X-ray emission from star-forming galaxies - II. Hot interstellar medium

By S. Mineo, M. Gilfanov, R. S. H. C. F. Astrophysics, Max Planck Institute for Astrophysics, S. Sciences. 2012

155 citations recorded by the source corpus.

We study the emission from the hot interstellar medium (ISM) in a sample of nearby late-type galaxies defined in Paper I. Our sample covers a broad range of star formation rates (SFRs) from ∼0.1 to ∼17 M⊙ yr−1 and stellar masses from ∼3 × 108 to ∼6 × 1010 M⊙. We take special care of systematic effects and contamination from bright and faint compact sources. We find that in all galaxies at least one optically thin thermal emission component is present in the unresolved emission, with the average temperature of 〈kT〉 = 0.24 keV. In about ∼1/3 of galaxies, a second, higher temperature component is required, with 〈kT〉 = 0.71 keV. Although statistically significant variations in temperature between galaxies are present, we do not find any meaningful trends with the stellar mass or SFR of the host galaxy. The apparent luminosity of the diffuse emission in the 0.5–2 keV band linearly correlates with the SFR with the scale factor of erg s−1 (M⊙ yr−1)−1, of which in average ∼30–40 per cent is likely produced by faint compact sources of various types. We attempt to estimate the bolometric luminosity of the gas and obtain results differing by an order of magnitude, , depending on whether intrinsic absorption in star-forming galaxies is allowed or not. Our theoretically most accurate, but in practice the most model-dependent result for the intrinsic bolometric luminosity of the ISM is erg s−1 (M⊙ yr−1)−1. Assuming that core-collapse supernovae are the main source of energy, it is implied that of mechanical energy of supernovae is converted into thermal energy of the ISM.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/da55754dfb65ade82d71f8a2e8b0338a4c0fd35d

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Citations in the corpus

High-mass X-ray binaries in the Milky Way (2013, methodology): “Therefore indirect methods, such as the construction of X-ray luminosity functions (LF), are needed to study of properties of populations of sources located in different regions of a galaxy (see, e.g., Gilfanov, 2004; Mineo et al., 2012a).”
THE COS-HALOS SURVEY: ORIGINS OF THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM OF STAR-FORMING GALAXIES (2016, background): “Soft X-ray emission from the ISM is known to correlate with the galaxy SFR, and in all star forming galaxies there is at least one optically thin thermal emission component with an average temperature of < kT > = 0.24 keV (e.g. Mineo et al. 2012).”
Active galactic nuclei: what’s in a name? (2017, background): “The hot-gas component can be up-to LX ≈ 1041–1042 erg s−1 from galaxies (e.g. Boroson et al. 2011; Mineo et al. 2012b) and can be as high as LX ≈ 1044–1045 erg s−1 in the cores of massive galaxy clusters (e.g. Stanek et al. 2006; Ebeling et al. 2010).”
An origin for multiphase gas in galactic winds and haloes (2015, background): “For example, Mineo et al. (2012) report the 0.5-2 keV X-ray luminosity of starforming galaxies to be LX ' 5 × 1038Ṁ? ergs s−1, implying LX/L?”