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We present CO J=4-3 line and 3 mm dust continuum observations of a 100kpc-scale filamentary Ly{\alpha} nebula (SSA22 LAB18) at z=3.1 using theAtacama Large Millimeter/submillimeter Array (ALMA). We detected the CO J=4-3line at a systemic z(CO)=3.093 {\pm} 0.001 at 11 {\sigma} from one of the ALMAcontinuum sources associated with the Ly{\alpha} filament. We estimated the COJ=4-3 luminosity of L'CO(4-3)=(2.3\pm0.2)x10^9 K km s^{-1} pc^2 for this COsource, which is one order of magnitude smaller than those of typical z>1 dustystar-forming galaxies (DSFGs) of similar far-infrared luminosity L(IR)~10^{12}Lsun. We derived a molecular gas mass of Mgas=(4.4^{+0.9}_{-0.6})x10^9 Msun anda star-formation rate of SFR=270\pm160 Msun yr^{-1}. We also estimated a gasdepletion time of {\tau}(dep)=17\pm10 Myr, being shorter than those of typicalDSFGs. It is suggested that this source is in a transition phase from DSFG to agas-poor, early-type galaxy. From ALMA to Herschel multi-band dust continuumobservations, we measured a dust emissivity index {\beta}=2.3\pm0.2, which issimilar to those of local gas-poor, early-type galaxies. Such a high {\beta}can be reproduced by specific chemical compositions for interstellar dust atthe submillimeter wavelengths from recent laboratory experiments. ALMA CO andmulti-band dust continuum observations can constrain the evolutionary stage ofhigh-redshift galaxies through {\tau}(dep) and {\beta}, and thus we caninvestigate dust chemical compositions even in the early Universe.

We present CO J=4-3 line and 3 mm dust continuum observations of a 100kpc-scale filamentary Ly{\alpha} nebula (SSA22 LAB18) at z=3.1 using theAtacama Large Millimeter/submillimeter Array (ALMA). We detected the CO J=4-3line at a systemic z(CO)=3.093 {\pm} 0.001 at 11 {\sigma} from one of the ALMAcontinuum sources associated with the Ly{\alpha} filament. We estimated the COJ=4-3 luminosity of L'CO(4-3)=(2.3\pm0.2)x10^9 K km s^{-1} pc^2 for this COsource, which is one order of magnitude smaller than those of typical z>1 dustystar-forming galaxies (DSFGs) of similar far-infrared luminosity L(IR)~10^{12}Lsun. We derived a molecular gas mass of Mgas=(4.4^{+0.9}_{-0.6})x10^9 Msun anda star-formation rate of SFR=270\pm160 Msun yr^{-1}. We also estimated a gasdepletion time of {\tau}(dep)=17\pm10 Myr, being shorter than those of typicalDSFGs. It is suggested that this source is in a transition phase from DSFG to agas-poor, early-type galaxy. From ALMA to Herschel multi-band dust continuumobservations, we measured a dust emissivity index {\beta}=2.3\pm0.2, which issimilar to those of local gas-poor, early-type galaxies. Such a high {\beta}can be reproduced by specific chemical compositions for interstellar dust atthe submillimeter wavelengths from recent laboratory experiments. ALMA CO andmulti-band dust continuum observations can constrain the evolutionary stage ofhigh-redshift galaxies through {\tau}(dep) and {\beta}, and thus we caninvestigate dust chemical compositions even in the early Universe.

We have identified a very interesting Lyα emitter (LAE), whose Lyα emission line has an extremely large observed equivalent width of EW0 = 436+422 - 149 Å, which corresponds to an extraordinarily large intrinsic rest-frame equivalent width of EWint 0 = 872 +844 - 298 Å after the average intergalactic absorption correction. The object was spectroscopically confirmed to be a real LAE by its apparent asymmetric Lyα line profile detected at z = 6.538. The continuum emission of the object was definitely detected in our deep z′-band image; thus, its EW0 was reliably determined. Follow-up deep near-infrared spectroscopy revealed emission lines of neither He II λ1640 as an apparent signature of Population III (Pop III) nor C IV λ1549 as proof of an active nucleus. No detection of the short-lived He II λ1640 line is not necessarily inconsistent with the interpretation that the underlying stellar population of the object is dominated by Pop III. We found that the observed extremely large EW0 of the Lyα emission and the upper limit on the EW0 of the He II λ1640 emission can be explained by population synthesis models favoring a very young age less than 2-4 Myr and massive metal-poor (Z < 10 -5) or even metal-free stars. The observed large EW0 of Lyα is insufficiently explained by Population I/II synthesis models with Z ≥ 10 -3. However, we cannot conclusively rule out the possibility that this object is composed of a normal stellar population with a clumpy dust distribution, which could enhance the Lyα EW0, though its significance is still unclear. © 2012. The American Astronomical Society. All rights reserved..

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. © 2011. The American Astronomical Society. All rights reserved.

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]

We present the properties of Ly Alpha emitters (LAEs) at z = 5.7 in theSubaru Deep Field. A photometric sample of 89 LAE candidates is constructedfrom narrow-band (NB816) data down to NB816 = 26.0 (AB) in a continuous 725arcmin^2 area. Spectra of 39 objects satisfying the photometric selectioncriteria for LAEs were obtained with Subaru and Keck II Telescopes, among which28 were confirmed LAEs, one was a nearby galaxy, and eight were unclassified.We also obtained spectra of another 24 NB816-excess objects in the field,identifying six additional LAEs. We find that the Ly Alpha luminosity functionderived from the photometric sample is reproduced well by a Schechter functionwith L* = (7.9+3.0-2.2) x 10^42 erg/s and phi* = (6.3+3.0-2.0) x 10^-4 Mpc^-3for alpha = -1.5 (fixed) over the whole luminosity range of L ~= 3x10^42 -3x10^43 erg/s. We then measure rest-frame Ly Alpha equivalent widths (EWs) forthe confirmed LAEs, to find that the median among the 28 objects satisfying thephotometric selection criteria is W_0^i = 233 A. We infer that 30% - 40% ofLAEs at z=5.7 exceed W_0^i = 240 A. These large-EW objects probably cannot beaccounted for by ordinary star-forming populations with a Salpeter IMF. We alsofind that LAEs with fainter far-UV luminosities have larger EWs. Finally, wederive the far-UV luminosity function of LAEs down to M_UV ~= -19.6 using thephotometric sample, and compare it with that of Lyman-break galaxies (LBGs). Wefind that as high as about 80% of LBGs at z ~ 6 have W_0^i >= 100 A, in sharpcontrast to lower-z counterparts.

We present the properties of Ly Alpha emitters (LAEs) at z = 5.7 in theSubaru Deep Field. A photometric sample of 89 LAE candidates is constructedfrom narrow-band (NB816) data down to NB816 = 26.0 (AB) in a continuous 725arcmin^2 area. Spectra of 39 objects satisfying the photometric selectioncriteria for LAEs were obtained with Subaru and Keck II Telescopes, among which28 were confirmed LAEs, one was a nearby galaxy, and eight were unclassified.We also obtained spectra of another 24 NB816-excess objects in the field,identifying six additional LAEs. We find that the Ly Alpha luminosity functionderived from the photometric sample is reproduced well by a Schechter functionwith L* = (7.9+3.0-2.2) x 10^42 erg/s and phi* = (6.3+3.0-2.0) x 10^-4 Mpc^-3for alpha = -1.5 (fixed) over the whole luminosity range of L ~= 3x10^42 -3x10^43 erg/s. We then measure rest-frame Ly Alpha equivalent widths (EWs) forthe confirmed LAEs, to find that the median among the 28 objects satisfying thephotometric selection criteria is W_0^i = 233 A. We infer that 30% - 40% ofLAEs at z=5.7 exceed W_0^i = 240 A. These large-EW objects probably cannot beaccounted for by ordinary star-forming populations with a Salpeter IMF. We alsofind that LAEs with fainter far-UV luminosities have larger EWs. Finally, wederive the far-UV luminosity function of LAEs down to M_UV ~= -19.6 using thephotometric sample, and compare it with that of Lyman-break galaxies (LBGs). Wefind that as high as about 80% of LBGs at z ~ 6 have W_0^i >= 100 A, in sharpcontrast to lower-z counterparts.

We explored the clustering properties of Lyman break galaxies at z = 4 and 5 with an angular two-point correlation function on the basis of the very deep and wide Subaru Deep Field data. We confirmed the previous result that the clustering strength of LBGs depends on the UV luminosity in the sense that brighter LBGs are more strongly clustered. In addition, we found an apparent dependence of the correlation function slope on UV luminosity for LBGs at both z = 4 and 5. More luminous LBGs have a steeper correlation function. The bias parameter was found to be a scale-dependent function for bright LBGs, whereas it appears to be almost scale-independent for faint LBGs. Luminous LBGs have a higher bias at smaller angular scales, which decreases as the scale increases. To compare these observational results, we constructed numerical mock LBG catalogs based on a semianalytic model of hierarchical clustering combined with high-resolution N-body simulation, carefully mimicking the observational selection effects. The luminosity functions and the overall correlation functions for LBGs at z = 4 and 5 predicted by this mock catalog were found to be almost consistent with the observation. The observed dependence of the clustering on UV luminosity was not reproduced by the model, unless subsamples of distinct halo mass were considered. That is, LBGs belonging to more massive dark halos had steeper and larger amplitude correlation functions. With this model, we found that LBG multiplicity in massive dark halos amplifies the clustering strength at small scales, which steepens the correlation function. The hierarchical clustering model could therefore be reconciled with the observed luminosity dependence of the correlation function if there is a tight correlation between UV luminosity and halo mass. Our finding that the slope of the correlation function depends on luminosity could be an indication that massive dark halos hosted multiple bright LBGs. © 2006. The American Astronomical Society. All rights reserved.

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]

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]

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]

Lyman-α emitters are thought to be young, low-mass galaxies with ages of ~[10.sup.8] yr (refs 1, 2). An overdensity of them in one region of the sky (the SSA 22 [...]

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]