[PDF] Top 20 Filament Fragmentation in High-Mass Star Formation

... the filament exceed the Jeans length at the given densities and ...resolved fragmentation and/or fragments below our sensitivity limit, the difference between Jeans length and projected frag- ment ... See full document

... The 30 Doradus region is a complex and dynamic region that contains multiple, although not necessarily spatially distinct, generations of stars (see Walborn & Blades 1997). The youngest population is dominated by the ... See full document

... total mass in compact ...the mass estimates for these sources, which are quite sensitive to the opacity correction term in equation 1 (in particular for MM2, see also Table 2 of Cyganowski et ...clump ... See full document

... relatively high intensities in all the mid-infrared and far-infrared bands and have high dust luminosity and dust ...has high surface brightness for most of the input values, regions 1, 2, and 9 to ... See full document

... the high density cavity walls, which dominated the image morphology, however the emission from the cavity, which dominated the total flux, was unchanged, and therefore the spectral index of the model integrated ... See full document

... at high-redshift as the gas fraction increases significantly ...and star formation simultane- ously, allowing a new episode of black hole ...to high-resolution imag- ing with HST (Miley et ... See full document

... mass star formation region ( HMSFR ) known, with only the Orion Nebula being ...generate high-mass ...individual high-mass ...and high angular resolution images of ... See full document

... To investigate how much millimetre emission might arise from the ionized material, we extrapolated the combined 6-cm flux of VLA 2 and VLA 3 to 2.7 mm, assuming a spectral index of α = 0.38 ± 0.14 and that the spectrum ... See full document

... galaxy formation, as originally proposed by White & Rees (1978), gas condenses at the center of hierarchically merging dark matter ...The mass function of dark matter halos, which grow hierarchically by ... See full document

... temperatures (T ≥ 100 K) than the conditions under which the 44.1- GHz maser is the strongest class I methanol transition. Gorski et al. (2017) show that much of the 36.2-GHz methanol emission is lo- cated at the edge of ... See full document

... the mass loading η , dened as the ratio of the outow rate to the ...total mass of gas particles passing through a plane at z = ± 5 kpc, where the z-axis is the rotation axis of the ...The mass ... See full document

... enough mass to become stars, whereas the ones that stay in the outer disc region increase in mass but not as much, becoming brown ...central star at relatively wide orbits (∼ 200 − 10 4 ... See full document

... tween the measured and the theoretical unattenuated flux is be- low 10%. The bright UCHII G049.4905 − 00.3688 has the high- est computed di ff erence ( ∼ 56.4%). The distribution of the flux difference due to ... See full document

... The uncertainties in μx , μy for both sources correspond to internal motions of 10 km s−1 in the maser emission and are consistent with proper motion estimates of 6.7-GHz methanol maser[r] ... See full document

... This work presented analyses of observations towards IRDC G035.39–00.33, previously found to be an excellent target to probe the initial conditions for high-mass star formation. Below the ... See full document

... with star formation ...with high-mass star formation (Young Stellar Objects, YSOs) and the other 10 per cent associated with either low-mass star formation ... See full document

... of star formation (SF) is still an ongoing research area in modern ...in star formation are: What is the effect of magnetic fields on MC core collapse? It has been suggested that magnetic ... See full document

... considering star-forming galax- ies only, with log 10 (sSF R) > ...selecting star-forming galaxies, we find no difference be- tween the median SFRs in low and high density ... See full document

... ded high-mass ...ing high optical depth toward these positions. This high optical depth as well as the missing flux only allows us to derive lower limits for the masses and column densities of ... See full document

... the fragmentation time-scale ...low star formation activity have been observed to contain significant density fluctuations ...the fragmentation of highly super-critical ... See full document