The solar neighbourhood is populated by nearby ($< 200 $), young ($< 100 $) moving groups (NYMGs) of stars, whose origins are still a matter of debate. One plausible explanation is that they are remnants of individual stellar clusters and associations that are currently dispersing throughout the galactic disc. pc Myr We aim to derive the initial mass function (IMF) of a large sample of NYMGs. We developed and applied an algorithm that uses photometric and astrometric data from DR3 to detect NYMGs as over-densities in a kinematic space, whose members distribute along young isochrones. We inferred individual masses from the photometry of both the detected and the previously known candidates. We estimated the IMFs for 33 groups, 30 of them for the first time, in an average mass range 0.1<m/M_⊙<5, with some groups going as low as 0.02 M_⊙ and as high as 10 M_⊙. We parameterised these IMFs using a log-normal for m<1 M_⊙ and a power-law for m>1 M_⊙. Gaia We detected 4166 source candidate members of 44 known groups, including 2545 new candidates. We recovered 44-54% of the literature candidates and estimated a contamination rate from old field stars of 16-24%. The candidates of the detected groups distribute along young isochrones, which suggests that they are potential members of NYMGs. Parameterisations of both the average of the 33 IMFs based on our detections (m_c=0.25 M_⊙, σ_c=0.45 and α=-2.26 and the one based on the known candidates from the literature (m_c=0.22 M_⊙, σ_c=0.45 and α=-2.45 are in agreement with the IMF parameterisation of the solar neighbourhood and young stellar associations. Our parameterisation of the average IMF, together with the distribution of the detected group members along young isochrones offer strong evidence suggesting that the NYMGs are remnants of individual stellar associations and clusters. We confirm that there are no systematic biases in our detection and in the literature in the range of 0.1<m/M_⊙<10.

Abstract We investigate the origin of the scatter in the stellar mass-halo mass (SMHM) relation using the colibre cosmological hydrodynamical simulations. At fixed halo mass, we find a clear positive correlation between stellar mass and halo concentration, particularly in low-mass haloes between 1011 and $10^{12}\, \rm M_\odot$, where all halo properties are computed from the corresponding dark-matter-only simulation. Two scenarios have been proposed to explain this trend: the earlier formation of higher-concentration haloes allows more time for star formation, or the deeper gravitational potential wells of higher-concentration haloes enhance baryon retention. To distinguish between them, we examine correlations between halo concentration, stellar mass, stellar age, and stellar metallicity. While, at fixed halo mass, halo concentration correlates with stellar age, stellar age itself shows only a weak correlation with stellar mass, indicating that early formation alone cannot account for the concentration-dependence in the scatter of the SMHM relation. In contrast, both stellar metallicity and halo concentration exhibit correlations with stellar mass. The connection between halo concentration and stellar metallicity persists even when simultaneously controlling for both halo mass and stellar mass. These results support the scenario in which the deeper gravitational potentials in higher-concentration haloes suppress feedback-driven outflows, thereby enhancing both baryon and metal retention.

Abstract We compare predictions of how active galactic nuclei (AGNs) populate host galaxies at low redshifts to observations, finding large discrepancies between cosmological simulation predictions and observed patterns. Modern cosmological simulations include AGN feedback models tuned to reproduce the observed galaxy stellar mass function. However, due to a lack of real understanding of the physics of AGN feedback, these models vary significantly across simulations. To distinguish between the models and potentially test the underlying physics, we carry out independent tests of these models. In an earlier study, we found that F AGN —the observed completeness-corrected fraction of galaxies hosting radio AGNs with an Eddington ratio λ > 10 −3 —to be a strong function of host-galaxy stellar mass ( M ⋆ ) but nearly independent of host specific star formation rates (sSFRs) at fixed M ⋆ . In this study, we test the radio mode AGN feedback models of the EAGLE, SIMBA, and TNG100 simulations by comparing their predictions of F AGN M ⋆ to our observational constraint. We find that none of these simulations even qualitatively reproduce the observed dependencies of F AGN on M ⋆ and sSFR. Finally, we find that although the given TNG100 model could be modified in order to better reproduce the observed F AGN trend, this modification would likely also change its prediction for the local stellar mass function and star formation rates—key observations used for calibrating the simulation in the first place. Our findings highlight a pressing need to revisit the AGN feedback prescriptions in EAGLE, SIMBA, TNG100, and other similar models.

Abstract Herbig Ae/Be stars (HAeBes) are critical tracers of intermediate- and high-mass star formation, yet their census remains incomplete compared to low-mass young stellar objects like T-Tauri stars. To expand the known population, we systematically searched for HAeBes in LAMOST DR7 low-resolution spectra. Following Sun et al., we applied Uniform Manifold Approximation and Projection for dimensionality reduction and Support Vector Machine classification, identifying ∼240,000 spectra with potential H α emission. After removing contaminants (nonstellar objects, extragalactic sources, cataclysmic variables, and Algol systems) and restricting to B/A-type stars, we obtained 1835 candidates through 2MASS/WISE visual inspection. Spectral energy distribution analysis confirmed 143 sources with infrared excess ( J band or longer wavelengths), including 92 known HAeBes. From the remaining 51 candidates, we classified 26 with strong infrared excess as new HAeBes. Color-index analysis of confirmed HAeBes and classical Ae/Be stars (CAeBes) revealed that the ( K − W 1) 0 versus ( W 2 − W 3) 0 diagram effectively separates these populations: CAeBes predominantly occupy ( K − W 1) 0 ≤ 0.5 and ( W 2 − W 3) 0 ≤ 1.1, while other regions trace transition disks (( K − W 1) 0 < 0.5 and ( W 2 − W 3) 0 > 1.1), globally depleted disks (( K − W 1) 0 > 0.5 and ( W 2 − W 3) 0 < 1.1), and Class I/Flat/II HAeBes (( K − W 1) 0 > 0.5 and ( W 2 − W 3) 0 > 1.1). More importantly, the HAeBes exhibit a clear evolutionary gradient on this diagram, with those in the Class III, Class II, Flat-SED, and Class I evolutionary stages being effectively distinguished by concentric ellipses that are roughly centered at (0, 0) with semimajor axes of a = 1.5, a = 3.0, and a = 4.0, and a semimajor to semiminor axis ratio of 1.6:1.

Abstract Velocity dispersion ( σ ) in stellar streams from globular clusters (GCs) is sensitive to heating by Galactic substructure, including dark matter (DM) subhalos. Recent studies have compared σ in observed and modeled streams to probe DM properties, but have relied on stream models that neglect strong encounters, black holes (BHs), and mass segregation in GCs. Such phenomena may inflate stream σ or introduce selection effects—e.g., a σ that depends on star mass ( m ). We investigate this prospect using Monte Carlo N -body simulations of GCs under static Galactic tides to generate mock streams with realistic mass and velocity distributions. We find σ correlates with m , especially after core collapse (the GC’s observable increase in central density upon ejecting its BHs), rising from 1.2 to 2.2 km s −1 between m = 0.3–0.8 M ⊙ , with typical kinematic cuts on stream membership. Similar in magnitude to heating by Galactic substructure, this enhancement occurs because the GC’s loss of BHs allows its most-massive stars to occupy its dense center, raising their likelihood of strong ejection via binary interactions and adding broad, exponential wings to the stream’s velocity distribution. Streams’ kinematics thus probe properties (density, BH retention) of their progenitor GCs. Our results also imply observations of streams from some GCs, especially those not subject to highly episodic mass loss, may select for higher σ than predicted by models neglecting σ ’s m dependence. This would cause observed σ in streams—already on the low side of expectations for cold DM—to further favor alternatives such as warm or ultralight DM.

Abstract Evidence suggests that protostellar outbursts likely play a critical role in the stellar mass assembly process, but the extent of this contribution is not well understood. Using the proposed observing program of PRIMA, a conceptual far-IR observatory (PRIMA GO Case #43 in A. Moullet et al 2023.), we examine the probe’s ability to unambiguously determine whether or not variable accretion events dominate the stellar mass assembly process ( M burst ≥ 0.5 M * ). To do this, we construct multiple protostellar ensembles using Herschel 70 μ m flux data and evolve them using a toy Monte Carlo simulation through steady-state and high-magnitude accretion events. Ensembles are observed at various epochs in the evolution process to conclude how many large-amplitude outbursts are observationally recoverable during the proposed program. Based on our synthetic observations and our simulation specifications, we determine that observing a protostellar ensemble of at least 2000 protostars using PRIMA’s proposed program is sufficient for determining the importance of protostellar outbursts in the stellar mass assembly process.

The Zwicky Transient Facility Data Release 2 (ZTF DR2) includes a total of 3,628 Type Ia supernovae (SNe Ia), providing the largest and most complete sample of spectroscopically confirmed SNe Ia at low redshift to date. In this paper, we present a photometric and spectroscopic analysis of 124 subluminous SNe Ia, the largest sample of spectroscopically classified subluminous Type Ia supernova observed with a single instrument, comprising 87 91bg-like, 12 86G-like, 18 04gs-like, and 7 02es-like events. We complement the published DR2 light-curve parameters with new parameters obtained using template-based fits from . We measured the expansion velocities and pseudo-equivalent widths (pEW) of key spectral features using . Next, the spectral averages were constructed for each subluminous subtype, binned by phase. We also analyzed the host galaxy environments, both global and local, in terms of g - z color, stellar mass, and directional light radius (d_DLR). We found that all subluminous SNe Ia (except the 02es-like subtype) are intrinsically red. This is made evident when we separate the extrinsic color components from intrinsic ones. Since has not been trained on subluminous SNe Ia, it compensates for their redder colors by inflating the c parameter, thereby extending the luminosity-width relation to negative values of x1. As expected, all subluminous SNe Ia fall within the cool region of the Branch et al. (2006) diagram, with the exception of 02es-like events, which display lower łambda5972 pEW values. All subluminous subtypes tend to occur in more massive, redder host galaxies and in the reddest local environments within their stellar mass bins. Notably, 91bg- and 86G-like SNe Ia explode at significantly larger normalized galactocentric distances. Finally, we identified the pEW of the blended + + absorption feature at 4300 Å, along with s_BV, as robust and sufficient indicators for subclassifying subluminous SNe Ia. SALT2 SNooPy Spextractor SALT2 Si ii Ti ii Si ii Mg ii

Abstract One of the nearest and best-studied open clusters, the Pleiades is an important cornerstone of stellar astrophysics. Despite its role as a reference coeval stellar population, its multiplicity properties are still not well characterized. The combined use of Gaia Data Release 3 multiband photometry, the renormalized unit weight error (RUWE) astrometric parameter, and non-single-star solutions, along with available ground-based spectroscopic, high-angular-resolution, and polarimetric observations, enable more robust constraints on the binary-star population in the cluster. Several conclusions may have broader implications for other stellar populations. Twin binaries, with mass ratios close to q ∼ 1, tend to have lower RUWE values, increasing their membership selection probability relative to q ∼ 0.5 systems that are disfavored. The frequently observed peak in mass ratio distribution for q ∼ 1 binaries may be partially attributed to this bias. Photometrically fitted mass ratios are underestimated for double-lined spectroscopic binaries, in agreement with other authors. Differential extinction photometrically mimics stellar binarity. An area of enlarged absorption is traced by increased polarization south of the Merope star and excluded from the analysis to avoid this bias. The fraction of systems with q > 0.6 companions is measured to be f = 16.4 % − 0.6 + 2.6 for m > 0.5 M ⊙ stars, which is larger than recent Gaia-based estimates, but compatible with the pre-Gaia values for Pleiades and the field population. The binary fraction shows no steady increase with stellar mass in the 0.5–1.2 M ⊙ range, while the mass ratio has a bimodal distribution with a minimum near q ∼ 0.7.

Abstract Galaxy mergers are key drivers of galaxy formation and evolution, including triggering AGN and star formation to a still unknown degree. We thus investigate the impact of galaxy mergers on star formation and AGN activity using 3,330 galaxies at z = 4.5 − 8.5 from eight JWST fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, MACS-0416), covering an unmasked area of 189 arcmin2. We focus on star formation rate (SFR) enhancement, AGN fraction, and AGN excess in close pairs defined by Δz < 0.3 and projected separations rp < 100 kpc, relative to non-merger samples. Close pairs with mass ratios greater than 1:4 are used for the SFR–enhancement analysis, whereas no mass–ratio constraint is applied for the AGN fraction and AGN excess measurements. We find SFR enhancement occurs only at rp < 20 kpc, with values 0.25 ± 0.10 dex and 0.26 ± 0.11 dex above non-merger medians for z = [4.5, 6.5] and z = [6.5, 8.5], respectively. No other statistically significant enhancements in galaxy sSFR or stellar mass are observed at any projected separation or redshift. We also compare observational results with predictions from the SC-SAM simulation, finding no evidence of star formation enhancement in simulations at any separation. Lastly, we examine the fraction and excess of AGNs identified through photometric SED fitting (Type-I) and BPT diagnostics (Type-II). We find $48^{+33}_{-7}\%$ of Type-I and $44^{+26}_{-20}\%$ of Type-II AGNs have a close companion within rp < 50 kpc and Δz < 0.3. Furthermore, $73^{+27}_{-32}\%$ of AGNs have companions within 100 kpc. Relative to isolated galaxies, we measure an AGN excess factor of $1.26^{+0.15}_{-0.04}$ for Type-I and $1.34^{+0.23}_{-0.11}$ for Type-II AGNs in close pairs, suggesting notable AGN enhancement in galaxy pairs at these higher redshifts.

Abstract How a seemingly “dead” host galaxy provides fuel for its active galactic nucleus (AGN) remains an unresolved problem. Using the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we present a new high-sensitivity atomic-hydrogen (H i ) observation toward the nearby elliptical galaxy NGC 4278 and its adjacent region. From the observation, we found that external gas accretion from a neighbouring galaxy fuels the low-luminosity AGN in NGC 4278 through tidal interactions. The accreted gas entering NGC 4278 exhibits a rotating gas disk. Moreover, the accreted galaxy has been gas poor and has an H i to stellar mass ratio of about 0.02. Due to the process of gas accretion, it is likely that relativistic jets are generated in the AGN of NGC 4278. The emission of TeV gamma rays in NGC 4278 is likely to be associated with the newly accreted H i gas.

Abstract We study the large-scale environments and clustering properties of 28 low-luminosity active galactic nuclei (AGNs) at z = 3.9–6 in the GOODS-N field. Our sample, identified from the JWST NIRCam Imaging and WFSS data in Complete NIRCam Grism Redshift Survey and First Reionization Epoch Spectroscopically Complete Observations surveys with either broad H α emission lines or V-shaped continua, are compared to 782 H α emitters (HAEs) selected from the same data. These AGNs are located in diverse large-scale environments and do not preferentially reside in denser environments compared to HAEs. Their overdensity field, δ , averaged over (15 h −1 cMpc) 3 , ranges from −0.56 to 10.56, and shows no clear correlation with broad-line luminosity, black hole (BH) masses, or the AGN fraction. It suggests that >10 cMpc structures do not significantly influence BH growth. We measure the two-point cross-correlation function of AGNs with HAEs, finding a comparable amplitude to that of the HAE autocorrelation. This indicates similar bias parameters and host dark matter halo masses for AGNs and HAEs. The correlation length of field AGNs is 4.26 h −1 cMpc and 7.66 h −1 cMpc at 3.9 < z < 5 and 5 < z < 6, respectively. We infer a median host dark matter halo mass of log ( M h / M ⊙ ) ≈ 11.0 − 11.2 and host stellar masses of log ( M ⋆ / M ⊙ ) ≈ 8.4 – 8.6 by comparing with the U niverse M achine simulation. Our clustering analysis suggests that low-luminosity AGNs at high redshift reside in normal star-forming galaxies with overmassive BHs. They represent an intrinsically distinct population from luminous quasars and could be a common phase in galaxy evolution.

Abstract Microlensing observations suggest that the mass distribution of free-floating planets (FFPs) follows a declining power law with increasing mass. The origin of such distribution is unclear. Using a population synthesis framework, we investigate the formation channel and properties of FFPs, and compare the predicted mass function with observations. Assuming FFPs originate from planet–planet scattering and ejection in single star systems, we model their mass function using a Monte Carlo based planet population synthesis model combined with N -body simulations. We adopt a realistic stellar initial mass function, which naturally results in a large fraction of planetary systems orbiting low-mass stars. The predicted FFP mass function is broadly consistent with observation: it follows the observed power law at higher masses (10 ≲ m / M ⊕ < 10 4 ), while at lower masses (0.1 < m / M ⊕ ≲ 10) it flattens, remaining marginally consistent with the lower bound of the observational uncertainties. Low-mass, close-in planets tend to remain bound, while Neptune-like planets at wide orbits dominate the ejected population due to their large Hill radii and shallow gravitational binding. We also compare the mass distribution of bound planets with microlensing observations and find reasonably good agreement with both surveys. Our model predicts ≃1.20 ejected planets per star in the mass range of 0.33 < m / M ⊕ < 6660, with a total FFP mass of ≃17.98 M ⊕ per star. Upcoming surveys will be crucial in testing these predictions and constraining the true nature of FFP populations.

Abstract We present FrankenBlast , a customized and improved version of the Blast web application. FrankenBlast associates transients to their host galaxies, performs host photometry, and runs a innovative spectral energy distribution fitting code to constrain host stellar population properties—all within minutes per object. We test FrankenBlast on 14,432 supernovae (SNe), ≈half of which are spectroscopically classified, and are able to constrain host properties for 9262 events. When contrasting the host stellar masses ( M * ), specific star formation rates (sSFR), and host dust extinction ( A V ) between spectroscopically and photometrically classified SNe Ia, Ib/c, II, and IIn, we determine that deviations in these distributions are primarily due to misclassified events contaminating the photometrically classified sample. We further show that the higher redshifts of the photometrically classified sample also force their M * and sSFR distributions to deviate from those of the spectroscopically classified sample, as these properties are redshift-dependent. We compare host properties between spectroscopically classified SN populations and determine if they primarily trace M * or SFR. We find that all SN populations seem to both depend on M * and SFR, with SNe II and IIn somewhat more SFR-dependent than SNe Ia and Ib/c, and SNe Ia more M * -dependent than all other classes. We find the difference in the SNe Ib/c and II hosts to be the most intriguing and speculate that SNe Ib/c must be more dependent on higher M * and more evolved environments for the right conditions for progenitor formation. All data products and FrankenBlast are publicly available, along with a developing FrankenBlast version intended for Rubin Observatory science products.

Extreme emission line galaxies (EELGs) are believed to significantly contribute to the star formation activity and mass assembly in galaxies. EELGs likely also play a leading role in the cosmic re-ionization as their interstellar medium may allow a significant fraction of their ionizing photons to escape ( > 5%). Finding low-redshift analogues of these high-z galaxies is therefore essential to characterizing the physical conditions in the interstellar medium of these galaxies and understanding the processes that re-ionized the Universe. We aimed to develop a robust and efficient method for the photometric identification of EELGs using the J-PAS survey. J-PAS will cover approximately 8500 deg2$ of the sky with 54 narrow-band filters in the optical range plus $i-SDSS, enabling detailed studies of the physical properties of these galaxies. In this work we focused on an initial subset of the survey: a 30 square degree area with complete observations in all bands. We combine equivalent width (EW) measurements from J-PAS narrow-band photometry with artificial intelligence techniques to identify galaxies with emission lines exceeding 300 Å. We validated our selection using spectroscopic data from DESI DR1 and characterized the selected sample through spectral energy distribution fitting with . CIGALE We identify 917 EELGs up to z = 0.8 over 30 deg2$, achieving a purity of 95% and a completeness of 96% for i-SDSS < 22.5 mag. Importantly, active galactic nucleus contamination was carefully considered and is estimated to be around 5%. Furthermore, a cross-match with DESI yielded 79 counterparts; their redshifts are in excellent agreement with our photometric estimates, thereby confirming the reliability of our redshift determination. In addition, the derived emission line fluxes are in good agreement with spectroscopic measurements. Moreover, the selected sample reveals strong correlations between the ionizing photon production efficiency (ξ_ ion ) and EW(H$β), which are consistent with previous observational studies at low and high redshifts and theoretical expectations. Finally, most of the sources surpass the ionizing efficiency threshold required for re-ionization, highlighting their relevance as local analogues of early-Universe galaxies.

Abstract We report the discovery of 45 compact hub-filament systems (HFSs; median size ∼2.4 pc) in infrared-dark clouds (IRDCs) in the W33 complex, located at the junction of the Scutum and Norma spiral arms. Using Spitzer 8 and 24 µ m, and unWISE 12 μ m images, HFSs are identified as regions where three or more filaments converge onto a central hub, appearing as absorption features toward IRDCs. In each IRDC, HFSs mainly lie at the intersections of elongated substructures, associated with groups of protostars and lacking radio continuum emission. Minimum Spanning Tree (MST) analysis shows that protostars are closely associated with the HFSs, with protostellar core separations of ≤0.7 pc, indicating strong clustering within fragmented structures. The HFSs form two main groupings spanning 10–15 pc, with member separations of 1–3.3 pc. Around 65% are tightly clustered (<2 pc), exhibiting rich small-scale structures and emphasizing the uniqueness of the complex. MST analysis of ALMAGAL 1.38 mm continuum cores—predominantly low-mass and embedded in 10 HFSs—reveals a median core separation of ∼0.03 pc. The protostellar spacing (∼0.7 pc) significantly exceeds the thermal Jeans length (∼0.08 pc for temperature ∼18 K and density ∼10 5 cm −3 ), whereas the core spacing is smaller than the Jeans length, suggesting that thermal fragmentation may influence core formation but alone cannot explain the larger-scale protostellar distribution. All these findings together support a picture in which fragments of clouds/filaments form clumps hosting compact HFSs that facilitate efficient and clustered star formation, often yielding massive stars.

Blue stragglers are anomalously massive core hydrogen-burning stars that, according to the theory of single star evolution, should not exist. They are suspected to form in mass-enhancement processes, involving binary evolution or stellar collisions. In dynamically active systems like globular clusters, the number of blue stragglers originated by collisions is expected to increase with the local density and the rate of stellar encounters. Here we analyze more than 3000 blue stragglers in 48 Galactic globular clusters with different structures, finding that their number normalized to the sampled luminosity anti-correlates (instead of correlating) with the central density, collision rate, and dynamical age of the parent cluster. Similar trends are also found for the cluster binary fraction. Once inserted in the context of the current knowledge of the BSS phenomenon, these correlations indicate that low-density regions (possibly because of a higher binary production/survival rate) are the natural habitat of both BSSs and binary systems, and the observed BSSs mostly have a binary-related origin mediated by the environmental conditions.

Boson Stars are macroscopic self-gravitating configurations made of complex scalar fields. These exotic compact objects would manifest as dark Boson stars and, in the absence of electromagnetic signatures, could mimic properties of compact stars in the gravitational wave spectrum. In a recent study, using the simplest potential for massive Boson stars, we demonstrated that fundamental non-radial oscillations (f-modes) obey scaling relations that allow them to be distinguished from neutron stars and black holes. In this work, we provide analytical fits for these scaling relations, valid for the dark matter parameter space compatible with current astrophysical and cosmological data, that can be directly incorporated into future studies of massive Boson stars in the strong coupling regime, avoiding the need for numerical calculations. We also provide analytical fits for empirical and universal relations for gravitational wave asteroseismology, which can be used to infer microscopic dark matter properties following a successful detection. Further, we investigate the possibility of detection of f-modes and the dark matter parameter space that can be probed with current and future gravitational wave detectors across multiple frequency bands.Assuming a burst GW model and demanding a signal-to-noise ratio of 5, we show that the current and future detectors can, in principle, probe Boson star f-modes up to cosmological distances: 1 Mpc with aLIGO, 30 Mpc with Cosmic Explorer and Einstein Telescope, and in the best case scenario, about 300 Mpc with LISA.

Maximum mass of singularity-free anisotropic compact stars in Rastall theory of gravity

Abstract For more than half a century, the puzzling W-type phenomenon in contact binaries has challenged astrophysicists. In these systems, the less massive component exhibits a higher surface temperature than its more massive companion, which is a reversal of the typical A-type configuration, where the more massive star is hotter. This counterintuitive temperature inversion defies basic stellar physics and still lacks a widely accepted explanation. In this study, we assembled a sample of over 3000 extensively observed contact binaries and derived their complete set of physical parameters. Our statistical analysis revealed a strong positive correlation between the occurrence of W-type contact binaries and the intensity and frequency of magnetic activities. This result strongly supports the hypothesis that magnetic activities are the primary driver of the W-type phenomenon and offers a compelling explanation for the observed transitions between the W-type and A-type.

Abstract We present a comprehensive analysis of four young open clusters, NGC 663, NGC 2301, NGC 2384, and NGC 7510, utilizing high-precision astrometric and photometric data from Gaia DR3. Cluster membership was determined using the UPMASK algorithm, resulting in probable member counts ranging from 337 to 1498 across the clusters. Bayesian MCMC isochrone fitting yielded cluster ages in the range log t ∼7.0–8.15, with uncertainties of ∼0.11–0.18. Reddening values ranged from E(B − V ) = 0.093 mag in NGC 2301 to 1.24 mag in NGC 7510, consistent with their positions near the Galactic plane. The stellar mass function slopes (α ≈ 2.00–2.26) closely match the Salpeter IMF, with total stellar masses spanning nearly an order of magnitude, from ∼486 M ⊙ in NGC 2301 to ∼3584 M ⊙ in NGC 663. Dynamical relaxation times indicate that only NGC 2301 ( τ ≈ 10.00) and NGC 2384b ( τ ≈ 2.03) are dynamically relaxed; the others remain dynamically evolving. Orbital integrations in the MWPotential2014 model reveal nearly circular Galactic orbits with very low eccentricities (e ≈ 0.003–0.014) and small vertical distances (Z max < 0.142 kpc), confirming their confinement to the thin disk. SED and kinematic analysis show that NGC 2384 a & b are separated by ∼0.55 kpc, indicating an optical pairs.