LEADER 01194nas 2200373- 450 001 9910131147903321 005 20210111025302.2 011 $a2331-9976 035 $a(OCoLC)819546186 035 $a(CKB)3460000000085222 035 $a(CONSER)--2013272072 035 $a(EXLCZ)993460000000085222 100 $a20121128b18541972 k-- a 101 0 $aeng 135 $aur|n||||||||| 181 $ctxt$2rdacontent 182 $cc$2rdamedia 183 $acr$2rdacarrier 200 10$aEvening star 210 1$aWashington, D.C. :$cWallach & Hope,$d1854-1972. 215 $a1 online resource 300 $a"From April 25 through May 24, 1861 one sheet issues were published intermittently owing to scarcity of paper." Cf. Library of Congress, Photoduplication Service. 300 $aPublisher varies: Noyes, Baker & Co., <1867>; Evening Star Newspaper Co., <1868- > 311 $a2331-9968 517 1 $aSunday star 517 1 $aStar 607 $aWashington (D.C.)$vNewspapers 607 $aWashington (D.C.)$2fast 608 $aNewspapers.$2fast 676 $a071 906 $aJOURNAL 912 $a9910131147903321 996 $aEvening star$92182421 997 $aUNINA LEADER 02804nam 2200589z- 450 001 9910557684203321 005 20220111 035 $a(CKB)5400000000044690 035 $a(oapen)https://directory.doabooks.org/handle/20.500.12854/76813 035 $a(oapen)doab76813 035 $a(EXLCZ)995400000000044690 100 $a20202201d2021 |y 0 101 0 $aeng 135 $aurmn|---annan 181 $ctxt$2rdacontent 182 $cc$2rdamedia 183 $acr$2rdacarrier 200 00$aThe Physical Properties of the Groups of Galaxies 210 $aBasel, Switzerland$cMDPI - Multidisciplinary Digital Publishing Institute$d2021 215 $a1 online resource (250 p.) 311 08$a3-0365-1773-1 311 08$a3-0365-1774-X 330 $aGalaxy groups consist of a few tens of galaxies bound in a common gravitational potential and contain a significant fraction of the overall universal baryon budget. Therefore, they are key to our understanding of how the bulk of matter in the Universe accretes and forms hierarchical structures and how different sources of feedback affect their gravitational collapse. However, despite their crucial role in cosmic structure formation and evolution, galaxy groups have received less attention compared to massive clusters. This is perhaps in part due to their rarity in being observed and properly characterized. With the advent of eROSITA, many thousands of galaxy groups will be detected by X-ray, complementing optical and SZ coverage. In this Special Issue we collected and organized the latest developments in our understanding of these systems and present future prospects from both observational and theoretical points of view. 606 $aResearch and information: general$2bicssc 610 $aactive galactic nuclei 610 $aactive nuclei 610 $ablack holes 610 $acosmological parameters 610 $aelliptical galaxies 610 $afossil galaxy groups 610 $agalaxies:abundances 610 $agalaxies:clusters:intracluster medium 610 $agalaxy clusters 610 $agalaxy groups 610 $agalaxy surveys 610 $ahydrodynamical and cosmological simulations 610 $ahydrodynamical simulations 610 $aintragroup medium/plasma 610 $an/a 610 $aUV observations 610 $aX-ray and optical observations 610 $aX-ray observations 610 $aX-rays:galaxies 615 7$aResearch and information: general 700 $aLovisari$b Lorenzo$4edt$01300053 702 $aEttori$b Stefano$4edt 702 $aLovisari$b Lorenzo$4oth 702 $aEttori$b Stefano$4oth 906 $aBOOK 912 $a9910557684203321 996 $aThe Physical Properties of the Groups of Galaxies$93025377 997 $aUNINA