Probing the nature of the di ff use ionized gas with Integral Field - - PowerPoint PPT Presentation

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Probing the nature of the di ff use ionized gas with Integral Field - - PowerPoint PPT Presentation

Jan 29, 2024 204 likes •464 views

Probing the nature of the di ff use ionized gas with Integral Field Spectroscopy F . Fabin Rosales-Ortega Instituto Nacional de Astrofsica, ptica y Electrnica 2nd SELGIFS Advanced School on Integral-Field Spectroscopy Data Analysis

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Probing the nature of the diffuse ionized gas with Integral Field Spectroscopy

F . Fabián Rosales-Ortega

Instituto Nacional de Astrofísica, Óptica y Electrónica

2nd SELGIFS Advanced School on Integral-Field Spectroscopy Data Analysis

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  • The existence of widespread

diffuse ionized gas in the ISM has been known for over 20 years

  • It was first detected from a

thin haze of electrons that affect radio radiation passing through the Milky Way Galaxy.

Diffuse ionized gas (DIG)

Also called warm ionized medium (WIM)

(Reynolds et al 1971; Monnet 1971)

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The DIG:

  • Produces a faint emission-line

spectrum that is seen in every direction of the Galaxy.

  • Occupies more than 20% of the

interstellar volume.

  • Contributes at least 1/3 of the

total HI column at the solar circle.

  • Constitutes 90% of the ionized

hydrogen mass in the Galaxy.

Diffuse ionized gas (DIG)

(Reynolds et al 1971; Monnet 1971)

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  • In other galaxies, the DIG is observed

to be in the form of discrete structures, such as loops, filaments, and shells.

  • Responsible for producing a faint but

pervasive Hα emission.

  • The observed Hα luminosities of the

DIG are considerable and account for 30%-50% of the total Hα emission of each galaxy.

Diffuse ionized gas (DIG)

(which are not obviously associated with discrete HII regions) (Ferguson et al. 1996)

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Diffuse ionized gas (DIG)

The source of this ionization remains the subject of much debate.

  • Lyc photon leakage from HII regions (e.g. Ferguson et al. 1996)
  • Dust scattering of UV light
  • Shocks (kinetic energy by SNe)
  • Decaying massive neutrinos (e.g. Sciama 1990)
  • Turbulent mixing layers (e.g. Slavin et al. 1993)
  • Galactic microflares (e.g. Raymond 1992).
  • Evolved stellar objects

(planetary nebula nuclei, hot white dwarfs, blue horizontal branch stars).

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Diffuse ionized gas (DIG)

Nearby galaxies

(Ferguson et al. 1996) 53% 41%

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Diffuse ionized gas (DIG)

(Ferguson et al. 1996)

Based on narrow-band imaging

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Diffuse ionized gas (DIG)

Emission line diagnostic

(Giammanco et al. 2004)

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Diffuse ionized gas (DIG)

Problems / challenges

  • The constancy of the diffuse fraction over

morphological type?

  • Energy budget of the DIG?
  • Relation of the DIF with HII Luminosity

function?

  • Effect of Inclination?

Large-scale structures, usually studied with small FoV

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Spectroscopic information over large FoV

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CALIFA

NGC 2906

The effects of spatial resolution in IFS

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CALIFA

NGC 2906

MUSE

The effects of spatial resolution in IFS

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Castellanos-Durán et al. in prep.

CALIFA

NGC 2906

MUSE

The effects of spatial resolution in IFS

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Wide-Field Integral Field Spectroscopy Survey of Nearby Galaxies (< 100 Mpc)

Rosales-Ortega PhD 2009 Rosales-Ortega et al. 2010

✴

PMAS/PPAK instrument at CAHA

✴

Spectral range: λ3700-7000 Å

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All-weather MUse Supernova Integral field Nearby Galaxies survey

AMUSING

Uses non-optimal weather at Paranal to observe SN host galaxies using MUSE-VLT, and as a by-product, full 2D coverage of nearby galaxies with superb spatial resolution.

0.2 arcsec per spaxel

(Anderson et al., in prep.)

(Galbany et al. 2016)

NGC 6754

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AMUSING

(Galbany et al. 2016)

NGC 7469 NGC 7742

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The effects of spatial resolution in IFS

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The effects of spatial resolution in IFS

Castellanos-Durán et al. in prep.

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The effects of spatial resolution in IFS

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Castellanos-Durán et al. in prep.

The effects of spatial resolution in IFS

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  • Previous attempts to do so were based either on narrow

band imaging or using spectroscopic methods in small field-of-views and/or with low spatial resolution.

  • New IFTS observations allow to sample a good range of

the HII region luminosity function

  • Potentially, to quantify the escape fraction of ionizing

radiation in sample of local star forming galaxies.

Probing the nature of the diffuse ionized gas wit IFS

2nd SELGIFS Advanced School on Integral-Field Spectroscopy Data Analysis

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Good, but we need spatial resolution and large Fov!

  • Large galaxy sample
  • Diffuse fraction over morphological type
  • Radial and azimuthal distribution of the DIG
  • Effects of Inclination

Energy budget of the DIG Relation of the DIF with HII Luminosity function Comparison with theoretical modelling

Probing the nature of the diffuse ionized gas wit IFS

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AMUSING

(Galbany et al. 2016)

NGC 7742

(Rosales-Ortega et al. 2010)

PINGS

Segmentation is crucial

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Beyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopy

OFIUCO: Optical Fourier-transform Imaging Unit for Cananea Observatory

OFIUCO

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Beyond MOS and fibers: large FoV Imaging Fourier Transform Spectroscopy

OFIUCO: Optical Fourier-transform Imaging Unit for Cananea Observatory

OFIUCO