The Southern Supercluster Strand is a galaxy filament that encompasses the Southern Supercluster and the Telescopium−Grus Cloud.

In 2014, it was announced that the Southern Supercluster Strand is a lobe in a greater supercluster, Laniakea, that is centered on the Great Attractor. This would mean that the Southern Supercluster Strand's components, the Telescopium−Grus Cloud and the Southern Supercluster would be part of this new supercluster. The Virgo Supercluster would also be part of this greater supercluster, thus becoming the local supercluster.

Physical characteristics The Southern Supercluster Strand is a galaxy filament that emerges from the Centaurus Cluster. The filament then branches off into two forks, SSCa, and SSCb, also known as the Southern Supercluster and the Telescopium−Grus Cloud respectively. The Southern Supercluster is a long major chain of galaxies, consisting of the major Dorado, Fornax, and Eridanus clusters while the Telescopium−Grus Cloud is a low density galaxy filament, with no central concentration of galaxies. The Telescopium−Grus Cloud along with the Pavo-Indus Supercluster form parts of a wall bounding the Local Void. Likewise, both structures along with the Southern Supercluster also form a wall bounding the Sculptor Void. The Southern Supercluster Srand extends all the way to the Perseus–Pisces Supercluster. The Southern Supercluster Strand, along with the Centaurus–Puppis–PP filament, which contains the Antila Wall and both extend to the Perseus–Pisces Supercluster, form a wall bounding the Sculptor Void.

Cetus-Aries Cloud The Cetus-Aries Cloud, is a minor filament that was identified and described in 1987 by astronomer Brent Tully with colleague Richard Fisher in his book The Nearby Galaxies Atlas, and connects the Southern Supercluster (though the Dorado Group) with the Telescopium−Grus Cloud.

List of Groups Below is a list of groups in the Cetus-Aries Cloud according to astronomer Brent Tully.

Column 1: The name of the group in Tully's NBGC Column 2: The right ascension for epoch 2000. Column 3: The declination for epoch 2000. Column 4: Number of members of the group. Column 5: Brightest member of the group Column 6: Redshift of the group. Column 7: Distance of the group (Millions of light-years). Column 8: Cross-Identifications with other catalogs.

(Sources for data columns:) +Groups within the Cetus-Aries CloudName of group R.A. (J2000)Dec. (J2000)Number of membersBrightest memberRedshiftDistance (Mly)Cross-IDNBGC 52-102h 41m 09.3s −08d 07m 10s 11 (Tully) 9 (Fourque) 14 (Garcia) 11 (Giuricin)NGC 10520.00493956NGC 988 Group, NGC 1052 Group, NGC 1084 Group, LGG 71, NOGG H 175, NOGG P1 162, NOGG P2 165, [FWB89] GrG 207, [HG82] 44NBGC 52-202h 42m 40.7s −00d 00m 48s 8 (Tully) 6 (Fourque) 6 (Garcia) 5 (Giuricin)NGC 10680.00377340NGC 1068 Group, M77 Group, LGG 73, NOGG H 178, NOGG P1 165, NOGG P2 168 [HG82] 48, [GH83] 032, [TSK2008] 0890NBGC 52-302h 28m 26.1s −01d 29m 16s 5 (Tully) 4 (Fourque) 7 (Garcia) 2/6 (Giuricin)NGC 9360.00487354NGC 936 Group, LGG 60, NOGG H 160, NOGG P1 147, NOGG P2 151 [TSK2008] 0891, [GH83] 028NBGC 52-402h 46m 25.1s −00d 29m 55s3 (Tully) 2 (Giuricin)NGC 10870.00508062NGC 1087 Group, NOGG H 182 NBGC 52-501h 59m 42.3s −05d 57m 47s 2 (Tully) 2 (Giuricin)NGC 7790.00464056NGC 779 Group, NOGG H 126, NOGG P1 111, NOGG P2 115NBGC 52-602h 22m 14.9s −21d 00m 04s 6 (Tully) 6 (Fourque) 8 (Garcia) 6 (Giuricin)NGC 9080.00501961NGC 908 Group LGG 56 NOGG H 158, NOGG P1 145, NOGG P2 148 [MdL89] 83, SSRS GROUP 83NBGC 52-701h 33m 21.4s −07d 01m 17s 6 (Tully) 8 (Fourque) 8 (Garcia) 9 (Giuricin)NGC 5840.00600467NGC 584 Group, Cetus Group, LGG 27, NOGG H 83, NOGG P1 71, NOGG P2 75, [HG82] 45, [TSK2008] 0895NBGC 52-801h 49m 49.7s −10d 03m 05s 3 (Tully) 3 (Fourque) 3 (Garcia) 2/3 (Giuricin)NGC 6810.00615870NGC 681 Group, LGG 33, NGC 701 Group, NOGG H 107, NOGG P1 90, NOGG P2 93, [TSK2008] 0896NBGC 52-901h 52m 57.5s -13d 30m 20s 4 (Tully) 4 (Fourque) 4 (Garcia) 3/6/2 (Giuricin)NGC 7200.00587167NGC 720 Group, LGG 38, NOGG H 103, NOGG P1 98, NOGG P2 103 NBGC 52-1002h 15m 27.6s 06d 00m 09s 2 (Tully) 3 (Fourque) 5 (Garcia) 2 (Giuricin)NGC 8640.00521067NGC 864 Group, NOGG H 150 NBGC 52-1101h 50m 54s05d 24m 02s2 (Tully) 3 (Fourque) 3/2 (Giuricin)NGC 6760.00480752NGC 676 Group NOGG H 108, NOGG P1 92, NOGG P2 95, NBGC 52-1201h 21m 18.8s 03d 31m 51s6 (Tully) 4 (Fourque) 5 (Garcia) 5 (Giuricin)NGC 4880.00781291NGC 488 Group, LGG 21, NGC 470 Group, LGG 20 NOGG H 70, NOGG P1 60, NOGG P2 62 G45NBGC 52-1301h 31m 10.3s 04d 13m 56s 2 (Tully) 2 (Giuricin)UGC 11330.00656183UGC 1133 Group, NOGG H 85, NOGG P1 74, NOGG P2 78NBGC 52-1401h 58m 26.7s 18d 45m 50s 3 (Tully) 3 (Garcia) 3 (Giuricin)NGC 7720.00802995NGC 772 Group, LGG 40, NOGG H 124, NOGG P1 109, NOGG P2 112, [TSK2008] 0915; [M98j] 032NBGC 52-1501h 50m 37.0s21h 54m 14s2 (Tully) 5 (Fourque) 10 (Garcia) 7 (Giuricin)NGC 691, NGC 6970.009762118NGC 691 Group, LGG 34, NGC 697 Group, NOGG H 109, NOGG P1 95, NOGG P2 99, HIPASS J0150+21, [GH83] 020

Observational history Before the Southern Supercluster Strand was identified, its two major components were already known: the Southern Supercluster which was discovered in 1953 by astronomer Gérard de Vaucouleurs, and the Telescopium−Grus Cloud which was discovered by astronomer Brent Tully with colleague Richard Fisher in 1987.

In 1987, astronomer Brent Tully with colleague Richard Fisher discovered and described the Cetus-Aries Cloud, a minor filament that connects the Southern Supercluster with the Telescopium−Grus Cloud. In 1992, Fouque et al. grouped the Cetus-Aries Cloud, also known as cloud 52 in the book The Nearby Galaxies Atlas along with the Southern Supercluster's three major clusters, the Fornax, Eridanus, and Dorado clusters (clouds 51 and 53).

In 2013, Courtois et al. discovered based on the distribution of galaxies inferred from their redshifts the Southern Supercluster Strand, which branches off into two forks that emerge from the Centaurus Cluster. These two forks were designated SSCa and SSCb, also known as the Southern Supercluster and the Telescopium−Grus Cloud. In 2017, Pomarède et al. revealed that the Southern Supercluster strand along with another filament known as the Antlia Strand, extend all the way to the Perseus–Pisces Supercluster.

See also Large-scale structure of the universe Galaxy filament

References