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The transition regime between giant planets (GPs) and brown dwarfs (BDs) is still an open subject of study in exoplanetary science. A complete understanding of the population of long-period GPs and BDs would be pivotal in understanding this topic, but the number of such objects with precisely measured orbital and physical parameters is still small. Moreover, their dynamical influence on smaller companions in inner orbits is still unclear. Within the GAPS programme, we aim to confirm and characterize sub-stellar companion candidates from Gaia DR3, and to study the potential presence of additional lower-mass planets in their systems. We present the results of an intensive high-precision RV monitoring of HD 128717, which hosts the astrometric candidate Gaia-ASOI-009. We used the HARPS-N spectrograph at TNG to collect a high-cadence RV time series of the target. We used MCMC analyses to refine the Gaia DR3 orbital solution of the companion and, finally, performed a combined model of RV and proper motion anomaly (PMa) to derive the complete 3-D orbit of the companion. We also ran a suite of numerical simulations to confirm our results. We confirm the sub-stellar nature of Gaia-ASOI-009, i.e. Gaia-6 B: from the combined RV+PMa fit, we confirm that it is a high-eccentricity low-mass brown dwarf with \\(P_B = 9.37^+0.06_-0.05\\) yr, \\(M_B = 19.8 0.5\\) \\(M_J\\), \\(e_B=0.85\\), \\(i_B = 130^\\). The derived orbital solution differs significantly from the one published in Gaia DR3. Through a series of dedicated simulations, we demonstrate that this discrepancy arises from a degeneracy in the Gaia DR3 astrometric solution. Specifically, the combination of Gaia-6 B long orbital period and high eccentricity, both poorly constrained by the limited timespan of DR3, led to an incorrect solution characterized by a shorter period and lower eccentricity.

Next-generation wide-field optical polarimeters like the Wide-Area Linear Optical Polarimeters (WALOPs) have a field of view (FoV) of tens of arcminutes. For efficient and accurate calibration of these instruments, wide-field polarimetric flat sources will be essential. Currently, no established wide-field polarimetric standard or flat sources exist. This paper tests the feasibility of using the polarized sky patches of the size of around ten-by-ten arcminutes, at a distance of up to 20 degrees from the Moon, on bright-Moon nights as a wide-field linear polarimetric flat source. We observed 19 patches of the sky adjacent to the bright-Moon with the RoboPol instrument in the SDSS-r broadband filter. These were observed on five nights within two days of the full-Moon across two RoboPol observing seasons. We find that for 18 of the 19 patches, the uniformity in the measured normalized Stokes parameters \\(q\\) and \\(u\\) is within 0.2 %, with 12 patches exhibiting uniformity within 0.07 % or better for both \\(q\\) and \\(u\\) simultaneously, making them reliable and stable wide-field linear polarization flats. We demonstrate that the sky on bright-Moon nights is an excellent wide-field linear polarization flat source. Various combinations of the normalized Stokes parameters \\(q\\) and \\(u\\) can be obtained by choosing suitable locations of the sky patch with respect to the Moon

Optical polarimeters are typically calibrated using measurements of stars with known and stable polarization parameters. However, there is a lack of such stars available across the sky. Many of the currently available standards are not suitable for medium and large telescopes due to their high brightness. Moreover, as we find, some of the used polarimetric standards are in fact variable or have polarization parameters that differ from their cataloged values. Our goal is to establish a sample of stable standards suitable for calibrating linear optical polarimeters with an accuracy down to \\(10^-3\\) in fractional polarization. For five years, we have been running a monitoring campaign of a sample of standard candidates comprised of 107 stars distributed across the northern sky. We analyzed the variability of the linear polarization of these stars, taking into account the non-Gaussian nature of fractional polarization measurements. For a subsample of nine stars, we also performed multiband polarization measurements. We created a new catalog of 65 stars (see Table 2) that are stable, have small uncertainties of measured polarimetric parameters, and can be used as calibrators of polarimeters at medium- and large-size telescopes.

We present the first Bayesian method for tomographic decomposition of the plane-of-sky orientation of the magnetic field with the use of stellar polarimetry and distance. This standalone tomographic inversion method presents an important step forward in reconstructing the magnetized interstellar medium (ISM) in 3D within dusty regions. We develop a model in which the polarization signal from the magnetized and dusty ISM is described by thin layers at various distances. Our modeling makes it possible to infer the mean polarization (amplitude and orientation) induced by individual dusty clouds and to account for the turbulence-induced scatter in a generic way. We present a likelihood function that explicitly accounts for uncertainties in polarization and parallax. We develop a framework for reconstructing the magnetized ISM through the maximization of the log-likelihood using a nested sampling method. We test our Bayesian inversion method on mock data taking into account realistic uncertainties from Gaia and as expected for the optical polarization survey PASIPHAE according to the currently planned observing strategy. We demonstrate that our method is effective at recovering the cloud properties as soon as the polarization induced by a cloud to its background stars is higher than \\(\\sim 0.1\\%\\) for the adopted survey exposure time and level of systematic uncertainty. Our method makes it possible to recover not only the mean polarization properties but also to characterize the intrinsic scatter, thus creating new ways to characterize ISM turbulence and the magnetic field strength. Finally, we apply our method to an existing data set of starlight polarization with known line-of-sight decomposition, demonstrating agreement with previous results and an improved quantification of uncertainties in cloud properties.

The transition regime between giant planets (GPs) and brown dwarfs (BDs) is still an open subject of study in exoplanetary science. A complete understanding of the population of long-period GPs and BDs would be pivotal in understanding this topic, but the number of such objects with precisely measured orbital and physical parameters is still small. Moreover, their dynamical influence on smaller companions in inner orbits is still unclear. Within the GAPS programme, we aim to confirm and characterize sub-stellar companion candidates from Gaia DR3, and to study the potential presence of additional lower-mass planets in their systems. We present the results of an intensive high-precision RV monitoring of HD 128717, which hosts the astrometric candidate Gaia-ASOI-009. We used the HARPS-N spectrograph at TNG to collect a high-cadence RV time series of the target. We used MCMC analyses to refine the Gaia DR3 orbital solution of the companion and, finally, performed a combined model of RV and proper motion anomaly (PMa) to derive the complete 3-D orbit of the companion. We also ran a suite of numerical simulations to confirm our results. We confirm the sub-stellar nature of Gaia-ASOI-009, i.e. Gaia-6 B: from the combined RV+PMa fit, we confirm that it is a high-eccentricity low-mass brown dwarf with \\(P_\\text{B} = 9.37^{+0.06}_{-0.05}\\) yr, \\(M_\\text{B} = 19.8 \\pm 0.5\\) \\(M_\\text{J}\\), \\(e_\\text{B}=0.85\\), \\(i_\\text{B} = 130^{\\circ}\\). The derived orbital solution differs significantly from the one published in Gaia DR3. Through a series of dedicated simulations, we demonstrate that this discrepancy arises from a degeneracy in the Gaia DR3 astrometric solution. Specifically, the combination of Gaia-6 B long orbital period and high eccentricity, both poorly constrained by the limited timespan of DR3, led to an incorrect solution characterized by a shorter period and lower eccentricity.

We present a detailed investigation of photometric, spectroscopic, and polarimetric observations of the Type II SN 2023ixf. Earlier studies have provided compelling evidence for a delayed shock breakout from a confined dense circumstellar matter (CSM) enveloping the progenitor star. The temporal evolution of polarization in SN~2023ixf revealed three distinct peaks in polarization evolution at 1.4 d, 6.4 d, and 79.2 d, indicating an asymmetric dense CSM, an aspherical shock front and clumpiness in the low-density extended CSM, and an aspherical inner ejecta/He-core. SN 2023ixf displayed two dominant axes, one along the CSM-outer ejecta and the other along the inner ejecta/He-core, showcasing the independent origin of asymmetry in the early and late evolution. The argument for an aspherical shock front is further strengthened by the presence of a high-velocity broad absorption feature in the blue wing of the Balmer features in addition to the P-Cygni absorption post 16 d. Hydrodynamical light curve modeling indicated a progenitor of 10 solar mass with a radius of 470 solar radii and explosion energy of 2e51 erg, along with 0.06 solar mass of 56-Ni, though these properties are not unique due to modeling degeneracies. The modeling also indicated a two-zone CSM: a confined dense CSM extending up to 5e14 cm, with a mass-loss rate of 1e-2 solar mass per year, and an extended CSM spanning from 5e14 cm to at least 1e16cm with a mass-loss rate of 1e-4 solar mass per year, both assuming a wind-velocity of 10 km/s. The early nebular phase observations display an axisymmetric line profile of [OI], red-ward attenuation of the emission of Halpha post 125 days, and flattening in the Ks-band, marking the onset of dust formation.

The synergy between different detection methods is a key asset in exoplanetology, allowing for both precise characterization of detected exoplanets and robust constraints even in the case of non-detection. Recently, the interplay between imaging, radial velocities and astrometry has produced significant advancements in exoplanetary science. We report a first result of an ongoing survey performed with SHARK-NIR, the new high-contrast near-infrared imaging camera at the Large Binocular Telescope, in parallel with LBTI/LMIRCam in order to detect planetary companions around stars with significant proper motion anomaly. In this work we focus on HD 57625, a F8 star for which we determine a \\(4.8^+3.7_-2.9\\)Ga age, exhibiting significant astrometric acceleration and for which archival radial velocities hint at the presence of a previously undetected massive long-period companion. We analyse the imaging data we collected with SHARK-NIR and LMIRCam in synergy with the available public SOPHIE radial velocity time series and Hipparcos-Gaia proper motion anomaly. With this joint multi-technique analysis, we aim at characterizing the companion responsible for the astrometric and radial velocity signals. The imaging observations result in a non-detection, indicating the companion to be in the substellar regime. This is confirmed by the synergic analysis of archival radial velocity and astrometric measurements resulting in the detection of HD 57625 b, a \\(8.43_-0.91^+1.10\\)M\\(_ Jup\\) planetary companion with an orbital separation of \\(5.70_-0.13^+0.14\\)au and \\(0.52_-0.03^+0.04\\) eccentricity. HD 57625 b joins the small but growing population of giant planets in outer orbits with true mass determination provided by the synergic usage of multiple detection methods, proving once again the importance of multi-technique analysis in providing robust characterization of planetary companions.

The synergy between different detection methods is a key asset in exoplanetology, allowing for both precise characterization of detected exoplanets and robust constraints even in the case of non-detection. Recently, the interplay between imaging, radial velocities and astrometry has produced significant advancements in exoplanetary science. We report a first result of an ongoing survey performed with SHARK-NIR, the new high-contrast near-infrared imaging camera at the Large Binocular Telescope, in parallel with LBTI/LMIRCam in order to detect planetary companions around stars with significant proper motion anomaly. In this work we focus on HD 57625, a F8 star for which we determine a \\(4.8^+3.7_-2.9\\)Ga age, exhibiting significant astrometric acceleration and for which archival radial velocities hint at the presence of a previously undetected massive long-period companion. We analyse the imaging data we collected with SHARK-NIR and LMIRCam in synergy with the available public SOPHIE radial velocity time series and Hipparcos-Gaia proper motion anomaly. With this joint multi-technique analysis, we aim at characterizing the companion responsible for the astrometric and radial velocity signals. The imaging observations result in a non-detection, indicating the companion to be in the substellar regime. This is confirmed by the synergic analysis of archival radial velocity and astrometric measurements resulting in the detection of HD 57625 b, a \\(8.43_-0.91^+1.10\\)M\\(_ Jup\\) planetary companion with an orbital separation of \\(5.70_-0.13^+0.14\\)au and \\(0.52_-0.03^+0.04\\) eccentricity. HD 57625 b joins the small but growing population of giant planets in outer orbits with true mass determination provided by the synergic usage of multiple detection methods, proving once again the importance of multi-technique analysis in providing robust characterization of planetary companions.

Plant roots, nematodes, and soil microorganisms have a complex interaction in the rhizosphere by exchanging or communicating through biomolecules or chemicals or signals. Some rhizospheric (including endophytic) microbes process such compounds via biogeochemical cycles to improve soil fertility, promote plant growth and development, and impart stress tolerance in plants. Some rhizospheric microbes can affect negatively on plant parasitic nematodes (PPNs) thus hindering the ability of nematodes in parasitizing the plant roots. Next-generation sequencing is one of the most widely used and cost-effective ways of determining the composition and diversity of microbiomes in such complex environmental samples. This study employed amplicon sequencing (Illumina/NextSeq) of 16S ribosomal RNA (16S rRNA) for bacteria and Internal Transcribed Spacer (ITS2) region for fungi to profile the soil microbiome in the rhizosphere of cotton grown in North Alabama. We isolated DNA (ZymoBIOMICS) from soil samples in triplicates from four representative locations of North Alabama. Based on the level of Reniform Nematode (RN) Infestation, these locations were classified as Group A-RN Not-Detected (ND), Group B-RN Low Infestation (LI), Group C-RN Medium Infestation (MI), and Group D-RN High Infestation (HI) and determined using sieving method and microscopic examination. Our analyses identified 47,893 bacterial and 3,409 fungal Amplicon Sequence Variants (ASVs) across all groups. Among the bacterial ASVs, 12,758, 10,709, 12,153, and 11,360 unique ASVs were determined in Groups A, B, C, and D, respectively. While 663, 887, 480, and 326 unique fungal ASVs were identified in Groups A, B, C, and D, respectively. Also, the five most abundant rhizospheric bacterial genera identified were , , , , . Moreover, five abundant fungal genera belonging to were identified. The tight clustering of bacterial nodes in , , and shows they are highly similar and often found together. On the other hand, the close association of and suggesting that they have different ecological roles but occupy similar niches and contribute similar functions within the microbial community. The abundant microbial communities identified in this study had a role in nutrient recycling, soil health, plant resistance to some environmental stress and pests including nematodes, and biogeochemical cycles. Our findings will aid in broadening our understanding of how microbial communities interact with crops and nematodes in the rhizosphere, influencing plant growth and pest management.

Medical students report high levels of perceived stress and burnout, especially during the preclinical years. The combination of physical stressors from poor posture, poor sleep quality, and mental stressors from the rigorous curriculum stimulates the sympathetic nervous system (SNS) to secrete cortisol. Previous studies have shown that persistent elevated cortisol levels are associated with negative health outcomes. We conducted an Institutional Review Board (IRB)-approved study to determine if regular osteopathic manipulative treatments (OMTs) could impact the stress levels of first-year osteopathic medical students (OMSs) at Touro College of Osteopathic Medicine (TouroCOM) Harlem campus by measuring physiologic stress through changes in weekly salivary cortisol levels, perceived emotional and psychological stress levels, and cognitive function. We recruited 10 first-year OMSs who were not currently receiving external OMT outside of weekly coursework; other forms of external stress management, such as yoga or meditation, were not controlled for in this study. Utilizing a random number generator, the 10 student respondents were split into a control group that received no treatment and a treatment group that received 15 min of weekly OMT for 6 weeks. The treatment consisted of condylar decompression, paraspinal inhibition, and supine rib raising, which are techniques that are known to balance the SNS and parasympathetic nervous system (PNS). Cortisol levels were quantified by enzyme-linked immunosorbent assay (ELISA) cortisol immunoassay via salivary samples collected at the beginning of each weekly session, prior to treatment for the treatment group, at the same time of day each week. We also measured participants' weekly subjective perception of stress utilizing the College Student Stress Scale (CSSS) and cognitive function utilizing the Lumosity Performance Index (LPI). We conducted a two-tailed, unpaired -test as well as a U test for the cortisol levels, given the smaller sample size and potential for a nonnormal distribution. A lower cortisol level was correlated to a higher optical density (OD), the logarithmic measure of percent transmission of light through a sample; analysis of our data from the ELISA cortisol immunoassay showed an average weekly change in OD (∆OD) for the treatment group of 0.0215 and an average weekly ∆OD of -0.0044 in the control group. The -test showed p=0.0497, and our U test showed a p=0.0317. Both tests indicated a statistically significant decrease across the weekly salivary cortisol levels in the treatment group utilizing a p<0.05. An additional effect-size analysis supported our finding of a significant decrease in weekly cortisol levels in the treatment group, Cohen's =1.460. Based on the CSSS responses, there was no significant difference in perceived stress between the control and treatment groups (p=0.8655, two-tailed). Analysis of the LPI revealed no statistically significant difference in cognitive performance (p=0.9265, two-tailed). Our study supports the claim that OMT that targets the SNS and PNS has a significant impact on cortisol levels. While the reduction in cortisol levels was statistically significant, the broader physiological impact remains unclear. Further research is necessary to determine whether this reduction translates to meaningful clinical benefits.