Access to Astronomical Catalogues

← Click to display the menu
J/A+A/612/A19       Abell 2052 VLT/MUSE datacubes            (Balmaverde+, 2018)

The VLT/MUSE view of the central galaxy in Abell 2052. Ionized gas swept by the expanding radio source. Balmaverde B., Capetti A., Marconi A., Venturi G. <Astron. Astrophys. 612, A19 (2018)> =2018A&A...612A..19B (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry Keywords: galaxies: active - galaxies: nuclei - galaxies: clusters: general - galaxies: clusters: individual (A2052) - galaxies: star formation - ISM: jets and outflows Abstract: We report observations of the radio galaxy 3C317 (at z=0.0345) located at the center of the Abell cluster A2052, obtained with the VLT/MUSE integral field spectrograph. The Chandra images of this cluster show cavities in the X-ray emitting gas, which were produced by the expansion of the radio lobes inflated by the active galactic nucleus (AGN). Our exquisite MUSE data show with unprecedented detail the complex network of line emitting filaments enshrouding the northern X-ray cavity. We do not detect any emission lines from the southern cavity, with a luminosity asymmetry between the two regions higher than ∼75. The emission lines produced by the warm phase of the interstellar medium (WIM) enable us to obtain unique information on the properties of the emitting gas. We find dense gas (up to 270cm-3) that makes up part of a global quasi spherical outflow that is driven by the radio source, and obtain a direct estimate of the expansion velocity of the cavities (265km/s). The emission lines diagnostic rules out ionization from the AGN or from star-forming regions, suggesting instead ionization from slow shocks or from cosmic rays. The striking asymmetric line emission observed between the two cavities contrasts with the less pronounced differences between the north and south sides in the hot gas; this represents a significant new ingredient for our understanding of the process of the exchange of energy between the relativistic plasma and the external medium. We conclude that the expanding radio lobes displace the hot tenuous phase of the interstellar medium (ISM), but also impact the colder and denser ISM phases. These results show the effects of the AGN on its host and the importance of radio mode feedback. Description: Combined datacube from OBJECT observations (with the SKY observation subtracted) for the programme 097.B-0766(A), "The AGN/clusters feedback: a direct measurement of the expansion speed of the X-rays cavities." The data have been reduced with the MUSE pipeline, as described in the paper. Objects: -------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------- 15 16 45.5 +07 00 01 A2052 = Abell 2052 -------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 165 1 Information on fits image fits/* 0 1 Fits image
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 22 F3.1 arcsec/pix scale Scale of the image 24- 26 I3 --- Nx Number of pixels along X-axis 28- 30 I3 --- Ny Number of pixels along Y-axis 32- 35 I4 --- Nz Number of slices 37- 59 A23 --- Observation date (YYYY-MM-DDThh:mm:ss.sss) 61- 67 F7.2 0.1nm blambda Lower value of wavelength interval 69- 75 F7.2 0.1nm Blambda Lower value of wavelength interval 77- 80 F4.2 0.1nm dlambda Spectral resolution 82- 88 I7 Kibyte size Size of FITS file 90-119 A30 --- FileName Name of FITS file, in subdirectory fits 121-165 A45 --- Title Title of the FITS file
Acknowledgements: Barbara Balmaverde, balmaverde(at)
(End) Barbara Balmaverde [SNS, Italy], Patricia Vannier [CDS] 24-Jan-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Université de Strasbourg/CNRS

    • Contact