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Loiseau, Gaëlla

doi:10.3917/graph.028.0013

Cited by 4 publications

(1 citation statement)

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“…Of the different ISM phases, the relatively cold and dense molecular gas phase is the one most directly related to star formation. Observations of cold molecular gas in starburstdriven galactic winds are few and are only available for a couple of objects: M82 (Nakai et al 1987;Loiseau et al 1990; García-Burillo et al 2001;Walter et al 2002;Kepley et al 2014), NGC253 (Bolatto et al 2013) and NGC3628 (Tsai et al 2012). However, these suggest that the relatively cool molecular gas phase is an important fraction of the wind mass budget.…”

Section: Introductionmentioning

confidence: 99%

EXTENDED HCN AND HCO⁺EMISSION IN THE STARBURST GALAXY M82

Salas

Galaz

Salter

et al. 2014

ApJ

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We mapped 3 mm continuum and line emission from the starburst galaxy M82 using the Combined Array for Research in Millimeter-wave Astronomy. We targeted the HCN, HCO + , HNC, CS and HC 3 N lines, but here we focus on the HCN and HCO + emission. The map covers a field of 1. ′ 2 with a ≈ 5 ′′ resolution. The HCN and HCO + observations are combined with single dish images. The molecular gas in M82 had been previously found to be distributed in a molecular disk, coincident with the central starburst, and a galactic scale outflow which originates in the central starburst. With the new short spacings-corrected maps we derive some of the properties of the dense molecular gas in the base of the outflow. From the HCN and HCO + J = (1 − 0) line emission, and under the assumptions of the gas being optically thin and in local thermodynamic equilibrium, we place lower limits to the amount of dense molecular gas in the base of the outflow. The lower limits are 7 × 10 6 M ⊙ and 21 × 10 6 M ⊙ , or 2% of the total molecular mass in the outflow. The kinematics and spatial distribution of the dense gas outside the central starburst suggests that it is being expelled through chimneys. Assuming a constant outflow velocity, the derived outflow rate of dense molecular gas is ≥ 0.3 M ⊙ yr −1 , which would lower the starburst lifetime by ≥ 5%. The energy required to expel this mass of dense gas is (1 − 10) × 10 52 erg.

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