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Abstract The phylum Mollusca constitutes one of the most taxonomically and morphologically diverse animal clades; however, the genomic exploration of this group has been hampered by fragmented and taxonomically incomplete transcriptomic resources. To address this fundamental limitation, we present MolluscaGenes, a centralized database that unifies transcriptomes from 299 molluscan species spanning all eight recognized classes, encompassing a broad array of tissues and developmental stages. MolluscaGenes provides searchable databases via BLAST and DIAMOND alongside a suite of 196 molluscan-optimized Hidden Markov Models (HMMs) for sensitive protein family identification. To demonstrate the utility of this resource, we performed a comprehensive phylum-wide characterization of the nicotinic acetylcholine receptor (nAChR) superfamily, recovering 3,586 sequences from over 190 species and resolving 15 distinct phylogenetic clades. This analysis revealed substantial lineage-specific expansions across multiple molluscan classes, the identification of novel clades with substitutions in canonical ligand-binding residues, and the evolutionary placement of chemotactile receptors (CRs) and CR-like sequences as predominantly cephalopod clades within the broader nAChR phylogeny. MolluscaGenes constitutes a foundational resource that will accelerate the elucidation of the unique biology and evolutionary history of Mollusca. 

We compare satellite quenched fractions across three cosmological simulation suites (FIREbox, the FIRE-2 zoom-ins, and IllustrisTNG50) and observational datasets from Satellites Around Galactic Analogs (SAGA), ELVES, and the combined satellite population of the Milky Way (MW) and M31. To enable consistent comparisons, we select MW-mass hosts withM_halo = 10^11.9–10^12.2M_⊙and satellites with stellar masses of 10⁷–10¹⁰M_⊙, applying nearly uniform radial selections and a common quenching definition. All three simulations reproduce the strong observed trend that lower-mass satellites are more likely to be quenched, closely matching the stellar mass dependence seen in SAGA, ELVES, and the MW and M31 system. This agreement indicates that the mass dependence of satellite quenching is a robust outcome of contemporary galaxy formation models. Radial trends, however, show greater diversity. SAGA and ELVES exhibit gently declining quenched fractions with projected distance, consistent with stronger quenching at small radii. TNG50 most closely matches this behavior, while FIREbox remains broadly consistent with a weak radial trend within uncertainties. The FIRE-2 zoom-ins show suppressed quenched fractions at small projected distances, driven primarily by their paired MW–M31 analogs. We show that this discrepancy is not explained by host environment alone, but instead reflects atypical satellite populations in the paired systems, where star-forming and quenched satellites occupy distinct spatial distributions. Overall, our results demonstrate that stellar-mass-quenched fraction trends are robust across simulations and observations, while radial trends are more sensitive to the detailed properties and distributions of satellite populations. 

Abstract While galaxy rotation curves (RCs) provide one of the most powerful methods for measuring dark matter profiles in the inner regions of rotation-supported galaxies, at the dwarf scale there are factors that can complicate this analysis. Given the expectation of a universal profile in dark-matter-only simulations, the diversity of the observed RCs has become an often-discussed issue in Lambda cold dark matter cosmology on galactic scales. We analyze a suite of Feedback in Realistic Environments simulations of 10¹⁰–10¹²M_⊙halos with standard cold dark matter and compare the true circular velocity to RC reconstructions. We find that, for galaxies with well-ordered gaseous disks, the measured RC may deviate from the true circular velocity by at most ∼10% within the radius of the disk. However, nonequilibrium behaviors, noncircular motions, and nonthermal and nonkinetic stresses may cause much larger discrepancies, of ∼50% or more. Most RC reconstructions underestimate the true circular velocity, while some reconstructions transiently overestimate it in the central few kiloparsecs, due to dynamical phenomena. We further demonstrate that the features that contribute to these failures are not always visibly obvious in HIobservations. If such dwarf galaxies are included in galaxy catalogs, they may give rise to the appearance of “artificial” RC diversity that does not reflect the true variation in underlying dark matter profiles. 

Abstract We explore how a realistic surface brightness (SB) detection limit ofμ_V≈ 32.5 mag arcsec⁻²for stars at the edges of ultrafaint galaxies affects our ability to infer their underlying properties. We use a sample of 19 galaxies with stellar masses ≈400–40,000M_⊙simulated with FIRE-2 physics and baryonic mass resolution of 30M_⊙. The SB cut leads to smaller sizes, lower stellar masses, and lower stellar velocity dispersions than the values inferred without the cut. However, by imposing this realistic limit, our inferred galaxy properties lie closer to observed populations in the mass-size plane, better match observed velocity dispersions as a function of stellar mass, and better reproduce derived circular velocities as a function of half-light radius. For the most massive galaxies in our sample, the SB cut leads to higher mean [Fe/H] values, but the increase is not enough to match the observed MZR. Finally, we demonstrate that the common J. Wolf et al. dynamical mass estimator is less accurate when the SB cut is applied. For our lowest-mass galaxies, in particular, excluding the low-surface brightness outskirts causes us to overestimate their central dark-matter densities and virial masses. This suggests that attempts to use mass estimates of ultrafaint galaxies to constrain dark-matter physics or to place constraints on the low-mass threshold of galaxy formation must take into account surface brightness limits or risk significant biases. 

Abstract We study the intrinsic and observable shapes of approximately 700 star-forming galaxies with stellar masses of 10⁸–10¹¹M_⊙from the FIREbox simulation atz= 0. We calculate intrinsic axis ratios using inertia tensors weighted by three morphology types: “All Stars,” “Young Stars,” and “Luminosity-weighted Stars.” Young Stars shows mass-dependent 3D configurations, with spheroidal, elongated, and disky shapes dominant at stellar masses of 10^8.5, 10^9.5, and 10^10.5M_⊙, respectively. Using the radiative transfer codeSKIRT, we construct mock images for each galaxy and show that projected short-to-long axis ratios,q, inferred from 2D Sérsic fits are most closely related to Luminosity-weighted Stars tensor shapes and least resemble the All Stars’ shapes. This suggests observed 2D shape distributions should not be compared to predictions based on 3D stellar mass shapes. Next, we construct a sample of mock images projected in random orientations and compare them to observed axis ratio distributions from the GAMA survey. At stellar masses below 10¹⁰M_⊙, we produce too few galaxies with observedq < 0.4 and none withq < 0.2, suggesting that FIREbox does not produce enough low-mass disk galaxies. At higher masses, 10¹⁰–10¹¹M_⊙, we find that the predictedqdistribution is sensitive to the dust-to-metal ratio; using our fiducial model, the distribution ofqvalues is formally consistent with observations, but there is tension with our ability to produce enough very thin systems withq < 0.2. Future observational and theoretical programs aimed at understanding disk and thin-disk fractions will provide crucial tests of galaxy formation models. 

It is widely believed that the ultraviolet background produced during the epoch of reionization conspires against the formation of low-mass galaxies. Indeed, this mechanism is often invoked as part of the solution to the so-called “missing satellites problem.” In this paper we employFIREbox, a large-volume cosmological simulation based on theFeedback In Realistic Environmentsphysics model, to characterize the mechanisms governing galaxy ignition in the postreionization era. By carefully matching recently ignited halos (with stellar ages below 100 Myr at the time of selection) to halos that failed to form any stars, we conclude that the presence of cold dense gas and halo concentration helps incite the process of galaxy formation. Concretely, we find that 100% of recently ignited halos experience cold dense gas enhancements relative to their matched failed counterparts. Likewise, approximately 83% display enhancements in both cold dense gas and Navarro–Frenk–White concentration (c_NFW), while the remaining ∼17% exhibit enhanced cold dense gas content and suppressedc_NFWvalues. Lastly, our simulation suggests that galaxy ignition can occur as late asz= 2, potentially allowing us to observationally catch this process “in the act” in the foreseeable future. 

ABSTRACT Decapod crustaceans regulate molting through steroid molting hormones (ecdysteroids) synthesized by the molting gland (Y-organ, YO). Molt-inhibiting hormone (MIH), a neuropeptide synthesized and secreted by the eyestalk ganglia, negatively regulates YO ecdysteroidogenesis. MIH signaling is mediated by cyclic nucleotide second messengers. cGMP-dependent protein kinase (PKG) is the presumed effector of MIH signaling by inhibiting mechanistic Target of Rapamycin Complex 1 (mTORC1)-dependent ecdysteroidogenesis. Phylogenetic analysis of PKG contiguous sequences in CrusTome, as well as 35 additional species in NCBI RefSeq, identified 206 PKG1 sequences in 108 species and 59 PKG2 sequences in 53 species. These included four PKG1α splice variants in the N-terminal region that were unique to decapods, as well as PKG1β and PKG2 homologs. In vitro assays using YOs from the blackback land crab (Gecarcinus lateralis) and green shore crab (Carcinus maenas) determined the effects of MIH±PKG inhibitors on ecdysteroid secretion. A general PKG inhibitor, Rp-8-Br-PET-cGMPS, countered the effects of MIH, as ecdysteroid secretion increased in PKG-inhibited YOs compared with C. maenas YOs incubated with MIH alone. By contrast, a PKG2-specific inhibitor, AP-C5 {4-(4-[1H-imidazol-1-yl]phenyl)-N-2-propyn-1-yl-2-pyrimidinamine}, enhanced the effects of MIH, as ecdysteroid secretion decreased in G. lateralis and C. maenas YOs incubated with AP-C5 and MIH compared with YOs incubated with MIH alone. These data suggest that both PKG1 and PKG2 are activated by MIH, but have opposing effects on mTORC1-dependent ecdysteroidogenesis. A model is proposed in which the dominant role of PKG1 is countered by PKG2, resulting in low ecdysteroid production by the basal YO during intermolt. 

Abstract Integral field units have extended our knowledge of galactic properties to kiloparsec (or, sometimes, even smaller) patches of galaxies. These scales are where the physics driving galaxy evolution (feedback, chemical enrichment, etc.) take place. Quantifying the spatially resolved properties of galaxies, both observationally and theoretically, is therefore critical to our understanding of galaxy evolution. To this end, we investigate spatially resolved scaling relations within galaxies ofM_⋆ > 10^9.0atz= 0 in IllustrisTNG. We examine both the resolved star formation main sequence (rSFMS) and the resolved mass–metallicity relation (rMZR) using 1 kpc × 1 kpc maps. We find that the rSFMS in IllustrisTNG is well described by a power law but is significantly shallower than the observed rSFMS. However, the disagreement between the rSFMS of IllustrisTNG and observations is likely driven by an overestimation of AGN feedback in IllustrisTNG for the higher-mass hosts. Conversely, the rMZR for IllustrisTNG has very good agreement with observations. Furthermore, we argue that the rSFMS is an indirect result of the Schmidt–Kennicutt law and local gas relation, which are both independent of host galaxy properties. Finally, we expand upon a localized leaky-box model to study the evolution of idealized spaxels and find that it provides a good description of these resolved relations. The degree of agreement, however, between idealized spaxels and simulated spaxels depends on the “net” outflow rate for the spaxel, and the IllustrisTNG scaling relations indicate a preference for a low net outflow rate. 

ABSTRACT We study the morphology of hundreds of simulated central galaxies in the stellar mass range $$M_\star =$$ 107.5–1011  $$\rm M_\odot$$ from the FIREbox cosmological volume. We demonstrate that FIREbox is able to predict a wide variety of morphologies, spanning from disc-dominated objects to spheroidal galaxies supported by stellar velocity dispersion. However, the simulations predict a strong relation between morphology (degree of rotational support) and stellar mass: galaxies comparable to the Milky Way are often disc-dominated while the presence of stellar discs mostly vanishes for dwarfs with $$M_\star < 10^9 ~$$\rm M_\odot$$. This defines a ‘morphology transition’ regime for galaxies with $$10^9 < M_\star /\rm {M_\odot }< 10^{10}$$ in which discs become increasingly common, but below which discs are rare. We show that burstiness in the star formation history and the deepening of the gravitational potential strongly correlate in our simulations with this transition regime, with discs forming in objects with lower levels of burstiness in the last $$\sim 6$$ Gyr and haloes with mass $$\sim 10^{11} ~ \rm {{\rm M}_{\odot }}$$ and above. While observations support a transition towards thicker discs in the regime of dwarfs, our results are in partial disagreement with observations of at least some largely rotationally supported gas discs in dwarfs with $$M_\star < 10^9$$\rm M_\odot$$. This study highlights dwarf morphology as a fundamental benchmark for testing future galaxy formation models. 

Abstract We utilize the cosmological volume simulation FIREbox to investigate how a galaxy’s environment influences its size and dark matter content. Our study focuses on approximately 1200 galaxies (886 central and 332 satellite halos) in the low-mass regime, with stellar masses between 10⁶and 10⁹M_⊙. We analyze the size–mass relation (r₅₀–M_⋆), the inner dark matter mass–stellar mass ( $M_{\mathrm{DM}}^{50}$–M_⋆) relation, and the halo mass–stellar mass (M_halo–M_⋆) relation. At fixed stellar mass, we find that galaxies experiencing stronger tidal influences, indicated by higher Perturbation Indices (PI > 1) are generally larger and have lower halo masses relative to their counterparts with lower Perturbation Indices (PI < 1). Applying a Random Forest regression model, we show that both the environment (PI) and halo mass (M_halo) are significant predictors of a galaxy’s relative size and dark matter content. Notably, becauseM_halois also strongly affected by the environment, our findings indicate that environmental conditions not only influence galactic sizes and relative inner dark matter content directly, but also indirectly, through their impact on halo mass. Our results highlight a critical interplay between environmental factors and halo mass in shaping galaxy properties, affirming the environment as a fundamental driver in galaxy formation and evolution.