Bulge Mass Research Articles

Smaller stellar disc scale lengths in rich environments

Abstract We investigate the dependence of stellar disc scale lengths on environment for a sample of Sloan Digital Sky Survey Data Release 7 galaxies with published photometric bulge-disc decompositions. We compare disc scale lengths at fixed bulge mass for galaxies in an isolated field environment to galaxies in X-ray rich and X-ray poor groups. At low bulge mass, stellar disc scale lengths in X-ray rich groups are smaller compared to discs in both X-ray poor groups and in isolated field environments. This decrease in disc scale length is largely independent of halo mass, though shows some dependence on group-centric distance. We also find that stellar disc scale lengths are smaller in X-ray rich environments for a subset of star-forming galaxies and for galaxies of different morphological types. We note that disc scale lengths of low mass galaxies are known to have large systematic uncertainties, however we focus on differences between samples with the same measurement biases. Our results show that stellar disc scale lengths depend on X-ray brightness, a tracer of IGM density, suggesting a role for hydrodynamic processes such as ram-pressure stripping and/or starvation.

On the role of supermassive black holes in quenching star formation in local central galaxies

ABSTRACT We analyse the role of AGN feedback in quenching star formation for massive, central galaxies in the local Universe. In particular, we compare the prediction of two semi-analytic models (l-galaxies and sage) featuring different schemes for AGN feedback, with the SDSS DR7 taking advantage of a novel technique for identifying central galaxies in an observational data set. This enables us to study the correlation between the model passive fractions, which is predicted to be suppressed by feedback from an AGN, and the observed passive fractions in an observationally motivated parameter space. While the passive fractions for observed central galaxies show a good correlation with stellar mass and bulge mass, passive fractions in l-galaxies correlate with the halo and black hole mass. For sage, the passive fraction correlate with the bulge mass as well. Among the two models, sage has a smaller scatter in the black hole–bulge mass $({M_{\rm BH}-M_{\rm Bulge}})$ relation and a slope that agrees better with the most recent observations at z ∼ 0. Despite the more realistic prescription of radio-mode feedback in sage, there are still tensions left with the observed passive fractions and the distribution of quenched galaxies. These tensions may be due to the treatment of galaxies living in non-resolved substructures and the resulting higher merger rates that could bring cold gas which is available for star formation.

Investigating the co-evolution of massive black holes in dual active galactic nuclei and their host galaxies via galaxy merger simulations

Major galaxy mergers can trigger nuclear activities and are responsible for high-luminosity quasi-stellar objects/active galactic nuclei (QSOs/AGNs). In certain circumstances, such mergers may cause dual active galactic nuclei (dAGN) phenomenon. This study investigates dAGN triggering and evolution of massive black holes (MBHs) during the merging processes using hydrodynamic code GADGET-2 to simulate several gas-rich major mergers at redshift $z=2$ and $3$, respectively. Results reveal that gas-rich major mergers can trigger significant nuclear activities after the second and third pericentric passages and the formation of dAGN with significant time duration ($\\sim$ 10-390 Myr). During the merging processes, galactic bulge evolves with time because of the rapid star formation in each (or both) galactic centers and initial mixing of stars in galactic disks due to violent relaxation. MBHs grow substantially due to accretion and finally merge into a bigger black hole. The growth of galactic bulges and corresponding increases of its velocity dispersions predate the growth of MBHs in the dAGN stages. The MBHs in these stages deviate below the relation between MBH mass and bulge mass (or velocity dispersion), and they revert to the relation after the final mergers due to the significant accretion that occurs mostly at a separation less than a few kpc. Then, the two MBHs merge with each other.

Development of a training program for the ultrasound screening of placenta accreta spectrum disorders.

To evaluate the impact of a training program using a systematic protocol on ultrasound signs of placenta accreta spectrum (PAS). Intra- and inter-observer variability rates and sensitivity were tested, before and after additional training, by two research fellows with a prior basic training in obstetric ultrasound using digitally recorded second-trimester ultrasound images from cases of anterior placenta previa with and without PAS. Fifty-two cases of anterior placenta previa with PAS (n=26) and without PAS (n=26) were included in the study. The highest level of inter-observer agreement for ultrasound signs was found for the absence of placental bulge and/or focal exophytic mass on gray-scale imaging and the absence of subplacental hypervascularity, bridging vessels and lacunar feeder vessels on color Doppler imaging. The level of inter-observer agreement increased from 39% before training to 40% after training; the numbers agreed as PAS by both trainees increased from four to 20. No cases were classified as inconclusive after training. There was a significant (P<0.001) change in sensitivity for both trainees after training. Additional training in detecting the ultrasound signs associated with PAS using a standardized protocol improves the diagnostic accuracy of operators with only a basic obstetric ultrasound training.

Idiopathic anterior dislocation of the radial head: symptoms, radiographic findings, and management of 8 patients

Radial head dislocation may occur during trauma or in association with congenital diseases, or it may be developmental or idiopathic. Reports of idiopathic dislocation of the radial head have been scarce. The symptoms, radiographic findings, and management of idiopathic dislocation of the radial head have not been well described in the literature. During the past 28 years, we have encountered 8 cases of idiopathic anterior dislocation of the radial head (mean patient age, 12.5 years). In only 1 case did the patientand/or the patient's parents recall any preceding trauma or injury to the affected limb. Patients' complaints included a bulging mass, pain, and limited elbow flexion. Radiographically, the shape of the radial head was flat or slightly convex. Seven of the patients were treated with open reduction of the radial head and angulation osteotomy of the ulna. The other patient's radial head was stabilized without osteotomy. The mean postoperative follow-up period was 4.5 years. In patients whose elbow flexion was limited before surgery, improvement to more than 125° occurred. The bulging mass in the cubital fossa disappeared. None of the patients complained of disability during activities of daily living or sports participation. Radiographically, the radial head remained in the reduced position in all patients in whom open reduction of the radial head with angulation osteotomy of the ulna was performed. We have described the symptoms, radiographic characteristics, and treatment of idiopathic anterior dislocation of the radial head. Open reduction of the radial head combined with angulation osteotomy of the ulna yielded favorable results both clinically and radiographically.

NGC 6388 reloaded: some like it hot, but not too much. New constraints on the first-generation polluters

Multiple stellar populations in globular clusters (GCs) are defined and recognized by their chemical signature. Second-generation stars show the effects of nucleosynthesis in the more massive stars of the earliest component that formed in the first star formation burst. High-temperature H-burning produces the whole pattern of (anti-) correlations in proton-capture elements that are widely found in GCs. However, it is still debated where this burning occurred. Here we introduce new powerful diagnostic plots to detect evidence (if any) of products from proton-capture reactions that occur at very high temperatures. To test these detectors of high-temperature H-burning plots, we show that stringent constraints can be placed on the temperature range of the first-generation polluters that contributed to shaping the chemistry of multiple stellar population in the massive bulge GC NGC 6388. Using the largest sample to date (185 stars) of giants with detailed abundance ratios in a single GC (except ω Cen), we may infer that the central temperature of part of the polluters must have been comprised between ∼100 and ∼150 MK if we consider hydrostatic H-burning in the core of massive stars. A much more narrow range (110−120 MK) is inferred if the polluters can be identified in massive asymptotic giant branch stars.

Müllerian Vaginal Cyst Mimicking Hysterocele

MA¼llerian and Gartner duct cysts are rare embryological remnants of the vaginal wall. Their sizes may vary from one to several centimeters. Dyspareunia, pelvic pain, pressure, bulging mass and urinary incontinence are the most frequent presenting symptoms associated with these vaginal cysts. The purpose of this report is to present a case of hysterocele associated with MA¼llerian vaginal cyst.

The demographics of central massive black holes in low-mass early-type galaxies

AbstractThe existence intermediate mass black holes (IMBH, MBH ≲ 106M⊙) at the centers low-mass galaxies with stellar masses between (1–10)×10M⊙ are key to constraining the origin of black hole (BH) seeds and understanding the physics deriving the co-evolution of central BHs and their host galaxies. However, finding and weighing IMBH is challenging. Here, we present the first observational evidence for such IMBHs at the centers of the five nearest early-type galaxies (D &lt; 3.5 Mpc, ETGs) revealed by adaptive optics kinematics from Gemini and VLT and high-resolution HST spectroscopy. We find that all five galaxies appear to host IMBHs with four of the five having masses below 1 million M⊙ and the lowest mass BH being only ∼7,000 M⊙. This work provides a first glimpse of the demographics of IMBHs in this galaxy mass range and at velocity dispersions &lt; 70 km/s, and thus provides an important extension to the bulge mass and galaxy dispersion scaling relations. The ubiquity of central BHs in these galaxies provides a unique constraint on BH seed formation scenarios, favoring a formation mechanism that produces an abundance of low-mass seed BHs.

Endometriosis of the Appendix

A 51-year-old healthy asymptomatic woman had an index colonoscopy for colorectal cancer screening, which was normal except for a prominent bulging mass at the appendiceal orifice (Figure A). Endoscopic evaluation of the overlying mucosa of the mass appeared normal using high-definition white light imaging, and mucosal biopsies were normal. Contrast-enhanced computed tomography imagines of the pelvis revealed a soft tissue density at the base of the appendix. Laparoscopy was unremarkable, aside from dense periappendiceal adhesions, and adhesiolysis with appendectomy and partial cecectomy was performed.

Reverberation Mapping of the Narrow-line Seyfert 1 Galaxy I Zwicky 1: Black Hole Mass

Abstract We report results of the first reverberation mapping campaign of I Zwicky 1 during 2014–2016, which showed unambiguous reverberations of the broad Hβ line emission in the varying optical continuum. From analysis using several methods, we obtain a reverberation lag of . Taking a virial factor of , we find a black hole mass of from the mean spectra. The accretion rate is estimated to be , suggesting a super-Eddington accretor, where L Edd is the Eddington luminosity and c is the speed of light. By decomposing Hubble Space Telescope images, we find that the stellar mass of the bulge of its host galaxy is . This leads to a black hole to bulge mass ratio of ∼10−4, which is significantly smaller than that of classical bulges and elliptical galaxies. After subtracting the host contamination from the observed luminosity, we find that I Zw 1 follows the empirical relation.

The evolution of SMBH spin and AGN luminosities for z &lt; 6 within a semi-analytic model of galaxy formation

Understanding how Active Galactic Nuclei (AGN) evolve through cosmic time allows us to probe the physical processes that control their evolution. We use an updated model for the evolution of masses and spins of supermassive black holes (SMBHs), coupled to the latest version of the semi-analytical model of galaxy formation GALFORM using the Planck cosmology and a high resolution Millennium style dark matter simulation to make predictions for AGN and SMBH properties for $0 < z < 6$. We compare the model to the observed black hole mass function and the SMBH versus galaxy bulge mass relation at $z=0$, and compare the predicted bolometric, hard X-ray, soft X-ray and optical AGN luminosity functions to observations at $z < 6$, and find that the model is in good agreement with the observations. The model predicts that at $z<2$ and $L_{\mathrm{bol}} < 10^{43} \mathrm{ergs^{-1}}$, the AGN luminosity function is dominated by objects accreting in an Advection Dominated Accretion Flow (ADAF) disc state, while at higher redshifts and higher luminosities the dominant contribution is from objects accreting via a thin disc or at super-Eddington rates. The model also predicts that the AGN luminosity function at $z<3$ and $L_{\mathrm{bol}} < 10^{44} \mathrm{ergs^{-1}}$ is dominated by the contribution from AGN fuelled by quiescent hot halo accretion, while at higher luminosities and higher redshifts, the AGN luminosity function is dominated by the contribution from AGN fuelled by starbursts triggered by disc instabilities. We employ this model to predict the evolution of SMBH masses, Eddington ratios, and spins, finding that the median SMBH spin evolves very little for $0<z<6$.

A new diagnostic for multiple populations: NGC 6388 as a test case

AbstractRecently, the sample size of stars with detailed, homogeneous abundances in the massive bulge Globular cluster NGC 6388 expanded to 185 giants. We use this wealth of data to present first results on its multiple stellar populations. In particular, i) we introduce a new diagnostic plot to survey the occurrence of very high temperature for H-burning in the first-generation polluters, and ii) we pinpoint a restricted temperature range reached by polluters at work in NGC 6388.

Expanding the Sample: The Relationship between the Black Hole Mass of BCGs and the Total Mass of Galaxy Clusters

Abstract Supermassive black holes (BHs) residing in brightest cluster galaxies (BCGs) are overly massive when considering the local relationships between the BH mass and stellar bulge mass or velocity dispersion. Because of the location of these BHs within the cluster, large-scale cluster processes may aid the growth of BHs in BCGs. In this work, we study a sample of 71 galaxy clusters to explore the relationship between the BH mass, stellar bulge mass of the BCG, and the total gravitating mass of the host clusters. Because of difficulties in obtaining dynamically measured BH masses in distant galaxies, we use the Fundamental Plane relationship of BHs to infer their masses. We utilize X-ray observations taken by Chandra to measure the temperature of the intracluster medium, which is a proxy for the total mass of the cluster. We analyze the M BH–kT and M BH–M bulge relationships and establish the best-fitting power laws: = −0.35+2.08 and = −1.09+1.92 . Both relations are comparable with that established earlier for a sample of brightest group/cluster galaxies with dynamically measured BH masses. Although both the M BH–kT and the M BH–M bulge relationships exhibit large intrinsic scatter, on the basis of Monte Carlo simulations, we conclude that dominant fraction of the scatter originates from the Fundamental Plane relationship. We split the sample into cool core and noncool core resembling clusters but do not find statistically significant differences in the M BH–kT relation. We speculate that the overly massive BHs in BCGs may be due to frequent mergers and cool gas inflows onto the cluster center.

Evident black hole-bulge coevolution in the distant universe

ABSTRACT Observations in the local universe show a tight correlation between the masses of supermassive black holes (SMBHs; MBH) and host-galaxy bulges (Mbulge), suggesting a strong connection between SMBH and bulge growth. However, direct evidence for such a connection in the distant universe remains elusive. We have studied sample-averaged SMBH accretion rate ($\overline{\rm BHAR}$) for bulge-dominated galaxies at z = 0.5–3. While previous observations found $\overline{\rm BHAR}$ is strongly related to host-galaxy stellar mass (M⋆) for the overall galaxy population, our analyses show that, for the bulge-dominated population, $\overline{\rm BHAR}$ is mainly related to SFR rather than M⋆. This ${\overline{\rm BHAR}}$–SFR relation is highly significant, e.g. 9.0σ (Pearson statistic) at z = 0.5–1.5. Such a $\overline{\rm BHAR}$–SFR connection does not exist among our comparison sample of galaxies that are not bulge dominated, for which M⋆ appears to be the main determinant of SMBH accretion. This difference between the bulge-dominated and comparison samples indicates that SMBHs only coevolve with bulges rather than the entire galaxies, explaining the tightness of the local MBH−Mbulge correlation. Our best-fitting ${\overline{\rm BHAR}}$–SFR relation for the bulge-dominated sample is ${\log \overline{\rm BHAR}= \log \mathrm{SFR} - (2.48\pm 0.05)}$ (solar units). The best-fitting $\overline{\rm BHAR}/\mathrm{SFR}$ ratio (10−2.48) for bulge-dominated galaxies is similar to the observed MBH/Mbulge values in the local universe. Our results reveal that SMBH and bulge growth are in lockstep, and thus non-causal scenarios of merger averaging are unlikely the origin of the MBH−Mbulge correlation. This lockstep growth also predicts that the MBH−Mbulge relation should not have strong redshift dependence.

Improvement of concomitant symptoms of pelvic organ prolapsed with applied pessary

Introduction: A common disorder among elderly ladies which causes urinary, gastrointestinal, sexual, and local symptoms is pelvic organ prolapse (POP). Two methods that include surgical and non-surgical (conservative) for POP treatment are recommended. Pessary is a advantageous and effective conservative treatment for POP. In this research the purpose was to assess the effect of pessary on concomitant symptoms of POP. Materials and Methods: In this paper randomized clinical trial (before and after), 120 patients had pessary implanted and completed study. In order to evaluate side effects following pessary use, especially urinary symptoms and their type and treatment, primary symptoms’ improvement and patients’ satisfaction were recorded with SPSS software version 17. For this purpose descriptive statistical methods such as abundance, median, ratio, standard deviation were applicated. Paired Samples t-test for quantity comparison before and after data results and for quality comparison intervention before and after data results were also applied using the McNemar Statistical test. A p-value of ≤0.05 was considered to be statistically significant. Results: Complications after embedment pessary occurred in 50.8%, with vaginal infection being the more prevalent and constipation and stress incontinence as the lower prevalent ones. Most complications occurred from the first trimester. Conclusion: Pessary application for improvement of POP accompanied with significant treatment of urinary sign and mass bulging increases the quality of life and patients’ satisfaction. Along with improvement of symptoms, pessary application has limited lower complications, indicative of advantageous and effectiveness of this device.

The Number of Dwarf Satellites of Disk Galaxies versus their Bulge Mass in the Standard Model of Cosmology

Abstract There is a correlation between the bulge mass of the three main galaxies of the Local Group (LG), i.e., M31, Milky Way (MW), and M33, and the number of their dwarf spheroidal galaxies. A similar correlation has also been reported for spiral galaxies with comparable luminosities outside the LG. These correlations do not appear to be expected in standard hierarchical galaxy formation. In this paper, and for the first time, we present a quantitative investigation of the expectations of the standard model of cosmology for this possible relation using a galaxy catalog based on the Millennium-II simulation. Our main sample consists of disk galaxies at the centers of halos with a range of virial masses similar to M33, MW, and M31. For this sample, we find an average trend (though with very large scatter) similar to that observed in the LG; disk galaxies in heavier halos on average host heavier bulges and a larger number of satellites. In addition, we study sub-samples of disk galaxies with very similar stellar or halo masses (but spanning a range of 2–3 orders of magnitude in bulge mass) and find no obvious trend in the number of satellites versus bulge mass. We conclude that, while for a wide galaxy mass range a relation arises (which seems to be a manifestation of the satellite number–halo mass correlation), for a narrow range there is no relation between number of satellites and bulge mass in the standard model. Further studies are needed to better understand the expectations of the standard model for this possible relation.

Prolonged Obstructed Labor Is an Uncommon Presentation of a Giant Bladder Calculus: A Case Report and Literature Review

Prolonged obstructed labor is a critical intrapartum emergency. This intricacy is, however, unusual as a primary presentation of a giant bladder calculus. We report a case of a 25-year-old Para 6 + 1, who presented with a history of labor pains of 72 hours duration. She had background lower urinary tract symptoms with supra-pubic swelling and hematuria of 2 years duration. She had a single antenatal visit at 32 weeks however; no obstetric ultrasound scan was done before she went into labor. Examination revealed a highly placed fetal head with increase fetal heart rate. There was a hard mass bulging under the anterior vaginal wall. The diagnosis was a prolonged obstructed labor secondary to bladder mass with fetal distress was made. She had a caesarean section (CS) with the delivery of fresh stillborn. The bi-manually palpable bladder mass persisted post-CS. Her abdominopelvic ultrasound scan and abdominal X-ray post-CS revealed giant vesical calculus with obstructive uropathy. Urine microscopy culture and sensitivity yielded E. coli sensitive to Ciprofloxacin; other laboratory investigations were normal. She was treated for UTI and 2 weeks post-CS, she had opened cystolithotomy. The stone weighed 536 g. Her postoperative recovery was uneventful.

Extraordinary Bulging Mass in the Foetus - A Case Report of Bladder Exstrophy

Abstract INTRODUCTION: Prenatal diagnosis of bladder exstrophy is extremley rare and difficult. BACKGROUND: Due to abnormal development of the cloacal membrane there is an incomplete closure of the lower abdominal wall, absence of the anterior wall of the bladder and external exposition of the posterior wall. The pubic bones are usually separated, the umbilical cord low inserted and there is abnormal external genitalia development. CASE REPORT: At 21st week of gestation of 39-year-old multigravida multipara referred by a primary care obstetrician to high-specialised centre for a detailed ultrasound examination with a suspicion of bladder absence and inferior umbilical localisation. At 29 weeks of gestation presence of bulging mass of 2 cm, between the umbilical outlet and labia was detected. At 31 weeks of gestation previously detected structure among thighs had 3 cm diameter with lateral umbilical outlet. Major labia were prominent and minor labia were within normal limits. Between two umbilical arteries with an appropriate intraabdominal course there were no transsonic area corresponding to the urinary bladder. The newborn baby was born at term in a good condition, but with an exposed bladder of 4 cm in diameter. The urethral outlet was not visualised and the female genitals were abnormal. After a month the girl underwent primary bladder exstrophy closure. Although she suffers from recurring urinary tract infections, she is in a good general condition. CONCLUSIONS: Due to prenatal diagnostics it was possible to detect and make an initial diagnosis of severe malformation. Early diagnosis allowed to prepare parents for a newborn with a defect and teach them how to take care of the baby.

SDSS-IV MaNGA: The Roles of AGNs and Dynamical Processes in Star Formation Quenching in Nearby Disk Galaxies

Abstract We study how star formation (SF) is quenched in low-redshift disk galaxies with integral-field spectroscopy. We select 131 face-on spiral galaxies with stellar mass greater than 3 × 1010 M ⊙, and with spatially resolved spectrum from MaNGA DR13. We subdivide the sample into four groups based on the offset of their global specific star formation rate (SFR) from the star-forming main sequence and stack the radial profiles of stellar mass and SFR. By comparing the stacked profiles of quiescent and star-forming disk galaxies, we find that the decrease of the global SFR is caused by the suppression of SF at all radii, but with a more significant drop from the center to the outer regions following an inside-out pattern. As the global specific SFR decreases, the central stellar mass, the fraction of disk galaxies hosting stellar bars, and active galactic nuclei (AGNs; including both LINERs and Seyferts) all increase, indicating dynamical processes and AGN feedback are possible contributors to the inside-out quenching of SF in the local universe. However, if we include only Seyferts, or AGNs with EW(Hα) &gt; 3 Å, the increasing trend of AGN fraction with decreasing global sSFR disappears. Therefore, if AGN feedback is contributing to quenching, we suspect that it operates in the low-luminosity AGN mode, as indicated by the increasing large bulge mass of the more passive disk galaxies.

Prevalence of Sonographic Markers of Placenta Accreta Spectrum in Low-Risk Pregnancies.

This study was aimed to evaluate the prevalence of sonographic markers for placenta accreta spectrum (PAS) in pregnancies at low-risk for PAS. Pregnant women at low-risk for PAS presenting for routine second trimester ultrasound who enrolled in the study were evaluated prospectively for sonographic markers of PAS during two ultrasounds at 18 to 24 and 28 to 34 weeks. Frequencies of PAS markers were compared between the second and third trimester and between those with and without prior cesarean deliveries (CD). Overall, 174 women were included. Several markers were seen frequently in the second trimester: vascular cervical invasion (57%), lacunae (46%), subplacental hypervascularity (37%), and irregularity of the posterior bladder wall (37%). Other markers were seen infrequently or not at all: loss of the retroplacental clear zone, uterovesical interface < 1 mm, bridging vessels, placental bulge or focal exophytic mass. Frequencies of markers did not differ between women with and without prior CD. Lacunae were larger and more numerous in the third trimester. Two or more PAS markers were observed in 98% of second trimester ultrasounds. Several PAS sonographic markers occur commonly in low-risk pregnancies. In the absence of risk factors, the independent predictive value of these markers is questionable.