NGC 4302

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NGC 4302
250px
SDSS image of NGC 4302. NGC 4298 can be seen to the right of the image.
Observation data (J2000 epoch)
Constellation Coma Berenices
Right ascension 12h 21m 42.5s[1]
Declination 14° 35′ 54″[1]
Redshift 0.003833[1]
Helio radial velocity 1149 km/s[1]
Distance 55 Mly (17 Mpc)[1]
Group or cluster Virgo Cluster
Type Sc[1]
Mass 1.0×1011[2] M
Size (ly) ~106,000 ly (32.5 kpc) (estimated)[1]
Apparent dimensions (V) 2.78 x 0.75[1]
Apparent magnitude (V) 13.6[1]
Other designations
CGCG 99-27, KCPG 332B, MCG 3-32-9, PGC 39974, UGC 7418, VCC 497[1]
See also: Galaxy, List of galaxies

NGC 4302 is an edge-on spiral galaxy[3] located about 55 million light-years away[3][4] in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784[5] and is a member of the Virgo Cluster.[6][4][7]

It is classified as a Seyfert galaxy and as a LINER galaxy.[8][3] It also has a prominent, extended dust lane.[9][10]

Physical characteristics

The disk of NGC 4302 contains extraplanar dust that is organized into filamentary structures and large dust complexes. The apparent bending of many of the large complexes toward the north of the galaxy appears to be due to an interaction with the intracluster medium caused by the motion of NGC 4302 as it falls into the Virgo Cluster.

The dense, dusty matter in the disk of NGC 4302 appears to be largely tracing matter ejected from the disk by energetic feedback from massive stars.[11]

File:NGC 4302 hst 08242 R814G555B450.png
Hubble image of the dust lane and bulge of NGC 4302.

Extraplanar Diffuse Ionized Gas

First detected by Pildis et al.,[12] NGC 4302 has a faint but prominent layer of extraplanar diffuse ionized gas (DIG) that extends out to a galactocentric radius of ~13,000 ly (4 kpc) and a height of ~6,500 ly (2 kpc) above the plane of the galaxy.[9][13][10][14][11]

The DIG appears to have been ionized by photoionization by OB stars.[13]

Box/Peanut Bulge

The presence of a boxy/peanut bulge in NGC 4302[15] suggests that the galaxy contains a thickened bar that is viewed edge-on.[16]

HI Disk

The HI disk of NGC 4302 is truncated to within the optical disk to the south of the galaxy.[17][16][18][19][20] This truncation appears to be the result of ram-pressure.[17][16][19]

Tidal Bridge

Kantharia et al. and Zschaechner et al. both independently detected a tidal bridge between NGC 4302 and NGC 4298. The bridge is the result of a tidal interaction between the two galaxies.[21][22][2]

HI tail

First identified by Chung et al., NGC 4302 has a ~52,000 ly (16 kpc)[17] tail of neutral atomic hydrogen (HI)[17][16][18][23][11][20][2] that extends to the north of the galaxy.[17][16] The tail appears to be a result of ram-pressure[17][16][23][11][2] or by a tidal interaction with NGC 4298.[18][23] However, NGC 4302 appears relatively undisturbed favoring the cause of the tail to be due to ram-pressure.[23]

The HI tail is pointed away from M87 which suggests that NGC 4302 is falling into the center of the Virgo Cluster on a highly radial orbit.[17][16]

SN 1986E

NGC 4302 has hosted one supernova,[24] a Type IIL Supernova designated as SN 1986.[25][26] The supernova by G. Candeo at the Asiago Observatory on April 13, 1986 with a Apparent magnitude of 14.5.[25][26]

See also

External link

References

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