Layer-by-layer assembly of nanotheranostic particles for simultaneous delivery of docetaxel and doxorubicin to target osteosarcoma

\ua9 2024 Author(s).Osteosarcoma (OS) is a rare form of primary bone cancer, impacting approximately 3.4 7 106 individuals worldwide each year, primarily afflicting children. Given the limitations of existing cancer therapies, the emergence of nanotheranostic platforms has generated considerable research interest in recent decades. These platforms seamlessly integrate therapeutic potential of drug compounds with the diagnostic capabilities of imaging probes within a single construct. This innovation has opened avenues for enhanced drug delivery to targeted sites while concurrently enabling real-time monitoring of the vehicle\u27s trajectory. In this study, we developed a nanotheranostic system employing the layer-by-layer (LbL) technique on a core containing doxorubicin (DOXO) and in-house synthesized carbon quantum dots. By utilizing chitosan and chondroitin sulfate as polyelectrolytes, we constructed a multilayered coating to encapsulate DOXO and docetaxel, achieving a coordinated co-delivery of both drugs. The LbL-functionalized nanoparticles exhibited an approximate size of 150 nm, manifesting a predominantly uniform and spherical morphology, with an encapsulation efficiency of 48% for both drugs. The presence of seven layers in these systems facilitated controlled drug release over time, as evidenced by in vitro release tests. Finally, the impact of the LbL-functionalized nanoparticles was evaluated on U2OS and Saos-2 osteosarcoma cells. The synergistic effect of the two drugs was found to be crucial in inducing cell death, particularly in Saos-2 cells treated with nanoparticles at concentrations higher than 10 μg/ml. Transmission electron microscopy analysis confirmed the internalization of the nanoparticles into both cell types through endocytic mechanisms, revealing an underlying mechanism of necrosis-induced cell death

Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems

The exoplanet population characterized by relatively short orbital periods ($P<100$ d) around solar-type stars is dominated by super-Earths and sub-Neptunes. However, these planets are missing in our Solar System and the reason behind this absence is still unknown. Two theoretical scenarios invoke the role of Jupiter as the possible culprit: Jupiter may have acted as a dynamical barrier to the inward migration of sub-Neptunes from beyond the water iceline; alternatively, Jupiter may have reduced considerably the inward flux of material (pebbles) required to form super-Earths inside that iceline. Both scenarios predict an anti-correlation between the presence of small planets (SPs) and that of cold Jupiters (CJs) in exoplanetary systems. To test that prediction, we homogeneously analyzed the radial-velocity (RV) measurements of 38 Kepler and K2 transiting SP systems gathered over almost 10 years with the HARPS-N spectrograph, as well as publicly available RVs collected with other facilities. We detected five CJs in three systems, two in Kepler-68, two in Kepler-454, and a very eccentric one in K2-312. We derived an occurrence rate of $9.3^{+7.7}_{-2.9}\%$ for CJs with $0.3-13~M_{Jup}$ and 1-10 AU, which is lower but still compatible at $1.3\sigma$ with that measured from RV surveys for solar-type stars, regardless of the presence or absence of SPs. The sample is not large enough to draw a firm conclusion about the predicted anti-correlation between SPs and CJs; nevertheless, we found no evidence of previous claims of an excess of CJs in SP systems. As an important by-product of our analyses, we homogeneously determined the masses of 64 Kepler and K2 small planets, reaching a precision better than 5, 7.5 and 10$\sigma$ for 25, 13 and 8 planets, respectively. Finally, we release the 3661 HARPS-N radial velocities used in this work to the scientific community. [Abridged]Comment: 21 pages, 10 figures, 10 tables, published in Astronomy and Astrophysics. The updated version of the article takes into account the A&A language editing and guidelines. Tables 1, A.1 and full Table 2 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A3

Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems

The exoplanet population characterized by relatively short orbital periods ($P<100$ d) around solar-type stars is dominated by super-Earths and sub-Neptunes. However, these planets are missing in our Solar System and the reason behind this absence is still unknown. Two theoretical scenarios invoke the role of Jupiter as the possible culprit: Jupiter may have acted as a dynamical barrier to the inward migration of sub-Neptunes from beyond the water iceline; alternatively, Jupiter may have reduced considerably the inward flux of material (pebbles) required to form super-Earths inside that iceline. Both scenarios predict an anti-correlation between the presence of small planets (SPs) and that of cold Jupiters (CJs) in exoplanetary systems. To test that prediction, we homogeneously analyzed the radial-velocity (RV) measurements of 38 Kepler and K2 transiting SP systems gathered over almost 10 years with the HARPS-N spectrograph, as well as publicly available RVs collected with other facilities. We detected five CJs in three systems, two in Kepler-68, two in Kepler-454, and a very eccentric one in K2-312. We derived an occurrence rate of $9.3^{+7.7}_{-2.9}\%$ for CJs with $0.3-13~M_{Jup}$ and 1-10 AU, which is lower but still compatible at $1.3\sigma$ with that measured from RV surveys for solar-type stars, regardless of the presence or absence of SPs. The sample is not large enough to draw a firm conclusion about the predicted anti-correlation between SPs and CJs; nevertheless, we found no evidence of previous claims of an excess of CJs in SP systems. As an important by-product of our analyses, we homogeneously determined the masses of 64 Kepler and K2 small planets, reaching a precision better than 5, 7.5 and 10$\sigma$ for 25, 13 and 8 planets, respectively. Finally, we release the 3661 HARPS-N radial velocities used in this work to the scientific community. [Abridged]Comment: 21 pages, 10 figures, 10 tables, published in Astronomy and Astrophysics. The updated version of the article takes into account the A&A language editing and guidelines. Tables 1, A.1 and full Table 2 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A3

Hard X-ray nanoscale imaging of carbon fibre composites using Near-Field Ptychography

Near-Field Ptychography (NFP) is a powerful technique that allows reconstruction of both the complex-valued illumination field and transmission function of the sample, owing to its data redundancy. When combined with tomography, NFP can produce highresolution quantitative volumetric datasets. Here we present the application of this technique, combining a synchrotron radiation source with NFP, yielding a novel approach capable of providing a deeper understanding of the failure processes in carbon fibre reinforced polymers. Volumes based on the phase information retrieved with NFP, thus, will provide insights directly on the 3D electron density distribution of the sample. We performed these measurements at a 150 nm pixel size on a CFRP sample that previously underwent a tensile test up to ∼ 93% its maximum load. High-resolution 3D imaging data for fibre and matrix damage is crucial to understanding tensile failures. In this work, we address some of the features that can be appreciated at this resolution, and their implication in the understanding of the failure processes mentioned above

CD133+ hematopoietic stem cells reinfusion in end-stage liver disease (ESLD): final results of a phase I clinical trial

none13nononeC. Margini, L. Brodosi, S. Lorenzini, L. Catani, V. Giudice, R. Giordano, A. Casadei, D. Sollazzo, F.G. Foschi, M. Baccarani, M. Bernardi, R. Lemoli, P. AndreoneC. Margini, L. Brodosi, S. Lorenzini, L. Catani, V. Giudice, R. Giordano, A. Casadei, D. Sollazzo, F.G. Foschi, M. Baccarani, M. Bernardi, R. Lemoli, P. Andreon