Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 2610.32826

Research of signs of star formation in three S0 galaxies - members of isolated pairs

I. S. Proshina·O. K. Sil'chenko·A. Yu. Kniazev·D. V. Oparin
View original source ↗Read source document ↗Export metadata ↓

Abstract

We obtained and analyzed long-slit spectra of three lenticular galaxies with optical rings: PGC 48114, ESO 234-011, and ESO 444-076. Ionized gas was detected in all of them. In PGC 48114, the excitation mechanism of the ionized gas differs along the ring, despite the consistent kinematics of the ionized gas and stars, as we showed earlier. Narrow-band images of PGC 48114 in the H$α$ and [NII]$λ$6583 emission lines revealed a star formation arc in the northwestern part of the ring. In ESO 234-011 and ESO 444-076, the ionized gas along the long slit is shock-excited and have kinematic discrepancy with the stars. This implies accretion of matter at an angle to the main disk of the S0 galaxies, which likely inhibits ongoing star formation. The companions of these S0 galaxies are late-type galaxies with extensive ongoing star formation. These companions may be the sources of the gas, or each pair may be feeding from a common gas reservoir.

Explore related subjects

astro-ph.GA

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

I. S. Proshina, O. K. Sil'chenko, A. Yu. Kniazev, D. V. Oparin. 2026-10-23. Research of signs of star formation in three S0 galaxies - members of isolated pairs. https://arxiv.org/abs/2610.32826

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

UCLCHEM 4.0: An open source gas-grain astrochemistry simulation framework

Astrochemical modelling is a key tool for interpreting the formation and destruction of molecules in the interstellar medium, complementing the increasingly detailed observations enabled by modern day observational facilities. UCLCHEM is a comprehensive gas-grain astrochemical modelling framework that can compute the chemical evolution inside a parcel of gas and dust under a specified, time-dependent physical description. This allows both the post-processing of hydrodynamical simulations and the usage of physical parametrizations, ranging in context from extra-galactic to protoplanetary disk scales. The framework consists of a core routine that solves gas-grain chemical reaction networks as a function of time, self-consistently coupled to either a user-defined or parametrized physical evolution of density, temperature and other physical input parameters. The chemistry is solved with a rate-equation formalism, and includes a three phase description, namely gas phase, ice surface and bulk ice. This includes transport between the gas and ice phases via freeze-out, thermal and non-thermal desorption mechanisms, as well as a geometrical treatment of the growth and shrinkage of the surface and bulk chemistry. The framework includes parametrizations for astrochemical modelling of cloud collapses, protostellar cores and shocks as well as the ability to provide user-defined inputs. This release of the framework focuses on many quality-of-life-improvements, including an object-oriented Python interface, an upgrade from two phase to three phases and expanded support for post-processing of hydrodynamical simulations and user-defined parametrizations. This manuscript provides an overview of the physics and chemistry included in UCLCHEM, as well as the inner workings of the solver routine and the programming interface.

astro-ph.GA↗
arXiv2026

Even central galaxies feel their environment: cosmic siphoning of cool gas accretion

Identifying the key processes regulating cool gas accretion in galaxies is essential for understanding the baryon cycle within galactic ecosystems. Recent studies indicate that the most fundamental internal process is likely the competition between halos and central black holes. This is revealed through a universal relation between increasing black hole masses and decreasing cool gas fraction ($μ_{\rm HI} \equiv M_{\rm HI}/M_{\star} \propto M_{\rm BH}^{-0.6}$). Here we further explore the primary external effects on cool gas accretion in central galaxies. We find that galaxies deviating significantly from the $μ_{\rm HI}-M_{\rm BH}$ relation are overwhelmingly isolated central galaxies without substantial satellites. These isolated, gas-poor centrals exhibit systematically higher black-hole-to-stellar-mass ratios and more prominent bulges. At larger scales, they are preferentially located near massive neighboring halos. We suggest that this may reflect a ``cosmic siphoning" scenario, replenished by their satellites and by gas flowing along the cosmic web. This model naturally explains the prevalence of gas-poor isolated central galaxies near massive halos. It complements internal regulation by supermassive black holes and suggests a cosmic 'rich get richer' scenario.

astro-ph.GA↗
arXiv2026

Decoupling candidate dual AGN from chance superpositions in the GOTHIC survey via a deep-learning framework

Dual active galactic nuclei (DAGN) mark a critical phase in the evolution of merging galaxies and the pairing of supermassive black holes, yet they remain difficult to identify in large imaging surveys because of projection effects and limited spatial resolution. Compact foreground stars and unresolved substructure can mimic dual nuclei through chance superposition, complicating automated detection. We revisit the 46,061 galaxies flagged but rejected as DAGN candidates by the GOTHIC pipeline, primarily because the two nuclei fell within the SDSS fibre aperture or exceeded its separation threshold. We train a supervised deep-learning framework based on the YOLOv11 oriented-bounding-box architecture on annotated SDSS imaging to separate genuine dual nuclei from foreground stellar contaminants and other spurious alignments. The final model attains a validation precision of 0.919, recall of 0.905, and $F_1$ of 0.912, and yields 29,605 dual-nucleus candidates after removing star-dominated and blended detections. Structured visual inspection indicates that $54.5$--$62\%$ are consistent with genuine dual nuclei, implying $\sim(1.4$--$1.8)\times10^{4}$ plausible systems. Cross-calibrating the YOLO separation against the deterministic GOTHIC centroid measurement and restricting to the compact regime ($d \le 6.87''$) gives a conservative subset of $\sim 13{,}672$ candidates, reaching calibrated separations of $\sim 0.56''$. Spectroscopy of the most compact ($\le 1$ kpc) systems shows spectra dominated by stellar absorption, with no resolved double-peaked emission, so confirmation requires higher-resolution follow-up. The catalogue is a statistically refined list of candidates, not confirmed DAGN. Nonetheless, deep-learning detection substantially reduces contamination and expands the plausible DAGN census.

astro-ph.GA↗