NGC 4299 | |
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SDSS image of NGC 4299 | |
Observation data ( J2000 epoch) | |
Constellation | Virgo |
Right ascension | 12h 21m 40.5s [1] |
Declination | 11° 30′ 00″ [1] |
Redshift | 0.000791 [1] |
Heliocentric radial velocity | 237 km/s [1] |
Distance | 55 Mly (16.8 Mpc) [1] |
Group or cluster | Virgo Cluster |
Apparent magnitude (V) | 12.88 [1] |
Characteristics | |
Type | SAB(s)dm [1] |
Size | ~36,000 ly (11 kpc) (estimated) [1] |
Apparent size (V) | 1.7 x 1.6 [1] |
Other designations | |
VCC 491, IRAS 12191+1146, UGC 7414, MCG +02-32-010, PGC 39968, CGCG 70-25 [1] |
NGC 4299 is a featureless spiral galaxy [2] located about 55 million light-years away [3] [4] in the constellation Virgo. It was discovered by astronomer William Herschel on March 15, 1784 [5] and is a member of the Virgo Cluster. [6] [4] [7]
NGC 4299 forms an interacting pair with NGC 4294. [8]
NGC 4299 has a fairly featureless disk [9] with a very small, weak bulge and weak, asymmetric spiral arms [10] plus numerous bright HII regions. [11] [12]
At the center of NGC 4299 lies a nuclear star cluster [13] [14] with a diameter of ~5.9 ly (1.8 pc). [15]
NGC 4299 has a truncated Hα disk with the outer extent of the Hα having an irregular distribution except in the southwest where it forms a well-defined ridge. This appears to be the result of ram-pressure. [12]
As a result of a tidal interaction with NGC 4294, NGC 4299 has a disturbed optical and HI 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 atomic hydrogen (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]
NGC 4299 may harbor an intermediate-mass black hole with an estimated mass ranging from 7,000 (7*10^3) to 200,000 (2*10^5) solar masses. [21]
NGC 4299 | |
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![]()
SDSS image of NGC 4299 | |
Observation data ( J2000 epoch) | |
Constellation | Virgo |
Right ascension | 12h 21m 40.5s [1] |
Declination | 11° 30′ 00″ [1] |
Redshift | 0.000791 [1] |
Heliocentric radial velocity | 237 km/s [1] |
Distance | 55 Mly (16.8 Mpc) [1] |
Group or cluster | Virgo Cluster |
Apparent magnitude (V) | 12.88 [1] |
Characteristics | |
Type | SAB(s)dm [1] |
Size | ~36,000 ly (11 kpc) (estimated) [1] |
Apparent size (V) | 1.7 x 1.6 [1] |
Other designations | |
VCC 491, IRAS 12191+1146, UGC 7414, MCG +02-32-010, PGC 39968, CGCG 70-25 [1] |
NGC 4299 is a featureless spiral galaxy [2] located about 55 million light-years away [3] [4] in the constellation Virgo. It was discovered by astronomer William Herschel on March 15, 1784 [5] and is a member of the Virgo Cluster. [6] [4] [7]
NGC 4299 forms an interacting pair with NGC 4294. [8]
NGC 4299 has a fairly featureless disk [9] with a very small, weak bulge and weak, asymmetric spiral arms [10] plus numerous bright HII regions. [11] [12]
At the center of NGC 4299 lies a nuclear star cluster [13] [14] with a diameter of ~5.9 ly (1.8 pc). [15]
NGC 4299 has a truncated Hα disk with the outer extent of the Hα having an irregular distribution except in the southwest where it forms a well-defined ridge. This appears to be the result of ram-pressure. [12]
As a result of a tidal interaction with NGC 4294, NGC 4299 has a disturbed optical and HI 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 atomic hydrogen (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]
NGC 4299 may harbor an intermediate-mass black hole with an estimated mass ranging from 7,000 (7*10^3) to 200,000 (2*10^5) solar masses. [21]