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We present a statistical study of the properties of diffuse H i in 10 nearby galaxies, comparing the H i detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H i with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse H i by subtracting the dense H i , which is obtained from the THINGS data with a uniform flux-density threshold, from the total H i detected by FAST. Among the sample, the median diffuse-H i fraction is 34%, and more diffuse H i is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse H i we detected seems to be distributed in disk-like layers within a typical thickness of 1 kpc, different from the more halo-like diffuse H i detected around NGC 4631 in a previous study. Most of the diffuse H i is cospatial with the dense H i and has a typical column density of 10 ^17.7 –10 ^20.1 cm ^−2 . The diffuse and dense H i exhibit a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circumgalactic medium properties and assuming pressure equilibrium, the volume density of diffuse H i appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse H i , and gas accretion.

This paper presents a newly established sample of 103 unique galaxies or galaxy groups at 0.4 ≲ z ≲ 0.7 from the Cosmic Ultraviolet Baryon Survey (CUBS) for studying the warm-hot circumgalactic medium (CGM) probed by both O vi and Ne viii absorption. The galaxies and associated neighbors are identified at 40 km s ^−1 for galaxies of $\mathrm{log}{M}_{\mathrm{star}}/{M}_{\odot }\gt 9$ within the virial radius, suggesting a more dynamic warm-hot halo around these galaxies. Finally, the warm-hot CGM probed by O vi and Ne viii is suggested to be the dominant phase in sub- L * galaxies with $\mathrm{log}{M}_{\mathrm{star}}/{M}_{\odot }\approx 9\mbox{--}10$ based on their high ionization fractions in the CGM.

We report the discovery of large, ionized, [O ii ]-emitting circumgalactic nebulae around the majority of 30 UV-luminous quasars at z = 0.4–1.4 observed with deep, wide-field integral field spectroscopy with the Multi-Unit Spectroscopy Explorer (MUSE) by the Cosmic Ultraviolet Baryon Survey and MUSE Quasar Blind Emitters Survey. Among the 30 quasars, seven (23%) exhibit [O ii ]-emitting nebulae with major axis sizes greater than 100 kpc, 20 greater than 50 kpc (67%), and 27 (90%) greater than 20 kpc. Such large, optically emitting nebulae indicate that cool, dense, and metal-enriched circumgalactic gas is common in the halos of luminous quasars at intermediate redshift. Several of the largest nebulae exhibit morphologies that suggest interaction-related origins. We detect no correlation between the sizes and cosmological-dimming-corrected surface brightnesses of the nebulae and quasar redshift, luminosity, black hole mass, or radio-loudness, but find a tentative correlation between the nebulae and rest-frame [O ii ] equivalent width in the quasar spectra. This potential trend suggests a relationship between interstellar medium content and gas reservoirs on CGM scales. The [O ii ]-emitting nebulae around the z ≈ 1 quasars are smaller and less common than Ly α nebulae around z ≈ 3 quasars. These smaller sizes can be explained if the outer regions of the Ly α halos arise from scattering in more neutral gas, by evolution in the cool circumgalactic medium content of quasar-host halos, by lower-than-expected metallicities on ≳50 kpc scales around z ≈ 1 quasars, or by changes in quasar episodic lifetimes between z = 3 and 1.

We investigate the group-scale environment of 15 luminous quasars (luminosity L _3000 > 10 ^46 erg s ^−1 ) from the Cosmic Ultraviolet Baryon Survey (CUBS) at redshift z ≈ 1. Using the Multi Unit Spectroscopic Explorer integral field spectrograph on the Very Large Telescope, we conduct a deep galaxy redshift survey in the CUBS quasar fields to identify group members and measure the physical properties of individual galaxies and galaxy groups. We find that the CUBS quasars reside in diverse environments. The majority (11 out of 15) of the CUBS quasars reside in overdense environments with typical halo masses exceeding 10 ^13 M _⊙ , while the remaining quasars reside in moderate-size galaxy groups. No correlation is observed between overdensity and redshift, black hole (BH) mass, or luminosity. Radio-loud quasars (5 out of 15 CUBS quasars) are more likely to be in overdense environments than their radio-quiet counterparts in the sample, consistent with the mean trends from previous statistical observations and clustering analyses. Nonetheless, we also observe radio-loud quasars in moderate groups and radio-quiet quasars in overdense environments, indicating a large scatter in the connection between radio properties and environment. We find that the most UV luminous quasars might be outliers in the stellar mass-to-halo mass relations or may represent departures from the standard single-epoch BH relations.

Turbulent motions in the circumgalactic medium play a critical role in regulating the evolution of galaxies, yet their detailed characterization remains elusive. Using two-dimensional velocity maps constructed from spatially extended [O ii ] and [O iii ] emission, Chen et al. measured the velocity structure functions (VSFs) of four quasar nebulae at z ≈ 0.5–1.1. One of these exhibits a spectacular Kolmogorov relation. Here, we carry out an ensemble study using an expanded sample incorporating four new nebulae from three additional quasi-stellar object (QSO) fields. The VSFs measured for all eight nebulae are best explained by subsonic turbulence revealed by the line-emitting gas, which in turn strongly suggests that the cool gas ( T ∼ 10 ^4 K) is dynamically coupled to the hot ambient medium. Previous work demonstrates that the largest nebulae in our sample reside in group environments with clear signs of tidal interactions, suggesting that environmental effects are vital in seeding and enhancing the turbulence within the gaseous halos, ultimately promoting the formation of the extended nebulae. No discernible differences are observed in the VSF properties between radio-loud and radio-quiet QSO fields. We estimate the turbulent heating rate per unit volume, Q _turb , in the QSO nebulae to be ∼10 ^−26 –10 ^−22 erg cm ^−3 s ^−1 for the cool phase and ∼10 ^−28 –10 ^−25 erg cm ^−3 s ^−1 for the hot phase. This range aligns with measurements in the intracluster medium and star-forming molecular clouds but is ∼10 ^3 times higher than the Q _turb observed inside cool gas clumps on scales ≲1 kpc using absorption-line techniques. We discuss the prospect of bridging the gap between emission and absorption studies by pushing the emission-based VSF measurements to below ≈10 kpc.

Quasar-driven galactic outflows are a major driver of the evolution of massive galaxies. We report observations of a powerful galactic-scale outflow in a z = 3 extremely red and intrinsically luminous ( L _bol ≃ 5 × 10 ^47 erg s ^−1 ) quasar SDSSJ1652 + 1728 with the Near-infrared Spectrograph on board JWST. We analyze the kinematics of rest-frame optical emission lines and identify the quasar-driven outflow extending out to ∼10 kpc from the quasar with a velocity offset of ( v _r = ± 500 km s ^−1 ) and high velocity dispersion (FWHM = 700–2400 km s ^−1 ). Due to JWST’s unprecedented surface brightness sensitivity in the near-infrared, we unambiguously show that the powerful high velocity outflow in an extremely red quasar encompasses a large swath of the host galaxy’s interstellar medium. Using the kinematics and dynamics of optical emission lines, we estimate the mass outflow rate—in the warm ionized phase alone—to be at least 2300 ± 1400 M _⊙ yr ^−1 . We measure a momentum flux ratio between the outflow and the quasar accretion disk of ∼1 on a kpc scale, indicating that the outflow was likely driven in a relatively high (>10 ^23 cm ^−2 ) column density environment through radiation pressure on dust grains. We find a coupling efficiency between the bolometric luminosity of the quasar and the outflow of 0.1%, matching the theoretical prediction of the minimum coupling efficiency necessary for negative quasar feedback. The outflow has sufficient energetics to drive the observed turbulence seen in shocked regions of the quasar host galaxy, which are likely directly responsible for prolonging the time that it takes for gas to cool efficiently.

The launch of JWST opens a new window for studying the connection between metal-line absorbers and galaxies at the end of the Epoch of Reionization. Previous studies have detected absorber–galaxy pairs in limited quantities through ground-based observations. To enhance our understanding of the relationship between absorbers and their host galaxies at z > 5, we utilized the NIRCam wide-field slitless spectroscopy to search for absorber-associated galaxies by detecting their rest-frame optical emission lines (e.g., [O III ] + H β ). We report the discovery of a Mg ii -associated galaxy at z = 5.428 using data from the JWST ASPIRE program. The Mg ii absorber is detected on the spectrum of quasar J0305–3150 with a rest-frame equivalent width of 0.74 Å. The associated galaxy has an [O III ] luminosity of 10 ^42.5 erg s ^−1 with an impact parameter of 24.9 pkpc. The joint Hubble Space Telescope–JWST spectral energy distribution (SED) implies a stellar mass and star formation rate of M _* ≈ 10 ^8.8 M _⊙ , star-formation rate ≈ 10 M _⊙ yr ^−1 . Its [O III ] equivalent width and stellar mass are typical of [O III ] emitters at this redshift. Furthermore, connecting the outflow starting time to the SED-derived stellar age, the outflow velocity of this galaxy is ∼300 km s ^−1 , consistent with theoretical expectations. We identified six additional [O III ] emitters with impact parameters of up to ∼300 pkpc at similar redshifts (∣ dv ∣ < 1000 km s ^−1 ). The observed number is consistent with that in cosmological simulations. This pilot study suggests that systematically investigating the absorber–galaxy connection within the ASPIRE program will provide insights into the metal-enrichment history in the early Universe.

This paper reports the first measurement of the relationship between turbulent velocity and cloud size in the diffuse circumgalactic medium (CGM) in typical galaxy halos at redshift z ≈ 0.4–1. Through spectrally resolved absorption profiles of a suite of ionic transitions paired with careful ionization analyses of individual components, cool clumps of size as small as l _cl ∼ 1 pc and density lower than n _H = 10 ^−3 cm ^−3 are identified in galaxy halos. In addition, comparing the line widths between different elements for kinematically matched components provides robust empirical constraints on the thermal temperature T and the nonthermal motions b _NT , independent of the ionization models. On average, b _NT is found to increase with l _cl following ${b}_{\mathrm{NT}}\propto {l}_{\mathrm{cl}}^{0.3}$ over three decades in spatial scale from l _cl ≈ 1 pc to l _cl ≈ 1 kpc. Attributing the observed b _NT to turbulent motions internal to the clumps, the best-fit b _NT – l _cl relation shows that the turbulence is consistent with Kolmogorov at

The [O iii ] 5007 Å emission line is the most common tracer of warm, ionized outflows in active galactic nuclei across cosmic time. JWST newly allows us to use mid-IR spectral features at both high spatial and spectral resolution to probe these same winds. Here we present a comparison of ground-based, seeing-limited [O iii ] and space-based, diffraction-limited [S iv ] 10.51 μ m maps of the powerful, kiloparsec-scale outflow in the Type 1 red quasar SDSS J110648.32+480712.3. The JWST data are from the Mid-InfraRed Instrument. There is a close match in resolution between the data sets (∼0.″6), in ionization potential of the O ^+2 and S ^+3 ions (35 eV) and in line sensitivity (1–2 × 10 ^−17 erg s ^−1 cm ^−2 arcsec ^−2 ). The [O iii ] and [S iv ] line shapes match in velocity and line width over much of the 20 kpc outflowing nebula, and [S iv ] is the brightest line in the rest-frame 3.5–19.5 μ m range, demonstrating its usefulness as a mid-IR probe of quasar outflows. [O iii ] is nevertheless intrinsically brighter and provides better contrast with the point-source continuum, which is strong in the mid-IR. There is a strong anticorrelation of [O iii ]/[S iv ] with average velocity, which is consistent with a scenario of differential obscuration between the approaching (blueshifted) and receding (redshifted) sides of the flow. The dust in the wind may also obscure the central quasar, consistent with models that attribute red quasar extinction to dusty winds.

Massive galaxies formed most actively at redshifts z = 1–3 during the period known as “cosmic noon.” Here we present an emission-line study of the extremely red quasar SDSSJ165202.64+172852.3’s host galaxy at z = 2.94, based on observations with the Near Infrared Spectrograph integral field unit on board JWST. We use standard emission-line diagnostic ratios to map the sources of gas ionization across the host and a swarm of companion galaxies. The quasar dominates the photoionization, but we also discover shock-excited regions orthogonal to the ionization cone and the quasar-driven outflow. These shocks could be merger-induced or—more likely, given the presence of a powerful galactic-scale quasar outflow—these are signatures of wide-angle outflows that can reach parts of the galaxy that are not directly illuminated by the quasar. Finally, the kinematically narrow emission associated with the host galaxy presents as a collection of 1 kpc–scale clumps forming stars at a rate of at least 200 M _⊙ yr ^−1 . The interstellar medium within these clumps shows high electron densities, reaching up to 3000 cm ^−3 , with metallicities ranging from half to a third solar with a positive metallicity gradient, and V -band extinctions up to 3 mag. The star formation conditions are far more extreme in these regions than in local star-forming galaxies but consistent with those of massive galaxies at cosmic noon. The JWST observations simultaneously reveal an archetypal rapidly forming massive galaxy undergoing a merger, a clumpy starburst, an episode of obscured near-Eddington quasar activity, and an extremely powerful quasar outflow.

Quasar feedback may regulate the growth of supermassive black holes, quench coeval star formation, and impact galaxy morphology and the circumgalactic medium. However, direct evidence for quasar feedback in action at the epoch of peak black hole accretion at z ≈ 2 remains elusive. A good case in point is the z = 1.6 quasar WISEA J100211.29+013706.7 (XID 2028), where past analyses of the same ground-based data have come to different conclusions. Here, we revisit this object with the integral-field unit of the Near Infrared Spectrograph on board the JWST as part of Early Release Science program Q3D. The excellent angular resolution and sensitivity of the JWST data reveal new morphological and kinematic substructures in the outflowing gas plume. An analysis of the emission-line ratios indicates that photoionization by the central quasar dominates the ionization state of the gas with no obvious sign for a major contribution from hot young stars anywhere in the host galaxy. The rest-frame near-UV emission aligned along the wide-angle cone of outflowing gas is interpreted as a scattering cone. The outflow has cleared a channel in the dusty host galaxy, through which some of the quasar ionizing radiation is able to escape and heat the surrounding interstellar and circumgalactic media. Although the warm ionized outflow is not powerful enough to impact the host galaxy via mechanical feedback, radiative feedback by the active galactic nucleus, aided by the outflow, may help to explain the unusually small molecular gas mass fraction in the galaxy host.

We report the discovery of giant (50−100 kpc) [O ii ] emitting nebulae with MUSE in the field of TXS 0206−048, a luminous quasar at z = 1.13. “Down-the-barrel” UV spectra of the quasar show absorption at velocities coincident with those of the extended nebulae, enabling new insights into inflows and outflows around the quasar host. One nebula exhibits a filamentary morphology extending over 120 kpc from the halo toward the quasar and intersecting with another nebula surrounding the quasar host with a radius of 50 kpc. This is the longest cool filament observed to date and arises at higher redshift and in a less massive system than those in cool-core clusters. The filamentary nebula has line-of-sight velocities >300 km s ^−1 from nearby galaxies but matches that of the nebula surrounding the quasar host where they intersect, consistent with accretion of cool intergalactic or circumgalactic medium or cooling hot halo gas. The kinematics of the nebulae surrounding the quasar host are unusual and complex, with redshifted and blueshifted spiral-like structures. The emission velocities at 5−10 kpc from the quasar match those of inflowing absorbing gas observed in UV spectra of the quasar. Together, the extended nebulae and associated redshifted absorption represent a compelling case of cool, filamentary gas accretion from halo scales into the extended interstellar medium and toward the nucleus of a massive quasar host. The inflow rate implied by the combined emission and absorption constraints is well below levels required to sustain the quasar’s radiative luminosity, suggesting anisotropic or variable accretion.

Nocturnal enuresis causes significant psychological distress to affected children and their family and requires appropriate management. A 12-member expert committee of pediatric urologists and pediatric nephrologists in Taiwan with extensive experience in treating enuresis was established to develop consensus statements and a recommended treatment algorithm for the management of patients with nocturnal enuresis in Taiwan after careful consideration of current evidence, existing guidelines, and expert opinion as well as local practice and culture. The finalized consensus statements were reviewed by and have received endorsement from the Taiwan Urological Association and the Taiwan Pediatric Association. Patients with suspected enuresis should undergo a thorough initial assessment to fully evaluate urinary signs and symptoms and to rule out underlying causes of diurnal and nocturnal incontinence. Behavioral therapy is recommended throughout the course of management. Desmopressin in the fast-melting formulation is the recommended first-line pharmacological treatment. Combination therapy may be effective in patients who have failed first-line treatment. These consensus statements and a recommended treatment algorithm were created by the expert committee to provide practical support for clinical decision making by physicians in Taiwan. Keywords: Consensus statements, Management, Nocturnal enuresis, Taiwan

Background: Urolithiasis is a common disease with high prevalence and recurrence. Its incidence varies in different geographic locations, and there are evidences that meteorological factors also affect urinary stone formation. The aim of this study is to analyze the effects of climate parameters on the numbers of shockwave treatments for urinary stones in our hospital, in order to understand the effects of these parameters on the prevalence of urolithiasis in northern Taiwan. Methods: We retrospectively reviewed the records of extracorporeal shockwave lithotripsy (ESWL) performed in our hospital from December 2006 to November 2011. Repeated ESWL performed in the same patient within 1 month was excluded, and we only counted as one ESWL in our study. Climate data of the corresponding months were collected from Central Weather Bureau. The available monthly meteorological data included highest, lowest, and average temperatures, humidity, rainfall, total rain days, sunshine hours, average atmospheric pressure, and wind speed. Results: Monthly ESWL number was positively correlated to temperature (r = 0.696), sunshine hours (r = 0.515), and wind speed (r = 0.369), while it was negatively correlated to humidity (r = -0.441) and atmospheric pressure (r = -0.568). Average monthly temperature had the strongest correlation to ESWL number (r2 = 0.484). Monthly rainfall and rain days were not significantly correlated to ESWL number. To investigate the climate parameters together, we introduced these correlated factors into the multivariate linear regression model which demonstrated only temperature (ß = 1.438, 95% CI: 3.703-9.144, p < 0.001) and atmospheric pressure (ß = 0.803, 95% CI: 0.790-5.428, p = 0.010) to be independently related to monthly ESWL number. Conclusion: Temperature and atmospheric pressure are associated with monthly ESWL number. Ambient temperature is the most important climate factor affecting the prevalence of urolithiasis in northern Taiwan.

High structural susceptibility of multiferroic BiFeO3 (BFO) makes it a potential replacement of current Pb-based piezoelectrics. In this study, a tetragonal phase is identified based on a combination of x-ray diffraction, scanning transmission electronic microscopy, x-ray absorption spectroscopy, and Raman spectroscopy when BFO is grown on yttria-stabilized zirconia (YSZ) substrates. To distinguish the discrepancy between this tetragonal phase and common cases of monoclinic BFO, piezoelectric force microscopy images and optical property are also performed. It shows a lower electrostatic energy of ferroelectric domains and a large reduction of band gap for BFO grown on YSZ substrate comparing to the well-known one grown on LaAlO3 substrate. Our findings in this work can provide more insights to understand the structural diversity of multiferroic BFO system for further applications.

Purpose: Benign prostatic hyperplasia is a common disease affecting older males. As obesity becomes an increasing problem worldwide, its role in prostatic hypertrophy has been discussed recently. The purpose of this study is to evaluate the relationship between waist circumferences and prostatic hyperplasia in Taiwan. Methods: There were 539 men enrolled in the study who had health examinations at the Healthcare Center of Chang Gung Memorial Hospital; 53 were excluded because of history of conditions affecting prostatic volume. Their anthropometry was measured and serum prostate-specific antigen (PSA) levels as well as lipid profiles were analyzed. Prostate volume was measured by transrectal ultrasonography performed by experienced urologists. Results: The mean prostate volume was 26.43 mL, whereas mean body mass index (BMI) was 25.27 kg/m2 and mean waist circumference (WC) was 90.81 cm. By age-adjusted logistic regression, PSA > 4 ng/mL, WC ≥ 90 cm, and BMI > 24 kg/m2 are associated with increased risk of developing prostatic hyperplasia; only WC ≥ 90 cm can be validated by multiple logistic regression. Further analysis of obesity patterns showed that abdominal overweight/obesity places patients at increased risk independently rather than high WC or high BMI alone. Conclusions: Study results showed that waist circumference ≥ 90 cm is an independent risk factor of prostatic hyperplasia in Taiwan. Men with abdominal overweight/obesity (WC ≥ 90 cm and BMI > 24 kg/m2) have a twofold risk of developing prostatic hyperplasia.

Gaseous, disc–halo interfaces are shaped by processes that are critical to galaxy evolution, including gas accretion and outflows. Extraplanar diffuse ionized gas (eDIG) layers are characterized by scale heights that largely exceed those predicted by their temperature, suggesting the presence of turbulent energy injection from star-formation feedback. However, the origin of this large-scale height remains uncertain. To explore the connection between eDIG and star-forming discs, we present a spatially resolved case study of a nearby pair of sub- |$L_*$|⁠ , intermediately inclined disc galaxies NGC 3511/3513. We decompose optical nebular lines observed using long-slit spectroscopy into narrow and broad velocity components. In NGC 3511, the broad component has three distinctive characteristics in comparison to the narrow component: (1) significantly higher velocity dispersions (a median |$\langle \sigma \rangle _{\text{Broad}} = 24$|  km s |$^{-1}$| compared to |$\langle \sigma \rangle _{\text{Narrow}} = 13$|  km s |$^{-1}$|⁠), (2) elevated [N  ii ] |$\lambda$| 6583/H |$\alpha$| and [S  ii ] |$\lambda$| 6716/H |$\alpha$| line ratios, and (3) a rotational velocity lag. These characteristics support the origin of the broad component in an extraplanar, gaseous disc. In NGC 3513, the broad component reveals disc–halo circulation via localized outflows at radius |$\lesssim 1$|  kpc. For NGC 3511, we test a vertical hydrostatic equilibrium model with pressure support supplied by thermal and turbulent motions. Under this assumption, the eDIG velocity dispersion corresponds to a scale height |$h_{z} \gtrsim 0.2 - 0.4$|  kpc at |$R = 3 - 5$|  kpc, a factor of a few above the thermal scale height (⁠|$h_{z} \lesssim 0.1$|  kpc). This highlights the importance of turbulent motions to the vertical structure of the gaseous, disc–halo interface. [ABSTRACT FROM AUTHOR]

This essay reads Toni Morrison’s 1973 novel Sula as a critical response to Daniel Patrick Moynihan’s 1965 report “The Negro Family” as well as to the various lines of criticism the report received. Blaming black female-headed households and the absence of black fathers for causing poverty in African American communities, the Moynihan Report provoked great controversy during the 1960s and 1970s. Although many black activists and writers were galvanized in opposition to the report’s racism and sexism, some of their critiques turned out to be problematic. This essay shows how some responses to the report reinforced white regulations imposed on black women, denied the possibility of black women serving as heads of families, celebrated black women’s resistance without delving into the underlying reasons, and dismissed the political importance of bonds between black women. By portraying two starkly different kinds of female-headed households and a disruptive friendship between two black women, Morrison’s Sula criticizes the Moynihan Report and addresses its problematic reception by recognizing and complicating the figure of the black matriarch, exposing the structural discrimi)nation that makes black women suffer and black families disintegrate in the first place, and proposing the feminist political work that uneasy black female friendships can launch. [ABSTRACT FROM AUTHOR]