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Molecular Hydrogen in the outer filaments surrounding NGC 1275

Molecular Hydrogen in the outer filaments surrounding NGC 1275. Nina Hatch CS Crawford, RM Johnstone, AC Fabian. IOA, Cambridge. Central Cluster Galaxy Emission-line nebulae. Emission line nebulae are found surrounding ~27% of CCG Bright and extended structure. Cowie et al 1983.

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Molecular Hydrogen in the outer filaments surrounding NGC 1275

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  1. Molecular Hydrogen in the outer filaments surrounding NGC 1275 Nina Hatch CS Crawford, RM Johnstone, AC Fabian IOA, Cambridge

  2. Central Cluster Galaxy Emission-line nebulae • Emission line nebulae are found surrounding ~27% of CCG • Bright and extended structure Cowie et al 1983 • Only find emission line nebulae if cluster • has a short radiative cooling time and • bright centrally peaked x-ray emission Conselice et al 2001

  3. Perseus: 200ks Chandra Fabian et al 03

  4. Unsharped mask of X-ray image of Perseus cluster Fabian et al, 2003

  5. NGC1275/Perseus cluster in Hα Conselice et al 2001

  6. Edge et al, 2002 Similar line ratios found in outer filaments as in the nucleus – indicating similar ionising mechanism

  7. Velocity shear across lower filaments ~ 175km/s

  8. Velocity shift relative to nucleus

  9. Ionisation Mechanisms • Excitation source of optical filaments still uncertain • -short cooling time → gas continually ionised • - Soft X-ray/Hα indicate filaments radiate predominantly in optical → soft x-rays do not ionise • Possible mechanisms • UV photoionisation from nearby stars • -likely to be dominant mechanism in Eastern knot • shocks • conduction from hot ICM Will analyse line ratios using CLOUDY

  10. Summary • Detection of molecular hydrogen ~ 25kpc from CCG, deeply embedded within hot ICM • Velocity shift between outer filaments and central nebula and within filaments • Spectra indicate different ionisation mechanisms acting on filaments

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