bluuebunny/crossref_metadata_2025_split huggingface dataset:
The pedicled gracilis muscle combined with the fascia lata: a preliminary clinical study of a new biomimetic dynamic phalloplasty method
Authors: Cao Zilong , Liu Liqiang , Yang Zhe , Li Yangqun , Jiao Hu , Zhang Tiran , Zhou Lu 
Published: January 2023

AbstractBackgroundPhalloplasty is a challenging procedure in the field of repair and reconstruction. Traditional skin flap methods with prostheses or autologous tissue implantation are still common; however, with this method the reconstructed phallus is static and has a high risk of complications.AimWe aimed to use novel methods for phalloplasty to mimic the normal structure of the phallus while maintaining the patient’s ability to obtain sufficient hardness and subjective controllability.MethodsThe neophallus comprised the bilateral pedicled neurovascular gracilis muscle, which provided neophallus volitional control; the pedicled fascia lata, which mimicked the tunica albuginea; the pedicled anterolateral thigh flap, which was used to reconstruct the neourethra and neoglans; and the thin split-thickness skin grafted on the surface of the fascia lata. The urethral anastomosis was performed simultaneously. The appearance and function of the neophallus, as well as patient satisfaction, were evaluated postoperatively.OutcomesThe biomimetic dynamic phalloplasty using the bilateral pedicled gracilis muscle combined with the fascia lata was successfully performed in 4 patients.ResultsDuring follow-up at 10-21 months after the procedure, all 4 patients could complete sexual intercourse and were satisfied with the appearance and self-controllability of the neophallus. The size of the neophallus stabilized within 6 months. The tactile, deep touch sensation, and pain sensations of the neophallus partially recovered. All of the patients could stand to urinate.Clinical ImplicationsWe used the gracilis muscle combined with the fascia lata to mimic the basic structure of the corpus cavernosum and tunica albuginea and successfully reconstructed the biomimetic dynamic neophallus.Strengths and LimitationsThis is to our knowledge the first report of biomimetic dynamic phalloplasty using the bilateral pedicled gracilis muscle combined with the fascia lata to mimic the complex structure of the phallus and enable the achievement of erection. However, due to the small number of patients included in this study, the data have no statistical significance. More cases are needed to obtain conclusive data and examine the long-term clinical effects of this procedure.ConclusionUsing novel methods for phalloplasty, we successfully maintained the patient’s ability to obtain sufficient hardness and subjective controllability without the use of implants, and the preliminary clinical results are encouraging.
Increasing role of counterincision for high submuscular penile prosthesis reservoir placement
Authors: VanDyke Maia E , Kavoussi Mehraban , Langford Brian T , Badkhshan Shervin , Nealon Samantha W , Franzen Bryce P , Sanders Sarah C , Morey Allen F 
Published: January 2023

AbstractBackgroundInflatable penile prosthesis (IPP) reservoir placement into the high submuscular (HSM) space is safe and well tolerated. Recent studies have proposed that reservoirs placed via an abdominal counterincision (CI) may offer more precise and durable positioning as compared with a transinguinal (TI) approach.AimHerein we compare the CI-HSM and TI-HSM techniques with respect to operative time, pain control, and postoperative complications.MethodsWe reviewed our penile prosthesis database at a large single-surgeon tertiary referral center from 2014 to 2021 to compare those who underwent virgin reservoir placement via the CI-HSM technique vs the TI-HSM technique. Statistical analysis was performed with the Mann-Whitney U test for continuous variables and the chi-square test and Fisher exact test for discrete variables.OutcomesOperative time, postoperative complications, morphine milligram equivalents prescribed, and postoperative correspondence were compared between patients undergoing the CI-HSM and TI-HSM techniques.ResultsAmong 456 virgin IPP implants, the CI-HSM technique was used in 34 cases (7.5%) and the TI-HSM technique in 422 cases (92.5%). Of these 456 cases, 92 (20.2%) were combined with ancillary procedures such as artificial urinary sphincter, urethral sling, or penile plication (6/34, CI; 86/422, TI). Cases employing the CI-HSM technique had a 19.9% greater median operative time: 81.5 minutes (IQR, 69.3-106.5) vs 68 minutes (IQR, 57.8-80.3; P &lt; .01). A similar proportion of patients in the CI-HSM group (2/34, 5.9%) were treated for infection as in the TI-HSM group (17/422, 4.0%; P = .64). Reservoir herniation was seen in 12 patients in the TI-HSM group (2.8%) and in none of the CI-HSM group, but this did not reach significance (P &gt; .99). No differences were identified between patients in the TI-HSM and CI-HSM groups with regard to postoperative morphine milligram equivalents prescribed, narcotic medication refills, or postoperative correspondence.Clinical ImplicationsCI-HSM reservoir placement was associated with similar surgical outcomes to TI-HSM without increased infection risk or need for narcotic pain management.Strengths and LimitationsAlthough this study is a large contemporary series addressing a clinically important subject, it is limited by its retrospective preliminary nature and nonrandomized unmatched design. Patient pain regimens were assessed via discharge prescriptions, although data regarding narcotic consumption were not available in the medical record.ConclusionsIPP reservoir placement via the CI-HSM technique is safe and well tolerated. Increased operative time of the CI-HSM technique as compared with the TI-HSM technique is clinically negligible given its potential safety benefits of direct visualization of reservoir placement.
QUIJOTE scientific results – V. The microwave intensity and polarization spectra of the Galactic regions W49, W51 and IC443
Authors: Tramonte D , Génova-Santos R T , Rubiño-Martín J A , Vielva P , Poidevin F , López-Caraballo C H , Peel M W , Ashdown M , Artal E , Barreiro R B , Casas F J , de la Hoz E , Fernández-Torreiro M , Guidi F , Herranz D , Hoyland R J , Lasenby A N , Martinez-Gonzalez E , Piccirillo L , Rebolo R , Ruiz-Granados B , Vansyngel F , Watson R A 
Published: January 2023

ABSTRACT
We present new intensity and polarization maps obtained with the QUIJOTE experiment towards the Galactic regions W49, W51 and IC443, covering the frequency range from 10 to 20 GHz at $\sim 1\, \text{deg}$ angular resolution, with a sensitivity in the range 35–79 $\mu \text{K}\, \text{beam}^{-1}$ for total intensity and 13–23 $\mu \text{K}\, \text{beam}^{-1}$ for polarization. For each region, we combine QUIJOTE maps with ancillary data at frequencies ranging from 0.4 to 3000 GHz, reconstruct the spectral energy distribution and model it with a combination of known foregrounds. We detect anomalous microwave emission (AME) in total intensity towards W49 at 4.7σ and W51 at 4.0σ with peak frequencies $\nu _{\rm AME}=(20.0\pm 1.4)\, \text{GHz}$ and $\nu _{\rm AME}=(17.7\pm 3.6)\, \text{GHz}$, respectively; this is the first detection of AME towards W51. The contamination from ultracompact H ii regions to the residual AME flux density is estimated at 10 per cent in W49 and 5 per cent in W51, and does not rule out the AME detection. The polarized SEDs reveal a synchrotron contribution with spectral indices αs = −0.67 ± 0.10 in W49 and αs = −0.51 ± 0.07 in W51, ascribed to the diffuse Galactic emission and to the local supernova remnant, respectively. Towards IC443 in total intensity we measure a broken power-law synchrotron spectrum with cut-off frequency $\nu _{\rm 0,s}=(114\pm 73)\, \text{GHz}$, in agreement with previous studies; our analysis, however, rules out any AME contribution which had been previously claimed towards IC443. No evidence of polarized AME emission is detected in this study.
Core-collapse supernovae in the Dark Energy Survey: luminosity functions and host galaxy demographics
Authors: Grayling M , Gutiérrez C P , Sullivan M , Wiseman P , Vincenzi M , Galbany L , Möller A , Brout D , Davis T M , Frohmaier C , Graur O , Kelsey L , Lidman C , Popovic B , Smith M , Toy M , Tucker B E , Zontos Z , Abbott T M C , Aguena M , Allam S , Andrade-Oliveira F , Annis J , Asorey J , Bacon D , Bertin E , Bocquet S , Brooks D , Carnero Rosell A , Carollo D , Carrasco Kind M , Carretero J , Costanzi M , da Costa L N , Pereira M E S , De Vicente J , Desai S , Diehl H T , Doel P , Everett S , Ferrero I , Friedel D , Frieman J , García-Bellido J , Gatti M , Gruen D , Gschwend J , Gutierrez G , Hinton S R , Hollowood D L , Honscheid K , James D J , Kuehn K , Kuropatkin N , Lewis G F , Malik U , March M , Menanteau F , Miquel R , Morgan R , Ogando R L C , Palmese A , Paz-Chinchón F , Pieres A , Plazas Malagón A A , Rodriguez-Monroy M , Romer A K , Roodman A , Sanchez E , Scarpine V , Sevilla-Noarbe I , Suchyta E , Tarle G , To C , Tucker D L , Varga T N ,   DES Collaboration
Published: January 2023

ABSTRACT
We present the luminosity functions and host galaxy properties of the Dark Energy Survey (DES) core-collapse supernova (CCSN) sample, consisting of 69 Type II and 50 Type Ibc spectroscopically and photometrically confirmed supernovae over a redshift range 0.045 &lt; z &lt; 0.25. We fit the observed DES griz CCSN light curves and K-correct to produce rest-frame R-band light curves. We compare the sample with lower redshift CCSN samples from Zwicky Transient Facility (ZTF) and Lick Observatory Supernova Search (LOSS). Comparing luminosity functions, the DES and ZTF samples of SNe II are brighter than that of LOSS with significances of 3.0σ and 2.5σ, respectively. While this difference could be caused by redshift evolution in the luminosity function, simpler explanations such as differing levels of host extinction remain a possibility. We find that the host galaxies of SNe II in DES are on average bluer than in ZTF, despite having consistent stellar mass distributions. We consider a number of possibilities to explain this – including galaxy evolution with redshift, selection biases in either the DES or ZTF samples, and systematic differences due to the different photometric bands available – but find that none can easily reconcile the differences in host colour between the two samples and thus its cause remains uncertain.
A unique, ring-like radio source with quadrilateral structure detected with machine learning
Authors: Lochner M , Rudnick L , Heywood I , Knowles K , Shabala S S 
Published: January 2023

ABSTRACT
We report the discovery of a unique object in the MeerKAT Galaxy Cluster Legacy Survey (MGCLS) using the machine learning anomaly detection framework astronomaly. This strange, ring-like source is 30′ from the MGCLS field centred on Abell 209, and is not readily explained by simple physical models. With an assumed host galaxy at redshift 0.55, the luminosity (1025 W Hz−1) is comparable to powerful radio galaxies. The source consists of a ring of emission 175 kpc across, quadrilateral enhanced brightness regions bearing resemblance to radio jets, two ‘ears’ separated by 368 kpc, and a diffuse envelope. All of the structures appear spectrally steep, ranging from −1.0 to −1.5. The ring has high polarization (25 per cent) except on the bright patches (&lt;10 per cent). We compare this source to the Odd Radio Circles recently discovered in ASKAP data and discuss several possible physical models, including a termination shock from starburst activity, an end-on radio galaxy, and a supermassive black hole merger event. No simple model can easily explain the observed structure of the source. This work, as well as other recent discoveries, demonstrates the power of unsupervised machine learning in mining large data sets for scientifically interesting sources.
Constraints on the X-ray luminosity function of AGN at z = 5.7–6.4 with the Extragalactic Serendipitous Swift Survey
Authors: Barlow-Hall C L , Delaney J , Aird J , Evans P A , Osborne J P , Watson M G 
Published: January 2023

ABSTRACT
X-ray luminosity functions (XLFs) of active galactic nuclei (AGNs) trace the growth and evolution of supermassive black hole populations across cosmic time. However, current XLF models are poorly constrained at redshifts of z &gt; 6, with a lack of spectroscopic constraints at these high redshifts. In this work, we place limits on the bright-end of the XLF at z = 5.7–6.4 using high-redshift AGN identified within the Extragalactic Serendipitous Swift Survey (ExSeSS) catalogue. Within ExSeSS, we find one serendipitously X-ray detected z &gt; 6 AGN, ATLAS J025.6821-33.4627, with an X-ray luminosity of $L_\mathrm{X}=8.47^{+3.40}_{-3.13}\times 10^{44}\mathrm{erg.s^{-1}}$ and z = 6.31 ± 0.03, making it the highest redshift, spectroscopically confirmed, serendipitously X-ray detected quasar known to date. We also calculate an upper limit on the space density at higher luminosities where no additional sources are found, enabling us to place constraints on the shape of the XLF. Our results are consistent with the rapid decline in the space densities of high-luminosity AGN towards high redshift as predicted by extrapolations of existing parametric models of the XLF. We also find that our X-ray based measurements are consistent with estimates of the bolometric quasar luminosity function based on UV measurements at z ≳ 6, although they require a large X-ray to bolometric correction factor at these high luminosities.
Transition of latitudinal differential rotation as a possible cause of weakened magnetic braking of solar-type stars
Authors: Tokuno Takato , Suzuki Takeru K , Shoda Munehito 
Published: January 2023

ABSTRACTWe investigate the role of latitudinal differential rotation (DR) in the spin evolution of solar-type stars. Recent asteroseismic observation detected the strong equator-fast DR in some solar-type stars. Numerical simulations show that the strong equator-fast DR is a typical feature of young fast-rotating stars and that this tendency is gradually reduced with stellar age. Incorporating these properties, we develop a model for the long-term evolution of stellar rotation. The magnetic braking is assumed to be regulated dominantly by the rotation rate in the low-latitude region. Therefore, in our model, stars with the equator-fast DR spin down more efficiently than those with the rigid-body rotation. We calculate the evolution of stellar rotation in ranges of stellar mass, $0.9 \, \mathrm{M}_{\odot } \le M \le 1.2\, \mathrm{M}_{\odot }$, and metallicity, $0.5\, \mathrm{Z}_{\odot } \le Z \le 2\, \mathrm{Z}_{\odot }$, where M⊙ and Z⊙ are the solar mass and metallicity, respectively. Our model, using the observed torque in the present solar wind, nicely explains both the current solar rotation and the average trend of the rotation of solar-type stars, including the dependence on metallicity. In addition, our model naturally reproduces the observed trend of the weakened magnetic braking in old slowly rotating solar-type stars because strong equator-fast DR becomes reduced. Our results indicate that latitudinal DR and its transition are essential factors that control the stellar spin down.
Real and counterfeit cores: how feedback expands haloes and disrupts tracers of inner gravitational potential in dwarf galaxies
Authors: Jahn Ethan D , Sales Laura V , Marinacci Federico , Vogelsberger Mark , Torrey Paul , Qi Jia , Smith Aaron , Li Hui , Kannan Rahul , Burger Jan D , Zavala Jesús 
Published: January 2023

ABSTRACT
The tension between the diverging density profiles in Lambda cold dark matter simulations and the constant-density inner regions of observed galaxies is a long-standing challenge known as the ‘core–cusp’ problem. We demonstrate that the SMUGGLE galaxy formation model implemented in the arepo moving mesh code forms constant-density cores in idealized dwarf galaxies of M⋆ ≈ 8 × 107 Msun with initially cuspy dark matter (DM) haloes of M200 ≈ 1010 Msun. Identical initial conditions run with an effective equation of state interstellar medium model preserve cuspiness. Literature on the subject has pointed to the low density threshold for star formation, ρth, in such effective models as an obstacle to baryon-induced core formation. Using a SMUGGLE run with equal ρth, we demonstrate that core formation can proceed at low density thresholds, indicating that ρth is insufficient on its own to determine whether a galaxy develops a core. We reaffirm that the ability to resolve a multiphase interstellar medium at sufficiently high densities is a more reliable indicator of core formation than any individual model parameter. In SMUGGLE, core formation is accompanied by large degrees of non-circular motion, with gas rotational velocity profiles that consistently fall below the circular velocity $v_\text{circ} = \sqrt{GM/R}$ out to ∼2 kpc. Asymmetric drift corrections help recover the average underlying DM potential for some of our less efficient feedback runs, but time-variations in the instantaneous azimuthal gas velocity component are substantial, highlighting the need for careful modelling in the inner regions of dwarfs to infer the true distribution of DM.
Inclination dependence of warm coronal flux in high-accretion-rate AGNs
Authors: Tang Ze-Yuan , Feng Jun-Jie , Fan Jun-Hui 
Published: January 2023

ABSTRACT
Most active galactic nucleus (AGN) spectra show a soft X-ray excess above the 2–10 keV power law extrapolation. A warm corona has been widely used to explain the excess, but its observed radiation flux in the actually physical environment has yet to be further studied. For the first time, we calculate the relativistic warm coronal flux under the finite disc-corona thickness in high-accretion-rate systems. The numerical results show that the warm coronal flux generally rises first and then drops with increasing inclination. The flux rise is more significant for a compact and low-temperature warm corona and can reach 1–2 dexes. Meanwhile, the flux drop is significant if and only if the warm corona is heavily obscured due to the finite thickness. Our model can successfully explain the soft excess variance and the X-ray weak fraction in a high-accretion-rate AGN sample. In conclusion, our study indicates that when fitting the soft X-ray spectra of AGNs, the relativistic inclination dependence of warm coronal flux is essential, especially for the high-accretion-rate systems with thick warm coronae.
Investigating the impact of reactions of C and CH with molecular hydrogen on a glycine gas-grain network
Authors: Heyl Johannes , Lamberts Thanja , Viti Serena , Holdship Jonathan 
Published: January 2023

ABSTRACT
The impact of including the reactions of C and CH with molecular hydrogen in a gas-grain network is assessed via a sensitivity analysis. To this end, we vary three parameters, namely, the efficiency for the reaction ${\rm C} + {\rm H}_2 \longrightarrow {\rm CH}_{2}$, and the cosmic ray ionization rate, with the third parameter being the final density of the collapsing dark cloud. A grid of 12 models is run to investigate the effect of all parameters on the final molecular abundances of the chemical network. We find that including reactions with molecular hydrogen alters the hydrogen economy of the network; since some species are hydrogenated by molecular hydrogen, atomic hydrogen is freed up. The abundances of simple molecules produced from hydrogenation, such as CH4, CH3OH, and NH3, increase, and at the same time, more complex species such as glycine and its precursors see a significant decrease in their final abundances. We find that the precursors of glycine are being preferentially hydrogenated, and therefore glycine itself is produced less efficiently.
Dust processing in protoplanetary envelopes as the origin of hot minerals in comets
Authors: Ali-Dib Mohamad 
Published: January 2023

ABSTRACT
Crystalline silicates are found in a large number of comets. These pose a long-standing conundrum for Solar system formation models as they can only be created in the inner hot disc at temperatures higher than 800 K, and there is no obvious mechanism to transport them out into the comets formation region. Here, we propose that these particles could have formed inside the hydrostatic envelopes surrounding young protoplanets still embedded in the protoplanetary disc. Using a simplified 1D model we investigate the thermal structure of these envelopes, and find that for core masses ranging from 0.08 to 1.5 M⊕, located anywhere between 1 and 30 au, the temperature and pressure at the base of the envelopes are high enough to quickly vapourize silicate particles of various sizes. Moreover, if the grain abundance is atleast solar, these envelopes become fully convective, allowing for dust ejection across the Bondi radius back into the disc. Amorphous silicates are hence thermally processed into crystalline particles in these envelopes, and then transported back to disc through convective diffusion to be finally incorporated into the cometary building blocks.
The homeodomain of Oct4 is a dimeric binder of methylated CpG elements
Authors: Tan Daisylyn Senna , Cheung Shun Lai , Gao Ya , Weinbuch Maike , Hu Haoqing , Shi Liyang , Ti Shih-Chieh , Hutchins Andrew P , Cojocaru Vlad , Jauch Ralf 
Published: January 2023

AbstractOct4 is essential to maintain pluripotency and has a pivotal role in establishing the germline. Its DNA-binding POU domain was recently found to bind motifs with methylated CpG elements normally associated with epigenetic silencing. However, the mode of binding and the consequences of this capability has remained unclear. Here, we show that Oct4 binds to a compact palindromic DNA element with a methylated CpG core (CpGpal) in alternative states of pluripotency and during cellular reprogramming towards induced pluripotent stem cells (iPSCs). During cellular reprogramming, typical Oct4 bound enhancers are uniformly demethylated, with the prominent exception of the CpGpal sites where DNA methylation is often maintained. We demonstrate that Oct4 cooperatively binds the CpGpal element as a homodimer, which contrasts with the ectoderm-expressed POU factor Brn2. Indeed, binding to CpGpal is Oct4-specific as other POU factors expressed in somatic cells avoid this element. Binding assays combined with structural analyses and molecular dynamic simulations show that dimeric Oct4-binding to CpGpal is driven by the POU-homeodomain whilst the POU-specific domain is detached from DNA. Collectively, we report that Oct4 exerts parts of its regulatory function in the context of methylated DNA through a DNA recognition mechanism that solely relies on its homeodomain.