Probing the filamentary nature of star formation in the California giant molecular cloud

Abstract

Recent studies suggest that filamentary structures are representative of the initial conditions of star formation in molecular clouds and support a filament paradigm for star formation, potentially accounting for the origin of the stellar initial mass function (IMF). Using Herschel imaging observations of the California giant molecular cloud, we aim to further investigate the filament paradigm for low- to intermediate-mass star formation and to better understand the exact role of filaments in the origin of stellar masses. Using the multiscale, multiwavelength extraction method getsf, we identify starless cores, protostars, and filaments in the Herschel data set and separate these components from the background cloud contribution to determine accurate core and filament properties. Both the prestellar core mass function (CMF) and the distribution of filament masses per unit length or filament line mass function (FLMF) are consistent with power-law distributions at the high-mass end, $\Delta N/\Delta \log M\propto M^{-1.4\pm 0.2}$ at $M>1M_{\odot }$ for the CMF and $\Delta N/\Delta \log M_{\mathrm{line}}\propto M_{\mathrm{line}}^{-1.5\pm 0.2}$ for the FLMF at $M_{\mathrm{line}}>10M_{\odot }\mathrm{p}{\mathrm{c}}^{-1}$, which are both consistent with the Salpeter power-law IMF. Based on these results, we propose a revised model for the origin of the CMF in filaments, whereby the global prestellar CMF in a molecular cloud arises from the integration of the CMFs generated by individual thermally supercritical filaments within the cloud. Our findings support the existence a tight connection between the FLMF and the CMF/IMF and suggests that filamentary structures represent a critical evolutionary step in establishing a Salpeter-like mass function.

16 pages, 22 figures, accepted for publication in Astronomy & Astrophysics

References in corpus (28)

• Filamentary structure of star-forming complexes
• On the Star Formation Efficiency of Turbulent Magnetized Clouds
• Identifying the Low Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores
• What determines the density structure of molecular clouds ? A case study of Orion B with Herschel
• A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition
• A Large Catalog of Accurate Distances to Molecular Clouds from PS1 Photometry
• The identification of filaments on far infrared and submillimiter images. Morphology, physical conditions and relation with star formation of filamentary structure
• Properties of the dense core population in Orion B as seen by the Herschel Gould Belt survey
• The Herschel view of the dense core population in the Ophiuchus molecular cloud
• Multiscale, multiwavelength extraction of sources and filaments using separation of the structural components: getsf
• From diffuse gas to dense molecular cloud cores
• Interstellar filaments and star formation
• Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds
• Probing fragmentation and velocity sub-structure in the massive NGC 6334 filament with ALMA
• On the typical width of Herschel filaments
• Fragmentation of star-forming filaments in the X-shape Nebula of the California molecular cloud
• Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds
• Analytical core mass function (CMF) from filaments: Under which circumstances can filament fragmentation reproduce the CMF?
• 3D shape explains star formation mystery of California and Orion A
• Compressed magnetized shells of atomic gas and the formation of the Corona Australis molecular cloud
• Witnessing the fragmentation of a filament into prestellar cores in Orion B/NGC 2024
• TRAO Survey of Nearby Filamentary Molecular clouds, the Universal Nursery of Stars (TRAO FUNS) I. Dynamics and Chemistry of L1478 in the California Molecular Cloud
• The Bolocam Galactic Plane Survey. XIII. Physical Properties and Mass Functions of Dense Molecular Cloud Structures
• Background derivation and image flattening: getimages
• Multicomponent, multiwavelength benchmarks for source- and filament-extraction methods
• A wide-field CO survey towards the California Molecular Filament
• Properties of the dense cores and filamentary structures in the Vela C molecular cloud
• Inaccuracies and biases of the Gaussian size deconvolution for extracted sources and filaments

Cited by in corpus (3)

• Understanding the Star Formation Efficiency in Dense Gas: Initial Results from the CAFFEINE Survey with ArTéMiS
• Investigations of MWISP Filaments. I. Filament Identification and Analysis Algorithms, and Source Catalogue
• Scale-dependent surface and volume density properties of filaments in molecular clouds