Asialoglycoprotein receptors (ASGPRs) are highly expressed on hepatocytes and have been used for liver-targeted delivery and hepatocellular carcinoma (HCC) therapy. However, targeted delivery of ...bortezomib (BTZ) to HCC has not been reported. In this study, N-stearyl lactobionamide (N-SALB) with galactose (Gal) moiety was synthesized as a targeting agent and its structure was confirmed by FT-IR and NMR analyses. N-SALB surface-modified solid lipid nanoparticles (SLNs) loaded with BTZ (Gal-SLNs/BTZ) were developed to target BTZ delivery into HCC cancer cells. The Gal-SLNs/BTZ had an average particle size of 116.3 nm, polydispersity index (PDI) of 0.210, and zeta potential of -13.8 mV. TEM analysis showed their nanometer-sized spherical morphology. The encapsulation efficiency (EE) and drug loading (DL) capacity were 84.5 % and 1.16 %, respectively. Release studies showed that BTZ loaded inside the SLNs was slowly released over a period of 72 h at pH 7.4. Flow cytometry analysis showed significantly higher intracellular uptake of N-SALB-targeted nanoparticles than non-targeted nanoparticles in HepG2 cells. All lipid formulations showed good biocompatibility in the cytotoxicity study using MTT assay. Concentration-dependent cytotoxicity was observed for all formulations, with N-SALB-targeted nanoparticles demonstrating more cytotoxicity against HepG2 cells. The highest percentage of apoptosis was obtained for N-SALB-targeted nanoparticles compared to non-targeted nanoparticles (42.2 % and 8.70 %, respectively). Finally, biodistribution studies in HepG2 bearing nude mice showed that the accumulation of targeted nanoparticles in the tumor was significantly higher than non-targeted nanoparticles.
Noble metal nanoparticles, due to their good physicochemical properties, have been exploited in biological applications. Among these metals, nanosilver has attracted great attention because of its ...optical properties and broad-spectrum antimicrobial activities with no drug tolerance.
The present study has attempted to conduct chemical synthesis of Fe
O
@PEG-Ag core/shell nanocomposites in aqueous solutions through co-precipitation of Fe
and Fe
ions, encapsulating the iron oxide core by poly (ethylene-glycol) (PEG) improve its hydrophilicity and biocompatibility, and immobilizing silver ions by application of NaBH
as a reducing agent.
The synthesized structures were characterized by Fourier-transform infrared (FT-IR), field emission scanning electron microscopy, energy-dispersive X-ray spectrum, wavelength-dispersive X-ray, vibrating sample magnetometer, inductively coupled plasma-mass spectrometry and transmission electron microscopy methods. Antimicrobial activity of the nanostructures against
,
and
was evaluated by broth microdilution based on the methods suggested by Clinical Laboratory Standard Institute. Furthermore, the nanocomposite was tested for possible anti-parasitic effects against
promastigotes by MTT assay. Also, its impacts on bacterial cell morphology were defined using atomic force microscopy. Moreover, toxicity of the nanostructure related to animal cell line was determined based on MTT assay.
In general, the synthesized core/shell nanostructure can demonstrate noticeable activity against the evaluated representative microorganisms while its toxicity against animal cell line is not considerable.
This nanostructure can be applied as a smart drug delivery system with the help of an external magnetic field or it can be used as a powerful antibiotic agent along with other antibiotics that can form a shell on its structure.
The aims of this research were to develop the first self-healing dental nanocomposite and to evaluate mechanical properties (compressive and flexural strength), crack-healing, and self-healing ...longevity after 90 days of water aging. The principal reasons for failure are microcracks formed by polymerization shrinkage, recurrent dynamic mechanical stress, water sorption, and thermal fatigue. N, N-dihydroxyethyl p-toluidine and triethylene glycol dimethacrylate (DEPT-TEGDMA) nanocapsules were synthesized as they have been proven previously to be biocompatible for dental materials. Nanoclay was used as a filler to improve the mechanical properties of self-healing tooth nanocomposites. Nanocapsules were prepared by in situ emulsion polymerization of poly urea-formaldehyde (PUF) shells. The synthesized PUF shells were characterized by FTIR, SEM, and DLS analyses. The results showed that incorporating nanocapsules at a 7.5% mass fraction into the nanocomposite increased the mechanical properties. A good self-healing efficiency ranging from 54.06 to 58% recovery was obtained. The 90 days of water-aging compared to 1 day did not reduce the self-healing efficiency (p > 0.1), showing water-aging did not damage the nanocapsules.
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•Cracks heal autonomously with self-healing dental composites.•Synthesized nanocapsule with high stirring rates had good mechanical properties in nanocomposite.•After 90 days immersed in distilled water, self-healing efficiency did not decrease.•Nanocomposite demonstrated high self-healing retention.•High self-healing retention overcomes microcracks and restore primary failures.
Euclid. III. The NISP instrument Schirmer, M.; Maciaszek, T.; Corcione, L. ...
Astronomy and astrophysics (Berlin),
08/2024
Journal Article
Recenzirano
Odprti dostop
The Near-Infrared Spectrometer and Photometer (NISP) on board the satellite provides multiband photometry and $R slitless grism spectroscopy in the 950--2020\,nm wavelength range. In this reference ...article, we illuminate the background of NISP's functional and calibration requirements, describe the instrument's integral components, and provide all its key properties. We also sketch the processes needed to understand how NISP operates and is calibrated as well as its technical potentials and limitations. Links to articles providing more details and the technical background are included. The NISP's 16 H2RG detectors with a plate scale of $ deliver a field of view of 0.57\,deg$^2$. In photometric mode, NISP reaches a limiting magnitude of sim \,24.5\,AB\,mag in three photometric exposures of about 100\,s in exposure time for point sources and with a S/N of five. For spectroscopy, NISP's point-source sensitivity is a SNR = 3.5 detection of an emission line with flux sim \,$2 $ integrated over two resolution elements of 13.4\ in 3times 560\,s grism exposures at 1.6\ (redshifted Halpha ). Our calibration includes on-ground and in-flight characterisation and monitoring of the pixel-based detector baseline, dark current, non-linearity, and sensitivity to guarantee a relative photometric accuracy better than 1.5<!PCT!> and a relative spectrophotometry better than 0.7<!PCT!>. The wavelength calibration must be accurate to 5\ or better. The NISP is the state-of-the-art instrument in the near-infrared for all science beyond small areas available from HST and JWST -- and it represents an enormous advance from any existing instrumentation due to its combination of field size and high throughput of telescope and instrument. During six-year survey covering 14\,000\,deg$^2$ of extragalactic sky, NISP will be the backbone in determining distances of more than a billion galaxies. Its near-infrared data will become a rich reference imaging and spectroscopy data set for the coming decades.
We investigate the properties of ~7000 narrow-band selected galaxies with strong Hβ+O III and O II nebular emission lines from the High-z Emission-Line Survey between z ~ 0.8 and 5.0. Our sample ...covers a wide range in stellar mass (...), rest-frame equivalent widths (...), and line luminosities (...). We measure the Hβ+O III-selected stellar mass functions out to z ~ 3.5 and find that both ... and ... increases with cosmic time. The O II-selected stellar mass functions show a constant ... and a strong, increasing evolution with cosmic time in ... in line with Hα studies. We also investigate the evolution of the EW^sub rest^ as a function of redshift with a fixed mass range (...) and find an increasing trend best represented by ... and ... up to z ~ 2 and ~3 for Hβ+O III and O II emitters, respectively. This is the first time that the EW^sub rest^ evolution has been directly measured for Hβ+O III and O II emitters up to these redshifts. There is evidence for a slower evolution for z > 2 in the Hβ+O III EW^sub rest^ and a decreasing trend for z > 3 in the O II EW^sub rest^ evolution, which would imply low O II EW at the highest redshifts and higher O III/O II line ratios. This suggests that the ionization parameter at higher redshift may be significantly higher than the local Universe. Our results set the stage for future near-IR space-based spectroscopic surveys to test our extrapolated predictions and also produce z > 5 measurements to constrain the high-z end of the EW^sub rest^ and O III/O II evolution. (ProQuest: ... denotes formulae/symbols omitted.)
We present a catalog of 10,718 objects in the COSMOS field, observed through multi-slit spectroscopy with the Deep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II telescope in the ...wavelength range ∼5500-9800 . The catalog contains 6617 objects with high-quality spectra (two or more spectral features), and 1798 objects with a single spectroscopic feature confirmed by the photometric redshift. For 2024 typically faint objects, we could not obtain reliable redshifts. The objects have been selected from a variety of input catalogs based on multi-wavelength observations in the field, and thus have a diverse selection function, which enables the study of the diversity in the galaxy population. The magnitude distribution of our objects is peaked at IAB ∼ 23 and KAB ∼ 21, with a secondary peak at KAB ∼ 24. We sample a broad redshift distribution in the range 0 < z < 6, with one peak at z ∼ 1, and another one around z ∼ 4. We have identified 13 redshift spikes at z > 0.65 with chance probabilities < 4 × 10−4, some of which are clearly related to protocluster structures of sizes >10 Mpc. An object-to-object comparison with a multitude of other spectroscopic samples in the same field shows that our DEIMOS sample is among the best in terms of fraction of spectroscopic failures and relative redshift accuracy. We have determined the fraction of spectroscopic blends to about 0.8% in our sample. This is likely a lower limit and at any rate well below the most pessimistic expectations. Interestingly, we find evidence for strong lensing of Ly background emitters within the slits of 12 of our target galaxies, increasing their apparent density by about a factor of 4.
We investigate the evolution of the H β + O III and O II luminosity functions from z ~ 0.8 to ~5 in four redshift slices per emission line using data from the High-z Emission Line Survey (HiZELS). ...This is the first time that the H β + O III and O II luminosity functions have been studied at these redshifts in a self-consistent analysis. This is also the largest sample of O II and H β + O III emitters (3475 and 3298 emitters, respectively) in this redshift range, with large comoving volumes ~1 x ... Mpc... in two independent volumes (COSMOS and UDS), greatly reducing the effects of cosmic variance. The emitters were selected by a combination of photometric redshift and colour-colour selections, as well as spectroscopic follow-up, including recent spectroscopic observations using DEIMOS and MOSFIRE on the Keck Telescopes and FMOS on Subaru. We find a strong increase in L... and a decrease in ... for both H β + O III and O II emitters. We derive the O ?II star formation history of the Universe since z ~ 5 and find that the cosmic star formation rate density (SFRD) rises from z ~ 5 to ~3 and then drops towards z ~ 0. We also find that our star formation history is able to reproduce the evolution of the stellar mass density up to z ~ 5 based only on a single tracer of star formation. When comparing the H β + O III SFRDs to the O II and H α SFRD measurements in the literature, we find that there is a remarkable agreement, suggesting that the H β + O III sample is dominated by star-forming galaxies at high-z rather than AGNs. (ProQuest: ... denotes formulae/symbols omitted.)
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![The nature of H[Beta]+[O II...](http://api.summon.serialssolutions.com/2.0.0/image/issn/XR4PS5YY4K/0035-8711/small "The nature of H[Beta]+[O III] and [O II] emitters to z ~ 5 with HiZELS: stellar mass functions and the evolution of EWs")
