A tale of two DIGs: The relative role of H II regions and low-mass hot evolved stars in powering the diffuse ionised gas (DIG) in PHANGS-MUSE galaxies - Archive ouverte HAL Access content directly
Journal Articles Astronomy and Astrophysics - A&A Year : 2022

A tale of two DIGs: The relative role of H II regions and low-mass hot evolved stars in powering the diffuse ionised gas (DIG) in PHANGS-MUSE galaxies

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F. Belfiore
  • Function : Author
F. Santoro
  • Function : Author
B. Groves
  • Function : Author
E. Schinnerer
  • Function : Author
K. Kreckel
  • Function : Author
S. C. O. Glover
  • Function : Author
R. S. Klessen
  • Function : Author
G. A. Blanc
  • Function : Author
E. Congiu
  • Function : Author
A. T. Barnes
  • Function : Author
M. Boquien
  • Function : Author
M. Chevance
  • Function : Author
D. A. Dale
  • Function : Author
J. M. Diederik Kruijssen
  • Function : Author
A. K. Leroy
  • Function : Author
H. -A. Pan
  • Function : Author
I. Pessa
  • Function : Author
A. Schruba
  • Function : Author
T. G. Williams
  • Function : Author

Abstract

We use integral field spectroscopy from the PHANGS-MUSE survey, which resolves the ionised interstellar medium structure at ∼50 pc resolution in 19 nearby spiral galaxies, to study the origin of the diffuse ionised gas (DIG). We examine the physical conditions of the diffuse gas by first removing morphologically defined H II regions and then binning the low-surface-brightness areas to achieve significant detections of the key nebular lines in the DIG. A simple model for the leakage and propagation of ionising radiation from H II regions is able to reproduce the observed distribution of Hα in the DIG. This model infers a typical mean free path for the ionising radiation of 1.9 kpc for photons propagating within the disc plane. Leaking radiation from H II regions also explains the observed decrease in line ratios of low-ionisation species ([S II]/Hα, [N II]/Hα, and [O I]/Hα) with increasing Hα surface brightness (Σ). Emission from hot low-mass evolved stars, however, is required to explain: (1) the enhanced low-ionisation line ratios observed in the central regions of some of the galaxies in our sample; (2) the observed trends of a flat or decreasing [O III]/Hβ with Σ; and (3) the offset of some DIG regions from the typical locus of H II regions in the Baldwin-Phillips-Terlevich (BPT) diagram, extending into the area of low-ionisation (nuclear) emission-line regions (LI[N]ERs). Hot low-mass evolved stars make a small contribution to the energy budget of the DIG (2% of the galaxy-integrated Hα emission), but their harder spectra make them fundamental contributors to [O III] emission. The DIG might result from a superposition of two components, an energetically dominant contribution from young stars and a more diffuse background of harder ionising photons from old stars. This unified framework bridges observations of the Milky Way DIG with LI(N)ER-like emission observed in nearby galaxy bulges.
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Dates and versions

insu-03711533 , version 1 (01-07-2022)

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F. Belfiore, F. Santoro, B. Groves, E. Schinnerer, K. Kreckel, et al.. A tale of two DIGs: The relative role of H II regions and low-mass hot evolved stars in powering the diffuse ionised gas (DIG) in PHANGS-MUSE galaxies. Astronomy and Astrophysics - A&A, 2022, 659, ⟨10.1051/0004-6361/202141859⟩. ⟨insu-03711533⟩
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