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M81 Group

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Template:Short description Template:Galaxy cluster

The M81 Group is a galaxy group in the constellations Ursa Major and Camelopardalis that includes the galaxies Messier 81 and Messier 82, as well as several other galaxies with high apparent brightnesses.<ref name="karachentsev2005">Template:Cite journal</ref> The approximate center of the group is located at a distance of 3.6 Mpc, making it one of the nearest groups to the Local Group.<ref name="karachentsev2005" /> The group is estimated to have a total mass of (1.03 ± 0.17)Template:ETemplate:Solar mass.<ref name="Karachentsevetal2006">Template:Cite journal</ref> The M81 Group, the Local Group, and other nearby groups all lie within the Virgo Supercluster (i.e. the Local Supercluster).<ref name="tully1982">Template:Cite journal</ref>

Members

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Template:More references needed The table below lists galaxies that have been identified as associated with the M81 Group by I. D. Karachentsev.<ref name="karachentsev2005" /> Template:Clear

Members of the M81 Group
Name Type<ref name="ned">Template:Cite web</ref> R.A. (J2000)<ref name="ned" /> Dec. (J2000)<ref name="ned" /> Redshift (km/s)<ref name="ned" /> Apparent Magnitude<ref name="ned" />
Arp's LoopTemplate:Cn Template:RA Template:DEC 99 16.1
DDO 78Template:Cn Im Template:RA Template:DEC 55 ± 10 15.8
F8D1Template:Cn dE Template:RA Template:DEC 13.9
FM1Template:Cn dSph Template:RA Template:DEC 17.5
HIJASS J1021+6842Template:Cn Template:RA Template:DEC 46 20
HS 117Template:Cn I Template:RA Template:DEC -37 16.5
Holmberg ITemplate:Cn IAB(s)m Template:RA Template:DEC 139 ± 0 13.0
Holmberg II Im Template:RA Template:DEC 142 ± 1 11.1
Holmberg IX Im Template:RA Template:DEC 46 ± 6 14.3
IC 2574 SAB(s)m Template:RA Template:DEC 57 ± 2 13.2
IKN Template:RA Template:DEC 17.0
KKH 57 dSph Template:RA Template:DEC 18.5
Messier 81 SA(s)ab Template:RA Template:DEC -34 ± 4 6.9
Messier 81 Dwarf A I Template:RA Template:DEC 113 ± 0 16.5
Messier 82 I0 Template:RA Template:DEC 203 ± 4 9.3
NGC 2366 IB(s)m Template:RA Template:DEC 80 ± 1 11.4
NGC 2403 SAB(s)cd Template:RA Template:DEC 131 ± 3 8.9
NGC 2976 SAc pec Template:RA Template:DEC 3 ± 5 10.8
NGC 3077 I0 pec Template:RA Template:DEC 14 ± 4 10.6
NGC 4236 SB(s)dm Template:RA Template:DEC 0 ± 4 10.1
PGC 28529 Im Template:RA Template:DEC -40 17.1
PGC 28731 dE Template:RA Template:DEC -135 ± 30 15.6
PGC 29231 dE Template:RA Template:DEC 16.7
PGC 31286 dSph Template:RA Template:DEC 16.7
PGC 32667 Im Template:RA Template:DEC 116 ± 1 14.9
UGC 4459 Im Template:RA Template:DEC 20 ± 0 14.5
UGC 4483 Template:RA Template:DEC 156 ± 0 15.1
UGC 5428 Im Template:RA Template:DEC -129 ± 0 18
UGC 5442 Im Template:RA Template:DEC -18 ± 14 18
UGC 5692 Sm Template:RA Template:DEC 56 ± 3 13.5
UGC 6456 Pec Template:RA Template:DEC -103 ± 0 14.5
UGC 7242 Scd Template:RA Template:DEC 68 ± 2 14.6
UGC 8201 Im Template:RA Template:DEC 31 ± 0 12.8
UGCA 133 dSph Template:RA Template:DEC 15.6

Note that the object names used in the above table differ from the names used by Karachentsev. NGC, IC, UGC, and PGC numbers have been used in many cases to allow for easier referencing.

Interactions within the group

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Messier 81, Messier 82, and NGC 3077 are all strongly interacting with each other.<ref name="yunetal1994">Template:Cite journal</ref> Observations of the 21-centimeter hydrogen line indicate how the galaxies are connected.<ref name="chynowethetal2008">Template:Cite journal</ref> The gravitational interactions have stripped some hydrogen gas away from all three galaxies, leading to the formation of filamentary gas structures within the group.<ref name="yunetal1994" /> Bridges of neutral hydrogen have been shown to connect M81 with M82 and NGC 3077.<ref name="chynowethetal2008" /><ref name="hulst1978">Template:Cite journal</ref> Moreover, the interactions have also caused some interstellar gas to fall into the centers of Messier 82 and NGC 3077, which has led to strong starburst activity (or the formation of many stars) within the centers of these two galaxies.<ref name="yunetal1994" /> Computer simulations of tidal interactions have been used to show how the current structure of the group could have been created.<ref name="yun1999">Template:Cite book</ref>

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See also

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References

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