A low-frequency radio halo survey of the South Pole Telescope SZ-selected clusters with the GMRT

Raja, Ramij; Rahaman, Majidul; Datta, Abhirup; Weeren, R. J. van; Intema, H. T.; Paul, Surajit

doi:10.1093/mnras/staa3432

Cited by 6 publications

(5 citation statements)

References 74 publications

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“…We update this relation at GHz and GHz following (van Weeren et al, 2020, hereafter vW20). For this work, we incorporate the compiled literature sample of halos reported by C13 and Martinez Aviles et al (2016), halos in Abell S1121 and Abell 2811 reported by Duchesne et al (2021b), and new halos reported in the literature from 2017 (Parekh et al, 2017; Wilber et al, 2018; Cassano et al, 2019; Brzan et al 2019; Xie et al, 2020; HyeongHan et al, 2020; Giovannini et al, 2020; Wilber et al, 2020; Hoeft et al, 2020; Hoang et al, 2021; Di Gennaro et al, 2020; van Weeren et al, 2020; Raja et al, 2020; Knowles et al, 2021; Raja et al, 2021), with the exception of the halo in ACT-CL J0528.8 –3927 reported by Knowles et al (2021) as its small size and coincidence with a radio-bright BCG suggests a mini-halo. For consistency, cluster masses are obtained from PSZ measurements where available (Planck Collaboration et al 2016c, with some masses obtained from the South Pole Telescope; Song et al, 2012; Reichardt et al, 2013), and only clusters with an SZ-derived mass are used.…”

Section: Resultsmentioning

confidence: 99%

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

Duchesne

Johnston‐Hollitt

Wilber

2021

Publ. Astron. Soc. Aust.

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We report on the detection of a giant radio halo in the cluster Abell 3404 as well as confirmation of the radio halo observed in Abell 141 (with linear extents $\sim\!770$ and $\sim\!850$ kpc, respectively). We use the Murchison Widefield Array, the Australian Square Kilometre Array Pathfinder, and the Australia Telescope Compact Array to characterise the emission and intervening radio sources from $\sim100$ to 1 000 MHz; power law models are fit to the spectral energy distributions with spectral indices $\alpha_{88}^{1\,110} = -1.66 \pm 0.07$ and $\alpha_{88}^{943} = -1.06 \pm 0.09$ for the radio halos in Abell 3404 and Abell 141, respectively. We find strong correlation between radio and X-ray surface brightness for Abell 3404 but little correlation for Abell 141. We note that each cluster has an atypical morphology for a radio-halo-hosting cluster, with Abell 141 having been previously reported to be in a pre-merging state, and Abell 3404 is largely relaxed with only minor evidence for a disturbed morphology. We find that the radio halo powers are consistent with the current radio halo sample and $P_\nu$ –M scaling relations, but note that the radio halo in Abell 3404 is an ultra-steep–spectrum radio halo (USSRH) and, as with other USSRHs lies slightly below the best-fit $P_{1.4}$ –M relation. We find that an updated scaling relation is consistent with previous results and shifting the frequency to 150 MHz does not significantly alter the best-fit relations with a sample of 86 radio halos. We suggest that the USSRH halo in Abell 3404 represents the faint class of radio halos that will be found in clusters undergoing weak mergers.

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Section: Resultsmentioning

confidence: 99%

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

Duchesne

Johnston‐Hollitt

Wilber

2021

Publ. Astron. Soc. Aust.

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“…We update this relation at ν = 1.4 GHz and ν = 0.15 GHz following van Weeren et al (2020, hereafter vW20). For this work, we incorporate the compiled literature sample of halos reported by C13 and Martinez Aviles et al (2016), halos in Abell S1121 and Abell 2811 reported by Duchesne et al (2017), and new halos reported in the literature from 2017 (Parekh et al, 2017;Wilber et al, 2018;Cassano et al, 2019;Bîrzan et al, 2019;Xie et al, 2020;HyeongHan et al, 2020;Giovannini et al, 2020;Wilber et al, 2020;Hoeft et al, 2020;Hoang et al, 2020;Di Gennaro et al, 2020;van Weeren et al, 2020;Raja et al, 2020;Knowles et al, 2020;Raja et al, 2021), with the exception of the halo in ACT-CL J0528.8−3927 reported by Knowles et al (2020) as its small size and coincidence with a radiobright BCG suggests a mini-halo. For consistency, cluster masses are obtained from PSZ measurements where available (Planck Collaboration et al, 2016c, with some masses obtained from the South Pole Telescope; Song et al 2012;Reichardt et al 2013), and only clusters with an SZ-derived mass are used.…”

Section: Radio Halo P ν -M 500 Scaling Relationsmentioning

confidence: 99%

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

Duchesne,

Johnston-Hollitt,

Wilber

2021

Preprint

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We report on the detection of a giant radio halo in the cluster Abell 3404 as well as confirmation of the radio halo observed in Abell 141 (with linear extents ∼ 770 kpc and ∼ 850 kpc, respectively). We use the Murchison Widefield Array (MWA) in conjunction with the Australian Square Kilometre Array Pathfinder (ASKAP) and the Australia Telescope Compact Array (ATCA) to characterise the emission and intervening radio sources from ∼ 100-1000 MHz; power law models are fit to the spectral energy distributions with spectral indices α 1110 88 = −1.80 ± 0.09 and α 944 88 = −1.13 ± 0.09 for the radio halos in Abell 3404 and Abell 141, respectively. Each cluster is noted to have an atypical morphology for a radio-halo-hosting cluster, with Abell 141 having been previously reported to be in a pre-merging state, and Abell 3404 is largely relaxed with only minor evidence for a disturbed morphology. We find that the radio halo power is consistent with the current radio halo sample and P ν -M scaling relations, but note that the radio halo in Abell 3404 is an ultra-steep-spectrum radio halo (USSRH) and, as with other USSRHs lies slightly below the best-fit P 1.4 -M relation. We find that an updated scaling relation is consistent with previous results and shifting the frequency to 150 MHz does not significantly alter the best-fit relations with a sample of 86 radio halos. We suggest that the USSRH halo in Abell 3404 represents the faint class of radio halos that will be found in clusters undergoing weak mergers.

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“…Hence, successfully calibrating and imaging this field would imply that we could apply the techniques on the rest of the sample. [25] and SPT [55] sample used for statistical studies of diffuse emission.…”

Section: The Actpol Samplementioning

confidence: 99%

“…The new studies have resulted in a different class of diffuse emission, such as; radio phoenices and gently re-energized tails (GReETs; [26,52]). The sensitivity of these telescopes have opened up a new observational window which probes lower mass (<4 × 10 14 M ) and higher redshift (z > 0.3) clusters [53][54][55]. Large cluster samples of this nature will help in the refinement of currently existing formation theories.…”

Section: Introductionmentioning

confidence: 99%

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A GMRT Narrowband vs. Wideband Analysis of the ACT−CL J0034.4+0225 Field Selected from the ACTPol Cluster Sample

et al. 2021

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Low frequency radio observations of galaxy clusters are a useful probe of the non-thermal intracluster medium (ICM), through observations of diffuse radio emission such as radio halos and relics. Current formation theories cannot fully account for some of the observed properties of this emission. In this study, we focus on the development of interferometric techniques for extracting extended, faint diffuse emissions in the presence of bright, compact sources in wide-field and broadband continuum imaging data. We aim to apply these techniques to the study of radio halos, relics and radio mini-halos using a uniformly selected and complete sample of galaxy clusters selected via the Sunyaev-Zel’dovich (SZ) effect by the Atacama Cosmology Telescope (ACT) project, and its polarimetric extension (ACTPol). We use the upgraded Giant Metrewave Radio Telescope (uGMRT) for targeted radio observations of a sample of 40 clusters. We present an overview of our sample, confirm the detection of a radio halo in ACT−CL J0034.4+0225, and compare the narrowband and wideband analysis results for this cluster. Due to the complexity of the ACT−CL J0034.4+0225 field, we use three pipelines to process the wideband data. We conclude that the experimental spam wideband pipeline produces the best results for this particular field. However, due to the severe artefacts in the field, further analysis is required to improve the image quality.

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A low-frequency radio halo survey of the South Pole Telescope SZ-selected clusters with the GMRT

Cited by 6 publications

References 74 publications

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

MWA and ASKAP observations of atypical radio-halo-hosting galaxy clusters: Abell 141 and Abell 3404

A GMRT Narrowband vs. Wideband Analysis of the ACT−CL J0034.4+0225 Field Selected from the ACTPol Cluster Sample

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