2017A&A...605A..48K


Query : 2017A&A...605A..48K

2017A&A...605A..48K - Astronomy and Astrophysics, volume 605A, 48-48 (2017/9-1)

LOFAR MSSS: The scaling relation between AGN cavity power and radio luminosity at low radio frequencies.

KOKOTANEKOV G., WISE M., HEALD G.H., McKEAN J.P., BIRZAN L., RAFFERTY D.A., GODFREY L.E.H., DE VRIES M., INTEMA H.T., BRODERICK J.W., HARDCASTLE M.J., BONAFEDE A., CLARKE A.O., VAN WEEREN R.J., ROTTGERING H.J.A., PIZZO R., IACOBELLI M., ORRU E., SHULEVSKI A., RISELEY C.J., BRETON R.P., NIKIEL-WROCZYNSKI B., SRIDHAR S.S., STEWART A.J., ROWLINSON A., VAN DER HORST A.J., HARWOOD J.J., GURKAN G., CARBONE D., PANDEY-POMMIER M., TASSE C., SCAIFE A.M.M., PRATLEY L., FERRARI C., CROSTON J.H., PANDEY V.N., JURUSIK W. and MULCAHY D.D.

Abstract (from CDS):

We present a new analysis of the widely used relation between cavity power and radio luminosity in clusters of galaxies with evidence for strong AGN feedback. We studied the correlation at low radio frequencies using two new surveys - the first alternative data release of the TIFR GMRT Sky Survey (TGSS ADR1) at 148MHz and LOFAR's firstall-sky survey, the Multifrequency Snapshot Sky Survey (MSSS) at 140MHz. We find a scaling relation Pcav∝Lβ148, with a logarithmic slope of β=0.51±0.14, which is in good agreement with previous results based on data at 327MHz. The large scatter present in this correlation confirms the conclusion reached at higher frequencies that the total radio luminosity at a single frequency is a poor predictor of the total jet power. Previous studies have shown that the magnitude of this scatter can be reduced when bolometric radio luminosity corrected for spectral aging is used. We show that including additional measurements at 148MHz alone is insufficient to improve this correction and further reduce the scatter in the correlation. For a subset of four well-resolved sources, we examined the detected extended structures at low frequencies and compare with the morphology known from higher frequency images and Chandra X-ray maps. In the case of Perseus we discuss details in the structures of the radio mini-halo, while in the 2A 0335+096 cluster we observe new diffuse emission associated with multiple X-ray cavities and likely originating from past activity. For A2199 and MS 0735.6+7421, we confirm that the observed low-frequency radio lobes are confined to the extents known from higher frequencies. This new low-frequency analysis highlights the fact that existing cavity power to radio luminosity relations are based on a relatively narrow range of AGN outburst ages. We discuss how the correlation could be extended using low frequency data from the LOFAR Two-metre Sky Survey (LoTSS) in combination with future, complementary deeper X-ray observations.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: clusters: individual: 2A 0335+096 - galaxies: clusters: individual: Perseus - X-rays: galaxies: clusters - galaxies: clusters: individual: A2199 - galaxies: clusters: individual: MS 0735.6+7421 - galaxies: clusters: intracluster medium - galaxies: clusters: intracluster medium

CDS comments: Fig.3 cavities not in SIMBAD.

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 LHA 115-N 31 Y*O 00 48 41.869 -73 26 15.17   14.92 15.1 15.27 15.60 B0 27 0
2 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 351 1
3 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 677 1
4 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2118 1
5 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3809 3
6 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 359 1
7 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 482 0
8 ZwCl 0735+7421 ClG 07 41 40.3 +74 14 58     17.70     ~ 236 0
9 ACO 780 ClG 09 18 30 -12 15.7           ~ 445 0
10 ClG J0947+7623 ClG 09 47 12.9 +76 23 13           ~ 139 1
11 ZwCl 0949+5207 ClG 09 52 49.1 +51 53 05           ~ 121 0
12 ZwCl 1021+0426 ClG 10 23 39.0 +04 11 14   15.6       ~ 264 0
13 MKW 3 ClG 11 48 29 -03 10.7     14.88     ~ 51 1
14 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1708 2
15 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6738 3
16 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 1022 2
17 HCG 62 CGG 12 53 05.6 -09 12 21           ~ 299 0
18 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1205 0
19 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 657 1
20 ClG J1423+2404 ClG 14 23 47.7 +24 04 40           ~ 191 0
21 3C 313 rG 15 10 57.0 +07 51 25   21.0       ~ 100 1
22 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 703 1
23 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 296 0
24 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1132 1
25 NAME Cyg A Sy2 19 59 28.35645829 +40 44 02.0966496   16.22 15.10     ~ 2257 2
26 * alf Pav SB* 20 25 38.85705 -56 44 06.3230 1.03 1.791 1.918     B2IV 282 0
27 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 243 1
28 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 519 0
29 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 369 1

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2022.10.02-02:24:38

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