| Pisces Dwarf | |
|---|---|
 The Pisces Dwarf in combined UV and visible light | |
| Observation data (J2000epoch) | |
| Constellation | Pisces |
| Right ascension | 01h 03m 55.0s[1] |
| Declination | +21° 53′ 06″[1] |
| Redshift | -287 ± 0 km/s[1] |
| Distance | 2.51 ± 0.08Mly (769 ± 25kpc)[2] |
| Apparent magnitude (V) | 14.2[1] |
| Characteristics | |
| Type | dIrr/dSph[1] |
| Apparent size (V) | 2′ × 2′[1] |
| Other designations | |
| Pisces I, Psc I, LGS 3,[1]PGC 3792,[1] LEDA 3792 | |
ThePisces Dwarf, also known asPisces I,[1] is anirregulardwarf galaxy that is part of theLocal Group. The galaxy, taking its name from theconstellationPisces where it appears, is suspected of being asatellite galaxy of theTriangulum Galaxy (M33). It displays ablueshift, as it is approaching theMilky Way at 287 km/s. It may be transition-type galaxy, somewhere betweendwarf spheroidal anddwarf irregular. Alternatively, it may be a rare, but statistically acceptable, version of one of the two types.[2]
It was discovered byValentina Karachentseva in 1976.[2][3][4]
Apparently, the star formation rate in the Pisces Dwarf has been declining for the past 10 billion years. Most of the galaxy's stars were formed in its early years, about 8 billion years ago. The study has also shown that there has been no significant star formation for the past 100 million years. Hence, most of the stars that populate this galaxy are old, metal-rich stars aged about 2.5 billion years. However, there are small clusters of young, hot, blue stars on the outer areas of the galaxy.[5]
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Media related toPisces Dwarf at Wikimedia Commons| Location | Triangulum Galaxy →Triangulum subgroup →Local Group→Local Sheet→Virgo Supercluster→Laniakea Supercluster →Local Hole →Observable universe →Universe Each arrow (→) may be read as "within" or "part of". |  |
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| H II regions | ||
| Suspectedsatellite galaxies | ||