NGC 4457
SDSS image of NGC 4457
Observation data (J2000 epoch)
Constellation	Virgo
Right ascension	12h 28m 59.0s[1]
Declination	03° 34′ 14″[1]
Redshift	0.002942[1]
Heliocentric radial velocity	882 km/s[1]
Distance	54,801,600 ly
Group or cluster	Virgo II Groups
Apparent magnitude (V)	11.76[1]
Characteristics
Type	(R)SAB(s)0/a, LINER[1]
Size	~ 38,687.32 ly
Apparent size (V)	2.7 × 2.3[1]
Other designations
CGCG 42-124, IRAS 12264+0350, MCG 1-32-75, PGC 41101, UGC 7609, VCC 1145 [1]

NGC 4457 is an intermediate spiral galaxy located about 55 million light-years away^[2] in the constellation of Virgo.^[3] It is also classified as a LINER galaxy, a class of active galaxy defined by their spectral line emissions.^[4][2] NGC 4457 Is inclined by about 33°.^[5] It was discovered by astronomer William Herschel on February 23, 1784.^[6] Despite being listed in the Virgo Cluster Catalog as VCC 1145,^[7] NGC 4457 is a member of the Virgo II Groups^[8][9][10] which form an extension of the Virgo cluster.^[8][11]

NGC 4457 may have had a recent minor merger with another galaxy.^[12]

On July 1 2020, an astronomical transient was discovered in NGC 4457 by astronomer Kiochi Itagaki and confirmed by ASAS-SN. Spectroscopic classification determined the object to be a Type Ia Supernova, SN 2020nvb.^[13]

Physical characteristics

NGC 4457 has a broad oval zone containing an inner spiral which is defined mainly by two fairly open arms. There is a well-defined outer ring that is completely detached from the inner regions of the galaxy.^[14]

Truncated disk

NGC 4457 has a severely reduced amount of star-formation in its disk while its inner regions have a normalized rate of massive star formation.^[14] This may have been caused by a recent interaction of the gas in the galaxy with the gas in the surrounding Virgo Cluster,^[15] causing the gas to be stripped away in an effect known as ram-pressure stripping.^[16]