J/A+A/695/A15ivo://CDS.VizieR/J/A+A/695/A15doi:10.26093/cds/vizier.36950015CDSZhao Y.Xu H.Liu A.Zhang X.Ji L.Chang J.Hu D.Werner N.,Zhang Z.Cui W.Wu X.2025-05-21T20:02:27Z2025-02-27T09:43:01ZCDS support team

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

cds-question@unistra.frinterstellar-mediumx-ray-sourcesgalaxy-classification-systemsCosmological simulations indicate that nearly half of the baryons in the nearby Universe are in the warm-hot intergalactic medium (WHIM) phase, with about half of which residing in cosmic filaments connecting galaxy clusters. Recent observational studies using stacked survey data and deep exposures of galaxy cluster outskirts have detected soft X-ray excess associated with optically identified filaments. However, the physical characteristics of WHIM in filaments remain largely undetermined due to the lack of direct spectral diagnostics of individual targets, limited by the spectral resolution of current instruments in the soft X-ray band. We aim to select appropriate targets for WHIM characterization through pointing observations with the future HUBS mission, which is designed with eV level energy resolution in the 0.1-2.0keV band and a 1 square degree field-of-view, complementing other planned microcalorimetry missions such as Athena.We built a sample of 1577 inter-cluster filaments based on the first eROSITA All-Sky Survey (eRASS1) supercluster catalog and estimated their soft X-ray emission. Their modeled geometrical properties and oxygen line intensities were used to select candidate targets for HUBS observations.Four inter-cluster filaments were selected as the most appropriated candidates. By simulating and analyzing their mock observations, we demonstrated that with 200ks HUBS exposure for each candidate, the gas properties of individual filaments can be accurately determined, with the temperature constrained to +/-0.01keV, metallicity constrained to <=+/-0.03 solar and density constrained to <+/-10%. Elemental abundance of O, Ne, Mg, and Fe can be measured separately, providing unprecedented insights into the chemical history of the filament gas. We also showed that direct mapping of the WHIM distribution is promising with narrow- band imaging of the O VIII line.Our work forecasts that next-generation X-ray missions such as HUBS will provide substantial improvement in our understanding of the physical status and evolution history of the diffuse WHIM gas in cosmic large-scale structure.2025A&A...695A..15Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A15CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/683/A130 : eRASS Western Galactic Hemisphere Superclusters (Liu+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/695/A15https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/695/A15http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/695/A15https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/695/A15https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/695/A15http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/695/A15GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/695/A15/tableb1 (Physical and emission properties of filament sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/695/A15/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/695/A15/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/695/A15/tableb1?GETtext/xml+votable180.050000true0.6583-47.18730.0055555555555555565/8451 8454 8482 9356 9736 6/4108 4110 4119 4175 4215 4363 4385 4417 4429 4435 4443 4447 4467 4508 4523 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35626 35634 35657 35661 35679 35682 35689 35695 35723-35724 35727 35745 35752 35755 35757 35782 35789 35806 35844 35855 35869 35872 35876 35886 35889 35916 35920 35922 35925 35927 35932 35950 35953 35957 35970 35980 35995 36006 36009 36011-36012 36017 36026 36035 36039-36042 36047 36062 36066 36070 36083 36091 36094 36098 36114 36116 36121 36131 36141 36144 36151 36170 36189-36190 36193 36205-36206 36210 36217 36237 36243 36284 36292-36293 36301-36302 36312 36347 36354 36366-36367 36380 36382 36388-36389 36393 36404 36421 36423 36427 36433-36434 36437 36440 36474 36476 36481 36491 36498 36515 36520 36556 36566 36580 36639 36661 36664 36702-36703 36726 36732-36733 36754 36869 36890 36901 36913 36919 36998 37011 37017-37018 37027 37034 37046 37055-37056 37088 37098 37377-37380 37383-37384 37387 37389 37391 37395 37399-37400 37402 37409 37412 37422-37423 37428 37430 37433-37436 37448 37473 37509 37517-37520 37522 37531 37541 37543 37550-37552 37561-37564 37568 37770 38353 38359 38392 38399 38678 38704 38742 38880 38882 38917-38919 38922 38926 38928 38948 38950-38951 38955 38965-38966 38973-38975 39008 39040 39043 39047-39050 39054 39059-39060 39063 39068-39069 39072-39073 39077 39079 39087 39091-39092 39102 39431 39442-39443 39456 39459 39462 39555-39556 39558 39562 39571 39598 39603 39608 40204 40246 40294 40340 40415 40430 40439 40758 40764 40776 40809 40816 40818 40894 40906 40924-40925 40929 40987 40993 41000 41077 41088 41090 41221 43423 43437 43439 43450 43452 43483 43503 43505 43507 43513 43612 43625 43632 43689 43736 43752 43757-43758 43798 43804 43806 43809 43811 43814 43823 43826 43830 43835-43836 43838 43840 43844 43861 43876 43881 43908 43916-43917 43938-43939 43941 43950 43968 43970-43971 43978 43988 44010 44177 44190-44191 44196 44211 44222 44227 44262 44267 44447 44526 44549-44550 44557 44580 44616 44621 44694 44778 44792 44794 44823 44888 44892 44896-44897 44951 44955 44959 44971 44993 45006 45013 45015 45032 45063 45068 45072-45074 45076 45080 45082-45083 45101 45114 45140 45197 45200 45233 45261 45267 45310 45324 45336 45351-45352 45354 45360 45363 45381-45382 45388 45390 45393 45398 45409 45415 45421 45427 45429 45433 45436-45437 45485 45498 45507 45523 45539 45554 45576 45584 45600 45609 45700 45715 45720 45734 45745 45795-45796 45856 45860 45893 45906 45915 45941 45963 45973 45979 45984 45997 46076 46115 46118 46127 46138 46178-46179 46219 46234 46237 46254 46257-46258 46264 46292 46301-46302 46311-46312 46326 46332 46341 46366 46390 46470 46481 46484 46512 46548 46595 46602 46612 46647 46652 46654 46744 47139 47164 47188 47207 47217 47314 47370 47374 47386 47408 47411 47465https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/695/A15?format=asciiX-rayOpticaldefaultJ/A+A/695/A15/tableb1Physical and emission properties of filament samplezAverage redshift of GC1 and GC2src.redshiftfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintnHTotal hydrogen column density in the direction of average coordinates between the clusters1e+20cm**-2phys.columnDensityfloatCoDistComoving distance between the clustersMpcpos.distancefloatPhysDistPhysical distance between the clustersMpcpos.distancefloatSepAngular separation between the clustersdegpos.angDistancefloatWidthWidth of the filamentarcminsrc.morph.scLengthfloatCoreWidthWidth of the filament corearcminsrc.morph.scLengthfloatLengthLength of the filamentarcminphys.angSizefloatIncAngleAngle of the filament w.r.t. line-of-sightdegpos.posAngfloatSNR-O8Signal-to-noise ratio of the OVIII line with bandwidth of 6eV (1)stat.snrfloat_RAPositions of the first cluster from eRASS (right ascension part)degpos.eq.ra;meta.main_DEPositions of the first cluster from eRASS (declination part)degpos.eq.dec;meta.mainGC1Name of the first galaxy cluster connecting to the filament (1eRASS JHHMMSS.s-DDMMSS)meta.id;meta.maincharGC2Name of the second galaxy cluster connecting to the filament (1eRASS JHHMMSS.s-DDMMSS)meta.idchar