Searcharxiv⌕ Search

arXiv · 2609.23302

Hierarchical Dynamics within Molecular Clouds: Type 4 Scaling Relations of Molecular Clouds in the Second Galactic Quadrant

Abstract

We present a statistical study of the hierarchical structure of molecular clouds in the second quadrant of the Galactic midplane (139.75 deg <= l <= 159.75 deg, -5.25 deg <= b <= 8.25 deg), based on high-sensitivity 12CO and 13CO J = 1-0 data from the Milky Way Imaging Scroll Painting survey. Using DBSCAN and a non-binary Dendrogram algorithm, we identify 2,912 13CO clouds. Type 2 (multicloud, single-tracer) scaling relations show arm-dependent trends: the power-law index of the linewidth-size relation is about 0.32 in the Local Arm and about 0.42 in the Perseus and Outer Arms. The classical Keto-Heyer relation is weak in the Local Arm but present in the Perseus and Outer Arms, with a slope of about 0.3. The virial parameter is anti-correlated with cloud size, mass, and surface density, consistent with previous surveys. Type 4 (single-cloud, single-tracer) scaling relations exhibit stronger internal correlations. The linewidth-size index spans about 0.3-0.8 and correlates positively with sonic Mach number, indicating that the relation is not universal but depends on cloud compressibility. While substructures do not follow the conventional surface-density-based Keto-Heyer relation, a volume-density formulation restores a clear virial scaling, with evolutionary tracks aligning along lines of constant virial parameter. Moreover, the structural complexity of molecular clouds, characterized by the relationship between the number of substructures and the min_delta parameter, correlates with surface density rather than sonic Mach number, contrary to results from turbulence-only magnetohydrodynamic simulations. Together, these results are more consistent with a gravity-regulated hierarchical dynamical picture than with a purely turbulence-supported scenario.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Suziye He, Yuehui Ma, Xuepeng Chen, Hongchi Wang, Miaomiao Zhang, Zhenyi Yue, Xiangyu Ou. 2026-09-20. Hierarchical Dynamics within Molecular Clouds: Type 4 Scaling Relations of Molecular Clouds in the Second Galactic Quadrant. https://arxiv.org/abs/2609.23302

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

KEEP EXPLORING

Related papers

Correcting for the effects of the point spread function in intra-halo light measurements and application to deep Hyper Suprime-Cam data

The intra-halo light (IHL) is the diffuse stellar component that surrounds galaxies, groups, and clusters. Its formation is linked to the hierarchical assembly of the system, making it a key tracer of galaxy evolution. However, the low surface brightness of the IHL makes it challenging to detect and distinguish from the point spread function (PSF) effect of the telescope. In this paper, we present an innovative technique that corrects for PSF-scattering effects in astronomical images. We use this method to provide a statistically robust estimation of the IHL in galaxy groups and clusters by fitting an exponential model to this component using an MCMC optimiser algorithm. To test our methodology, we build 5440 mock observations of Galaxy And Mass Assembly (GAMA) groups using data from the Hyper Suprime-Cam Subaru Strategic Program Public Data Release 3 (HSC-SSP PDR3). Each mock contains an IHL component with a flux fraction ($f_{\mathrm{IHL}}$) ranging from 0.01 to 0.5. Our results demonstrate the importance of properly removing the PSF-scattered light, especially at lower $f_{\mathrm{IHL}}$. The IHL effective radius is overestimated by $\sim9.1$ and $\sim2$ at $f_{\mathrm{IHL}}=0.01$ and $0.5$, respectively, while the IHL flux requires correction for $f_{\mathrm{IHL}} < 0.4$, with an overestimate of $\sim84.4$ at $f_{\mathrm{IHL}} = 0.01$. After applying our PSF correction, the recovered flux and effective radius are much closer to their true values. inally, we apply our methodology to HSC-PDR3 UD real observations of the GAMA group G400138 in the $\textit{g,r}$ and $\textit{i}$-bands, finding median IHL fractions of: $f_{\mathrm{g,IHL}}$ $\sim$ 0.19$^{+0.09}_{-0.01}$, $f_{\mathrm{r,IHL}}$ $\sim$ 0.08$^{+0.06}_{-0.02}$, and $f_{\mathrm{i,IHL}}$ $\sim$ 0.06$^{+0.04}_{-0.02}$.

astro-ph.GA↗

ASKAP discovery of a pair of large radio bubbles: on the origin of odd radio circles

We report the serendipitous discovery of a large, low-surface-brightness radio bubble in 944 MHz continuum data from the ASKAP Evolutionary Map of the Universe (EMU) survey. The structure, centred on the elliptical galaxy LEDA 217397 at a redshift of $z=0.040$, spans $\sim$8.4 arcmin, corresponding to a projected diameter of $\sim$399 kpc, and consists of two partly overlapping shells both with radii of $\sim$114 kpc. The integrated flux density of the bubble is $56.8\pm2.9$ mJy at 944 MHz, implying a rest-frame 1.4 GHz luminosity of $\sim$ $1.4\times10^{23}$ W Hz$^{-1}$. Combining the EMU measurement with MWA GLEAM-X data at 88--185 MHz, we derive a steep integrated spectral index of $α=-1.04\pm0.04$, and a two-frequency spectral-index map suggesting a possible exterior flattening. Spectral Energy Distribution (SED) fitting indicates a massive ($\log M_{\ast}/M\odot = 10.97\pm0.09$), quiescent (SFR=$0.025\pm0.083\,M\odot$ yr$^{-1}$) early-type host with no mid-infrared AGN signature and no overdense environment. We compare the bubble with odd radio circles (ORCs) and large radio shells, and discuss three scenarios for its origin: a starburst-driven wind, a merger-driven shock, and AGN jet-inflated bubbles. The starburst wind is disfavoured on energetic grounds ($\gtrsim$$10^{59}$ erg required versus $\sim$$10^{8}$ yr electron lifetimes), and neither a halo-scale merger shock nor a spherical nuclear blast wave can explain the unusually regular, double-shell geometry; a bipolar nuclear outburst -- a relic AGN jet episode, possibly triggered by a supermassive-black-hole merger -- provides the most natural explanation, with later shocks possibly re-energising the plasma. Deeper broad-band radio, polarimetric, spectroscopic and X-ray observations are needed to confirm its nature.

astro-ph.GA↗

Rapid Growth of Intermediate-Mass Black Holes through Disk-induced Stellar Disruptions

Dense nuclear star clusters provide unique environments for studying the dynamical interactions between stars and massive black holes. When an accretion disk is present, dissipative star--disk interactions can capture surrounding stars, drive their inward migration, and ultimately lead to disk-induced tidal disruption events\,(dTDEs). The long-term feeding rate from this process, however, cannot be inferred from single-orbit migration estimates alone, as it depends on the coupled evolution of disk capture, collisional relaxation, stellar depletion and replenishment, and physical mergers within the star cluster. In this work, we use high-performance direct $N$-body simulations combined with analytic prescriptions for star--disk interactions to follow this coupled evolution for intermediate-mass black holes\,(IMBHs) with accretion disks embedded in dense stellar clusters. The simulations track the formation of the stellar cusp, the capture of stars by repeated disk crossings, their subsequent orbital damping and migration, and their eventual consumption by the central IMBH. We find that dTDEs can sustain stellar mass supply rates of $\sim10^{-3}\,M_\odot \,\mathrm{yr}^{-1}$, which exceeds the Eddington-limited gas accretion rate for IMBHs with $M_\bullet<10^5\,M_\odot$. These results identify dTDEs as an efficient stellar feeding channel for IMBHs in gas-rich dense stellar systems. As one possible application, this mechanism may help transform $\sim10^3\,M_\odot$ IMBHs into more massive black-hole seeds, provided that compact stellar clusters and accretion disks persist for $>30$ Myr.

astro-ph.GA↗