NGC 4299 has a truncated Hα disk with the outer extent of theHα having an irregular distribution except in the southwest where it forms a well-defined ridge. This appears to be the result ofram-pressure.[12]
As a result of a tidal interaction withNGC 4294, NGC 4299 has a disturbed optical andHI morphology,[16][11] with asymmetric spiral arms, a small, weak bar[10] and a high global star formation rate that appears to have been enhanced by ram-pressure.[12]
Chung et al. identified that NGC 4299 has a one sided[17][18] tail of neutral atomichydrogen (HI).[10][19] The tail points to the southwest[17][8] and appears to be a result of ram-pressure[19][20][10] or by a tidal interaction with NGC 4294.[10] The tail has no optical counterpart[10][17] and is oriented parallel to the HI tail found in NGC 4294.[17]
NGC 4299 appears to have a second tail pointing to the southeast that is much broader and lower in HI surface density than the main tail.[17]
^Binggeli, B.; Sandage, A.; Tammann, G. A. (September 1985). "Studies of the Virgo Cluster. II - A catalog of 2096 galaxies in the Virgo Cluster area. V - Luminosity functions of Virgo Cluster galaxies".The Astronomical Journal.90: 1681.Bibcode:1985AJ.....90.1681B.doi:10.1086/113874.ISSN0004-6256.
^Boker, Torsten; Sarzi, Marc; McLaughlin, Dean E.; van der Marel, Roeland P.; Rix, Hans-Walter; Ho, Luis C.; Shields, Joseph C. (2004-01-01). "A Hubble Space Telescope Census of Nuclear Star Clusters in Late-Type Spiral Galaxies. II. Cluster Sizes and Structural Parameter Correlations".The Astronomical Journal.127 (1):105–118.arXiv:astro-ph/0309761.Bibcode:2004AJ....127..105B.doi:10.1086/380231.ISSN0004-6256.S2CID16746074.
^Warmels, R. H. (1988-01-01). "The H I properties of spiral galaxies in the Virgo Cluster. I - Westerbork observations of 15 Virgo Cluster galaxies. II - One-dimensional Westerbork observations of 21 galaxies".Astronomy and Astrophysics Supplement Series.72:19–87.Bibcode:1988A&AS...72...19W.ISSN0365-0138.
