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We investigate the global properties of the straight and isolated filamentarycloud G350.54+0.69 using Herschel continuum and APEX molecular line data. Theoverall straight morphology is similar to two other well studied nearbyfilaments (Musca and Taurus-B211/3) while the isolated nature of G350.54+0.69appears similar to Musca. G350.54+0.69 is composed of two distinct filamentswith a length ~5.9 pc for G350.5-N (~2.3 pc for G350.5-S), a total mass of ~810$M_{\odot}$ (~ 110 $M_{\odot}$), and a mean temperature of ~ 18.2 K (~17.7 K).We identify 9 dense and gravitationally bound cores in the whole cloudG350.54+0.69. The separations between cores and the line mass of the wholecloud appear to follow the predictions of the "sausage" instability theory,which suggests that G350.54+0.69 could have undergone radial collapse andfragmentation. The presence of young protostars is consistent with thishypothesis. The line masses of the two filaments (~120 $M_{\odot}$ pc$^{-1}$for G350.5-N, and ~45 $M_{\odot}$ pc$^{-1}$ for G350.5-S), mass-sizedistributions of the dense cores, and low-mass protostars collectively suggestthat G350.54+0.69 is a site of ongoing low-mass star formation. Based on theabove evidence, we place G350.54+0.69 in an intermediate evolutionary statebetween Musca and Taurus-B211/3. We suggest that investigations into straight(and isolated) versus those distributed inside molecular clouds may provideimportant clues into filament formation and evolution.

The straight and isolated G350.54+0.69 filament: density profile and star formation content