J/A+A/665/A48 RXC J2014.8-2430 fits images (Mroczkowski+, 2022)
The strongest cool core in REXCESS: Missing X-ray cavities in RXC J2014.8-2430.
Mroczkowski T., Donahue M., van Marrewijk J., Clarke T.E., Hoffer A.,
Intema H., Di Mascolo L., Popping G., Pratt G.W., Sun M., Voit M.
<Astron. Astrophys. 665, A48 (2022)>
=2022A&A...665A..48M 2022A&A...665A..48M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Radio sources
Keywords: galaxies: clusters: intracluster medium -
galaxies: clusters: individual: RXC J2014.8-2430 -
X-rays: galaxies: clusters - submillimeter: galaxies -
radio continuum: galaxies - galaxies: clusters: general
Abstract:
We present a broad, multi-wavelength study of RXC J2014.8-2430, the
most extreme cool-core cluster in the Representative XMM-Newton
Cluster Structure Survey (REXCESS), using Chandra X-ray, Southern
Astrophysical Research (SOAR) Telescope spectroscopic and narrow-band
imaging, Atacama Large Millimeter/submillimeter Array (ALMA), Very
Large Array, and Giant Metrewave Radio Telescope observations. While
feedback from an active galactic nucleus (AGN) is thought to be the
dominant mechanism by which a cooling flow is suppressed, the
Chandra imaging observations surprisingly do not reveal the
bi-lateral X-ray cavities one might expect to see in the intracluster
medium (ICM) of an extreme cool core hosting a powerful radio source,
though cavities commonly appear in many similar sources. We discuss
the limits on the properties of putative radio bubbles associated with
any undetected X-ray cavities. We place upper limits on any
significant X-ray AGN in the brightest cluster galaxy (BCG), and show
that the X-ray peak is offset from the central radio source, which
exhibits a steep low-frequency radio spectrum indicative of electron
ageing. The imaging and spectroscopy provided by SOAR reveal an
extended, luminous optical emission-line source. From our narrow-band
Hα imaging of the BCG, the central Hα peak is coincident
with the radio observations, yet offset from the X-ray peak,
consistent with sloshing found previously in this cluster. ALMA
observations of the CO(1-0) emission reveal a large reservoir of
molecular gas that traces the extended Hα emission in the
direction of the cool core.
We conclude either that the radio source and its cavities in the X-ray
gas are nearly aligned along the line of sight, or that ram pressure
induced by sloshing has significantly displaced the cool molecular gas
feeding it, perhaps preempting the AGN feedback cycle. We argue that
the sloshing near the core is likely subsonic, as expected, given the
co-location of the Hα, CO(1-0), radio continuum, and stellar
emission peaks and their proximity to the X-ray peak. Further, the
X-ray emission from the core is strongly concentrated, as is the
distribution of metals, indicating the cool core remains largely
intact. Deeper Chandra observations will be crucial for definitively
establishing the presence or lack of X-ray cavities, while X-ray
micro-calorimetric observations from Athena could establish if the
motion of the cold and warm gas is dominated by large-scale motions of
the surrounding ICM.
Description:
A 20 ks Chandra observation of RXC J2014.8-2430 was taken on August
25, 2009 (ObsID 11757) as part of the Chandra Guest Observers
programme.
Narrow-band optical imaging was taken on the SOAR Telescope with the
SOAR Optical Imager on September 6, 2010.
We use millimetre-wave observations performed by ALMA on December 24,
2018, to probe the location and dynamics of the molecular gas traced
by the lowest transition of the dominant form of carbon monoxide,
CO(1-0), which has a rest frequency of 115.271GHz.
The VLA performed L-band (1-2GHz) observations on May 29, 2014, of
the continuum radio emission from RXC J2014.8-2430 as part of Project
code 14A-280.
As part of a larger observing programme (project code 14JHC01), RXC
J2014.8-2430 was observed at 610MHz by the GMRT for 3.1h in 6 equal
blocks during the night of June 21, 2008.
The VLITE is a commensal 338MHz system that operates on the NRAO VLA
in parallel with standard observing programmes that use the 1-50GHz
feeds. RXC J2014.8-2430 was detected in six separate VLITE
observations at distances between 0.5° and 1.4° from the phase
centre between December 10, 2017, and November 22, 2020.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lines.dat 65 74 Lines for the SOAR spectroscopy
list.dat 188 12 List of fits images and datacubes
fits/* . 12 Individual fits images and datacubes
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Byte-by-byte Description of file: lines.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Line Spectral line
11- 13 I3 pix RegCent ? Region centre
15- 21 F7.2 0.1nm LineCent Line centre
23- 27 F5.2 0.1nm e_LineCent Line centre error
29- 34 F6.1 0.1nm EW Equivalent width
36- 39 F4.1 0.1nm e_EW Equivalent width error
41- 47 F7.4 10-19W/m2 Flux Flux
49- 52 F4.2 10-19W/m2 e_Flux Flux error
54- 59 F6.3 0.1nm FWHM FWHM
61- 65 F5.2 0.1nm e_FWHM FWHM error
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 32 I3 --- Nz ? Number of slices for the datacubes
34- 55 A22 "datime" Obs.date Observation date
57- 62 I6 Kibyte size Size of FITS file
64-128 A65 --- FileName Name of FITS file, in subdirectory fits
130-188 A59 --- Title Title of the FITS file
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Acknowledgements:
Tony Mroczkowski, tony.mroczkowski(at)eso.org
(End) Patricia Vannier [CDS] 22-Jul-2022