Small Halos Research Articles

Time delay of light in the gravitational lensing of supermassive black holes in dark matter halos

AbstractThe dark matter halo has non-negligible effects on the gravitational lensing of supermassive black hole in the galaxy center. Our work presents a study on the time-delay of light in gravitational lensing of black holes enclosed by dark matter halos. To provide a precise description on the distribution of dark matter in galaxies, we choose several famous phenomenological dark matter halo models in astrophysics, including the NFW, Beta, Burkert and Moore models, to carry out the present study. Through numerically calculating the time-delay of light in gravitational lensing, a comparative analysis of the dark matter effects within different halo models has been performed. Assuming typical length scales associated with the galactic gravitational lensing, numerical results indicate that the NFW, Beta, Burkert and Moore dark matter halos can significantly enhance the time delay of light in gravitational lenisng of central supermassive black holes. The enhancing effect becomes more pronounced with a small dark matter halo scale and an increasing dark matter halo mass.

Lower dose radiotherapy did not alter cardiac function and was not pro-arrhythmic: results of the small prospective HALO trial

Abstract Background Stereotactic arrhythmia radiotherapy (STAR) is a highly promising bail-out treatment for patients with therapy-refractory ventricular tachycardia (VT). Despite precise, noninvasive targeting of the pro-arrhythmic area, surrounding healthy cardiac tissue inadvertently receives low-dose radiation. There is a historical notion that collateral cardiac damage from radiation of extra-cardiac structures can cause heart failure and arrhythmias. In the HALO trial, where non-small cell lung cancer (NSCLC) patients treated with stereotactic ablative radiotherapy (SABR) received relatively low-dose radiotherapy to the heart, detailed cardiac safety after radiotherapy was therefore evaluated. Objective The aim of this study was to prospectively evaluate cardiac function after collateral radiotherapy on the heart in patients with NSCLC treated with SABR. Methods The HALO trial was a prospective observational trial evaluating cardiac adverse effects in patients treated with SABR for early stage NSCLC. Patients with a tumour within 3cm of the pericardium were eligible to participate. The mean radiotherapy dose per segment was calculated by semi-automated angulation and segmentation using an in-house developed tool. The heart was segmented according to the AHA 17-segment model. Patients underwent cardiac magnetic resonance imaging (CMR) pre-treatment, 3 and 12 months after treatment. CMR strain-analysis was conducted by two independent observers using cvi42 software. Longitudinal, radial and circumferential strain were measured both globally and segmentally and evaluated for dose-dependent effects. Results Ten patients were included in this study. Two patients dropped out before first follow-up and were not included in this analysis. Median age was 66 years (range 58-81) and four were male (50%). Median distance between the tumour and pericardium was 0.46cm (range 0.00-2.80). Patients were treated with 8 fractions of 7.0-7.5 Gy (n=6), 5 fractions of 11.0 Gy (n=1) or 3 fractions of 18.0 Gy (n=1). Median global cardiac radiotherapy dose was 6.7 Gy (range 0.1-17.9). Pre-treatment, median left ventricular ejection fraction as measured on CMR was 65% (range 40-75), global longitudinal strain was -15% (-20 - -9), global circumferential strain was -17% (-26 - -9) and global radial strain was 28% (11-60). These did not significantly change comparing 3 months and 12 months after treatment with pre-treatment. As can be appreciated from Table 1, there were no dose-dependent effects on segmental longitudinal, radial and circumferential strain both 3 months or 12 months after SABR. There were no ventricular arrhythmias observed during follow-up. Conclusion In this small study, collateral radiotherapy in patients with NSCLC treated with SABR did not significantly alter cardiac function as measured on CMR, and no relevant pro-arrhythmic effects were observed during short term follow-up. Extending the research into a larger dataset is warranted.

Three-dimensional stellar orbits due to off-centered dark matter halo at the center of the disc galaxies

Stellar orbits and the evolution of galaxies are intertwined processes that have long-term implications on each other. This paper studies how stellar orbits at the galaxy’s central region are disturbed by an asymmetric dark matter halo potential. Evidence from the observations and simulations in the Milky Way type galaxy suggests that the center of the dark matter halo could be off-centered by a few parsecs concerning the center of the core. The equations of motion of stars in the core of galaxies are expressed in terms of three-dimensional perturbed potential arising from the offset halo. The central region’s azimuthal variation in the effective potential is obtained and the first-order epicyclic theory is used to solve for the orbits. The magnitude of this perturbation potential grows at small radii and exhibits m=1 azimuthal fluctuations. In the central region, within 3 kpc radius, even a small halo offset of 300 pc can cause a surprisingly strong spatial and kinematical lopsidedness. A planar orbit, initially assumed to be in disc plane, tends to leave the plane giving rise to non-planar configuration. Furthermore, as long as the halo offset persists, the central region will stay lopsided. The dark matter halo would significantly impact the dynamic development of this region and could help fuel the active galactic nucleus.

Fast forward modelling of galaxy spatial and statistical distributions

A forward modelling approach provides simple, fast and realistic simulations of galaxy surveys, without a complex underlying model. For this purpose, galaxy clustering needs to be simulated accurately, both for the usage of clustering as its own probe and to control systematics. We present a forward model to simulate galaxy surveys, where we extend the Ultra-Fast Image Generator to include galaxy clustering. We use the distribution functions of the galaxy properties, derived from a forward model adjusted to observations. This population model jointly describes the luminosity functions, sizes, ellipticities, SEDs and apparent magnitudes. To simulate the positions of galaxies, we then use a two-parameter relation between galaxies and halos with Subhalo Abundance Matching (SHAM). We simulate the halos and subhalos using the fast PINOCCHIO code, and a method to extract the surviving subhalos from the merger history. Our simulations contain a red and a blue galaxy population, for which we build a SHAM model based on star formation quenching. For central galaxies, mass quenching is controlled with the parameter Mlimit, with blue galaxies residing in smaller halos. For satellite galaxies, environmental quenching is implemented with the parameter tquench, where blue galaxies occupy only recently merged subhalos. We build and test our model by comparing to imaging data from the Dark Energy Survey Year 1. To ensure completeness in our simulations, we consider the brightest galaxies with i < 20. We find statistical agreement between our simulations and the data for two-point correlation functions on medium to large scales. Our model provides constraints on the two SHAM parameters Mlimit and tquench and offers great prospects for the quick generation of galaxy mock catalogues, optimized to agree with observations.

Diffuse Light in Milky Way–like Haloes

We investigate the diffuse light (DL) content of dark matter haloes in the mass range 11.5≤logMhalo≤13 , a range that also includes the dark matter halo of the Milky Way, taking advantage of a state-of-the-art semianalytic model run on the merger trees extracted from a set of high-resolution cosmological simulations. The fraction of DL in such relatively small haloes is found to progressively decrease from the high- to the low-mass end, in good agreement with analytic and numerical results from simulations, and in good agreement also with the fraction of the DL observed in the Milky Way and M31. Haloes with different masses have different efficiencies in producing DL: logMhalo≃13 is found to be the characteristic halo mass where the production of DL is the most efficient, while the overall efficiency decreases at both larger and smaller scales (this work). The DL content in this range of halo mass is the result of stellar stripping due to tidal interaction between satellites and their hosts (95%) and mergers between satellites and the central galaxy (5%), with preprocessed material, a subchannel of mergers and stripping, and so already included in the 100%, that contributes no more than 8% on average. The halo concentration is the main driver of the DL formation: more concentrated haloes have higher DL fractions that come from the stripping of more massive satellites in the high-halo-mass end, while dwarfs contribute mostly in the low-halo-mass end.

DARK MATTER HALOS IN NUMERICAL MODELS AT REDSHIFTS 0 ≤ &lt;i&gt;z&lt;/i&gt; ≤ 9

For the numerical model in the range of redshifts \(0 \leqslant z \leqslant 9\), we examined the properties and evolution of dark matter haloes using a previously proposed method of compact analysis that allows separating the influence of random and regular factors on the main characteristics of the dark matter halo. In the investigated range of redshifts, a monotonic evolution of the average values of the basic parameters of small halo structures into a central massive object is observed through sequential hierarchical merging. These basic parameters include the circular velocity \( {{{v}}_{c}} \), the parameter \( {{w}_{c}} = {{{v}}_{c}}{\text{/}}r \), and the mass. In the range \(3 \leqslant z \leqslant 9\), the parameters evolve slowly, while in the range \(0 \leqslant z \leqslant 3\), they evolve rapidly. The evolution of the dark matter halos formed before reionization is characterized by a slow change in their average characteristics and the properties of the halo outskirts. The important role of early-formed massive structural elements is emphasized.

First Report of Colletotrichum fioriniae Infecting Hop (Humulus lupulus) in Michigan.

In July of 2020, a hop (Humulus lupulus L.) grower in Berrien County, Michigan submitted 'Chinook' leaf samples to MSU Plant & Pest Diagnostics. The leaves were covered in small, tan colored lesions, with a small chlorotic halo with an approximate diameter of 5 mm. The grower reported that foliar lesions were in the lower 2 m of the fully developed hop canopy. Disease incidence and severity were estimated at approximately 20% and 5 to 10%, respectively. After incubation at 100% relative humidity, acervuli with orange spore masses and a few setae were present. A pure culture was obtained from these sporulating lesions using water agar. The isolate was hyphal tipped onto potato dextrose agar (PDA) and stored in a glycerol-salt solution at -80o C (isolate CL001) (Miles et al. 2011). On PDA, cultures displayed gray growth on the top of the colony and a red color on the underside of the Petri dish. After 14 days, acervuli with no setae appeared exuding orange conidial masses on the surface of the culture. Conidia were hyaline, aseptate, smooth-walled and rounded at the ends and measured on average 15.89 μm (13.81 to 16.91 μm) × 7.26 (6.82 to 8.41 μm) (n = 20). The color and size of the conidia matched other descriptions of C. acutatum sensu lato (Damm et al. 2012). Four loci (ITS/515 bp - OQ026167, GAPDH/238 bp - OQ230832, CHS1/228 bp -OQ230830, and TUB2/491 bp - OQ230831) were amplified from isolate CL001 (using the primers ITS1/ITS4, GDF1/GDR1, CSH-79f/CHS-354R, and T1/Bt-2b, respectively) and had 100% pairwise identity with C. fioriniae 125396 (JQ948299, JQ948629, JQ948960, JQ949950, respectively, Damm et al. 2012). The GAPDH, CSH1, and TUB2 sequences from isolate CL001 were trimmed, concatenated and aligned with 31 different members of Colletotrichum acutatum sensu lato and C. gloesporioides 356878 (Damm et al. 2012; Kennedy et al. 2022). The alignment was then used to produce a maximum likehood phylogenetic tree using Geneious Prime (Biomatters Ltd.) with the PHYML add on using the HKY + G model (G = 0.34) (Guindon et al. 2010). Isolate CL001 had the closest similarity to C. fioriniae with a bootstrap value of 100. Pathogenicity tests were performed on 2 month-old 'Chinook' hop plants. Twelve plants were inoculated with 50 ml of a conidial suspension (7.95 x 106 conidia/ml) of isolate CL001 (n = 6) or water (n = 6) using a spray bottle until runoff. Inoculated plants were sealed in clear plastic bags and grown in a greenhouse at 21o C with a photoperiod of 14 h. After 7 days, lesions appeared on the hop plants inoculated with CL001, but no symptoms appeared on the water inoculated hop plants. Lesions with a chlorotic halo were observed but they were smaller than field lesions and no setae were present (approx. 1 mm in diam.). Leaves were surface sterilized (0.3% sodium hypochlorite solution for 15 s and then rinsed three times) and the leading margin of the lesions or healthy tissue (water control) were placed on 1% ampicillin amended PDA. Fungal isolates on PDA morphologically matched C. fioriniae were recovered from all CL001-inoculated plants. No C. fioriniae isolates were recovered from the water-inoculated plants. Based on conidial morphology, the four loci, and the phylogenetic tree, isolate CL001 was identified as C. fioriniae. This is the first report of Colletotrichum fioriniae (syn = Glomerella acutata var. fioriniae Marcelino & Gouli) infecting common hop and further investigation is needed to determine if management is needed for this pathogen.

Searching for Dwarf Hα Emission-line Galaxies within Voids. I. Survey Methods and First Observations

The population density of dwarf galaxies in low-density voids is likely determined by the dark matter halo mass function and how galaxy formation proceeds in smaller halos. This depends on the nature of dark matter itself, making the dwarf galaxy population a tracer of its properties. While dwarfs have been found in smaller, closer voids, they have proven difficult to find in larger, more distant voids through magnitude-limited spectroscopic surveys. This is because these surveys detect an overwhelmingly large number of objects behind the voids that must be verified spectroscopically, making void surveys prohibitively inefficient and expensive in terms of large-telescope time. Narrowband imaging for emission lines such as Hα reduces the number of background objects, although the overall number remains large. If imaging is done through a filter set with overlapping transmission wings, then object redshift can be estimated from photometry alone. The precision possible is an order of magnitude greater than single-band photometry, with the caveat that the captured line must be identified through other means. Broadband photometry can be used to reject enough objects with emission of an unwanted type to make obtaining spectra of the remaining objects feasible. In this study, we present an Hα survey for dwarf galaxies with M r ′ fainter than −14 mag through the center 4.3 square degrees of the void FN8. Using Sloan photometry, we exclude enough [O ii] and [O iii] emitters that follow-up spectra of only a few dozen objects are required to statistically estimate the void population density.

First emergence of cold accretion and supermassive star formation in the early universe

ABSTRACT We investigate the first emergence of the so-called cold accretion, the accretion flows deeply penetrating a halo, in the early universe with cosmological N-body/SPH simulations. We study the structure of the accretion flow and its evolution within small haloes with ≲108 M⊙ with sufficiently high spatial resolutions down to ∼1 pc scale. While previous studies only follow the evolution for a short period after the primordial cloud collapse, we follow the long-term evolution until the cold accretion first appears, employing the sink particle method. We show that the cold accretion emerges when the halo mass exceeds ∼2.2 × 107 M⊙{(1 + z)/15}−3/2, the minimum halo masses above which the accretion flow penetrates haloes. We further continue simulations to study whether the cold accretion provides the dense shock waves, which have been proposed to give birth to supermassive stars (SMSs). We find that the accretion flow eventually hits a compact disc near the halo centre, creating dense shocks over a wide area of the disc surface. The resulting post-shock gas becomes dense and hot enough with its mass comparable to the Jeans mass MJ ∼ 104–5 M⊙, a sufficient amount to induce the gravitational collapse, leading to the SMS formation.

Fuzzy Dark Matter as a Solution to Reconcile the Stellar Mass Density of High-z Massive Galaxies and Reionization History

The JWST early release data show unexpected high stellar mass densities of massive galaxies at 7 < z < 11. A high star formation efficiency is probably needed to explain this. However, such a high star formation efficiency would greatly increase the number of ionizing photons, which would be in serious conflict with current cosmic microwave background (CMB) and other measurements of cosmic reionization history. To solve this problem, we explore fuzzy dark matter (FDM), which is composed of ultra-light scalar particles, e.g., ultra-light axions, and calculate its halo mass function and stellar mass density for different axion masses. We find that a FDM model with m a ≃ 5 × 10−23 eV and a possible uncertainty range ∼3 × 10−23–10−22 eV can effectively suppress the formation of small halos and galaxies, so that with higher star formation efficiency both the JWST data at z ∼ 8 and the reionization history measurements from optical depth of CMB scattering and ionization fraction can be simultaneously matched. We also find that the JWST data at z ∼ 10 are still too high to fit in this scenario. We note that the estimated mean redshift of the sample may have large uncertainty, that it can be as low as z ∼ 9 depending on adopted spectral energy distribution templates and photometric-redshift code. In addition, warm dark matter with ∼keV mass can also be an alternative choice, since it should have similar effects on halo formation as FDM.

Stellar prospects for FRB gravitational lensing

ABSTRACTGravitational lensing of fast radio bursts (FRBs) offers an exciting avenue for several cosmological applications. However, it is not yet clear how many such events future surveys will detect nor how to optimally find them. We use the known properties of FRBs to forecast detection rates of gravitational lensing on delay time-scales from microseconds to years, corresponding to lens masses spanning 15 orders of magnitude. We highlight the role of the FRB redshift distribution on our ability to observe gravitational lensing. We consider cosmological lensing of FRBs by stars in foreground galaxies and show that strong stellar lensing will dominate on microsecond time-scales. Upcoming surveys such as DSA-2000 and CHORD will constrain the fraction of dark matter in compact objects (e.g. primordial black holes) and may detect millilensing events from intermediate mass black holes (IMBHs) or small dark matter halos. Coherent all-sky monitors will be able to detect longer-duration lensing events from massive galaxies, in addition to short time-scale lensing. Finally, we propose a new application of FRB gravitational lensing that will measure directly the circumgalactic medium of intervening galaxies.

Boosting the 21 cm forest signals by the clumpy substructures

We study the contribution of subhalos to the 21 cm forest signal. The halos can host the substructures and including the effects of those small scale clumps can potentially boost the 21 cm optical depth in favor of detecting the 21 cm forest signals. We estimate the boost factor representing the ratio of the optical depth due to the subhalo contribution and that due to the host halo alone (without subhalos). Even though the optical depth boost factor is negligible for a small host halo with the mass of order 105 M ⊙, the subhalo contribution can enhance the optical depth by an order of magnitude for a host halo of order 107 M ⊙. The resultant 21 cm absorption line abundance which is obtained by integrating over the halo mass range relevant for the 21 cm forest signal can be enhanced by up to of order 10% due to the substructures. The larger boost factor for a larger host halo would be of particular interest for the 21 cm forest detection because the contribution of the larger host halos to the 21 cm forest signals is smaller due to their higher temperature and less abundance than the smaller host halos. The subhalos hence can well help the larger host halos more important for the signal estimation which, without considering the subhalos, may not give appreciable contribution to 21 cm forest signals.

Deep Learning-Based Robust Automated System for Predicting Human Sperm DNA Fragmentation Index.

Determining the DNA fragmentation index (DFI) by the sperm chromatin dispersion (SCD) test involves manual counting of stained sperms with halo and no halo. The aim of this study is to build a robust artificial intelligence-based solution to predict the DFI. This is a retrospective experimental study conducted in a secondary in vitro fertilisation setup. We obtained 24,415 images from 30 patients after the SCD test using a phase-contrast microscope. We classified the dataset into two, binary (halo/no halo) and multiclass (big/medium/small halo/degraded (DEG)/dust). Our approach consists of a training and prediction phase. The 30 patients' images were divided into training (24) and prediction (6) sets. A pre-processing method M was developed to automatically segment the images to detect sperm-like regions and was annotated by three embryologists. To interpret the findings, the precision-recall curve and F1 score were utilised. Binary and multiclass datasets containing 8887 and 15,528 cropped sperm image regions showed an accuracy of 80.15% versus 75.25%. A precision-recall curve was determined and the binary and multiclass datasets obtained an F1 score of 0.81 versus 0.72. A confusion matrix was applied for predicted and actuals for the multiclass approach where small halo and medium halo confusion were found to be highest. Our proposed machine learning model can standardise and aid in arriving at accurate results without using expensive software. It provides accurate information about healthy and DEG sperms in a given sample, thereby attaining better clinical outcomes. The binary approach performed better with our model than the multiclass approach. However, the multiclass approach can highlight the distribution of fragmented and non-fragmented sperms.

From Images to Dark Matter: End-to-end Inference of Substructure from Hundreds of Strong Gravitational Lenses

Constraining the distribution of small-scale structure in our universe allows us to probe alternatives to the cold dark matter paradigm. Strong gravitational lensing offers a unique window into small dark matter halos (<1010 M ⊙) because these halos impart a gravitational lensing signal even if they do not host luminous galaxies. We create large data sets of strong lensing images with realistic low-mass halos, Hubble Space Telescope (HST) observational effects, and galaxy light from HST’s COSMOS field. Using a simulation-based inference pipeline, we train a neural posterior estimator of the subhalo mass function (SHMF) and place constraints on populations of lenses generated using a separate set of galaxy sources. We find that by combining our network with a hierarchical inference framework, we can both reliably infer the SHMF across a variety of configurations and scale efficiently to populations with hundreds of lenses. By conducting precise inference on large and complex simulated data sets, our method lays a foundation for extracting dark matter constraints from the next generation of wide-field optical imaging surveys.

The Cosmic Graph: Optimal Information Extraction from Large-Scale Structure using Catalogues

We present an implicit likelihood approach to quantifying cosmological information over discrete catalogue data, assembled as graphs. To do so, we explore cosmological parameter constraints using mock dark matter halo catalogues. We employ Information Maximising Neural Networks (IMNNs) to quantify Fisher information extraction as a function of graph representation. We a) demonstrate the high sensitivity of modular graph structure to the underlying cosmology in the noise-free limit, b) show that graph neural network summaries automatically combine mass and clustering information through comparisons to traditional statistics, c) demonstrate that networks can still extract information when catalogues are subject to noisy survey cuts, and d) illustrate how nonlinear IMNN summaries can be used as asymptotically optimal compressed statistics for Bayesian simulation-based inference. We reduce the area of joint $\Omega_m$, $\sigma_8$ parameter constraints with small ($\sim$ 100 object) halo catalogues by a factor of 42 over the two-point correlation function, and demonstrate that the networks automatically combine mass and clustering information. This work utilizes a new IMNN implementation over graph data in Jax, which can take advantage of either numerical or auto-differentiability. We also show that graph IMNNs successfully compress simulations away from the fiducial model at which the network is fitted, indicating a promising alternative to $n$-point statistics in catalogue simulation-based analyses. <em>Code and a tutorial for the analysis and relevant software can be found <a href="https://github.com/tlmakinen/cosmicGraphs"> here </a>. </em>

Rapid simulations of halo and subhalo clustering

The analysis of cosmological galaxy surveys requires realistic simulations for their interpretation. Forward modelling is a powerful method to simulate galaxy clustering without the need for an underlying complex model. This approach requires fast cosmological simulations with a high resolution and large volume, to resolve small dark matter halos associated to single galaxies. In this work, we present fast halo and subhalo clustering simulations based on the Lagrangian perturbation theory code PINOCCHIO, which generates halos and merger trees. The subhalo progenitors are extracted from the merger history and the survival of subhalos is modelled. We introduce a new fitting function for the subhalo merger time, which includes a redshift dependence of the fitting parameters. The spatial distribution of subhalos within their hosts is modelled using a number density profile. We compare our simulations with the halo finder ROCKSTAR applied to the full N-body code GADGET-2. The subhalo velocity function and the correlation function of halos and subhalos are in good agreement. We investigate the effect of the chosen number density profile on the resulting subhalo clustering. Our simulation is approximate yet realistic and significantly faster compared to a full N-body simulation combined with a halo finder. The fast halo and subhalo clustering simulations offer good prospects for galaxy forward models using subhalo abundance matching.

Growth of fluctuations in Chaplygin gas cosmologies: A nonlinear Jeans scale for unified dark matter

Unified dark matter cosmologies economically combine missing matter and energy in a single fluid. Of these models, the standard Chaplygin gas is theoretically motivated, but faces problems in explaining large scale structure if linear perturbations are directly imposed on the homogeneous fluid. However, early formation of a clustered component of small halos is sufficient (and necessary) for hierarchical clustering to proceed in a cold dark matter (CDM) component as in the standard scenario, with the remaining homogeneous component acting as dark energy. We examine this possibility. A linear analysis shows that a critical Press-Schechter threshold for collapse can generally only be reached for generalized Chaplygin gas models that mimic $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$, or ones where superluminal sound speeds occur. However, the standard Chaplygin gas case turns out to be marginal, with overdensities reaching order one in the linear regime. This motivates a nonlinear analysis. A simple infall model suggests that collapse is indeed possible for perturbations of order 1 kpc and above; for, as opposed to standard gases, pressure forces decrease with increasing densities, allowing for the collapse of linearly stable systems. This suggests that a cosmological scenario based on the standard Chaplygin gas may not be ruled out from the viewpoint of structure formation, as often assumed. On the other hand, a ``nonlinear Jeans scale,'' constricting growth to scales $R\ensuremath{\gtrsim}\mathrm{kpc}$, which may be relevant to the small scale problems of CDM, is predicted. Finally, the background dynamics of clustered Chaplygin gas cosmologies is examined and confronted with observational datasets. It is found to be viable (at 1-sigma), with a mildly larger ${H}_{0}$ than $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$, if the clustered fraction is larger than 90%.

Testing strong lensing subhalo detection with a cosmological simulation

ABSTRACT Strong gravitational lensing offers a compelling test of the cold dark matter paradigm, as it allows for subhaloes with masses of ∼109 M⊙ and below to be detected. We test commonly used techniques for detecting subhaloes superposed in images of strongly lensed galaxies. For the lens we take a simulated galaxy in a ∼1013 M⊙ halo grown in a high-resolution cosmological hydrodynamical simulation, which we view from two different directions. Though the resolution is high, we note the simulated galaxy still has an artificial core which adds additional complexity to the baryon dominated region. To remove particle noise, we represent the projected galaxy mass distribution by a series of Gaussian profiles which precisely capture the features of the projected galaxy. We first model the lens mass as a (broken) power-law density profile and then search for small haloes. Of the two projections, one has a regular elliptical shape, while the other has distinct deviations from an elliptical shape. For the former, the broken power-law model gives no false positives and correctly recovers the mass of the superposed small halo; however, for the latter we find false positives and the inferred halo mass is overestimated by ∼4–5 times. We then use a more complex model in which the lens mass is decomposed into stellar and dark matter components. In this case, we show that we can capture the simulated galaxy’s complex projected structures and correctly infer the input small halo.

Combination of Poly(ε-Caprolactone) Biomaterials and Essential Oils to Achieve Anti-Bacterial and Osteo-Proliferative Properties for 3D-Scaffolds in Regenerative Medicine.

Biomedical implants, an essential part of the medical treatments, still suffer from bacterial infections that hamper patients’ recovery and lives. Antibiotics are widely used to cure those infections but brought antibiotic resistance. Essential oils (EOs) demonstrate excellent antimicrobial activity and low resistance development risk. However, EO application in medicine is still quite scarce and almost no research work considers its use in combination with bioresorbable biomaterials, such as the poly(ε-caprolactone) (PCL) polymer. This work aimed to combine the antibacterial properties of EOs and their components, particularly eugenol and cinnamon oil, against Staphylococcus aureus, S. epidermidis and Escherichia coli, with those of PCL for medical applications in which good tissue regeneration and antimicrobial effects are required. The PCL porous scaffolds, added with increasing (from 30% to 50%) concentrations of eugenol and cinnamon oil, were characterized by square-shaped macropores. Saos-2 cells’ cell viability/proliferation was hampered by 40 and 50% EO-enriched PCL, whereas no cytotoxic effect was recorded for both 30% EO-added PCL and pure-PCL. The antibacterial tests revealed the presence of a small inhibition halo around the 30% eugenol and cinnamon oil-functionalized PCL scaffolds only for staphylococci, whereas a significant decrease on both adherent and planktonic bacteria was recorded for all the three microorganisms, thus proving that, even if the EOs are only in part released by the EO-added PCL scaffolds, an anti-adhesive feature is anyway achieved. The scaffold will have the ability to support new tissue formation and simultaneously will be able to prevent post-surgical infection. This research shows the great potential in the use of EOs or their single components, at low concentrations, for biomaterial functionalization with enhanced anti-bacterial and biointegration properties.

Fingerprints of modified gravity on galaxies in voids

ABSTRACT We search for detectable signatures of f(R) gravity and its chameleon screening mechanism in the baryonic and dark matter (DM) properties of simulated void galaxies. The enhancement of the gravitational acceleration can have a meaningful impact on the scaling relations as well as on the halo morphology. The galaxy rotational velocity field (calculated with the velocity of the gas disc and the acceleration fields) deviates from the typical values of the Tully–Fisher Relation in General Relativity (GR). For a given stellar mass, f(R) gravity tends to produce greater maximum velocities. On the other hand, the mass in haloes in f(R) gravity is more concentrated than their counterparts in GR. This trend changes when the concentration is calculated with the dynamical density profile, which takes into account the unscreened outer regions of the halo. Stellar discs interact with the overall potential well in the central regions, modifying the morphology of the screening regions and reshaping them. We find a trend for galaxies with a more dominant stellar disc to deviate further from round screening regions. We find that small haloes are less triaxial and more round in f(R) than their GR counterparts. The difference between halo morphology becomes smaller in f(R) haloes whose inner regions are screened. These results suggest possible observables that could unveil modified gravity effects on galaxies in voids in future cosmological tests of gravity.