Disk-halo interface: Kinematics and physical conditions at the ``foot point'' of two Galactic Molecular Loops

Details Disk-halo interface: Kinematics and physical conditions at the ``foot point'' of two Galactic Molecular Loops Disk-halo interface: Kinematics and physical conditions at the ``foot point'' of two Galactic Molecular Loops

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009atnf.prop.2294r&link_type=abstract

ATNF proposal M312, Semester: April, 2009

Physics

Galactic, Mopra

Scientific paper

Using Mopra telescope, we began to map (in the last winter season; proposal M312) two molecular clumps toward l~356.17 and l~ 5.45 (Clump C and Clump D) considered to be the foot points of the "Galactic Molecular Loops" to study the disk-halo interaction in the Galaxy. According to Fukui's model, these clumps are produced when the gas of the loops flows down their sides, along the magnetic field lines, and joins with the gas layer of the Galactic plane producing shocks. Our previous results are very promising, but we need to extend the mapped region to draw clear conclusions about the morphology and kinematics at larger scale to reveal if this picture is correct . Mopra with its broadband spectrometer, MOPS,is the telescope in the world able to carry out this project in a reasonable amount of observing time. Obviously, the IRAM 30-m telescope is not very well suited for this project. Our maps of fundamental molecules that trace shocks (SiO, SO), UV radiation fields (HNCO), high density gas (CS, HCN, HNC) and magnetic field interactions (HCO+, N2H+) will allow to establish the origin of the Giant Molecular Loops.

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