Gas properties in the Medusa minor merger - comparing with ULIRGs

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dc.creatorAalto, S.
dc.creatorHuttemeister, S.
dc.creatorWalter, F.
dc.date2001-08-06
dc.date.accessioned2026-07-07T01:59:33Z
dc.date.available2026-07-07T01:59:33Z
dc.descriptionHigh resolution observations of CO and 13CO 1--0 in the Medusa (NGC4194) minor merger show the CO/13CO 1--0 intensity ratio (R) increasing from normal values (5-10) in the outer parts of the galaxy to high (>20) values in the central, extended starburst region. Ratios >20 are otherwise typical of more luminous mergers. The Medusa L_FIR/L_CO ratio rivals that of ultraluminous galaxies (ULIRGs), despite the comparatively modest luminosity, indicating an exceptionally high star formation efficiency (SFE). We present models of the high pressure ISM in a ULIRG and the relatively low pressure ISM of the Medusa. We discuss how these models may explain large R in both types of distributions. Since the HCN emission is faint towards the Medusa, we suggest that the SFE is not primarily controlled by the mass fraction of dense (n > 10^4 cm-3) gas, but is probably strongly dependent on dynamics. The bright HCN emission towards ULIRGs is not necessarily evidence that the IR emission there is always powered by starbursts.
dc.description6 pages, 3 included figures, conference "The Central kpc of Starbursts and AGN" La Palma, 2001
dc.identifierhttps://arxiv.org/abs/astro-ph/0108083
dc.identifierhttp://arxiv.org/abs/astro-ph/0108083
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3160
dc.subjectAstrophysics
dc.titleGas properties in the Medusa minor merger - comparing with ULIRGs
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