M87 at metre wavelengths

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Virgo A (3C274) Flux: ~1700 Jy @ 100 MHz Size (core): 5 kpc (1’) Size (halo): 80 kpc (16’) BH mass: 6.4 10^9 M Amorphous source 2054 E. T. Million et al. Fig. 2a Fig. 2b fig. 2afig. 2b Fig. 2.—Images of the seven ACIS-I pointings after background subtraction and ‘‘flat fielding’’ in the energy band 0.5Y1.0 keV with 1 pixel ¼ 3 00 at two different scales. (a) The very prominent eastern and southwestern arms (see also Fig. 5, where these are labeled in both the X-ray and radio images). (b)Amoredetailedviewofthe tracery of filaments that suggests the similarity between the structures in the eastern and southwestern arms. The long southwestern arm appears to be composed of several intertwined filaments (see location indicated by the label ‘‘Filament’’). The eastern arm can be interpreted as a series of bubbles (several labeled inrightpanel)atdifferent evolutionary stages as they rise in the atmosphere of M87. The filamentary structures are very soft and are not apparent at energies above 2 keV (e.g., see Fig. 7). X-ray maps from: Million et al. (2010) Forman et al. (2007) For the 1.2Y2.5 keV band, Figure 1 (upper solid curve)shows that the count rate for a unit volume of unit density is independent of gas temperature, for gas temperatures above about 1 keV. If we express the count rate as Z C / (T ) dl; ð1Þ n 2 e where n e is the electron density, (T ) is the volume emissivity of the gas convolved with the Chandra response, and l is the path length along the line of sight, the independence of the1.2Y2.5 keV ‘‘density’’ image (actually the square of the density integrated along the line of sight). The properties of the 3.5Y7.5 keV band can be determined by rewriting equation (1) using the ideal gas law, p / n e T,to eliminate the gas density. We find Z C / p 2 (T ) T 2 dl: ð2Þ The lower dashed curve in Figure 1 is (T )/T 2 for a unit density and unit volume of gas. For gas temperatures from 1 to
M87 HBA map: RMS: 6 mJy/beam Beam: 19” x 14” Dyn Range > 13000 Frequency: 140 MHz NOTES: •Other strong sources uv-subtracted •Imaging of the core with standard Clean algorithm •Imaging of the extended emission with Maximum Entropy (flat prior)
Page 1 and 2: Leiden - 15/05/2012 M87 at metre wa
Page 3 and 4: M90 NGC4435 NGC4402 NGC4438 M86 M84
Page 6 and 7: Virgo A (3C274) Flux: ~1700 Jy @ 10
Page 8 and 9: Virgo A (3C274) Flux: ~1700 Jy @ 10
Page 14 and 15: M87 LBA map: RMS: 0.6 Jy/beam Beam:
Page 16 and 17: M87 - spectral index Low-freq Spect
Page 18 and 19: M87 - Core Spectral index analysis:
Page 20 and 21: Slope of injected electrons fixed t
Page 22 and 23: M87 - Results Discrepancy with dyna
Page 24 and 25: The Virgo Campaign 2011 LOFAR Obser
Page 26 and 27: The Virgo Campaign 2011 LOFAR Obser
Page 29 and 30: M88 NGC4402 M90 NGC4438 M58 NGC4388
Page 31 and 32: Conclusions: • Virgo A extended h
Page 33 and 34: JP Model ⌫ b / 1 t 2 B 3
Page 35 and 36: M87 - Jet Power dU int dt = P ⌘ p
Page 37 and 38: The Calibration Vir A
Page 39: The Calibration Vir A Cyg A Cas A D

M87 at metre wavelengths

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