J/A+A/622/A22 Abell 1914 multiwavelength radio images (Mandal+, 2019)
Ultra-steep spectrum emission in the merging galaxy cluster Abell 1914.
Mandal S., Intema H.T., Shimwell T.W., van Weeren R.J., Botteon A.,
Roettgering H.J.A., Hoang D.N., Brunetti G., de Gasperin F., Giacintucci S.,
Hoekstra H., Stroe A., Brueggen M., Cassano R., Shulevski A., Drabent A.,
Rafferty D.
<Astron. Astrophys. 622, A22 (2019)>
=2019A&A...622A..22M 2019A&A...622A..22M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radio sources
Keywords: galaxies: clusters: intracluster medium -
galaxies: clusters: individual: Abell 1914 -
radio continuum: general - radiation mechanisms: non-thermal -
shock waves
Abstract:
A number of radio observations have revealed the presence of large
synchrotron-emitting sources associated with the intra-cluster medium.
There is strong observational evidence that the emitting particles
have been (re-)accelerated by shocks and turbulence generated during
merger events. The particles that are accelerated are thought to have
higher initial energies than those in the thermal pool but the origin
of such mildly relativistic particles remains uncertain and needs to
be further investigated. The galaxy cluster Abell 1914 is a massive
galaxy cluster in which X-ray observations show clear evidence of
merging activity. We carried out radio observations of this cluster
with the LOw Frequency ARay (LOFAR) at 150MHz and the Giant Metrewave
Radio Telescope (GMRT) at 610MHz. We also analysed Very Large Array
(VLA) 1.4GHz data, archival GMRT 325MHz data, CFHT weak lensing data
and Chandra observations. Our analysis shows that the ultra-steep
spectrum source (4C38.39; α≲-2), previously thought to be part
of a radio halo, is a distinct source with properties that are
consistent with revived fossil plasma sources. Finally, we detect some
diffuse emission to the west of the source 4C38.39 that could belong
to a radio halo.
Description:
We observed Abell 1914 in HBADUALINNER mode on 13 April 2013. The
observation (with ID: 248837) was centred on RA=14:26:01.6 and
DE=+37:49:38. The duration of the observation was 8 hours. We observed
the bright source 3C 295 as flux and bandpass calibrator. The
frequency coverage for both the calibrator and cluster was 120 to
168MHz. The visibility data was recorded every 1 second over 64
channels per 0.195MHz sub-band. As per default, the data were flagged
for interference by the observatory with AOFLAGGER (Offringa et al.
2012A&A...539A..95O 2012A&A...539A..95O), averaged to 2 seconds and 10 channels per
sub-band, and stored in the LOFAR long-term archive (LTA,
https://lta.lofar.eu).
Objects:
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RA (2000) DE Designation(s)
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14 26 01.3 +37 49 36 Abell 1914 = ACO 1914
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 125 7 List of fits images
fits/* . 7 Individual fits images
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See also:
J/A+A/622/A1 : LOFAR Two-metre Sky Survey DR1 source catalog (Shimwell+, 2019)
J/A+A/622/A4 : LOFAR observations XMM-LSS field (Hale+, 2019)
J/A+A/622/A8 : NGC 3184, 4736, 5055 and 5194 LOFAR + WSRT maps (Heesen+, 2019)
J/A+A/622/A11 : LoTSS/HETDEX. Optical quasars. I. (Guerkan+, 2019)
J/A+A/622/A13 : VLA double-double radio galaxy candidates images
(Mahatma+, 2019)
J/A+A/622/A15 : Broad absorption line quasars in LDR1 (Morabito+, 2019)
J/A+A/622/A23 : LoTSS HCG and MLCG systems (Nikiel-wroczynski+, 2019)
https://lofar-surveys.org : Lofar Surveys Home page
https://lta.lofar.eu : Lofar Long Term Archive Home page
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- 50 A21 "datime" Obs.date Observation date
52- 62 E11.6 Hz Freq ? Observed frequency
64- 68 I5 Kibyte size Size of FITS file
70- 95 A26 --- FileName Name of FITS file, in subdirectory fits
97-125 A29 --- Title Title of the FITS file
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Acknowledgements:
Soumyajit Mandal, mandal(at)strw.leidenuniv.nl
Shimwell et al., Paper I 2019A&A...622A...1S 2019A&A...622A...1S, Cat. J/A+A/622/A1
Williams et al., Paper II 2019A&A...622A...2W 2019A&A...622A...2W
Duncan et al., Paper III 2019A&A...622A...3D 2019A&A...622A...3D
Hale et al., Paper IV 2019A&A...622A...4H 2019A&A...622A...4H, Cat. J/A+A/622/A4
de Gasperin et al., Paper V 2019A&A...622A...5D 2019A&A...622A...5D
Arias et al., Paper VI 2019A&A...622A...6A 2019A&A...622A...6A
Emig et al., Paper VII 2019A&A...622A...7E 2019A&A...622A...7E
Heesen et al., Paper VIII 2019A&A...622A...8H 2019A&A...622A...8H, Cat, J/A+A/622/A8
Miskolczi et al., Paper IX 2019A&A...622A...9M 2019A&A...622A...9M
Croston et al., Paper X 2019A&A...622A..10C 2019A&A...622A..10C
Gurkan et al., Paper XI 2019A&A...622A..11G 2019A&A...622A..11G, Cat. J/A+A/622/A11
Hardcastle et al., Paper XII 2019A&A...622A..12H 2019A&A...622A..12H
Mahatma et al., Paper XIII 2019A&A...622A..13M 2019A&A...622A..13M, Cat. J/A+A/622/A13
Mooney et al., Paper XIV 2019A&A...622A..14M 2019A&A...622A..14M
Morabito et al., Paper XV 2019A&A...622A..15M 2019A&A...622A..15M, Cat. J/A+A/622/A15
O'Sullivan et al., Paper XVI 2019A&A...622A..16O 2019A&A...622A..16O
Sabater et al., Paper XVII 2019A&A...622A..17S 2019A&A...622A..17S
Stacey et al., Paper XVIII 2019A&A...622A..18S 2019A&A...622A..18S
Botteon et al., Paper XIX 2019A&A...622A..19B 2019A&A...622A..19B
Hoang et al., Paper XX 2019A&A...622A..20H 2019A&A...622A..20H
Hoang et al., Paper XXI 2019A&A...622A..21H 2019A&A...622A..21H
Mandal et al., Paper XXII 2019A&A...622A..22M 2019A&A...622A..22M, Cat. J/A+A/622/A22
Nikiel-Wroczynski et al., Paper XXIII 2019A&A...622A..23N 2019A&A...622A..23N
Savini et al., Paper XXIV 2019A&A...622A..24S 2019A&A...622A..24S
Wiber et al., Paper XXV 2019A&A...622A..25W 2019A&A...622A..25W
(End) Patricia Vannier CDS 15-Jan-2019