IC 2613,
UGC 5931,
Arp 270, VV 246b,
MCG +06-24-017,
PGC 32424
NGC 3395 is a
peculiarspiral galaxy in the constellation
Leo Minor. The galaxy lies about 55 million
light years away from Earth, which means, given its apparent dimensions, that NGC 3395 is approximately 35,000 light years across.[1] It was discovered by
William Herschel on December 7, 1785.[3] NGC 3395 interacts with
NGC 3396.
NGC 3395 forms an interacting pair with NGC 3396, a
magellanic spiral galaxy that lies 1.5 arcminutes from the nucleus of NGC 3395. The mass ratio of the two galaxies is about 1.5 to 1. The two galaxies appear separate but a bridge of material is visible between them and
tidal tails are observed.[4] Dynamical modelling of the pair suggests that the two galaxies had a first close encounter in the past, which resulting in gas been stripped from NGC 3395 and forming a tidal tail to the south-east.[5] A second close encounter took place about 50 million years ago, resulting to
starburst activity. The two galaxies will most likely
merge in the next 500 million years.[5]
The galaxy hosts a number of
HII regions that are star forming[6] with the region of most intense
star formation being in the northwest of the center, while star formation has also being in observed in the end of the spiral arm northeast of the nucleus and in three regions in the bridge between the two galaxies.[7] Three more star forming regions are visible in a tail southwest of the galaxy.[8] The average size of the knots in NGC 3395 is an order of magnitude smaller than those in NGC 3396.[9] The nucleus of NGC 3395 doesn't appear to be
active.[7]
^
abcClemens, M. S.; Baxter, K. M.; Alexander, P.; Green, D. A. (19 September 1999). "Observations and modelling of the interacting galaxies NGC 3395 and 3396". Monthly Notices of the Royal Astronomical Society. 308 (2): 364–376.
Bibcode:
1999MNRAS.308..364C.
doi:
10.1046/j.1365-8711.1999.02730.x.
^Zaragoza-Cardiel, J.; Font-Serra, J.; Beckman, J. E.; Blasco-Herrera, J.; García-Lorenzo, B.; Camps, A.; Gonzalez-Martin, O.; Ramos Almeida, C.; Loiseau, N.; Gutiérrez, L. (17 April 2013). "Kinematics of Arp 270: gas flows, nuclear activity and two regimes of star formation". Monthly Notices of the Royal Astronomical Society. 432 (2): 998–1009.
arXiv:1303.5020.
doi:
10.1093/mnras/stt527.
^Smith, Beverly J.; Soria, Roberto; Struck, Curtis; Giroux, Mark L.; Swartz, Douglas A.; Yukita, Mihoko (10 February 2014). "Extra-Nuclear Starbursts: Young Luminous Hinge Clumps in Interacting Galaxies". The Astronomical Journal. 147 (3): 60.
arXiv:1401.0338.
Bibcode:
2014AJ....147...60S.
doi:
10.1088/0004-6256/147/3/60.
^Hancock, Mark; Weistrop, Donna; Eggers, Diane; Nelson, Charles H. (April 2003). "Star-forming Knots in the UV-bright Interacting Galaxies NGC 3395 and NGC 3396". The Astronomical Journal. 125 (4): 1696–1710.
Bibcode:
2003AJ....125.1696H.
doi:
10.1086/368234.