NGC 1672 | |
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![]() The galaxy photographed with the Víctor M. Blanco Telescope | |
Observation data (J2000 epoch) | |
Constellation | Dorado |
Right ascension | 04h 45m 42.500s[1] |
Declination | −59° 14′ 49.85″[1] |
Redshift | 1331 ± 3 km/s[1] |
Distance | 51.7 ± 3.0 Mly (15.86 ± 0.92 Mpc)[2] |
Apparent magnitude (V) | 10.3[1] |
Characteristics | |
Type | (R')SB(r)bc[1] |
Apparent size (V) | 6.6′ × 5.5′[1] |
Other designations | |
PGC 15941[1] |
NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826.[3] It was originally unclear whether it was a member of the Dorado Group, with some sources[4] finding it to be a member and other sources[5] rejecting its membership. However, recent tip of the red-giant branch (TRGB) measurements indicate that NGC 1672 is located at the same distance as other members, suggesting it is indeed a member of the Dorado Group.[2]
NGC 1672 has a large bar which is estimated to measure around 20 kpc.[6] It has very strong radio emissions emanating from its nucleus, bar, and the inner portion of the spiral arm region.[6] The nucleus is Seyfert type II and is engulfed by a starburst region.[6] The strongest polarized emissions come from the northeastern region which is upstream from its dust lanes.[6] Magnetic field lines are at large angles with respect to the bar and turn smoothly to the center.[6]
Two supernovae have been observed in NGC 1672: SN 2017gax (type Ib/c, mag. 14.1)[7] and SN 2022aau (type II, mag. 16.3).[8]