350 μm map of the Ophiuchus molecular cloud: core mass function

Zhang, Guo Yin; Li, Di; Hyde, A.; Qian, Lei; Lyu, Hua Lei; Wu, Zhong Zu

doi:10.1007/s11433-014-5561-7

Cited by 2 publications

(1 citation statement)

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“…Space telescopes avoid the absorption, distortion and contamination of light by Earthʼs atmosphere. The detected cores with Herschel can be an order of magnitude more in number than ground-based telescopes (e.g., Könyves et al 2015;Zhang et al 2015). Observations with Herschel show that filamentary structures at temperatures around 10-20 K are indeed ubiquitous in the cold ISM.…”

Section: Introductionmentioning

confidence: 94%

Herschel Investigation of Cores and Filamentary Structures in the Perseus Molecular Cloud

zhang¹,

Zhang²,

Li³

et al. 2022

Res. Astron. Astrophys.

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Cores and filamentary structures are the prime birthplaces of stars, and play key roles in the process of star formation. Latest advances in the methods of multi-scale source and filament extraction, and in making high-resolution column density map from Herschel multi-wavelength observations enable us to detect the filamentary network structures in highly complex molecular cloud environments. The statistics for physical parameters shows that core mass strongly correlates with core dust temperature, and M/L strongly correlates with M/T , which is in line with the prediction of the blackbody radiation, and can be used to trace evolutionary sequence from unbound starless cores to robust prestellar cores. Crest column densities of the filamentary structures are clearly related with mass per unit length (Mline ), but are uncorrelated by three orders ranging from ∼ 1020 to ∼ 1022 cm -2 with widths. Full width at half maximum (FWHM) have a median value of 0.15 pc, which is consistent with the 0.1 pc typical inner width of the filamentary structures reported by previous research. We find 70% of robust prestellar cores (135/199) embedded in supercritical filaments with M line > 16 M⊙ /pc, which implies that the gravitationally bound cores come from fragmentation of supercritical filaments. And on the basis of observational evidences that probability distribution function (PDF) with power-law distribution in the Perseus south is flatter than north, YSO number is significantly less than that in the north, and dust temperature difference. We infer that south region is more gravitationally bound than north region.

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Section: Introductionmentioning

confidence: 94%