J/A+A/699/A375ivo://CDS.VizieR/J/A+A/699/A375doi:10.26093/cds/vizier/bc-nv/ldhfCDSMajumder A.Simionescu A.Plsek T.Brienza M.Churazov E.,Khabibullin I.Gastaldello F.Botteon A.Roettgering H.Brueggen M.,Lyskova N.Rajpurohit K.Sunyaev R.A.Wise M.W.2026-08-03T06:55:57Z2025-07-25T08:02:28ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fractive-galactic-nucleix-ray-sourcesGalaxy groups are more susceptible to feedback from the central active galactic nuclei (AGN) due to their lower gravitational binding energy compared to clusters. This makes them ideal laboratories to study feedback effects on the overall energy and baryonic mass budget. We study the LOFAR-detected galaxy group Nest200047, where there is clear evidence of multiple generations of radio lobes from the AGN. Using 140ks Chandra and 25ks XMM-Newton data, we investigate thermodynamic properties of the intragroup medium including any excess energy due to the central AGN. We also investigate the X-ray properties of the central black hole and constrain the 2-10keV X-ray flux. We used spectral analysis techniques to measure various thermodynamic profiles across the whole field of view. We also used both imaging and spectral analysis to detect and estimate the energy deposited by potential shocks and cavities. Due to the faint emission from the object beyond the core, various background effects were considered. Nest200047 has significant excess entropy, and the AGN likely contributes to a part of it. There is an excess energy of (5-6.5)x10^60^erg within 400kpc, exceeding the binding energy. The pressure profile indicates that gas is likely being ejected from the system, resulting in a baryon fraction of ~4% inside r500. From scaling relations, we estimate a black hole mass of (1=4)x10^9^M_{sun}_. An upper limit of 2.1c10^40^erg/s was derived on the black hole bolometric luminosity, which is ~2.5% of the Bondi accretion power. Nest200047 is likely part of a class of over-heated galaxy groups like ESO 3060170, AWM 4 and AWM 5. Such excessive heating may lead to high quenching of star formation. Moreover, the faint X-ray nuclear emission in Nest is likely due to the accretion energy being converted into jets rather than radiation.2025A&A...699A.375Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/699/A375CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/699/A375https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/699/A375http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/699/A375https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/699/A375https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/699/A375http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/699/A375GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/699/A375/list (List of images)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/699/A375/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/699/A375/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/699/A375/list?GETtext/xml+votable180.050000true61.6025830.476330.0055555555555555566/1200https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/699/A375?format=asciiX-raydefaultJ/A+A/699/A375/listList of imagesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.dateObservation datestime.epoch;obsnullablesizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory imgmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar