J/A+A/686/A137ivo://CDS.VizieR/J/A+A/686/A137doi:10.26093/cds/vizier.36860137CDSOei M.S.S.L.van Weeren R.J.Hardcastle M.J.Gast A.R.D.J.G.I.B.,Leclercq F.Roettgering H.J.A.Dabhade P.Shimwell T.W.Botteon A.2024-11-29T20:02:43Z2024-06-19T08:11:05ZCDS support team

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

cds-question@unistra.frradio-galaxiesredshiftedGiant radio galaxies (GRGs, giant RGs, or giants) are megaparsec-scale, jet-driven outflows from accretion disks of supermassive black holes, and represent the most extreme pathway by which galaxies can impact the Cosmic Web around them. A long-standing but unresolved question is why giants are so much larger than other radio galaxies. It has been proposed that, in addition to having higher jet powers than most RGs, giants might live in especially low-density Cosmic Web environments. In this work, we aim to test this hypothesis by pinpointing Local Universe giants and other RGs in physically principled, Bayesian large-scale structure reconstructions. More specifically, we localised a LOFAR Two-metre Sky Survey (LoTSS) DR2-dominated sample of luminous (l_{nu}_({nu}=150MHz>=10^24^W/Hz)) giants and a control sample of LoTSS DR1 RGs, both with spectroscopic redshifts up to z_max_=0.16, in the BORG SDSS CosmicWeb reconstructions.We measured the CosmicWeb density on a smoothing scale of 2.9Mpc/h for each RG; for the control sample, we then quantified the relation between RG radio luminosity and Cosmic Web density. With the BORG SDSS tidal tensor, we also measured for each RG whether the gravitational dynamics of its Cosmic Web environment resemble those of clusters, filaments, sheets, or voids. For both luminous giants and general RGs, the Cosmic Web density distribution is gamma distribution-like. Luminous giants populate large-scale environments that tend to be denser than those of general RGs. This result is corroborated by gravitational dynamics classification and a cluster catalogue crossmatching analysis. We find that the Cosmic Web density around RGs with 150 MHz radio luminosity l_{nu}_ is distributed as 1+{DELTA}_RG_|L_{nu}_=l_{nu}_~{GAMMA}(k,{theta}), where k=4.8+0.2.l, {theta}=1.4+0.02.L, and L:=log10(l_{nu}_(10^23^W/Hz)^-1^). This work presents more than a thousand inferred megaparsec-scale densities around radio galaxies, which may be correct up to a factor of order unity - except in clusters of galaxies, where the densities can be more than an order of magnitude too low. We pave the way to a future in which megaparsec-scale densities around RGs are common inferred quantities, which help to better understand their dynamics, morphology, and interaction with the enveloping Cosmic Web. Our data demonstrate that luminous giants inhabit denser environments than general RGs. This shows that - at least at high jet powers - low-density environments are no prerequisite for giant growth. Using general RGs, we quantified the relation between radio luminosity at 150MHz and Cosmic Web density on a smoothing scale of ~2.9Mpc/h. This positive relation, combined with the discrepancy in radio luminosity between known giants and general RGs, reproduces the discrepancy in Cosmic Web density between known giants and general RGs. Our findings are consistent with the view that giants are regular, rather than mechanistically special, members of the radio galaxy population.2024A&A...686A.137Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/686/A137CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/672/A163 : Properties of the 2060 giant radio galaxies (Oei+, 2023)J/ApJ/807/178 : Newly rich galaxy clusters identified in SDSS-DR12 (Wen+ 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/686/A137https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/686/A137http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/686/A137https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/686/A137https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/686/A137http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/686/A137GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/686/A137/tab1grs (Cosmic Web properties for BORG SDSS-constrained giant radio galaxies (table 1))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/686/A137/tab1grs?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/686/A137/tab1grs?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/686/A137/tab1grs?GETtext/xml+votable180.050000true111.57678238.6331660.005555555555555556Cone search capability for table J/A+A/686/A137/tab1rg (Cosmic Web properties for BORG SDSS-constrained radio galaxies (table 1))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/686/A137/tab1rg?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/686/A137/tab1rg?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/686/A137/tab1rg?GETtext/xml+votable180.050000true161.0390286852.136629890.0055555555555555564/686-687 698 707 5/1396 1398 1401-1404 1479 1488-1489 1493-1495 1497-1500 1509 2680 2735 2742-2743 2758-2759 2764 2766-2767 2769 2771-2772 2774-2778 2780 2786-2790 2825 2827 2840 2849 2851 2853-2855 2857-2858 2860 2944 6/4270 4327 4426 4432 4472 4479 4514 4522 4586 4642 4655 4845 4977-4978 4995 5031 5048 5120 5152 5180 5214 5221 5279 5311 5365 5368-5369 5375 5378 5426 5432 5438 5449 5499 5501-5503 5517 5521 5538 5552 5559 5563 5565-5567 5581-5583 5589 5591 5596-5597 5599 5601-5603 5621-5626 5628-5630 5644 5671 5679 5692 5711-5712 5738 5756 5775 5781 5905-5909 5911-5913 5931 5940-5941 5943 5945 5947-5949 5951 5960-5962 5964 5966-5967 5969 5971 5985 5987 6004 6008 6044-6045 6049 6058 6067 6070 6075 6081-6082 6088 6105 6217 6225 6228 6241 6262 6393 6434 6443 6459 6463 6470 6489-6490 6493 6499 6517 6528 6547-6548 6571 6573 6584 6628 6645 6652 7182 7196 7205 7207 7271 7290 7334 7360-7361 7367 7394 7458 7460 7559-7560 7566 7585 8197 8208 8245 8260 8290 8330 8345 8348 8395 8520-8521 8555 8618 8647 8659 8671 8748 8835 8843 8863 8870 9028 9037-9038 9042 9050 9123 9130 9162 9172 9184 9200 9204 9246 9254 9263 9269 9295 9315 9338 9350 9384 9393 9428 9434 9513 9642 9754 9756 9775 9784 9822 10188 10214 10253 10297 10328 10332 10345 10353 10410 10412 10459 10512 10534 10548 10583 10619-10622 10657 10679 10685-10687 10700-10701 10703 10706-10708 10710 10712 10714-10716 10718 10724-10725 10727-10730 10733-10735 10737-10740 10745 10747 10750 10800 10840 10847 10856 10874 10895 10939 10955 10957-10959 10961-10964 10966 11022-11023 11025 11027-11030 11041-11045 11047 11049 11051 11053-11055 11061-11063 11072 11074 11080-11082 11093-11095 11116-11118 11127-11128 11136-11137 11139-11141 11143 11164-11166 11184-11186 11188 11192 11195 11200-11202 11210 11255 11260 11278-11279 11286-11287 11290-11292 11294-11295 11297-11298 11304 11306-11307 11338 11349 11368-11370 11392-11393 11395 11401 11408 11436-11438 11444 11448 11453 11456 11458 11464 11591 11780 11782 11784 11803 11817 11846 11925 11931 21972 25843 25854 25970 25976 26069 26257 26455 26469 27261 27430 27506 27594 27621 27860 27886 27927 27994 28184 28198 28234 28328 28367 28378 28409 28431 28456 28464 28466 28470-28471 28476 28479 28515 28521 28554 28608 28617 28643 28654 31294 31423 31467-31468 31635 31722 32503https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/686/A137?format=asciiRadiodefaultJ/A+A/686/A137/tab1grsCosmic Web properties for BORG SDSS-constrained giant radio galaxies (table 1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Host right ascension (J2000) (host_right_ascension_J2000_(deg))degpos.eq.ra;meta.mainDEJ2000Host declination (J2000) (host_declination_J2000_(deg))degpos.eq.dec;meta.mainzspHostHost spectroscopic redshift (host_spectroscopic_redshift_(1))src.redshift;pos.heliocentricdoublee_zspHost? Host spectroscopic redshift uncertainty (host_spectroscopic_redshift_uncertainty_(1))stat.errordoublenullablemuFixCosmic Web density distribution lognormal fit MLE mu (fixed voxel method; unit: 1) (Cosmic_Web_density_mu_fixed_(1)) (1)phot.mag.sbfloatsigma2FixCosmic Web density distribution lognormal fit MLE sigma^2^ (fixed voxel method; unit: 1) (1) (Cosmic_Web_density_sigma2_fixed_(1))stat.errorfloatmuFlexCosmic Web density distribution lognormal fit MLE mu (flexible voxel method; unit: 1) (Cosmic_Web_density_mu_flexible_(1)) (1)phot.mag.sbfloatsigma2FlexCosmic Web density distribution lognormal fit MLE sigma^2^ (flexible voxel method; unit: 1) (1) (Cosmic_Web_density_sigma2_flexible_(1))stat.errorfloatPcluster[0/1] Cosmic Web dynamical environment cluster probability (unit: 1) (Cosmic_Web_probability_cluster_(1)) (2)stat.fit.goodnessfloatPfilament[0/1] Cosmic Web dynamical environment filament probability (unit: 1) (Cosmic_Web_probability_filament_(1)) (2)stat.fit.goodnessfloatPsheet[0/1] Cosmic Web dynamical environment sheet probability (unit: 1) (Cosmic_Web_probability_sheet_(1)) (2)stat.fit.goodnessfloatPvoid[0/1] Cosmic Web dynamical environment void probability (unit: 1) (Cosmic_Web_probability_void_(1)) (2)stat.fit.goodnessfloatMassHost? Cosmic Web host galaxy cluster mass (Cosmic_Web_cluster_mass_(1e14_Solar_mass))1e+14solMassphys.massfloatnullablePBCG[0/1] Cosmic Web host galaxy is brightest cluster galaxy (1: yes, 0: no) (Cosmic_Web_cluster_host_is_BCG)meta.codeintJ/A+A/686/A137/tab1rgCosmic Web properties for BORG SDSS-constrained radio galaxies (table 1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Host right ascension (J2000) (host_right_ascension_J2000_(deg))degpos.eq.ra;meta.mainDEJ2000Host declination (J2000) (host_declination_J2000_(deg))degpos.eq.dec;meta.mainzspHostHost spectroscopic redshift (host_spectroscopic_redshift_(1))src.redshift;pos.heliocentricdoublee_zspHost? Host spectroscopic redshift uncertainty (host_spectroscopic_redshift_uncertainty_(1))stat.errordoublenullablemuFixCosmic Web density distribution lognormal fit MLE mu (fixed voxel method; unit: 1) (Cosmic_Web_density_mu_fixed_(1)) (1)phot.mag.sbfloatsigma2FixCosmic Web density distribution lognormal fit MLE sigma^2^ (fixed voxel method; unit: 1) (1) (Cosmic_Web_density_sigma2_fixed_(1))stat.errorfloatmuFlexCosmic Web density distribution lognormal fit MLE mu (flexible voxel method; unit: 1) (Cosmic_Web_density_mu_flexible_(1)) (1)phot.mag.sbfloatsigma2FlexCosmic Web density distribution lognormal fit MLE sigma^2^ (flexible voxel method; unit: 1) (1) (Cosmic_Web_density_sigma2_flexible_(1))stat.errorfloatPcluster[0/1] Cosmic Web dynamical environment cluster probability (unit: 1) (Cosmic_Web_probability_cluster_(1)) (2)stat.fit.goodnessfloatPfilament[0/1] Cosmic Web dynamical environment filament probability (unit: 1) (Cosmic_Web_probability_filament_(1)) (2)stat.fit.goodnessfloatPsheet[0/1] Cosmic Web dynamical environment sheet probability (unit: 1) (Cosmic_Web_probability_sheet_(1)) (2)stat.fit.goodnessfloatPvoid[0/1] Cosmic Web dynamical environment void probability (unit: 1) (Cosmic_Web_probability_void_(1)) (2)stat.fit.goodnessfloatMassHost? Cosmic Web host galaxy cluster mass (Cosmic_Web_cluster_mass_(1e14_Solar_mass))1e+14solMassphys.massfloatnullablePBCG[0/1] Cosmic Web host galaxy is brightest cluster galaxy (1: yes, 0: no) (Cosmic_Web_cluster_host_is_BCG)meta.codeint