (A/C) between the nondominant adrenal vein and the inferior vena cava is one of the best criteria for determining lateralized aldosterone secretion. Despite successful cannulation in some patients, the A/C ratios in the adrenal veins are bilaterally lower than that in the inferior vena cava (bilateral aldosterone suppression; BAS). Objectives To investigate the prevalence of BAS in AVS and how to resolve this condition. Design and setting Retrospective study involving nine referral centres. Patients Four hundred and ninety-one patients who were confirmed as having primary aldosteronism and had an AVS between January 2006 and December 2013. Measurements The prevalence of BAS before and after ACTH stimulation was compared. In addition, we investigated other methods for overcoming BAS. Results In 304 patients with successful AVS before ACTH stimulation, BAS was observed in 29 (9·5%). BAS was resolved after ACTH stimulation in 22 patients. In 276 patients with successful AVS both before and after ACTH stimulation, the frequency of BAS was significantly reduced after ACTH (8·7% vs 2·5%, P < 0·01). In a few patients, BAS was also resolved by adding a sampling point at the common trunk of the left adrenal vein and by an alternative drainage vein from the adrenal tumour. Conclusions BAS sometimes occurs in AVS without ACTH stimulation. ACTH stimulation significantly reduces BAS with a single AVS procedure. [ABSTRACT FROM AUTHOR]

Context Although adrenal vein sampling (AVS) is the standard method for subtype diagnosis in primary aldosteronism (PA), protocol details including the sampling position in the adrenal vein are not standardized. Objective To establish the optimum sampling position in the left adrenal vein based on postoperative outcome in PA patients. Design and Setting Retrospective study in nine referral centres. Participants Of 496 consecutive PA patients who underwent AVS between 2006 and 2013, 217 with successful AVS under cosyntropin stimulation, and with concomitant data from two positions: proximal (common trunk) and distal (central vein) to the junction with the inferior phrenic vein, were included. Main outcome measures Discordant rate of subtype diagnosis between common trunk and central vein, and postoperative outcomes in patients with discordant results. Results Subtype diagnosis using common trunk and central vein was discordant in 10 (4.6%) of the 217 patients (κ = 0.87, P < 0.05). Of these 10 patients, eight with left unilateral subtype and two with bilateral subtype using common trunk data showed bilateral subtype and unilateral subtype, respectively, using central vein data. Five patients with left unilateral subtype and one with bilateral subtype by common trunk data underwent unilateral adrenalectomy. All six patients were cured of PA after adrenalectomy, resulting in false-negative rates of 17% (1/ 6) by common trunk data, and 83% (5/6) by central vein data. Conclusion In view of its better potential diagnostic accuracy, technical ease, lower cost and lower risk of vein rupture, blood sampling from the common trunk of the left adrenal vein may be preferable as the standard method of AVS in patients with PA, although additional studies in a larger number of cases are required. [ABSTRACT FROM AUTHOR]

Objectives Adrenal vein sampling ( AVS) is the standard criterion for the subtype diagnosis in primary aldosteronism ( PA). Although lateralized index ( LI) ≥4 after cosyntropin stimulation is the commonly recommended cut-off for unilateral aldosterone hypersecretion, many of the referral centres in the world use LI cut-off of <4 without sufficient evidence for its diagnostic accuracy. Aim The aim of the study was to establish the diagnostic significance of contralateral ( CL) aldosterone suppression for the subtype diagnosis in patients with LI <4 in AVS. Design and patients A retrospective multicentre study was conducted in Japan. Of 124 PA patients subjected to unilateral adrenalectomy after successful AVS with cosyntropin administration, 29 patients with LI < 4 were included in the study. The patients were divided into Group A with CL suppression ( n = 16) and Group B ( n = 13) without CL suppression. Three outcome indices were assessed after 6 months postoperatively: normalization/significant improvement of hypertension, normalization of the aldosterone to renin ratio ( ARR) and normalization of hypokalaemia. Results The normalization/significant improvement of hypertension was 81% in Group A and 54% in Group B ( P = 0·2). The normalization of ARR was 100% in Group A and 46% in Group B ( P = 0·004). Hypokalaemia was normalized in all patients of both groups. The overall cure rate of PA based on meeting all the three criteria was 81% in Group A and 31% in Group B ( P = 0·01). Conclusions In patients with PA, where the LI is <4 on AVS, CL suppression of aldosterone is an accurate predictor of a unilateral source of aldosterone excess. CL suppression data should be interpreted in conjunction with computed tomographic adrenal imaging findings to guide surgical management. [ABSTRACT FROM AUTHOR]

We exploit wide-field Ly α imaging with Subaru to probe the environment around TN J1338−1942, a powerful radio galaxy with a > 100 kpc Ly α halo at z = 4.11. We used a sample of Ly α emitters (LAEs) down to log (LLyα[ erg s−1]) ∼ 42.8 to measure the galaxy density around TN J1338−1942, compared to a control sample from a blank field taken with the same instrument. We found that TN J1338−1942 resides in a region with a peak overdensity of δLAE = 2.8 ± 0.5 on scales of 8 h− 1 Mpc (on the sky) and 112 h− 1 Mpc (line of sight) in comoving coordinates. Adjacent to this overdensity, we found a strong underdensity where virtually no LAEs are detected. We used a semi-analytical model of LAEs derived from the Millennium Simulation to compare our results with theoretical predictions. While the theoretical density distribution is consistent with the blank field, overdense regions such as that around TN J1338−1942 are very rare, with a number density of 6.4 × 10− 8 Mpc− 3 (comoving), corresponding to the densest <0.4 percentile at z ≃ 4.1. We also found that the Ly α luminosity function in the TN J1338−1942 field differs from that in the blank field: the number of bright LAEs (log (LLyα[ erg s− 1]) ≳ 43.3) is enhanced, while the number of fainter LAEs is relatively suppressed. These results suggest that some powerful radio galaxies associated with Ly α nebulae reside in extreme overdensities on ∼3–6 Mpc scales, where star formation and AGN activity may be enhanced via frequent galaxy mergers or high rates of gas accretion from the surroundings. [ABSTRACT FROM AUTHOR]

The intergalactic medium (IGM) is the dominant reservoir of baryons, delineates the large-scale structure of the universe at low to moderate overdensities, and provides gas from which galaxies form and evolve. Simulations of a cold-dark-matter- (CDM-) dominated universe predict that the IGM is distributed in a cosmic web of filaments and that galaxies should form along and at the intersections of these filaments. While observations of QSO absorption lines and the large-scale distribution of galaxies have confirmed the CDM paradigm, the cosmic web of IGM has never been confirmed by direct imaging. Here we report our observation of the Lyα blob 2 (LAB2) in SSA22 with the Cosmic Web Imager (CWI). This is an integral field spectrograph optimized for low surface brightness, extended emission. With 22 hr of total on- and off-source exposure, CWI has revealed that LAB2 has extended Lyα emission that is organized into azimuthal zones consistent with filaments. We perform numerous tests with simulations and the data to secure the robustness of this result, which relies on data with modest signal-to-noise ratios. We have developed a smoothing algorithm that permits visualization of data cube slices along image or spectral image planes. With both raw and smoothed data cubes we demonstrate that the filaments are kinematically associated with LAB2 and display double-peaked profiles characteristic of optically thick Lyα emission. The flux is 10-20 times brighter than expected for the average emission from the IGM but is consistent with boosted fluorescence from a buried QSO or gravitation cooling radiation. Using simple emission models, we infer a baryon mass in the filaments of at least 1-4 × 1011M☼, and the dark halo mass is at least 2 × 1012M☼. The spatial-kinematic morphology is more consistent with inflow from the cosmic web than outflow from LAB2, although an outflow feature maybe present at one azimuth. LAB2 and the surrounding gas have significant and coaligned angular momentum, strengthening the case for their association. [ABSTRACT FROM AUTHOR]

This paper presents new deep and wide narrow-band surveys undertaken with United Kingdom Infrared Telescope (UKIRT), Subaru and the Very Large Telescope (VLT), a unique combined effort to select large, robust samples of Hα star-forming galaxies at z = 0.40, 0.84, 1.47 and 2.23 (corresponding to look-back times of 4.2, 7.0, 9.2 and 10.6 Gyr) in a uniform manner over ∼2 deg2 in the Cosmological Evolution Survey and Ultra Deep Survey fields. The deep multi-epoch Hα surveys reach a matched 3σ flux limit of ≈3 M⊙ yr−1 out to z = 2.2 for the first time, while the wide area and the coverage over two independent fields allow us to greatly overcome cosmic variance and assemble by far the largest samples of Hα emitters. Catalogues are presented for a total of 1742, 637, 515 and 807 Hα emitters, robustly selected at z = 0.40, 0.84, 1.47 and 2.23, respectively, and used to determine the Hα luminosity function and its evolution. The faint-end slope of the Hα luminosity function is found to be α = −1.60 ± 0.08 over z = 0–2.23, showing no significant evolution. The characteristic luminosity of star-forming galaxies, L*Hα, evolves significantly as log L*Hα(z) = 0.45z + log L*z = 0. This is the first time Hα has been used to trace star formation activity with a single homogeneous survey at z = 0.4–2.23. Overall, the evolution seen with Hα is in good agreement with the evolution seen using inhomogeneous compilations of other tracers of star formation, such as far-infrared and ultraviolet, jointly pointing towards the bulk of the evolution in the last 11 Gyr being driven by a statistically similar star-forming population across cosmic time, but with a strong luminosity increase from z ∼ 0 to ∼2.2. Our uniform analysis allows us to derive the Hα star formation history (SFRH) of the Universe, showing a clear rise up to z ∼ 2.2, for which the simple parametrization log10ρSFR = −2.1(1 + z)−1 is valid over 80 per cent of the age of the Universe. The results reveal that both the shape and normalization of the Hα SFRH are consistent with the measurements of the stellar mass density growth, confirming that our Hα SFRH is tracing the bulk of the formation of stars in the Universe for z < 2.23. The star formation activity over the last ∼11 Gyr is responsible for producing ∼95 per cent of the total stellar mass density observed locally, with half of that being assembled in 2 Gyr between z = 1.2 and 2.2, and the other half in 8 Gyr (since z < 1.2). If the star formation rate density continues to decline with time in the same way as seen in the past ∼11 Gyr, then the stellar mass density of the Universe will reach a maximum which is only 5 per cent higher than the present-day value. [ABSTRACT FROM PUBLISHER]

A 77-year-old man developed pulmonary tumor thrombotic microangiopathy (PTTM) 2 days after undergoing transurethral resection for urothelial carcinoma (G3) of the urinary bladder and died of respiratory failure 6 days later. Histological findings demonstrated marked intimal fibrocellular proliferation, fibrin thrombi, and both cancer cells and fibrin thrombi in the arteries of the lungs, findings consistent with PTTM. Prominent stenosis in arteries smaller than 300 μm was also seen. The Ki-67 labeling index of primary and metastasized cancer cells was 62.4 % and 70.2 %, respectively. The membranes of metastasized cancer cells expressed E-cadherin, similar to membranes in the urinary bladder. An aggressive PTTM course is affected by intimal fibrocellular proliferation and the high cell proliferation of cancer cells. Furthermore, prominent stenosis in small arteries and membranous staining of E-cadherin of metastasized cells suggest that cancer cells formed clusters by maintaining adhesion molecules and migrated into the arteries of the lungs, where they easily caused damage to the endothelium of small arteries, in contrast to dispersed cancer cells. [ABSTRACT FROM AUTHOR]

ABSTRACT This paper presents the results from the first wide and deep dual narrow-band survey to select Hα and [O ii] line emitters at z= 1.47 ± 0.02, exploiting synergies between the United Kingdom Infrared Telescope and the Subaru telescope by using matched narrow-band filters in the H and z′ bands. The Hα survey at z= 1.47 reaches a 3σ flux limit of FHα≈ 7 × 10−17 erg s−1 cm−2 (corresponding to a limiting star formation rate (SFR) in Hα of ≈7 M⊙ yr−1) and detects ≈200 Hα emitters over 0.7 deg2, while the much deeper [O ii] survey reaches an effective flux of ≈7 × 10−18 erg s−1 cm−2 (SFR in [O ii] of ∼1 M⊙ yr−1), detecting ≈1400 z= 1.47 [O ii] emitters in a matched comoving volume of ∼2.5 × 105 Mpc3. The combined survey results in the identification of 190 simultaneous Hα and [O ii] emitters at z= 1.47. Hα and [O ii] luminosity functions are derived and both are shown to evolve significantly from z∼ 0 in a consistent way. The SFR density of the Universe at z= 1.47 is evaluated, with the Hα analysis yielding ρSFR= 0.16 ± 0.05 M⊙ yr−1 Mpc−3 and the [O ii] analysis ρSFR= 0.17 ± 0.04 M⊙ yr−1 Mpc−3. The measurements are combined with other studies, providing a self-consistent measurement of the star formation history of the Universe over the last ∼11 Gyr. By using a large comparison sample at z∼ 0.1, derived from the Sloan Digital Sky Survey (SDSS), [O ii]/Hα line ratios are calibrated as probes of dust extinction. Hα emitters at z∼ 1.47 show on average AHα≈ 1 mag, the same as found by SDSS in the local Universe. It is shown that although dust extinction correlates with SFR, the relation evolves by about ∼0.5 mag from z∼ 1.5 to ∼0, with local relations overpredicting the dust extinction corrections at high z by that amount. Stellar mass is found to be a much more fundamental extinction predictor, with the same relation between mass and dust extinction being valid at both z∼ 0 and ∼1.5, at least for low and moderate stellar masses. The evolution in the extinction-SFR relation is therefore interpreted as being due to the evolution in median specific SFRs over cosmic time. Dust extinction corrections as a function of optical colours are also derived and shown to be broadly valid at both z∼ 0 and ∼1.5, offering simpler mechanisms for estimating extinction in moderately star-forming systems over the last ∼9 Gyr. [ABSTRACT FROM AUTHOR]

In order to constrain the bolometric luminosities, dust properties, and molecular gas content of giant Lyα nebulae, the so-called Lyα blobs, we have carried out a study of dust continuum and CO line emission in two well-studied representatives of this population at z ~ 3: an Lyα blob discovered by its strong Spitzer Multiband Infrared Photometer 24 µm detection (LABd05) and the Steidel blob 1 (SSA22-LAB01). We find that the spectral energy distribution of LABd05 is well described by an active-galactic-nucleus--starburst composite template with LFIR = (4.0 ± 0.5) x 1012 L⊙, comparable to high-z submillimeter galaxies and ultraluminous infrared galaxies. New Large APEX Bolometer Camera 870 µm measurements rule out the reported Submillimeter Common-User Bolometer Array detection of the SSA22-LAB01 (S850 µm = 16.8 mJy) at the >4σ level. Consistent with this, ultradeep Plateau de Bure Interferometer observations with ~2" spatial resolution also fail to detect any 1.2 mm continuum source down to ≈0.45 mJy beam-1 (3σ). Combined with the existing (sub)millimeter observations in the literature, we conclude that the FIR luminosity of SSA22-LAB01 remains uncertain. No CO line is detected in either case down to integrated flux limits of SvΔV ≲ 0.25-1.0 Jy km s-1, indicating a modest molecular gas reservoir, M(H2) < (1-3) x 1010 M⊙. The non-detections exclude, with high significance (12σ), the previous tentative detection of a CO J = 4-3 line in the SSA22-LAB01. The increased sensitivity afforded by the Atacama Large Millimeter/submillimeter Array will be critical in studying molecular gas and dust in these interesting systems. [ABSTRACT FROM AUTHOR]

We present Keck spectroscopic observations of z > 6 Lyman-break galaxy (LBG) candidates in the Subaru Deep Field (SDF). The candidates were selected as i'-dropout objects down to z' = 27 AB magnitudes from an ultra-deep SDF z'-band image. With the Keck spectroscopy we identified 19 LBGs with prominent Lyα emission lines at 6 ≤ z ≤ 6.4. The median value of the Lyα rest-frame equivalent widths (EWs) is ~50Å, with four EWs > 100 Å. This well-defined spectroscopic sample spans a UV-continuum luminosity range of -21.8 ≤ MUV ≤ -19.5 (0.6 ~ 5 L*UV) and a Lyα luminosity range of (0.3-3) x 1043 erg s-1 (0.3-3 L*Lyα). We derive the UV and Lyα luminosity functions (LFs) from our sample at (z) ~ 6.2 after we correct for sample incompleteness. We find that our measurement of the UV LF is consistent with the results of previous studies based on photometric LBG samples at 5 < z < 7. Our Lyα, LF is also generally in agreement with the results of Lyα-emitter surveys at z ~ 5.7 and 6.6. This study shows that deep spectroscopic observations of LBGs can provide unique constraints on both the UV and Lyα LFs at z > 6. [ABSTRACT FROM AUTHOR]

We carried out extended spectroscopic confirmations of Lyα emitters (LAEs) at z = 6.5 and 5.7 in the Subaru Deep Field. Now, the total number of spectroscopically confirmed LAEs is 45 and 54 at z = 6.5 and 5.7, respectively, and at least 81% (70%) of our photometric candidates at z = 6.5 (5.7) have been spectroscopically identified as real LAEs. We made careful measurements of the Lyα luminosity, both photometrically and spectroscopically, to accurately determine the Lyα and rest-UV luminosity functions (LFs). The substantially improved evaluation of the Lyα LF at z 6.5 shows an apparent deficit from z 5.7 at least at the bright end, and a possible decline even at the faint end, though small uncertainties remain. The rest-UV LFs at z = 6.5 and 5.7 are in good agreement, at least at the bright end, in clear contrast to the differences seen in the Lyα LF. These results imply an increase in the neutral fraction of the intergalactic medium from z = 5.7 to 6.5. The rest-frame equivalent width (EW0) distribution at z = 6.5 seems to be systematically smaller than z = 5.7, and it shows an extended tail toward larger EW0. The bright end of the rest-UV LF can be reproduced from the observed Lyα LF and a reasonable EW0-UV luminosity relation. Integrating this rest-UV LF provides the first measurement of the contribution of LAEs to the photon budget required for reionization. The derived UV LF suggests that the fractional contribution of LAEs to the photon budget among Lyman break galaxies significantly increases toward faint magnitudes. Low-luminosity LAEs could dominate the ionizing photon budget, though this inference depends strongly on the uncertain faint-end slope of the Lyα LF. [ABSTRACT FROM AUTHOR]

The article focuses on the study that explores the relationship between dynamic balance and standard leg extension strength, right and left leg differences and gender of healthy elderly people in Japan. The right and left leg differences were revealed in the leg extension strengths of females that shows significant link with knee extension strength. The study suggests that leg extension strength is strongly correlated with dynamic balance than the knee extension strength.

We present the environmental properties of a sample of 260 Lyα emitters (LAEs) with extremely large equivalent widths (EW0 > 240 Å) at z ∼ 3. Such large EW LAEs may be very low-metal / young starbursts in void regions or Hi gas /galaxies illuminated by ionizing radiation from the QSO. We undertook Subaru/HSC Lyα imaging observations around a hyper luminous QSO at z = 2.84. We identified 3490 LAEs including 260 large EW LAEs. We found that the large EW LAEs tend to lie at galaxy over-dense regions surrounding the QSO, suggesting that most of the large EW LAEs are illuminated by the QSO. From the radial distribution of the large EW LAEs from the QSO, we found that the fraction of large EW LAE shows two excesses in the range of 2 to 5 Mpc and 14 to 16 Mpc from the QSO. If the two peaks are reflected with the QSO activity, the QSO should have episodic lifetimes with ∼10 Myr duration and ∼30 Myr separations. However, we require future spectroscopic observations to investigate if the large EW LAEs far from the QSO are low-metal young starbursts. [ABSTRACT FROM AUTHOR]

We present the environmental properties of a sample of 260 Lyα emitters (LAEs) with extremely large equivalent widths (EW0 > 240 Å) at z ∼ 3. Such large EW LAEs may be very low-metal / young starbursts in void regions or Hi gas /galaxies illuminated by ionizing radiation from the QSO. We undertook Subaru/HSC Lyα imaging observations around a hyper luminous QSO at z = 2.84. We identified 3490 LAEs including 260 large EW LAEs. We found that the large EW LAEs tend to lie at galaxy over-dense regions surrounding the QSO, suggesting that most of the large EW LAEs are illuminated by the QSO. From the radial distribution of the large EW LAEs from the QSO, we found that the fraction of large EW LAE shows two excesses in the range of 2 to 5 Mpc and 14 to 16 Mpc from the QSO. If the two peaks are reflected with the QSO activity, the QSO should have episodic lifetimes with ∼10 Myr duration and ∼30 Myr separations. However, we require future spectroscopic observations to investigate if the large EW LAEs far from the QSO are low-metal young starbursts. [ABSTRACT FROM AUTHOR]

Study objective – The aim was to clarify the effects of endothelin on coronary vasculature in the intact rabbit by coronary angiographic examination.Design – By selective coronary angiography bolus injections of various amounts of endothelin (0.01-1 nmol) were given into the right coronary artery of anaesthetised rabbits. The preventive effects of nifedipine on endothelin induced myocardial ischaemia were examined.Subjects – Adult male Japanese white rabbits (2.7-3.5 kg, n=29) were used for in vivo and in vitro studies.Measurements and main results – Intracoronary administration of 0.1 nmol endothelin led to the delayed filling of contrast medium into the distal coronary artery and the sustained retention of contrast medium in both large and small coronary arteries, associated with distinct ST elevation in leads II, III and aVF on the electrocardiogram. However, endothelin produced no evident constriction at any site in the large epicardial coronary arteries. Intracoronary administration of glyceryl trinitrate (50 μg) or nifedipine (5 μg) failed to reverse myocardial ischaemic changes induced by endothelin. Pretreatment with intravenous administration of nifedipine (3 μg·kg−1) partially inhibited the endothelin induced vasoconstrictor effect on small coronary arteries and subsequent ischaemic changes. In isolated coronary arterial preparation, endothelin produced long lasting contraction in a dose dependent manner [ED50=3.7 (SEM 1.8) nM]. Pretreatment with nifedipine inhibited the maximum contraction induced by endothelin, but did not affect the threshold dose or the half maximal effective dose (ED50). Endothelin (0.1 μM) per se did not produce aggregatory responses of rabbit platelets.Conclusions – Endothelin induced myocardial ischaemia cannot be ascribed to vasospastic constriction of large coronary arteries nor to platelet thrombi, but diffuse constriction of small coronary arteries occurs in the intact rabbit. [ABSTRACT FROM PUBLISHER]