Kavli Affiliate: Ke Wang
| First 5 Authors: Yu Cheng, Xing Lu, Patricio Sanhueza, Hauyu Baobab Liu, Qizhou Zhang
| Summary:
Filamentary structures are ubiquitously found in high-mass star-forming
clouds. To investigate the relationship between filaments and star formation,
we carry out the INFANT (INvestigations of massive Filaments ANd sTar
formation) survey, a multi-scale, multi-wavelength survey of massive
filamentary clouds with ALMA band 3/band 6 and VLA K band. In this first paper,
we present the ALMA band 6 continuum observations toward a sample of 8
high-mass star forming filaments. We covered each target with approximately
rectangular mosaic field of view with two 12-m array configurations, achieving
an angular resolution of $sim$0.6" (2700 AU at 4.5 kpc) and a continuum rms of
$sim$0.1 mJy/beam ($sim$0.06 Msun in gas mass assuming 15 K). We identify
cores using the getsf and astrodendro and find the former is more robust in
terms of both identification and measuring flux densities. We identify in total
183 dense cores (15–36 cores in each cloud) and classify their star formation
states via outflow and warm gas tracers. The protostellar cores are
statistically more massive than the prestellar cores, possibly indicating
further accretion onto cores after formation of protostars. For the high-mass
end ($M_text{core}$ $>$ 1.5 Msun) of the core mass function (CMF) we derive a
power-law index of $-$1.15 $pm$ 0.12 for the whole sample, and $-$1.70 $pm$
0.25 for the prestellar population. We also find a steepening trend in CMF with
cloud evolution ($-$0.89 $pm$ 0.15 for the young group v.s. $-$1.44 $pm$ 0.25
for the evolved group) and discuss its implication for cluster formation.
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