Molecular gas in the centers of Arp220 and NGC6240: nuclear accretion disks?

Details Molecular gas in the centers of Arp220 and NGC6240: nuclear accretion disks? Molecular gas in the centers of Arp220 and NGC6240: nuclear accretion disks?

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7882v&link_type=abstract

HST Proposal ID #7882

Computer Science

Hst Proposal Id #7882 Galaxies

Scientific paper

NIC2 will be used to image the H_2 1-0 S{1} emission in the prototypical ultraluminous infrared galaxies {ULIRGs} Arp220 and NGC6240. In ground-based observations, we have found that the H_2 emission peaks between the two remnant stellar nuclei of the merging galaxies. This is a result of dissipation in shocks in the gas, which makes the gas components merge before the dissipationless stellar components merge. The shock- excited H_2 emission is the direct signature of this dissipation and can be used to trace the flow of molecular gas towards the bottom of the potential well. ULIRGs are suspected to harbour dust-embedded quasars, formed in their dusty centers. The immense concentrations of dissipative material, in a deep potential well, may form ideal birth places for active nuclei. Aim of the HST observations is a determination of the morphology of the molecular concentration, in particular the presence of a molecular accretion disk {as suggested by 1'' resolution CO observations}, its radial profile around the central peak, and substructure within the central concentration. Combined with existing ground-based spectroscopy, the HST will provide the information required for understanding the dynamical state of these regions. Since these regions will form the birth places of extreme starbursts or a luminous active nucleus, the programme will have implications on the formation of active nuclei and extreme starbursts in general, and the possible relation between the two.

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