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Coordinates: Sky map 00h 20m 17.3s, +59° 18′ 14″
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{{short description|Irregular starburst galaxy in the constellation Cassiopeia}}
{{Use dmy dates|date=October 2011}}
{{Use dmy dates|date=July 2019}}
{{Infobox Galaxy
{{Infobox Galaxy
| image = IC10 BVHa.jpg
| image = IC10 BVHa.jpg
| image_size = 250px
| image_size = 250px
|caption = Irregular Galaxy IC 10.
|caption = Irregular Galaxy IC 10
| name = IC 10
| name = IC 10
| type = dIrr IV/BCD<ref name="ned">{{cite web
| type = dIrr IV/BCD<ref name="ned">{{cite web
Line 9: Line 10:
| work=Results for IC 10
| work=Results for IC 10
| url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?search_type=Obj_id&objid=58126&objname=57
| url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?search_type=Obj_id&objid=58126&objname=57
| accessdate=2007-03-15 }}</ref>
| access-date=2007-03-15 }}</ref>
| epoch = [[Epoch (astronomy)#Julian years and J2000|J2000]]
| epoch = [[Epoch (astronomy)#Julian years and J2000|J2000]]
| ra = {{RA|00|20|17.3}}<ref name="ned" />
| ra = {{RA|00|20|17.3}}<ref name="ned" />
| dec = {{DEC|+59|18|14}}<ref name="ned" />
| dec = {{DEC|+59|18|14}}<ref name="ned" />
| dist_ly = 2.2 ± 0.2 [[light-year|Mly]] (660 ± 60 [[parsec|kpc]])<ref name="Karachentsevetal2006">{{cite journal
| dist_ly = 2.5 ± 0.5 [[light-year|Mly]] (750 ± 150 [[parsec|kpc]])<ref>{{Cite web|title=NED Query Results for IC 0010|url=http://ned.ipac.caltech.edu/cgi-bin/nDistance?name=IC+0010|access-date=2021-08-08|website=ned.ipac.caltech.edu}}</ref>
⚫
| z = {{val|0.001161|0.000003}}<ref name="ned" />
|author1=Karachentsev, I. D. |author2=Kashibadze, O. G. | title=Masses of the local group and of the M81 group estimated from distortions in the local velocity field
| journal=Astrophysics
| date=2006
| volume=49
| issue=1
| pages=3–18
| bibcode=2006Ap.....49....3K | doi=10.1007/s10511-006-0002-6
⚫
}}</ref>
⚫
| z = -0.001161 +/- 0.000003<ref name="ned" />
| appmag_v = 10.4 ± 0.2 <ref name="Star-Watcher IC 10">{{cite web
| appmag_v = 10.4 ± 0.2 <ref name="Star-Watcher IC 10">{{cite web
| title=IC 10
| title=IC 10
| work=Star-Watcher
| work=Star-Watcher
| url=http://www.star-watcher.org/IC10.html}}</ref>
| url=http://www.star-watcher.org/IC10.html}}</ref>
| size_v = 6&prime;.8 × 5&prime;.9<ref name="ned" />
| size_v = 6.8{{prime}} × 5.9{{prime}}<ref name="ned" />
| size = 5000 [[Light-year|light years]] (diameter)<ref>{{Cite web|title=APOD: 2012 January 4 – Starburst Galaxy IC 10|url=https://apod.nasa.gov/apod/ap120104.html|access-date=2021-08-08|website=apod.nasa.gov}}</ref>
| constellation name = [[Cassiopeia (constellation)|Cassiopeia]]
| constellation name = [[Cassiopeia (constellation)|Cassiopeia]]
| notes = mild [[starburst galaxy]]
| notes = mild [[starburst galaxy]]
Line 37: Line 31:
| work=SEDS Messier Database
| work=SEDS Messier Database
| url=http://messier.seds.org/xtra/ngc/i0010.html
| url=http://messier.seds.org/xtra/ngc/i0010.html
| accessdate=2006-05-15}}</ref> and in 1935 [[Nicholas Mayall]] became the first to suggest that the object is extragalactic. [[Edwin Hubble]] suspected it might belong to the [[Local Group]] of [[Galaxy|galaxies]], but its status remained uncertain for decades. The [[radial velocity]] of IC 10 was measured in 1962, and it was found to be approaching the [[Milky Way]] at approximately
| access-date=2006-05-15}}</ref> and in 1935 [[Nicholas Mayall]] became the first to suggest that the object is extragalactic. [[Edwin Hubble]] suspected it might belong to the [[Local Group]] of [[Galaxy|galaxies]], but its status remained uncertain for decades. The [[radial velocity]] of IC 10 was measured in 1962, and it was found to be approaching the [[Milky Way]] at approximately
350&nbsp;km/s, strengthening the evidence for its membership in the Local Group.<ref name="SEDS"/> Its membership in the group was finally confirmed in 1996 by direct measurements of its
350&nbsp;km/s, strengthening the evidence for its membership in the Local Group.<ref name="SEDS"/> Its membership in the group was finally confirmed in 1996 by direct measurements of its
distance based on observations of [[Cepheid variable|Cepheid]]s. Despite its closeness, the galaxy is rather difficult to study because it lies near the plane of the [[Milky Way]] and is therefore
distance based on observations of [[Cepheid variable|Cepheid]]s; most estimates place the galaxy 2–3 million [[light years]] from Earth, with some estimates ranging from 1.5–4.5 million [[light years]].<ref>{{Cite web|title=NED Query Results for IC 0010|url=http://ned.ipac.caltech.edu/cgi-bin/nDistance?name=IC+0010|access-date=2021-08-08|website=ned.ipac.caltech.edu}}</ref> Despite its closeness, the galaxy is rather difficult to study because it lies near the plane of the [[Milky Way]] and is therefore
heavily obscured by [[Interstellar medium|interstellar matter]].<ref name="Bergh">{{cite book
heavily obscured by [[Interstellar medium|interstellar matter]].<ref name="Bergh">{{cite book
| first=Sidney
| first=Sidney
Line 51: Line 45:
The apparent distance between IC 10 and the [[Andromeda Galaxy]] is about the same as the apparent distance between the Andromeda Galaxy and the [[Triangulum Galaxy]], which suggests that IC 10 may belong to the M31 subgroup.<ref name="Bergh"/>
The apparent distance between IC 10 and the [[Andromeda Galaxy]] is about the same as the apparent distance between the Andromeda Galaxy and the [[Triangulum Galaxy]], which suggests that IC 10 may belong to the M31 subgroup.<ref name="Bergh"/>


IC 10 is the only known [[starburst galaxy]] in the Local Group of galaxies. It has many more [[Wolf–Rayet star]]s per square [[parsec|kiloparsec]] (5.1 stars/kpc²) than the [[Large Magellanic Cloud]] (2.0 stars/kpc²) or the [[Small Magellanic Cloud]] (0.9 stars/kpc²). Although the galaxy has a luminosity similar to the SMC, it is considerably smaller. Its higher [[metallicity]] compared to the SMC suggests that star formation activity has continued for a longer time period. The [[Stellar evolution|evolutionary]] status of the Wolf–Rayet stars suggests that they all formed in a relatively short timespan. The ratio between the two types of [[Wolf–Rayet star]]s (WC stars and WN stars) in IC 10 is very different from the ratio in other galaxies in the Local Group, which may be somehow due to the starburst nature of the galaxy. Currently, the galaxy produces stars at the rate of 0.04–0.08 [[solar mass]]es per year, which means that the gas supply in the galaxy can last for only a few billion years longer.<ref name="Bergh"/>
IC 10 is the only known [[starburst galaxy]] in the Local Group of galaxies; it has many more [[Wolf–Rayet star]]s per square [[parsec|kiloparsec]] (5.1 stars/kpc<sup>2</sup>) than the [[Large Magellanic Cloud]] (2.0 stars/kpc<sup>2</sup>) or the [[Small Magellanic Cloud]] (0.9 stars/kpc<sup>2</sup>). Although the galaxy has a luminosity similar to the SMC, it is considerably smaller, with an estimated diameter of around 5000 [[Light-year|light years]].<ref>{{Cite web|title=APOD: 2012 January 4 – Starburst Galaxy IC 10|url=https://apod.nasa.gov/apod/ap120104.html|access-date=2021-08-08|website=apod.nasa.gov}}</ref> Its higher [[metallicity]] compared to the SMC suggests that star formation activity has continued for a longer time period. The [[H II region]]s in IC 10 have all formed recently, within the last 10 Myr.<ref name=Cosens>{{cite journal|doi=10.3847/1538-4357/ac52f3|title=Kinematics and Feedback in H II Regions in the Dwarf Starburst Galaxy IC 10|year=2022|last1=Cosens|first1=Maren|last2=Wright|first2=Shelley A.|last3=Murray|first3=Norman|last4=Armus|first4=Lee|last5=Sandstrom|first5=Karin|last6=Do|first6=Tuan|last7=Larson|first7=Kirsten|last8=Martinez|first8=Gregory|last9=Sabhlok|first9=Sanchit|last10=Vayner|first10=Andrey|last11=Wiley|first11=James|journal=The Astrophysical Journal|volume=929|issue=1|page=74|arxiv=2202.04098|bibcode=2022ApJ...929...74C|s2cid=246679827 |doi-access=free }}</ref> The [[Stellar evolution|evolutionary]] status of the Wolf–Rayet stars suggests that they all formed in a relatively short timespan. The ratio between the two types of [[Wolf–Rayet star]]s (WC stars and WN stars) in IC 10 is very different from the ratio in other galaxies in the Local Group, which may be somehow due to the starburst nature of the galaxy. Currently, the galaxy produces stars at the rate of 0.04–0.08 [[solar mass]]es per year, which means that the gas supply in the galaxy can last for only a few billion years longer.<ref name="Bergh"/>


Observations of IC 10 in the [[far-infrared]] show that the [[Cosmic dust|dust]] in this mild starburst galaxy is deficient in small grains.<ref>{{cite journal | last=Bolatto | first = A. D. |author2=Jackson, J. M. |author3=Wilson, C. D. |author4=Moriarty-Schieven, G. | title = Submillimeter Observations of IC 10: The Dust Properties and Neutral Carbon Content of a Low-Metallicity Starburst | date = 2000 | journal=Astrophysical Journal | volume = 532 | issue=2 | pages = 909–921 | bibcode = 2000ApJ...532..909B | doi = 10.1086/308590 |arxiv = astro-ph/9910564 }}</ref> It is hypothesized that any small grains that formerly existed were destroyed by strong [[ultraviolet]] radiation in the areas around the hot luminous stars that were formed in the galaxy's recent burst of star formation.<ref name="Bergh2000">{{Cite journal
Observations of IC 10 in the [[far-infrared]] show that the [[Cosmic dust|dust]] in this mild starburst galaxy is deficient in small grains.<ref>{{cite journal | last=Bolatto | first = A. D. |author2=Jackson, J. M. |author3=Wilson, C. D. |author4=Moriarty-Schieven, G. | title = Submillimeter Observations of IC 10: The Dust Properties and Neutral Carbon Content of a Low-Metallicity Starburst | date = 2000 | journal=Astrophysical Journal | volume = 532 | issue=2 | pages = 909–921 | bibcode = 2000ApJ...532..909B | doi = 10.1086/308590 |arxiv = astro-ph/9910564 | s2cid = 15330330 }}</ref> It is hypothesized that any small grains that formerly existed were destroyed by strong [[ultraviolet]] radiation in the areas around the hot luminous stars that were formed in the galaxy's recent burst of star formation.<ref name="Bergh2000">{{Cite journal
| last1 = van den Bergh
| last1 = van den Bergh
| first1 = Sidney
| first1 = Sidney
| authorlink1 = Sidney van den Bergh
| author-link1 = Sidney van den Bergh
| title = Updated Information on the Local Group
| title = Updated Information on the Local Group
| date = April 2000
| date = April 2000
Line 65: Line 59:
| pages = 529–536
| pages = 529–536
| doi = 10.1086/316548
| doi = 10.1086/316548
|arxiv = astro-ph/0001040 | s2cid = 1805423
| postscript = <!--None-->
|arxiv = astro-ph/0001040 }}</ref>
}}</ref>


The galaxy has a huge envelope of [[hydrogen]] gas, with an apparent size measuring 68′ × 80′, which is far larger than the apparent size of the galaxy in visible light (5.5′ × 7.0′). IC 10 is also unusual in the respect that the visible part of the galaxy seems to rotate in a different direction than the outer envelope.<ref name="Bergh"/> It has a [[H II|H&nbsp;II]] nucleus.<ref name="hoetal1997">{{Cite news
The galaxy has a huge envelope of [[hydrogen]] gas, with an apparent size measuring 68{{prime}} × 80{{prime}}, which is far larger than the apparent size of the galaxy in visible light (5.5{{prime}} × 7.0{{prime}}). IC 10 is also unusual in the respect that the visible part of the galaxy seems to rotate in a different direction than the outer envelope.<ref name="Bergh"/> It has an [[H II|H&nbsp;II]] nucleus.<ref name="hoetal1997">{{Cite journal
| last1 = Ho
| last1 = Ho
| first1 = Luis C.
| first1 = Luis C.
Line 80: Line 74:
| journal = Astrophysical Journal Supplement
| journal = Astrophysical Journal Supplement
| volume = 112
| volume = 112
| pages = 315
| issue = 2
| pages = 315–390
| url = http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997ApJS..112..315H
| url = http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997ApJS..112..315H
| doi = 10.1086/313041
| doi = 10.1086/313041
⚫
|arxiv = astro-ph/9704107 |bibcode = 1997ApJS..112..315H | s2cid = 17086638
| postscript = <!--None-->
⚫
}}</ref>
⚫
|arxiv = astro-ph/9704107 |bibcode = 1997ApJS..112..315H }}</ref>

==Gallery==
<gallery>
Spiral, elliptical, irregular IC 10.jpg|IC 10 taken by [[Hubble Space Telescope|Hubble]].<ref>{{cite web |title=Spiral, elliptical, irregular |url=https://www.spacetelescope.org/images/potw1924a/ |website=www.spacetelescope.org |access-date=17 June 2019 |language=en}}</ref>
</gallery>


==References==
==References==
Line 90: Line 90:


==External links==
==External links==
{{commonscat}}
* [http://messier.seds.org/xtra/ngc/i0010.html Irregular Galaxy IC 10 @ SEDS IC objects pages]
* [http://messier.seds.org/xtra/ngc/i0010.html Irregular Galaxy IC 10 @ SEDS IC objects pages]
* [https://web.archive.org/web/20120110121132/http://www.stargazer-observatory.com/IC10.html IC 10 imaged through a semi-professional amateur-telescope]
⚫
{{Sky|00|20|17.3|+|59|18|14|2200000}}



⚫
{{Sky|00|20|17.3|+|59|18|14|2200000}}
{{Catalogs|IC=10|UGC=192|PGC=1305}}
{{Catalogs|IC=10|UGC=192|PGC=1305}}
{{Cassiopeia (constellation)}}


{{DEFAULTSORT:IC 0010}}
{{DEFAULTSORT:IC 0010}}

Latest revision as of 19:59, 4 June 2024

IC 10
Irregular Galaxy IC 10
Observation data (J2000 epoch)
ConstellationCassiopeia
Right ascension00h 20m 17.3s[1]
Declination+59° 18′ 14″[1]
Redshift0.001161±0.000003[1]
Distance2.5 ± 0.5 Mly (750 ± 150 kpc)[2]
Apparent magnitude (V)10.4 ± 0.2 [3]
Characteristics
TypdIrr IV/BCD[1]
Size5000 light years (diameter)[4]
Apparent size (V)6.8′ × 5.9′[1]
Notable featuresmild starburst galaxy
Other designations
UGC 192,[1] PGC 1305[1]

IC 10 is an irregular galaxy in the constellation Cassiopeia. It was discovered by Lewis Swift in 1887[5] and in 1935 Nicholas Mayall became the first to suggest that the object is extragalactic. Edwin Hubble suspected it might belong to the Local Group of galaxies, but its status remained uncertain for decades. The radial velocity of IC 10 was measured in 1962, and it was found to be approaching the Milky Way at approximately 350 km/s, strengthening the evidence for its membership in the Local Group.[5] Its membership in the group was finally confirmed in 1996 by direct measurements of its distance based on observations of Cepheids; most estimates place the galaxy 2–3 million light years from Earth, with some estimates ranging from 1.5–4.5 million light years.[6] Despite its closeness, the galaxy is rather difficult to study because it lies near the plane of the Milky Way and is therefore heavily obscured by interstellar matter.[7]

The apparent distance between IC 10 and the Andromeda Galaxy is about the same as the apparent distance between the Andromeda Galaxy and the Triangulum Galaxy, which suggests that IC 10 may belong to the M31 subgroup.[7]

IC 10 is the only known starburst galaxy in the Local Group of galaxies; it has many more Wolf–Rayet stars per square kiloparsec (5.1 stars/kpc2) than the Large Magellanic Cloud (2.0 stars/kpc2) or the Small Magellanic Cloud (0.9 stars/kpc2). Although the galaxy has a luminosity similar to the SMC, it is considerably smaller, with an estimated diameter of around 5000 light years.[8] Its higher metallicity compared to the SMC suggests that star formation activity has continued for a longer time period. The H II regions in IC 10 have all formed recently, within the last 10 Myr.[9] The evolutionary status of the Wolf–Rayet stars suggests that they all formed in a relatively short timespan. The ratio between the two types of Wolf–Rayet stars (WC stars and WN stars) in IC 10 is very different from the ratio in other galaxies in the Local Group, which may be somehow due to the starburst nature of the galaxy. Currently, the galaxy produces stars at the rate of 0.04–0.08 solar masses per year, which means that the gas supply in the galaxy can last for only a few billion years longer.[7]

Observations of IC 10 in the far-infrared show that the dust in this mild starburst galaxy is deficient in small grains.[10] It is hypothesized that any small grains that formerly existed were destroyed by strong ultraviolet radiation in the areas around the hot luminous stars that were formed in the galaxy's recent burst of star formation.[11]

The galaxy has a huge envelope of hydrogen gas, with an apparent size measuring 68′ × 80′, which is far larger than the apparent size of the galaxy in visible light (5.5′ × 7.0′). IC 10 is also unusual in the respect that the visible part of the galaxy seems to rotate in a different direction than the outer envelope.[7] It has an H II nucleus.[12]

[edit]

References

[edit]
  1. ^ a b c d e f g "NASA/IPAC Extragalactic Database". Results for IC 10. Retrieved 15 March 2007.
  2. ^ "NED Query Results for IC 0010". ned.ipac.caltech.edu. Retrieved 8 August 2021.
  3. ^ "IC 10". Star-Watcher.
  4. ^ "APOD: 2012 January 4 – Starburst Galaxy IC 10". apod.nasa.gov. Retrieved 8 August 2021.
  5. ^ a b "IC 10". SEDS Messier Database. Retrieved 15 May 2006.
  6. ^ "NED Query Results for IC 0010". ned.ipac.caltech.edu. Retrieved 8 August 2021.
  7. ^ a b c d Van den Bergh, Sidney (2000). Galaxies of the Local Group (1st ed.). Cambridge University Press. ISBN 0-521-65181-6.
  8. ^ "APOD: 2012 January 4 – Starburst Galaxy IC 10". apod.nasa.gov. Retrieved 8 August 2021.
  9. ^ Cosens, Maren; Wright, Shelley A.; Murray, Norman; Armus, Lee; Sandstrom, Karin; Do, Tuan; Larson, Kirsten; Martinez, Gregory; Sabhlok, Sanchit; Vayner, Andrey; Wiley, James (2022). "Kinematics and Feedback in H II Regions in the Dwarf Starburst Galaxy IC 10". The Astrophysical Journal. 929 (1): 74. arXiv:2202.04098. Bibcode:2022ApJ...929...74C. doi:10.3847/1538-4357/ac52f3. S2CID 246679827.
  10. ^ Bolatto, A. D.; Jackson, J. M.; Wilson, C. D.; Moriarty-Schieven, G. (2000). "Submillimeter Observations of IC 10: The Dust Properties and Neutral Carbon Content of a Low-Metallicity Starburst". Astrophysical Journal. 532 (2): 909–921. arXiv:astro-ph/9910564. Bibcode:2000ApJ...532..909B. doi:10.1086/308590. S2CID 15330330.
  11. ^ van den Bergh, Sidney (April 2000). "Updated Information on the Local Group". The Publications of the Astronomical Society of the Pacific. 112 (770): 529–536. arXiv:astro-ph/0001040. Bibcode:2000PASP..112..529V. doi:10.1086/316548. S2CID 1805423.
  12. ^ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search for 'Dwarf' Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". Astrophysical Journal Supplement. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.
  13. ^ "Spiral, elliptical, irregular". www.spacetelescope.org. Retrieved 17 June 2019.
[edit]
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