| NGC 4410 | |
|---|---|
 The interacting pair of galaxies NGC 4410. | |
| Observation data (J2000epoch) | |
| Constellation | Virgo |
| Right ascension | 12h 26m 28.89s[1] |
| Declination | +09° 01′ 10.03″[1] |
| Redshift | 0.024197[1] |
| Heliocentric radial velocity | 7,254km/s ± 109[1] |
| Distance | 365Mly |
| Apparent magnitude (V) | 13.8 (NGC 4410A), 13.6 (NGC 4410B)[2] |
| Characteristics | |
| Type | DBL SYS Sy3[1] |
| Size | ~142,000 ly (43.5 kpc) (estimated) (NGC 4410A), ~250,000 ly (76.7 kpc) (estimated) (NGC 4410B) |
| Other designations | |
| UGC 7535,MK 1325,MCG 2-32-47,PGC 40694 & PGC 40697 | |
NGC 4410 is a pair ofinteracting galaxies located in the constellation ofVirgo. Theredshift of the pair is (z) 0.0241[1] and it was first discovered by the BritishastronomerJohn Herschel in January 1828. It is listed as a member of theVirgo Cluster, but in reality the galaxies lie at a much further distance.[3] The galaxy pair are members of the NGC 4410 group, make up of at least a dozen galaxies, of which a few are found stronglyinteracting with each other.[4]
NGC 4410 is made up of two close galaxies undergoing stronggravitational interactions.[5][6] The first galaxy isNGC 4410A (PGC 40694), classified as apeculiarspiral galaxy of type Sab whileNGC 4410B (PGC 40697) is alenticular galaxy or anelliptical galaxy.[7][3][4][8] The nucleus of NGC 4410A has been categorized asactive and it has been described as both aradio galaxy of low luminosity and aLINER galaxy. NGC 4410B has an active galactic nucleus like NGC 4410A and is also a LINER galaxy.[9][4] There is aring-like structure in NGC 4410A based onoptical imaging, with numerousH II regions present along the ring direction.X-ray emission has been detected. Bright knot features have also been detected, mainly in southeast and northeast directions from its bright central nucleus.[4] Both nuclei of the galaxies are clearly seen, with the nucleus of NGC 4410A being depicted as elongated by 10 arcseconds from southwest to northeast. Thestar formation of NGC 4410A has been estimated to be 1-4 Mʘ per year.[9]
The radio structure of NGC 4410A is peculiar. When observed by theVery Large Array (VLA), it is revealed as extended by around four arcseconds, with the presence of opticalradio emission in its large region. A single compact component was detected through observations at 6 and 2centimeters.[10] Other observations also found there are at least tworadio lobes depicted as edge-brightened and it has an overall size of around 90kiloparsecs when seen from east to west direction. Theradio spectrum of the source in the central region and the knot feature is flat, but when going towards the south-east part, it becomes steep.[11]
A study published in 2008 found there are complicated structures inside NGC 4410A, with a small prominent H II region that is located southeast from the nucleus and also atidal arm feature both west and northwest from it. There is also adust lane present. Aspiral arm structure is seen within theradius of the central regions of NGC 4410A by around 4 to 5arcseconds.Axisymetrical structures are also detected in NGC 4410B from southeast to northwest, which in turn, run through the center. This is suggested to be an edge-ongalaxy disc. NGC 4410B also has boxy isothopes.[12]
It is confirmed NGC 4410A and NGC 4410B aremerging with each other, that the merger also includes two other galaxies;IC 790 orNGC 4410C (alenticular galaxy) andNGC 4410D, given there are tidal features and bridges of emission connecting each other.[12][4][11] AH I tail feature has been found in a southeast direction from NGC 4410A and NGC 4410B, and is extended by 50 kiloparsecs. The total combined H2 mass for both galaxies has been estimated as 3.9 x 109 Mʘ.[6]
Onesupernova has been observed in NGC 4410:SN 1965A (type unknown, mag. 16) was discovered by Enrique Chavira on 1 January 1965.[13]
