Recent Merger Research Articles

An intriguing coincidence between the majority of vast polar structure dwarfs and a recent major merger at the M31 position

A significant part of the Milky Way (MW) dwarf galaxies orbit within a Vast POlar Structure (VPOS), which is perpendicular to the Galactic disc and whose origin has not yet been identified. It includes the Large Magellanic Cloud (LMC) and its six dynamically associated dwarf galaxies. Andromeda Galaxy (M31) experienced a major merger two to three billion years ago, and its accurate modelling predicts that an associated tidal tail is pointing towards the Galaxy. Here, we tested a possible association between M31 tidal tail particles and MW dwarf galaxies, focusing first on the LMC and its associated dwarfs since they are less affected by ram pressure. We traced back these dwarf galaxy orbits by one billion years and calculated their association with the tidal tail particles in the 6D phase space, based on their proper motion from Gaia DR3. We find that for low-mass MW models (total mass less than 5 × 1011 M⊙), the separation in the 6D space can be less than 1σ for most of the M31 modelling, albeit with a significant degree of freedom due to the still unknown proper motion of M31. We further discover that many other dwarfs could also be associated with the M31 tidal tails if their motions had been radially slowed, as expected from the ram pressure exerted by the MW corona. This intriguing coincidence could explain the origin of the VPOS, which resulted from a matter exchange between M31 and MW.

Embracing Change Through Team Diversity: The Impact of Age Diversity on Civil Servants’ Perceptions of Organizational Change

This study explores the influence of age diversity within teams on civil servants’ perceptions of organizational change. Age diversity is examined through two dimensions: age variety, which refers to the range of different ages within a team, and age polarization, which denotes the extent to which age groups are segregated or clustered within a team. Individual perceptions of change are based on how civil servants evaluated a recent merger. While age polarization shows a significant effect—with less polarized teams exhibiting more positive perceptions of the merger—age variety does not demonstrate a notable impact. These results highlight that while age diversity is important, its impact is nuanced: simply having a range of ages is not sufficient, but reducing age polarization is crucial.

A Case Study of Financial Integration in Cross-Border Mergers and Acquisitions

This paper focuses on the financial integration strategies used by Microsoft and Tesla in recent cross-border mergers and acquisitions (M&As), with a particular focus on their acquisitions of Nuance Communications and Maxwell Technologies, respectively, and analyzes and highlights the importance of strategic financial integration in achieving synergies, managing goodwill, and navigating regulatory and cultural complexities. For Microsoft, the acquisition of Nuance was intended to enhance its artificial intelligence capabilities in healthcare and enterprise services, while Tesla's acquisition of Maxwell was intended to secure a key technological advantage in electric vehicle (EV) battery production. In addition, both companies faced a range of challenges in aligning financial systems, managing cost structures, and ensuring compliance with international regulatory standards. Drawing on relevant literature to contextualize the case studies, this paper discusses how such companies conducted financial integration and how their experiences may impact future cross-border M&A transactions. The findings suggest that financial integration is critical to maximizing value in cross-border M&As, and that effective management of this process plays an important role in the long-term success of the firm.

Cloud-scale elemental abundance variations and the CO-to-dust-mass conversion factor in M31

Abstract From a spectroscopic survey of candidate H ii regions in the Andromeda galaxy (M31) with MMT/Hectospec, we have identified 294 H ii regions using emission line ratios and calculated elemental abundances from strong-line diagnostics (values ranging from sub-solar to super-solar) producing both Oxygen and Nitrogen radial abundance gradients. The Oxygen gradient is relatively flat, while the Nitrogen gradient is significantly steeper, indicating a higher N/O ratio in M31’s inner regions, consistent with recent simulations of galaxy chemical evolution. No strong evidence was found of systematic galaxy-scale trends beyond the radial gradient. After subtracting the radial gradient from abundance values, we find an apparently stochastic and statistically significant scatter of standard deviation 0.06 dex, which exceeds measurement uncertainties. One explanation includes a possible collision with M32 200 - 800 Myrs ago. Using the two-point correlation function of the Oxygen abundance, we find that, similar to other spiral galaxies, M31 is well-mixed on sub-kpc scales but less so on larger (kpc) scales, which could be a result of an exponential decrease in mixing speed with spatial scale, and the aforementioned recent merger. Finally, the MMT spectroscopy is complemented by a dust continuum and CO survey of individual Giant Molecular Clouds, conducted with the Submillimeter Array. By combining the MMT and SMA observations, we obtain a unique direct test of the Oxygen abundance dependence of the α′(12CO) factor which is crucial to convert CO emission to dust mass. Our results suggest that within our sample there is no trend of the α′(12CO) with Oxygen abundance.

MeerKAT discovery of a MIGHTEE Odd Radio Circle

ABSTRACT We present the discovery of a new Odd Radio Circle (ORC J0219−0505) in 1.2 GHz radio continuum data from the MIGHTEE survey taken with the MeerKAT telescope. The radio-bright host is a massive elliptical galaxy, which shows extended stellar structure, possibly tidal tails or shells, suggesting recent interactions or mergers. The radio ring has a diameter of 35 arcsec, corresponding to 114 kpc at the host galaxy redshift of $z_{\rm spec} = 0.196$. This MIGHTEE ORC is a factor 3–5 smaller than previous ORCs with central elliptical galaxies. The discovery of this MIGHTEE ORC in a deep but relatively small-area radio survey implies that more ORCs will be found in deeper surveys. While the small numbers currently available are insufficient to estimate the flux density distribution, this is consistent with the simplest hypothesis that ORCs have a flux density distribution similar to that of the general population of extragalactic radio sources.

Unveiling the shape: A multi-wavelength analysis of the galaxy clusters Abell 76 and Abell 1307

We analyse the dynamical state of the galaxy clusters Abell 76 and Abell 1307 from the optical point of view, presenting a coherent scenario that responds to the X-ray emissions observed in these structures. Our study is based on 231 and 164 spectroscopic redshifts, for the clusters A76 and A1307, respectively, obtained mostly with the Telescopio Nazionale Galileo, and complemented with others collected from the SDSS DR16 spectroscopic database and the literature. We find that A76 and A1307 are two galaxy clusters at z = 0.0390 and 0.0815, respectively, with a velocity dispersion of 650 ± 56 km s−1 and 863 ± 85 km s−1, and they show velocity distributions following, in practice, Gaussian profiles. From our dynamical analysis, X-ray studies and SZ-Planck emission, we obtain a mean total mass M500 = 1.7 ± 0.6 ⋅ 1014 M⊙ and 3.5 ± 1.3 ⋅ 1014 M⊙ for A76 and A1307, respectively. Using the SDSS DR16 photometric database, we find that the spatial distribution of likely cluster members in the case of A76 is very anisotropic, while A1307 shows a compact distribution of galaxies, but it is double peaked and elongated in the south-north direction. Using XMM-Newton X-ray data, we compared the surface brightness maps with galaxy distributions and noticed that both distributions are correlated. We reconstructed the total mass profile and velocity anisotropy of both clusters by analysing the full projected phase space, through the MG-MAMPOSSt code. Our study reveals a slight indication of radial orbits for A76, while A1307 seems to prefer more isotropic orbits in the whole cluster range. In summary, A76 represents a typical young cluster, in an early stage of formation, with a very low X-ray surface brightness but a high temperature showing a very anisotropic galaxy distribution. A1307 is however more consolidated and massive showing in-homogeneous galaxy distribution and an asymmetric X-ray emission, which suggest a scenario characterised by recent minor mergers.

Market concentration of the Brazilian hospital medical supplementary health system

BackgroundThe Brazilian supplementary health market has undergone transformations in recent years due to constant mergers and acquisitions of by large corporations, contributing to the increase in market concentration, especially in the poorest and least developed regions of the country. Thus, given the care it provides and its economic relevance, understanding the fundamentals of these movements, the likely consequences and trends for the health market are relevant, important, and strategic.ObjectiveTo understand the general and specific context of Brazilian supplementary health, its scenarios, and trends, with emphasis on the analysis of market concentration and recent mergers and acquisitions.MethodologyThe research is applied, descriptive and exploratory and uses secondary data from various sources, submitted to quantitative data analysis methods. The data are organized into three groups: historical and regulatory documents; industry data; and market.ResultsThe results show the growing concentration of the market promoted by large publicly traded corporations, the growing relevance of tech startups on the healthcare landscape, the predominant use of the relative valuation model, with implicit multiples for asset pricing and the prevalence of corporate health plans.ConclusionThe growing concentration of the system projects a market with fewer options and less competitiveness, since the growth of large operators is evident, in addition to the relevant increase in the number of complaints from users of the system, which signals the growing gap between the expectations of users and the levels of quality care offered. The study also highlights the predominance of corporate health plans, revealing the direct relationship between access to supplementary health services and employability rates. The analysis of M&A operations, in addition to the increase in market concentration, reveals the prevalence of the use of the relative valuation model and implicit multiples for the pricing of traded assets. This denotes the future expectation of wealth generation, at least equivalent to the historical series of the sector, on the part of investors, whose frustration may signal the decreasing attractiveness of resources and M&A operations in the sector in the coming years.

An Analytical Study on Account Holders' Perceptions and Satisfaction with reference to Banking Service Quality Post Merger of selected Public Sector Bank in India

Public Sector Banks in India have undergone significant mergers, which enable them to expand their activities, develop further, and strengthen their position as a key sector in the economy. Despite challenges such as rising non-performing assets, increasing frauds, political interference, and favouritism, mergers and acquisitions are graceful to benefit the newly formed banks, the economy, and the industry as a whole. This study examines the impact of recent bank mergers on customer awareness, perceptions, and satisfaction levels, focusing on four major public sector banks: Bank of Baroda, Canara Bank, Union Bank of India, and Indian Bank. Data were collected using structured questionnaires and personal interviews, incorporating 16 variables measured on a five-point Likert scale. The reliability of the data was confirmed with a Cronbach's Alpha value of 0.816, indicating high internal consistency. Analysis using One-Way ANOVA and descriptive statistics revealed significant variations in service quality perceptions across different age groups and bank affiliations, while awareness, digital banking, product/service efficiency, and trust/confidence showed consistent perceptions. The study highlights the positive reception of technological improvements post-merger and provides insights for banks to tailor their communication and service strategies to different customer demographics.

The Most Massive Early-type Galaxies Exhibit Tidal Features More Frequently in Lower-density Environments

The most massive early-type galaxies (ETGs) are known to form through numerous galaxy mergers. Thus, it is intriguing to study whether their formation in low-density environments, where nearby companions are almost absent, is associated with mergers, which are directly traced by tidal features. Using the 436 most massive ETGs with M star > 1011.2 M ⊙ at z < 0.04, we determine the variation in the fraction of massive ETGs with tidal features (f T ) across different environments and verify whether the most massive ETGs commonly have tidal features in very low density environments. Our main discovery is that the most massive ETGs exhibit tidal features more frequently in lower-density environments. In the highest-density environments, like galaxy clusters, f T is 0.21 ± 0.06, while in the lowest-density environments it triples to 0.62 ± 0.06. This trend is stronger for more extremely massive ETGs, with f T reaching 0.92 ± 0.08 in the lowest-density environments. One explanation for our finding is that the most massive ETGs in lower-density environments have genuinely experienced recent mergers more frequently than their counterparts in higher-density environments, suggesting that they possess extended formation histories that continue into the present. Another possibility is that tidal features last shorter in denser environments owing to external factors inherent in these environments. Our additional findings that massive ETGs with bluer u − r colors are a more dominant driver of our main discovery and that dust lanes are more commonly observed in massive ETGs in low-density environments imply that gas-abundant mergers primarily contribute to the increased rate of recent mergers in low-density environments.

Anatomy of the Star Formation in a Tidally Disturbed Disk Galaxy: NGC 3718

We present a UV, optical, and near-IR study of the star-forming complexes in the nearby peculiar galaxy NGC 3718, using Ultraviolet Imaging telescope, Galaxy Evolution Explorer, Spitzer, and DECam Legacy Survey imaging data. The galaxy has a disturbed optical morphology owing to the multiple tidal arms, the warped disk, and the prominent curved dust lanes, but in the near-IR it appears to be a bulge-dominated galaxy. Its disturbed morphology makes it an excellent case to study star formation in a tidally disturbed galaxy that may have undergone a recent minor merger. To study the distribution and properties of the star-forming clumps (SFCs), we divided the galaxy within the R 25 (B band) radius into three parts—the upper, central, and lower regions. Using the UV band images, we investigated the warped star-forming disk, the extended tidal arms, and the distribution and sizes of the 182 SFCs. Their distribution is 49, 60, and 73 in the galaxy’s upper, central, and lower regions, respectively. We determined the UV color, star formation rates (SFRs), star formation density (ΣSFR), and ages of the SFCs. The central disk of the galaxy has a larger mean ΣSFR that is ∼3.3 and ∼1.6 times higher than the upper and lower regions, respectively. We also find that the SFCs in the central disk are older than those in the tidal arms. Our study thus shows that minor mergers can trigger the inside-out growth of galaxy disks, where the younger SFCs are in outer tidal arms and not in the inner disk.

JP Morgan Chase

The following research has been based on the company profile and capital structure of JP Morgan. The notion was to analyze and find the fault lines for a potential employer. In this research, it has been clear that the brand name and reputation of JPM acts as a strong influence over the market. However, because of the economic meltdown in the market, the total debt to equity ratio and cost of capital has drifted away from the ideal value. It was analyzed that SVA model is more appropriate for analyzing the performance of the shareholders as well as the organizational structure of the company. The recent and potential merger and acquisitions are analyzed and thus far a potential synergy is established between Viacom and JPM. The discussion of HRM as well as other sectoral review also substantiate dif erent the assertions made in the report

New Observational Recipes for Measuring Dynamical States of Galaxy Clusters

During cluster assembly, a cluster’s virialization process leaves behind signatures that can provide information on its dynamical state. However, no clear consensus yet exists on the best way to achieve this. Therefore, we attempt to derive improved recipes for classifying the dynamical states of clusters in observations using cosmological simulations. The cluster halo mass and their subhalos’ mass are used to 1014 M ⊙ h −1 and 1010 M ⊙ h −1 to calculate five independent dynamical state indicators. We experiment with recipes by combining two to four indicators for detecting specific merger stages, like recent and ancient mergers. These recipes are made by plotting merging clusters and a control sample of relaxed clusters in multiple-indicator parameter space, then applying a rotation matrix method to derive the best way to separate mergers from the control sample. The success of the recipe is quantified using the success rate and overlap percentage of the merger and control histograms along the newly rotated x-axis. This provides us with recipes using different numbers of combined indicators and for different merger stages. Among the recipes, the stellar mass gap and center offset are the first and second most dominant of the indicators, and using more indicators improves the effectiveness of the recipe. When applied to observations, our results show good agreement with literature values of cluster dynamical states.

Evidence builds for recent merger

Evidence builds for recent merger

Structure and Kinematics of Star-forming Elliptical Galaxies in SDSS-MaNGA

Using “spatially” resolved spectroscopy, we investigated the characteristics and different modes of formation of stars in elliptical galaxies. We identified an unusual population of 59 star-forming elliptical (SF-E) galaxies in SDSS-MaNGA, our primary sample. To identify these rare star-forming ellipticals, we combined GSWLC-A2 containing outputs of stellar population synthesis models with morphological results from the deep-learning catalog and resolved and integrated properties from the MaNGA Pipe3D value-added catalog. We have also constructed two control samples of star-forming spirals (SF-Sps; 2419 galaxies) and quenched ellipticals (Q-Es; 684 galaxies) to compare with our primary sample of SF-Es. Hα emission line flux of SF-Es is similar to spiral galaxies. The D4000 spectral index indicates that SF-Es have a mixture of old and young stellar populations. Mass-weighted stellar age and metallicity for the SF-Es are lower than the Q-Es and 67% of stellar- and gas-velocity maps of the primary sample show signs of kinematic disturbance. All of these indicate that SF-Es have acquired metal-poor gas through recent mergers or interactions with other galaxies and are forming a new generation of stars. Further, we subdivide our primary sample of SF-Es into four classes based on their bulge to total luminosity ratio (B/T) and spin parameter λre . These four classes have their distinct evolutionary history and modes of formation. Based on these results, we suggest that the Hubble diagram does not accurately capture galaxy evolution processes, and we need a revised morphology diagram like the comb morphology diagram to get a complete picture of the galaxy evolution processes.

Devouring the Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus

For the first time, systematic studies of dwarf galaxies are being conducted throughout the Local Volume, including the dwarf satellites of the nearby giant elliptical galaxy Centaurus A (NGC 5128). Given Centaurus A's mass (roughly 10 times larger than that of the Milky Way), AGN activity, and recent major mergers, investigating the dwarf galaxies of Centaurus A and their star formation physics is imperative. However, simulating the faintest dwarfs around a galaxy of Centaurus A's mass with sufficient resolution in a hydrodynamic simulation is computationally expensive and currently infeasible. In this study, we seek to reproduce the properties of Centaurus A dwarfs using the semianalytic model Galacticus to model dwarfs within a 700 kpc region around Centaurus A, corresponding approximately to its splashback radius. We investigate the effects of host halo mass and environment and predict observable properties of Centaurus A dwarfs using astrophysical prescriptions and parameters previously tuned to match properties of the Milky Way’s satellite galaxies. This approach allows us to approximately replicate cumulative luminosity functions, and luminosity–metallicity and luminosity–half-light-radii relations observed in the Centaurus A satellites. We provide predictions for the velocity dispersions, and star formation histories of Centaurus A dwarfs. The agreement between our predicted star formation histories for Centaurus A dwarfs and those of the Milky Way dwarfs implies the presence of universal processes governing star formation in dwarf galaxies. Overall, our findings shed light on the star formation physics of dwarf galaxies in the Centaurus A system, revealing insights into their properties and dependence on the host environment.

Imprints of the internal dynamics of galaxy clusters on the Sunyaev–Zeldovich effect

Context. Forthcoming measurements of the Sunyaev–Zeldovich (SZ) effect in galaxy clusters will dramatically improve our understanding of the main intra-cluster medium (ICM) properties and how they depend on the particular thermal and dynamical state of the associated clusters. Aims. Using a sample of simulated galaxy clusters, whose dynamical history can be well known and described, we assess the impact of the ICM internal dynamics on both the thermal and kinetic SZ effects (tSZ and kSZ, respectively). Methods. We produced synthetic maps of the SZ effect, both thermal and kinetic, for the simulated clusters obtained in a cosmological simulation produced by a cosmological adaptive mesh refinement code. For each galaxy cluster in the sample, its dynamical state is estimated by using a combination of well-established indicators. We used the correlations between SZ maps and cluster dynamical state to look for the imprints of the evolutionary events, mainly mergers, on the SZ signals. Results. While the tSZ effect only shows dependency on dynamical state in its radial distribution, the kinetic effect shows a remarkable correlation with this property: unrelaxed clusters present a higher radial profile and an overall stronger signal at all masses and radii. The reason for this correlation is the fuzziness of the ICM produced by recent merging episodes. Furthermore, the kSZ signal is correlated with rotation for relaxed clusters, while for the disturbed systems, the effect is dominated by other motions such as bulk flows, turbulence, and so on. The kSZ effect shows a dipolar pattern when averaging over cluster dynamical classes, especially for the relaxed population. This feature can be exploited to stack multiple kSZ maps in order to recover a stronger dipole signal that would be correlated with the global rotation properties of the sample. Conclusions. The SZ effect can be used as a tool to estimate the dynamical state of galaxy clusters, especially to segregate those clusters with a quiescent evolution from those with a rich record of recent merger events. Our results suggest that the forthcoming observational data measuring the SZ signal in clusters could be used as a complementary strategy for classifying the evolutionary history of galaxy clusters.

A Study and Analysis on Recent Mergers in India

This research paper aims to provide a comprehensive study and analysis of recent merger and demerger activities in India. It examines the motivations, strategies, and impacts of mergers and demergers on the Indian corporate landscape. Through a detailed analysis of recent case studies, the paper delves into the key factors driving these corporate restructuring activities, including regulatory changes, market dynamics, and strategic imperatives. Additionally, it evaluates the financial performance, market reactions, and implications for stakeholders involved in such transactions. The research contributes to the understanding of the merger and demerger trends in India, offering insights into the evolving corporate strategies and their implications for the Indian economy. Furthermore, it explores the legal and regulatory framework surrounding mergers and demergers, providing a holistic view of the process and its challenges.

A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies

We study the global kinematics of the Perseus galaxy cluster (A426) at redshift z = 0.017 using a large sample of galaxies from our new MMT/Hectospec spectroscopic observation for this cluster. The sample includes 1447 galaxies with measured redshifts within 60′ from the cluster center (1148 from this MMT/Hectospec program and 299 from the literature). The resulting spectroscopic completeness is 67% at r-band apparent magnitude r Petro,0 ≤ 18.0 within 60′ from the cluster center. To identify cluster member galaxies in this sample, we develop a new open-source Python package, CausticSNUpy. This code implements the algorithm of the caustic technique and yields 418 member galaxies within 60′ of the cluster. We study the cluster using this sample of member galaxies. The cluster shows no significant signal of global rotation. A statistical test shows that the cluster does not have a noticeable substructure within 30′. We find two central regions where the X-ray-emitting intracluster medium and galaxies show significant velocity differences (>7σ). On a large scale, however, the overall morphology and kinematics between the intracluster medium and galaxies agree well. Our results suggest that the Perseus cluster is a relaxed system and has not experienced a recent merger.

IMPACT OF BANK MERGER ON NSE NIFTY: A CASE STUDY ON MERGING OF BANKS IN 2020

Narasimham Committee in the late 1990s recommended consolidation through a process of merging of strong banks. The Committee recommended the closure of the banks those are weaker in comparison to other banks, instead of merging them. The biggest positive aspect of the merging of banks will lead to the formation of banks of scale. There are a large number of banks which are of very small in size in terms of global standards &amp; their growth is restricted by their inability to expand. India needs more global level banks to face global competitiveness. The recent merging of the banks were aimed at addressing this problem. The announcement of merging of the banks by Finance Minister Nirmala Sitharaman on 30/08/2019, raised the expectation that it would be the most significant event that the country has witnessed since nationalization. The intention to create banks that could compete with the banks of global level &amp; would also serve the needs of a $ 5 trillion economy by 2025. Keeping in view the above intentions, Finance Minister, Nirmala Sitharaman, declared the merging of ten public sector banks into four entities to improve their liquidity, tackling the issues of non performing assets &amp; risk diversification. The present paper aims to explore the impact of the merging of the Banks on NSE Nifty, with respect to Stock returns, Volume of share trading &amp; Volume of share turnover.

Genetic characterization of a captive marmoset (Callithrix jacchus) colony using genotype-by-sequencing.

The marmoset is a fundamental nonhuman primate model for the study of aging, neurobiology, and many other topics. Genetic management of captive marmoset colonies is complicated by frequent chimerism in the blood and other tissues, a lack of tools to enable cost-effective, genome-wide interrogation of variation, and historic mergers and migrations of animals between colonies. We implemented genotype-by-sequencing (GBS) of hair follicle derived DNA (a minimally chimeric DNA source) of 82 marmosets housed at the Southwest National Primate Research Center (SNPRC). Our primary goals were the genetic characterization of our marmoset population for pedigree verification and colony management and to inform the scientific community of the functional genetic makeup of this valuable resource. We used the GBS data to reconstruct the genetic legacy of recent mergers between colonies, to identify genetically related animals whose relationships were previously unknown due to incomplete pedigree information, and to show that animals in the SNPRC colony appear to exhibit low levels of inbreeding. Of the >99,000 single-nucleotide variants (SNVs) that we characterized, >9800 are located within gene regions known to harbor pathogenic variants of clinical significance in humans. Overall, we show the combination of low-resolution (sparse) genotyping using hair follicle DNA is a powerful strategy for the genetic management of captive marmoset colonies and for identifying potential SNVs for the development of biomedical research models.