The dusty emission filaments of M87

Details The dusty emission filaments of M87 The dusty emission filaments of M87

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...413..531s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 413, no. 2, p. 531-541.

Astronomy and Astrophysics

Astronomy

70

Cosmic Dust, Galactic Evolution, Ionized Gases, Radio Jets (Astronomy), Stellar Mass Ejection, Astronomical Spectroscopy, Emission Spectra, Space Plasmas

Scientific paper

Emission-line and continuum images show that the H-alpha + forbidden N II filaments in M87 have a double stranded or ribbon-like morphology and that they are dusty. Spectroscopy of the filaments shows smoothly varying velocities within individual features. The innermost filaments are blueshifted with respect to systemic velocity. The presence of absorption associated with the emission filaments and alignment with the radio/optical jet suggests that this is foreground material, in which case it is flowing out from the nucleus rather than falling in. Conversely, line-emitting gas associated with the more distant radio lobe, as deduced from Faraday rotation observations, appears to be background material, in which case it is infalling and not outflowing. By assuming pressure equilibrium between the filaments and coronal X-ray emitting gas, we estimate a high dust-to-ionized gas ratio, indicating that either the filaments are very dusty or there is a significant neutral fraction of gas. The amount of ionized gas in the filament system is estimated to be of order 10 exp 5 - 10 exp 7 solar masses.

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