INvestigations of massive Filaments ANd sTar formation (INFANT). I. Core Identification and Core Mass Function
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866909161873211392 |
|---|---|
| author | Cheng, Yu Lu, Xing Sanhueza, Patricio Liu, Hauyu Baobab Zhang, Qizhou Galván-Madrid, Roberto Wang, Ke Nakamura, Fumitaka Liu, Tie Feng, Siyi Li, Shanghuo Jiao, Sihan Tanaka, Kei E. I. Liu, Xunchuan Li, Pak Shing Luo, Qiuyi Gu, Qilao Lin, Yuxin Guzmán, András E. |
| author_facet | Cheng, Yu Lu, Xing Sanhueza, Patricio Liu, Hauyu Baobab Zhang, Qizhou Galván-Madrid, Roberto Wang, Ke Nakamura, Fumitaka Liu, Tie Feng, Siyi Li, Shanghuo Jiao, Sihan Tanaka, Kei E. I. Liu, Xunchuan Li, Pak Shing Luo, Qiuyi Gu, Qilao Lin, Yuxin Guzmán, András E. |
| contents | 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_03858 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | INvestigations of massive Filaments ANd sTar formation (INFANT). I. Core Identification and Core Mass Function Cheng, Yu Lu, Xing Sanhueza, Patricio Liu, Hauyu Baobab Zhang, Qizhou Galván-Madrid, Roberto Wang, Ke Nakamura, Fumitaka Liu, Tie Feng, Siyi Li, Shanghuo Jiao, Sihan Tanaka, Kei E. I. Liu, Xunchuan Li, Pak Shing Luo, Qiuyi Gu, Qilao Lin, Yuxin Guzmán, András E. Astrophysics of Galaxies 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. |
| title | INvestigations of massive Filaments ANd sTar formation (INFANT). I. Core Identification and Core Mass Function |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2404.03858 |