The multi-phase gaseous halos of star forming late-type galaxies - II. Statistical analysis of key parameters

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dc.creatorTuellmann, R.
dc.creatorBreitschwerdt, D.
dc.creatorRossa, J.
dc.creatorPietsch, W.
dc.creatorDettmar, R. -J.
dc.date2006-04-26
dc.date.accessioned2026-07-07T10:23:03Z
dc.date.available2026-07-07T10:23:03Z
dc.descriptionIn Paper I we showed that multi-phase gaseous halos of late-type spiral galaxies, detected in the radio continuum, in Halpha, and in X-rays, are remarkably well correlated regarding their morphology and spatial extent. In this work we present new results from a statistical analysis in order to specify and quantify these phenomenological relations. This is accomplished by investigating soft X-ray (0.3-2.0keV) luminosities, FIR, radio continuum, Halpha, B-band, and UV luminosities for a sample of 23 edge-on late-type spiral galaxies. Typical star formation indicators, such as SFRs, are determined and a statistical correlation analysis is carried out. We find strong linear correlations, covering at least two orders of magnitude, between star formation indicators and integrated (disk+halo) luminosities in all covered wavebands. In addition to the well established L_FIR/L_1.4GHz-relation, we show new and highly significant linear dependencies between integrated soft X-ray luminosities and FIR, radio continuum, Halpha, B-band, and UV luminosities. Moreover, integrated soft X-ray luminosities correlate well with SFRs and the energy input into the ISM by SNe. The same holds if these quantities are plotted against soft halo X-ray luminosities. Only a weak correlation exists between the dust mass of a galaxy and the corresponding X-ray luminosity. Among soft X-ray luminosities, baryonic, and HI-gas masses, no significant correlations are found. There seems to exist a critical input energy by SNe into the ISM or a SFR threshold for multi-phase halos to show up. It is still not clear whether this threshold is a physical or an instrument dependent sensitivity limit. These findings strongly support our previous results, but conflict with the concept of halos being due to infalling gas from the IGM.
dc.description8 pages, 3 figures, 1 table, accepted for publication in A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/0604542
dc.identifierhttp://arxiv.org/abs/astro-ph/0604542
dc.identifierAstron.Astrophys.457:779,2006
dc.identifierdoi:10.1051/0004-6361:20054743
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175689
dc.subjectAstrophysics
dc.titleThe multi-phase gaseous halos of star forming late-type galaxies - II. Statistical analysis of key parameters
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