V. Lebouteiller

TL;DR: In this paper, the authors used the CIGALE SED fitting code to model the far UV to the far IR emission of a set of 7 reasonably face-on spiral galaxies from the HRS.

Abstract: We report on the energetics of molecular outflows in 14 local Ultraluminous Infrared Galaxies (ULIRGs) that show unambiguous outflow signatures (P-Cygni profiles or high-velocity absorption wings) in the far-infrared lines of OH measured with the Herschel/PACS spectrometer. Detection of both ground-state (at 119 and 79 um) and one or more radiatively-excited (at 65 and 84 um) lines allows us to model the nuclear gas (<~300 pc) as well as the more extended components using spherically symmetric radiative transfer models. The highest molecular outflow velocities are found in buried sources, in which slower but massive expansion of the nuclear gas is also observed. With the exception of a few outliers, the outflows have momentum fluxes of (2-5)xL_IR/c and mechanical luminosities of (0.1-0.3)% of L_IR. The moderate momentum boosts in these sources (<~3) suggest that the outflows are mostly momentum-driven by the combined effects of AGN and nuclear starbursts, as a result of radiation pressure, winds, and supernovae remnants. In some sources (~20%), however, powerful (10^{10.5-11} Lsun) AGN feedback and (partially) energy-conserving phases are required, with momentum boosts in the range 3-20. These outflows appear to be stochastic strong-AGN feedback events that occur throughout the merging process. In a few sources, the outflow activity in the innermost regions has subsided in the last ~1 Myr. While OH traces the molecular outflows at sub-kpc scales, comparison of the masses traced by OH with those previously inferred from tracers of more extended outflowing gas suggests that most mass is loaded (with loading factors of Mdot/SFR=1-10) from the central galactic cores (a few x 100 pc). Outflow depletion timescales are <10^8 yr, shorter than the gas consumption timescales by factors of 1.1-15, and are anti-correlated with the AGN luminosity.

TL;DR: In this article, a multi-phase ISM of the IR bright low-metallicity galaxy Haro 11 is described by dissecting the photoionised and photodissociated gas components.

TL;DR: In this paper, the Herschel PACS instrument was used to measure the photodissociation region associated with starbursts in the same way as the PAH feature, and a calibration of star formation rate for the starburst component in any source having [CII] is derived comparing [C II] luminosity L(CII]) to L(IR) with the result that log SFR = log L([CII)]) - 708 +- 03, for SFR in solar masses per year and L(CIII]) in solar luminosities