X-ray Emission and Radio Emission from the Jets and Lobes of the Spiderweb Radio Galaxy

Abstract

Deep Chandra and VLA imaging reveals a clear correlation between X-ray and radio emission on scales ∼ 100 kpc in the Spiderweb radio galaxy at z=2.16. The Xray emission associated with the extended radio source is likely dominated by inverse Compton up-scattering of cosmic microwave background photons by the radio emitting relativistic electrons. For regions dominated by high surface brightness emission, such as hot spots and jet knots, the implied magnetic fields are ∼ 50 µG to 70 µG. The nonthermal pressure is these brighter regions is then ∼ 9 × 10 −10 dyne cm −2 , or three times larger than the non-thermal pressure derived assuming minimum energy conditions, and an order of magnitude larger than the thermal pressure in the ambient cluster medium. Assuming ram pressure confinement implies an average advance speed for the radio source of ∼ 2400 km s −1 , and a source age of ∼ 3 × 10 7 years. Considering the lower surface brightness, diffuse radio emitting regions, we identify an evacuated cavity in

Signs of environmental effects on star-forming galaxies in the Spiderweb protocluster at z = 2.16

“…From that moment, the Spiderweb protocluster has been subject to exhaustive spectrophotometric campaigns to unveil the properties and distribution of its galaxy populations. This includes the characterization of the central radio galaxy (Pentericci et al 2000;Carilli et al 2002;Miley et al 2006;Hatch et al 2008Hatch et al , 2009Emonts et al 2016: De Breuck et al 2022, Carilli et al 2022, the location of several X-ray emitters (Pentericci et al 2002;Croft et al 2005;Tozzi et al 2022), the observation of an emerging red sequence within the cluster core (Kurk et al 2004;Kodama et al 2007;Zirm et al 2008;Tanaka et al 2010Tanaka et al , 2013, the discovery of a network of starbursty submillimeter galaxies (SMGs, Dannerbauer et al 2014Dannerbauer et al , 2017, the location of a rich population of H𝛼 emitters (HAEs) which represent the bulk of the known cluster members up to date (Kuiper et al 2011;Hatch et al 2011;Koyama et al 2013;Shimakawa et al 2014Shimakawa et al , 2015Shimakawa et al , 2018b, and the use of (sub-)millimeter observations to trace the dust content and gas reservoirs of several protocluster members (Emonts et al 2018;Tadaki et al 2019) as well as the mapping of the protocluster large scale structure in CO(1-0) using ATCA (Jin et al 2021).…”