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The understating of the origin of the H2 line emission from the centralregions of galaxies represent an important key to improve our knowledge aboutthe excitation and ionization conditions of the gas in these locations. Usuallythese lines can be produced by Starburts, shocks and/or radiation from anactive galactic nucleus (AGN). Luminous Infrared Galaxies (LIRG) representideal and challenging objects to investigate the origin of the H2 emission, asall processes above can be observed in a single object. In this work, we useK-band integral field spectroscopy to map the emission line flux distributionsand kinematics and investigate the origin of the molecular and ionized gas lineemission from inner 1.4x2.4 kpc2 of the LIRG NGC6240, known to be the galaxywith strongest H2 line emission. The emission lines show complex profiles atlocations between both nuclei and surrounding the northern nucleus, while atlocations near the southern nucleus and at 1" west of the northern nucleus,they can be reproduced by a single gaussian component. We found that the H2emission is originated mainly by thermal processes, possible being dominated byheating of the gas by X-rays from the AGN at locations near both nuclei. Forthe region between the northern and southern nuclei shocks due to theinteracting process may be the main excitation mechanism, as indicated by thehigh values of the H2l2.12um/Brg line ratio. A contribution of fluorescentexcitation may also be important at locations near 1" west of the northernnucleus, which show the lowest line ratios. The [FeII]l2.072um/Brg ratio show asimilar trend as observed for H2l2.12um/Brg, suggesting that [FeII] and H2 lineemission have similar origins. Finally, the [CaVIII]l2.32um coronal lineemission is observed mainly in regions next to the nuclei, suggesting it isoriginated gas ionized by the radiation from the AGN.

The origin of the near-IR line emission from molecular, low and high ionization gas in the inner kiloparsec of NGC6240