Abstract
Recent work has found evidence for a difference in the bias and dark matter halo masses of WISE (Wide-field Infrared Survey Explorer)-selected obscured and unobscured quasars, implying a ...distinction between these populations beyond random line-of-sight effects. However, the significance of this difference in the most up-to-date measurements is relatively weak, at ∼2σ for individual measurements, but bolstered by agreement from different techniques, including angular clustering and cross-correlations with cosmic microwave background lensing maps. Here, we expand the footprint of previous work, aiming to improve the precision of both methods. In this larger area, we correct for position-dependent selection effects, in particular fluctuations of the WISE-selected quasar density as a function of Galactic latitude. We also measure the cross-correlation of the obscured and unobscured samples and confirm that they are well matched in redshift, both centred at z = 1. Combined with very similar detection fractions and magnitude distributions in the long-wavelength WISE bands, this redshift match strongly supports the fact that infrared selection identifies obscured and unobscured quasars of similar bolometric luminosity. Finally, we perform cross-correlations with confirmed spectroscopic quasars, again confirming the results from other methods – obscured quasars reside in haloes a factor of 3 times more massive than unobscured quasars. This difference is significant at the ∼5σ level when the measurements are combined, providing strong support for the idea that obscuration in at least some quasars is tied to the larger environment, and may have an evolutionary component.
Abstract
We present the most precise estimate to date of the clustering of quasars on very small scales, based on a sample of 47 binary quasars with magnitudes of g < 20.85 and proper transverse ...separations of ∼25 h
−1 kpc. Our sample of binary quasars, which is about six times larger than any previous spectroscopically confirmed sample on these scales, is targeted using a kernel density estimation (KDE) technique applied to Sloan Digital Sky Survey (SDSS) imaging over most of the SDSS area. Our sample is ‘complete’ in that all of the KDE target pairs with 17.0 ≲ R ≲ 36.2 h
−1 kpc in our area of interest have been spectroscopically confirmed from a combination of previous surveys and our own long-slit observational campaign. We catalogue 230 candidate quasar pairs with angular separations of <8 arcsec, from which our binary quasars were identified. We determine the projected correlation function of quasars (
$\bar{W}_{\rm p}$
) in four bins of proper transverse scale over the range 17.0 ≲ R ≲ 36.2 h
−1 kpc. The implied small-scale quasar clustering amplitude from the projected correlation function, integrated across our entire redshift range, is A = 24.1 ± 3.6 at ∼26.6 h
−1 kpc. Our sample is the first spectroscopically confirmed sample of quasar pairs that is sufficiently large to study how quasar clustering evolves with redshift at ∼25 h
−1 kpc. We find that empirical descriptions of how quasar clustering evolves with redshift at ∼25 h
−1 Mpc also adequately describe the evolution of quasar clustering at ∼25 h
−1 kpc.
Abstract
We combine the most precise small-scale ($\lt 100\, \rm h^{-1}kpc$) quasar clustering constraints to date with recent measurements at large scales ($\gt 1\, \rm h^{-1}Mpc$) from the extended ...Baryon Oscillation Spectroscopic Survey (eBOSS) to better constrain the satellite fraction of quasars at z ∼ 1.5 in the halo occupation formalism. We build our Halo Occupation Distribution (HOD) framework based on commonly used analytic forms for the one and two-halo terms with two free parameters: the minimum halo mass that hosts a central quasar and the fraction of satellite quasars that are within one halo. Inspired by recent studies that propose a steeper density profile for the dark matter haloes that host quasars, we explore HOD models at kiloparsec scales and best-fit parameters for models with 10 × higher concentration parameter. We find that an HOD model with a satellite fraction of $f_{\rm sat} = 0.071_{-0.004}^{+0.009}$ and minimum mass of $\rm M_{m} = 2.31_{-0.38}^{+0.41} \times 10^{12}\, \, \rm h^{-1} M_{\odot }$ for the host dark matter haloes best describes quasar clustering (on all scales) at z ∼ 1.5. Our results are marginally inconsistent with earlier work that studied brighter quasars, hinting at a luminosity-dependence to the one-halo term.
We present a measurement of the quasar luminosity function in the range 0.68 < z < 4 down to extinction corrected magnitude gdered = 22.5, using a simple and well understood target selection ...technique based on the time-variability of quasars. The completeness of our sample was derived directly from a control sample of quasars, without requiring complex simulations of quasar light-curves or colors. A total of 1877 quasar spectra were obtained from dedicated programs on the Sloan telescope (as part of the SDSS-III/BOSS survey) and on the Multiple Mirror Telescope. They allowed us to derive the quasar luminosity function. It agrees well with results previously published in the redshift range 0.68 < z < 2.6. Our deeper data allow us to extend the measurement to z = 4. We measured quasar densities to gdered < 22.5, obtaining 30 QSO per deg2 at z < 1, 99 QSO per deg2 for 1 < z < 2.15, and 47 QSO per deg2 at z > 2.15. Using pure luminosity evolution models, we fitted our LF measurements and predicted quasar number counts as a function of redshift and observed magnitude. These predictions are useful inputs for future cosmology surveys such as those relying on the observation of quasars to measure baryon acoustic oscillations.
Bilateral ureteral reimplantation at the time of the complete primary repair of bladder exstrophy (BUR-CPRE) has been proposed and has demonstrated favorable outcomes in the past. However, the ...potential benefits, including prevention of vesicoureteral reflux (VUR) and renal scarring must be tempered with any risks of reimplantation, persistent VUR, and the potential for overtreatment. We aimed to determine the impact of BUR-CPRE on reflux rates, renogram findings and bladder capacity.
An IRB approved registry of children treated for bladder exstrophy epispadias complex (BEEC) during a long-term international collaboration hosted in a region with high prevalence of BEEC was queried. Children undergoing primary CPRE for bladder exstrophy (BE) were identified. Surgical procedure and outcome measures nuclear medicine dimercaptosuccinic acid (DMSA) scintigraphy scans, voiding cystourethrogram (VCUG), and urodynamic study (UDS) were assessed for presence and degree of VUR, renogram abnormalities, and bladder capacity.
A total cohort of 147 patients with BEEC was queried; 52 children (37 males, 71%) underwent primary CPRE for BE between 2009 and 2019 at median age of 1.1 years (IQR 0.6–1.9 years) with median follow up 4.4 years (IQR 2.4–6.4 years). BUR-CPRE was performed in 22/52 (42%). After BUR-CPRE, children were less likely to have VUR (any VUR present in 9 of 20 with imaging (45%) compared to 23 of 26 with imaging (82%) in the CPRE alone group (p = 0.007)). VUR in the BUR-CPRE group tended to be unilateral and lower grade in comparison to the CPRE alone group. DMSA abnormalities were less common in the BUR-CPRE group (4/19 (21%) vs.12/27 (44%)), although the difference did not reach statistical significance (p = 0.1). At 4 years follow-up, the BUR-CPRE group had a larger bladder capacity (p = 0.016).
After BUR-CPRE, children had a lower rate of VUR, and when present, VUR was more often unilateral and lower grade compared to the CPRE alone group. Fewer numbers of children in the BUR-CPRE group depicted DMSA abnormalities. No children developed obstruction after BUR-CPRE and none have undergone repeat reimplantation. We documented a larger bladder capacity at the time of maximum follow-up available (4 years)—but further data are needed to confirm this observation.
BUR-CPRE decreases the incidence and severity of VUR after CPRE, but the clinical significance of this remains unclear. We are encouraged by these initial results, but since BUR-CPRE does not uniformly eliminate VUR, we continue to proceed carefully in the well selected patient.Summary TablePrimary outcomes – VUR status and DMSA abnormalitiesSummary TableOutcomeBUR at the time of CPRE (n = 20)No BUR at time of CPRE (n = 28)p-valueAny VUR present∗9 (45%)23 (82%)0.007Bilateral VUR∗4 (20%)19 (68%)0.004High-grade VUR∗ (grades 4 or 5)2 (10%)11 (44%)0.016DMSA abnormalities4/19 (21%)12/27 (44%)0.1Bladder capacity at 1 year of follow-up (n, median, IQR)N = 19Median = 20 (15–30) mlN = 13Median = 30 (15–40) ml0.25Bladder capacity at 4 years of follow-up (n, median, IQR)∗N = 6Median = 78.5 (60–130) mlN = 16Median = 40 (32–56) ml0.02
Abstract
The Dark Energy Spectroscopic Instrument (DESI) will precisely constrain cosmic expansion and the growth of structure by collecting ∼40 million extragalactic redshifts across ∼80% of cosmic ...history and one-third of the sky. The Emission Line galaxy (ELG) sample, which will comprise about one-third of all DESI tracers, will be used to probe the universe over the 0.6 <
z
< 1.6 range, including the 1.1 <
z
< 1.6 range, which is expected to provide the tightest constraints. We present the target selection for the DESI Survey Validation (SV) and Main Survey ELG samples, which relies on the imaging of the Legacy Surveys. The Main ELG selection consists of a
g
-band magnitude cut and a (
g
−
r
) versus (
r
−
z
) color box, while the SV selection explores extensions of the Main selection boundaries. The Main ELG sample is composed of two disjoint subsamples, which have target densities of about 1940 deg
−2
and 460 deg
−2
, respectively. We first characterize their photometric properties and density variations across the footprint. We then analyze the DESI spectroscopic data that have been obtained from 2020 December to 2021 December in the SV and Main Survey. We establish a preliminary criterion for selecting reliable redshifts, based on the O
ii
flux measurement, and assess its performance. Using this criterion, we are able to present the spectroscopic efficiency of the Main ELG selection, along with its redshift distribution. We thus demonstrate that the Main selection 1940 deg
−2
subsample alone should provide 400 deg
−2
and 460 deg
−2
reliable redshifts in the 0.6 <
z
< 1.1 and the 1.1 <
z
< 1.6 ranges, respectively.
We present a measurement of the quasar luminosity function in the range 0.68 < z < 4 down to extinction corrected magnitude gdered = 22.5, using a simple and well understood target selection ...technique based on the time-variability of quasars. The completeness of our sample was derived directly from a control sample of quasars, without requiring complex simulations of quasar light-curves or colors. A total of 1877 quasar spectra were obtained from dedicated programs on the Sloan telescope (as part of the SDSS-III/BOSS survey) and on the Multiple Mirror Telescope. They allowed us to derive the quasar luminosity function. It agrees well with results previously published in the redshift range 0.68 < z < 2.6. Our deeper data allow us to extend the measurement to z = 4. We measured quasar densities to gdered < 22.5, obtaining 30 QSO per deg2 at z < 1, 99 QSO per deg2 for 1 < z < 2.15, and 47 QSO per deg2 at z > 2.15. Using pure luminosity evolution models, we fitted our LF measurements and predicted quasar number counts as a function of redshift and observed magnitude. These predictions are useful inputs for future cosmology surveys such as those relying on the observation of quasars to measure baryon acoustic oscillations.
We combine the most precise small scale ($< 100\, \rm h^{-1}kpc$) quasar
clustering constraintsto date with recent measurements at large scales ($> 1\,
\rm h^{-1}Mpc$) from the extended Baryon ...Oscillation Spectroscopic Survey
(eBOSS) to better constrain the satellite fraction of quasars at $z\sim 1.5$ in
the halo occupation formalism. We build our Halo Occupation Distribution (HOD)
framework based on commonly used analytic forms for the one and two-halo terms
with two free parameters: the minimum halo mass that hosts a central quasar and
the fraction of satellite quasars that are within one halo. Inspired by recent
studies that propose a steeper density profile for the dark matter haloes that
host quasars, we explore HOD models at kiloparsec scales and best-fit
parameters for models with $10\times$ higher concentration parameter. We find
that an HOD model with a satellite fraction of $f_{\rm sat} =
0.071_{-0.004}^{+0.009}$ and minimum mass of $\rm M_{m} = 2.31_{-0.38}^{+0.41}
\times 10^{12}\, \, \rm h^{-1} M_{\odot}$ for the host dark matter haloes best
describes quasar clustering (on all scales) at $z \sim 1.5$. Our results are
marginally inconsistent with earlier work that studied brighter quasars,
hinting at a luminosity-dependence to the one-halo term.
We combine the most precise small scale (\(< 100\, \rm h^{-1}kpc\)) quasar clustering constraintsto date with recent measurements at large scales (\(> 1\, \rm h^{-1}Mpc\)) from the extended Baryon ...Oscillation Spectroscopic Survey (eBOSS) to better constrain the satellite fraction of quasars at \(z\sim 1.5\) in the halo occupation formalism. We build our Halo Occupation Distribution (HOD) framework based on commonly used analytic forms for the one and two-halo terms with two free parameters: the minimum halo mass that hosts a central quasar and the fraction of satellite quasars that are within one halo. Inspired by recent studies that propose a steeper density profile for the dark matter haloes that host quasars, we explore HOD models at kiloparsec scales and best-fit parameters for models with \(10\times\) higher concentration parameter. We find that an HOD model with a satellite fraction of \(f_{\rm sat} = 0.071_{-0.004}^{+0.009}\) and minimum mass of \(\rm M_{m} = 2.31_{-0.38}^{+0.41} \times 10^{12}\, \, \rm h^{-1} M_{\odot}\) for the host dark matter haloes best describes quasar clustering (on all scales) at \(z \sim 1.5\). Our results are marginally inconsistent with earlier work that studied brighter quasars, hinting at a luminosity-dependence to the one-halo term.
Background: The medicinal use of onion dates back to ancient China and India. Men with epilepsy have reduced fertility, and antiepileptic drugs may affect semen quality. Disturbances of reproductive ...endocrine hormones are more often found in men with epilepsy than in the general population. There is an ongoing debate whether this can be attributed to chronic use of antiepileptic drugs or to the epilepsy itself. Objective: The aim of the present study was to evaluate the beneficial degree of sexual behavior in male rats after inducement onion in lamotrigine receiving groups. Methods: Forty wistar rats, randomized into four groups (n = 10), were used for this study, five of them male and five of them female. Animals in Group A served as the control and was drinking distilled water. Animals in Groups B: treated with 3cc/rat of onion juice, in Groups C: received10mg/kg/day lamotrigine, in Groups D: received10mg/kg/day lamotrigine plus 3cc/rat of onion juice. In All treatments were for 5 weeks. 48 hours before end of study estradiol benzoate (25 micro gr/kg/day, s.c.) and 6 hours before end of study progesterone 0.3muM were injected. Results: Results showed the percentage of erections and couplings and serum testosterone in onion treated groups were significantly increased (p<0/01) when compared to other groups. onion and its constituents are stated to has antioxidant. Enhanced oxidative stress and changes in antioxidant capacity are considered to play an important role in the pathogenesis in diseases. Conclusion: These findings lead to the conclusion that onion significantly lowered the adverse effects of lamotrigine, and can do beneficial effect on sexual behavior in male rat.
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