Galactic star formation MIOP: From clouds to cores


PIs: Karl M. Menten (DE), Friedrich Wyrowski (DE), Henrik Beuther (DE)

Gisela Ortiz Leon (DE), Thanh Dat Hoang (DE), Antonio Hernandez-Gomez (DE), Sumeyye Suri (DE), Caroline Gieser (DE), Nicola Schneider (DE), Timea Csengeri (FR), Sylvain Bontemps (FR), Nichol Cunningham (IRAMF), Jan Martin Winters (IRAMF), Ka Tat Wong (IRAMF), Wonju Kim (IRAMS)


Project ID: L19MA


Observing band: 3mm

Configurations: C,D

Observing type: Mosaic (40 fields with 16 arcmin² each)



High-mass star formation research over the last decades has concentrated on either the large-scale molecular cloud environments or on the small-scale core and disk formation. However, questions regarding the gas flow from large to small scales, and how the gas is transferred via intermediate-scale filaments and clumps have so far been largely neglected. Here, we want to overcome this missing gap via studying one well-known molecular cloud complex with the new NOEMA facilities from small to large scales connecting these important physical processes. In the nearby (1.4 kpc) luminous Cygnus X region recent and on-going star formation combine to present a rich Northern hemisphere laboratory in which star formation and feedback processes can be studied globally as well as locally in detail. Using the new and unique 4 mm capabilities of NOEMA, the flow of gas from cloud- to core-scales will be probed with observations of large mosaics covering the ground state lines of many molecules with the unique large bandwidth only possible with this facility.


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