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{{about|the suspected satellite galaxy of the Triangulum Galaxy|other dwarf galaxies labelled Pisces|Pisces (disambiguation)}}
{{Infobox Galaxy {{Infobox Galaxy
| name = Pisces Dwarf | name = Pisces Dwarf
| image = ] | image = LGS 3 ubv.jpg
| epoch = ] | image_size = 250px
| caption= The Pisces Dwarf in combined UV and visible light
| epoch = ]
| type = dIrr/dSph<ref name="ned">{{cite web | type = dIrr/dSph<ref name="ned">{{cite web
| title=NASA/IPAC Extragalactic Database | title=NASA/IPAC Extragalactic Database
| work=Results for Pisces Dwarf | work=Results for Pisces Dwarf
| url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Pisces+Dwarf#ObjNo1 | url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Pisces+Dwarf#ObjNo1
| accessdate=2007-03-15 }}</ref> | access-date=2007-03-15 }}</ref>
| ra = {{RA|01|03|55.0}}<ref name="ned" /> | ra = {{RA|01|03|55.0}}<ref name="ned" />
| dec = {{DEC|+21|53|06}}<ref name="ned" /> | dec = {{DEC|+21|53|06}}<ref name="ned" />
| dist_ly = ] ] (769 ± 25 ])<ref name="McConnachieetal2005" /> | dist_ly = ] ] (769 ± 25 ])<ref name="McConnachieetal2005" />
| z = -287 ± 0 km/]<ref name="ned" /> | z = -287 ± 0&nbsp;km/]<ref name="ned" />
| appmag_v = 14.2<ref name="ned" /> | appmag_v = 14.2<ref name="ned" />
| size_v = 2&prime; &times; 2&prime;<ref name="ned" /> | size_v = 2′ × 2′<ref name="ned" />
| constellation name = ] | constellation name = ]
| names = LGS 3,<ref name="ned" /> ] 3792<ref name="ned" /> | names = Pisces I, Psc I, LGS 3,<ref name="ned" /> ] 3792,<ref name="ned" /> LEDA 3792
}} }}


'''Pisces Dwarf''' is an ] ] ] that is part of the ]. The galaxy is also suspected of being a ] of the ] (M33). Because it is in the ] ], the ] is called the ''Pisces Dwarf''. It displays a ], as it is approaching the ] at 287&nbsp;]. It may be transition-type galaxy, somewhere between ] and ]. Alternatively, it may be a rare, but statistically acceptable, version of one of the two types.<ref name="McConnachieetal2005">{{cite journal The '''Pisces Dwarf''', also known as '''Pisces I''',<ref name="ned" /> is an ] ] that is part of the ]. The galaxy, taking its name from the ] ] where it appears, is suspected of being a ] of the ] (M33). It displays a ], as it is approaching the ] at 287&nbsp;]. It may be transition-type galaxy, somewhere between ] and ]. Alternatively, it may be a rare, but statistically acceptable, version of one of the two types.<ref name="McConnachieetal2005">{{cite journal
| author=McConnachie, A. W.; Irwin, M. J.; Ferguson, A. M. N.; Ibata, R. A.; Lewis, G. F.; Tanvir, N. | author=McConnachie, A. W.
| author2=Irwin, M. J.
| author3=Ferguson, A. M. N.
| author4=Ibata, R. A.
| author5=Lewis, G. F.
| author6=Tanvir, N.
| title=Distances and metallicities for 17 Local Group galaxies | title=Distances and metallicities for 17 Local Group galaxies
| journal=Monthly Notices of the Royal Astronomical Society | journal=]
| year=2005 | date=2005
| volume=356 | volume=356
| issue=4 | issue=4
| pages=979–997 | pages=979–997
| bibcode=2005MNRAS.356..979M | bibcode=2005MNRAS.356..979M
| doi=10.1111/j.1365-2966.2004.08514.x |arxiv = astro-ph/0410489 }}</ref> | doi=10.1111/j.1365-2966.2004.08514.x | doi-access=free
|arxiv = astro-ph/0410489 }}</ref>


==History== == History ==
It was discovered by Karachentseva in 1976.<ref name="McConnachieetal2005" /> It was discovered by ] in 1976.<ref name="McConnachieetal2005" /><ref name="Karachentseva1976">{{cite journal
| author=Karachentseva, V. E.
| title=Some characteristics of isolated pairs composed of a normal galaxy and DDO-dwarf
| journal=Soobshch. Spets. Astrofiz. Obs.
| volume=18
| date=1976
| issue=18
| pages=42–51
| bibcode=1976SoSAO..18...42K
| url=https://books.google.com/books?id=A20hAAAAMAAJ&q=%D0%BA%D0%B0%D1%80%D0%B0%D1%87%D0%B5%D0%BD%D1%86%D0%B5%D0%B2%D0%B0+%22%D1%85%D0%B0%D1%80%D0%B0%D0%BA%D1%82%D0%B5%D1%80%D0%B8%D1%81%D1%82%D0%B8%D0%BA%D0%B8+%D0%B8%D0%B7%D0%BE%D0%BB%D0%B8%D1%80%D0%BE%D0%B2%D0%B0%D0%BD%D0%BD%D1%8B%D1%85%22 }}</ref><ref name="Hidalgo2011">{{cite journal|doi=10.1088/0004-637X/730/1/14|title=The Acs Lcid Project. V. The Star Formation History of the Dwarf Galaxy Lgs-3: Clues to Cosmic Reionization and Feedback|journal=The Astrophysical Journal|volume=730|issue=1|pages=14|year=2011|last1=Hidalgo|first1=Sebastian L.|last2=Aparicio|first2=Antonio|last3=Skillman|first3=Evan|last4=Monelli|first4=Matteo|last5=Gallart|first5=Carme|last6=Cole|first6=Andrew|last7=Dolphin|first7=Andrew|last8=Weisz|first8=Daniel|last9=Bernard|first9=Edouard J.|last10=Cassisi|first10=Santi|last11=Mayer|first11=Lucio|last12=Stetson|first12=Peter|last13=Tolstoy|first13=Eline|last14=Ferguson|first14=Henry|arxiv = 1101.5762 |bibcode = 2011ApJ...730...14H |s2cid=118411768}}</ref>


==Star Formation History== == Star formation history ==
⚫ 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.<ref>{{cite journal |author=Miller, B. W., Dolphin, A. E., Lee, M. G., Kim, S. C., Hodge, P. |title=The Star Formation History of LGS3 |journal=The Astrophysical Journal |volume=562 |issue=2 |pages=713–726 |doi=10.1086/323853 |arxiv = astro-ph/0108408 |bibcode = 2001ApJ...562..713M |year=2001 |s2cid=119089499 }}</ref>


== References ==
⚫ A study of the star formation history conducted by Miller et al. 2001 provide much information on how this galaxy developed. 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 Miller 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. But there are small clusters of young, hot, blue stars on the outer areas of the galaxy.
⚫ {{reflist}}


==References== ==External links==
* {{commonscat-inline}}


⚫ {{reflist}}
{{Sky|01|03|55.0|+|21|53|06|2510000}} {{Sky|01|03|55.0|+|21|53|06|2510000}}
{{Triangulum Galaxy}}

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{{galaxy-stub}}

Latest revision as of 20:12, 19 August 2024

This article is about the suspected satellite galaxy of the Triangulum Galaxy. For other dwarf galaxies labelled Pisces, see Pisces (disambiguation).
Pisces Dwarf
The Pisces Dwarf in combined UV and visible light
Observation data (J2000 epoch)
ConstellationPisces
Right ascension01 03 55.0
Declination+21° 53′ 06″
Redshift-287 ± 0 km/s
Distance2.51 ± 0.08 Mly (769 ± 25 kpc)
Apparent magnitude (V)14.2
Characteristics
TypedIrr/dSph
Apparent size (V)2′ × 2′
Other designations
Pisces I, Psc I, LGS 3, PGC 3792, LEDA 3792

The Pisces Dwarf, also known as Pisces I, is an irregular dwarf galaxy that is part of the Local Group. The galaxy, taking its name from the constellation Pisces where it appears, is suspected of being a satellite galaxy of the Triangulum Galaxy (M33). It displays a blueshift, as it is approaching the Milky Way at 287 km/s. It may be transition-type galaxy, somewhere between dwarf spheroidal and dwarf irregular. Alternatively, it may be a rare, but statistically acceptable, version of one of the two types.

History

It was discovered by Valentina Karachentseva in 1976.

Star formation history

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.

References

  1. ^ "NASA/IPAC Extragalactic Database". Results for Pisces Dwarf. Retrieved 2007-03-15.
  2. ^ McConnachie, A. W.; Irwin, M. J.; Ferguson, A. M. N.; Ibata, R. A.; Lewis, G. F.; Tanvir, N. (2005). "Distances and metallicities for 17 Local Group galaxies". Monthly Notices of the Royal Astronomical Society. 356 (4): 979–997. arXiv:astro-ph/0410489. Bibcode:2005MNRAS.356..979M. doi:10.1111/j.1365-2966.2004.08514.x.
  3. Karachentseva, V. E. (1976). "Some characteristics of isolated pairs composed of a normal galaxy and DDO-dwarf". Soobshch. Spets. Astrofiz. Obs. 18 (18): 42–51. Bibcode:1976SoSAO..18...42K.
  4. Hidalgo, Sebastian L.; Aparicio, Antonio; Skillman, Evan; Monelli, Matteo; Gallart, Carme; Cole, Andrew; Dolphin, Andrew; Weisz, Daniel; Bernard, Edouard J.; Cassisi, Santi; Mayer, Lucio; Stetson, Peter; Tolstoy, Eline; Ferguson, Henry (2011). "The Acs Lcid Project. V. The Star Formation History of the Dwarf Galaxy Lgs-3: Clues to Cosmic Reionization and Feedback". The Astrophysical Journal. 730 (1): 14. arXiv:1101.5762. Bibcode:2011ApJ...730...14H. doi:10.1088/0004-637X/730/1/14. S2CID 118411768.
  5. Miller, B. W., Dolphin, A. E., Lee, M. G., Kim, S. C., Hodge, P. (2001). "The Star Formation History of LGS3". The Astrophysical Journal. 562 (2): 713–726. arXiv:astro-ph/0108408. Bibcode:2001ApJ...562..713M. doi:10.1086/323853. S2CID 119089499.{{cite journal}}: CS1 maint: multiple names: authors list (link)

External links


Triangulum Galaxy
LocationTriangulum 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".
Triangulum Galaxy
Triangulum Galaxy
H II regions
Suspected satellite galaxies
Categories: