The warm ionized medium in spiral galaxies

By L. M. Haffner, Ralf-Jurgen Dettmar, J. E. Beckman, K. Wood, J. Slavin, Corrado Giammanco, G. Madsen, Almudena Zurita, R. J. Reynolds. 2009

198 citations recorded by the source corpus.

This article reviews observations and models of the diffuse ionized gas that permeates the disk and halo of our Galaxy and others. It was inspired by a series of invited talks presented during an afternoon scientific session of the 65th birthday celebration for Professor Carl Heiles held at Arecibo Observatory in August 2004. This review is in recognition of Carl's long-standing interest in and advocacy for studies of the ionized as well as the neutral components of the interstellar medium.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c2127213f70f22f4d6b0814bf6d18eabe51b9a60

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

THE SPATIALLY RESOLVED STAR FORMATION LAW FROM INTEGRAL FIELD SPECTROSCOPY: VIRUS-P OBSERVATIONS OF NGC 5194 (2009, background): “The role of the diffuse ionized gas (DIG, a.k.a. warm ionized medium, WIM) as an important component of the ISM of star-forming disk galaxies in the local universe has been properly established during the last two decades (e.g. see reviews by Mathis 2000 and Haffner et al. 2009).”
Physical Processes in the Interstellar Medium (2014, background): “Evidence for an additional phase, the so-called Warm Ionized Medium (WIM), comes from a variety of observations, including free-free absorption of the Galactic synchrotron background (Hoyle & Ellis, 1963), the dispersion of radio signals from pulsars (Reynolds, 1989; Gaensler et al., 2008), and fain”
SDSS IV MaNGA – spatially resolved diagnostic diagrams: a proof that many galaxies are LIERs (2016, background): “Diffuse ionised gas (DIG) with LINER-like emission is observed surrounding the plane of the Milky Way and other spiral galaxies (Hoopes & Walterbos 2003; Rossa & Dettmar 2003; Oey et al. 2007; Haffner et al. 2009; Blanc et al. 2009; Flores-Fajardo et al. 2011).”
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “Mierkiewicz et al. (2006) show that [O ii]/Hα and [N ii]/Hα correlate positively with temperature variation and they concluded that the variation of line ratios is driven by temperature variations (Haffner et al. 1999; Haffner et al. 2009).”
Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, background): “The DIG is hot (∼ 104 K) and tenuous gas (∼ 10−1 cm−3) permeating the interstellar space and extending more than 1 kpc above the disk plane (seeMathis 2000and Haffner et al. 2009for reviews).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…spiral and irregular galaxies, is observed to be spatially correlated with H ii regions and believed to also be ionized by massive stars (e.g., Haffner et al. 2009, and references therein; see also Hunter & Gallagher 1990; Martin 1997; Oey & Kennicutt 1997; Wang et al. 1997; Ascasibar et al.…”
ENVIRONMENTAL DEPENDENCE OF THE KENNICUTT–SCHMIDT RELATION IN GALAXIES (2010, background): “In the Milky Way, for example, the warm ionized gas accounts for ∼ 25% of the total hydrogen column density of the disk (Reynolds 1991; Haffner et al. 2009).”
Gaseous Galaxy Halos (2012, background): “See Haffner et al. (2009) for a further review of the warm ionized gas of spiral galaxies detected in emission.”
A Herschel [C ii] Galactic plane survey - I. The global distribution of ISM gas components (2013, background): “…evolution of the interstellar medium (ISM) has traditionally been studied with radio continuum and Hα observations for the ionized component (e.g. Haffner et al. 2009), with observations of the H i 21 cm line for the atomic gas component (e.g. Kalberla & Kerp 2009), and with rotational…”