NGC 2366

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NGC 2366

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{{Short description|Galaxy in the constellation Camelopardalis}}
{{Short description|Galaxy in the constellation Camelopardalis}}
{{Infobox Galaxy
{{Infobox Galaxy

|name = [[New General Catalogue|NGC]] 2366
|name = [[New General Catalogue|NGC]] 2366

|image = NGC 2366 2363 GALEX WikiSky.jpg
|image = NGC 2366 2363 GALEX WikiSky.jpg
|image_size = 300px
|image_size = 300px

|caption = [[GALEX]] image of NGC 2366
|caption = [[GALEX]] image of NGC 2366

|epoch = [[J2000]]
|epoch = [[J2000]]

|type = IB(s)m {{cite web| title=NASA/IPAC Extragalactic Database| work=Results for NGC 2366
|type = IB(s)m {{cite web| title=NASA/IPAC Extragalactic Database| work=Results for NGC 2366
| url=http://nedwww.ipac.caltech.edu/| access-date=2007-04-08}}
| url=http://nedwww.ipac.caltech.edu/| access-date=2007-04-08}}

|ra = {{RA|7|28|54.6}}
|ra = {{RA|7|28|54.6}}

|dec = {{DEC|+69|12|57}}
|dec = {{DEC|+69|12|57}}

|dist_ly = 10 million [[light-year]]s{{cite news| title=Hubble Observes a Dwarf Galaxy with a Bright Nebula| url=http://www.spacetelescope.org/news/heic1207/| access-date=10 May 2012| newspaper=ESA/Hubble Press Release}}
|dist_ly = 10 million [[light-year]]s{{cite news| title=Hubble Observes a Dwarf Galaxy with a Bright Nebula| url=http://www.spacetelescope.org/news/heic1207/| access-date=10 May 2012| newspaper=ESA/Hubble Press Release}}

| z = 80 ± 1 km/[[second|s]]
| z = 80 ± 1 km/[[second|s]]

| appmag_v = 11.4
| appmag_v = 11.4

| size_v = 8.1{{prime}} × 3.3{{prime}}
| size_v = 8.1{{prime}} × 3.3{{prime}}

| constellation name = [[Camelopardalis]]
| constellation name = [[Camelopardalis]]

| notes = The southern part of NGC 2366 is called Markarian 71.
| notes = The southern part of NGC 2366 is called Markarian 71.
| names = [[Uppsala General Catalogue|UGC]] 3851, [[Principal Galaxies Catalogue|PGC]] 21102 }}
| names = [[Uppsala General Catalogue|UGC]] 3851, [[Principal Galaxies Catalogue|PGC]] 21102
}}
'''NGC 2366''' is a [[Magellanic Catalogue of Stars|Magellanic]] [[barred irregular galaxy|barred irregular]] [[dwarf galaxy]] located in the [[constellation]] [[Camelopardalis]].{{cite journal| author1=G. Micheva| author2=M.S. Oey| author3=A.E. Jaskot| author4=B.L. James| title=Mrk 71/NGC 2366: The Nearest Green Pea Analog| journal=The Astrophysical Journal| volume=845| issue=2| pages=13| date=August 2017| arxiv=1704.01678| bibcode=2017ApJ...845..165M| doi=10.3847/1538-4357/aa830b| s2cid=119049347| doi-access=free}}{{cite book| author1=G. de Vaucouleurs| author2=A. de Vaucouleurs| author3=H.G. Corwin| author4=R.J. Buta| author5=G. Paturel| author6=P. Fouque| title=Third Reference Catalogue of Bright Galaxies. Volume I: Explanations and references. Volume II: Data for galaxies between 0h and 12h. Volume III: Data for galaxies between 12h and 24h| publisher=Springer, New York| date=1991| pages=2091| isbn=978-0-387-97552-8| bibcode=1991rc3..book.....D}}
'''NGC 2366''' is a [[Magellanic Catalogue of Stars|Magellanic]] [[barred irregular galaxy|barred irregular]] [[dwarf galaxy]] located in the [[constellation]] [[Camelopardalis]].{{cite journal| author1=G. Micheva| author2=M.S. Oey| author3=A.E. Jaskot| author4=B.L. James| title=Mrk 71/NGC 2366: The Nearest Green Pea Analog| journal=The Astrophysical Journal| volume=845| issue=2| pages=13| date=August 2017| arxiv=1704.01678| bibcode=2017ApJ...845..165M| doi=10.3847/1538-4357/aa830b| s2cid=119049347| doi-access=free}}{{cite book| author1=G. de Vaucouleurs| author2=A. de Vaucouleurs| author3=H.G. Corwin| author4=R.J. Buta| author5=G. Paturel| author6=P. Fouque| title=Third Reference Catalogue of Bright Galaxies. Volume I: Explanations and references. Volume II: Data for galaxies between 0h and 12h. Volume III: Data for galaxies between 12h and 24h| publisher=Springer, New York| date=1991| pages=2091| isbn=978-0-387-97552-8| bibcode=1991rc3..book.....D}}


⚫
At the southern end of NGC 2366 is the large, luminous HII region known as [[Markarian galaxies|Markarian 71]] (Mrk 71). To the west of Mrk 71 is another dwarf galaxy NGC 2363 which is interacting with NGC 2366.{{cite web| author=H.G. Corwin| title=Historical Notes: NGC 2000 through NGC 2999| url=http://www.ngcicproject.org/corwin/DataFiles/Aug_2006/ngcnotes_2.txt| date=2006| access-date=29 October 2017| archive-date=4 March 2016| archive-url=https://web.archive.org/web/20160304115034/http://www.ngcicproject.org/corwin/DataFiles/Aug_2006/ngcnotes_2.txt| url-status=dead}}> There has been confusion about the various components of NGC 2366 and its neighbouring galaxy NGC 2363.> Corwins' notes remark that there are two galaxies with two NGC numbers clearly attached to each one: ''We shall just have to get used to calling the HII region "Markarian 71" (or one of its other names) since it is not N2363 as we've thought all these years.''
There has been confusion about the various components of NGC 2366 and its neighbouring galaxy NGC 2363. At the southern end of NGC 2366 is the large, luminous HII region known as [[Markarian galaxies|Markarian 71]] (Mrk 71).


⚫
Within Mrk 71, there are two [[super star clusters]] (SSC) which are named 'A' and 'B' or 'Knot A' and 'Knot B'.{{cite journal| author1=R.M. Gonzalez-Delgado| author2=E. Perez| author3=G. Tenorio-Tagle| display-authors=etal| title=Violent star formation in NGC 2363| journal=The Astrophysical Journal| date=1994| volume=437| pages=239–261| bibcode=1994ApJ...437..239G| doi=10.1086/174992| hdl=10486/13452| url=https://repositorio.uam.es/bitstream/10486/13452/1/63308_63308.pdf| hdl-access=free}}
⚫
To the west of Mrk 71 is another dwarf galaxy NGC 2363 which is interacting with NGC 2366.{{cite web| author=H.G. Corwin| title=Historical Notes: NGC 2000 through NGC 2999| url=http://www.ngcicproject.org/corwin/DataFiles/Aug_2006/ngcnotes_2.txt| date=2006| access-date=29 October 2017| archive-date=4 March 2016| archive-url=https://web.archive.org/web/20160304115034/http://www.ngcicproject.org/corwin/DataFiles/Aug_2006/ngcnotes_2.txt| url-status=dead}} Corwins' notes remarks that there are two galaxies with two NGC numbers clearly attached to each one. "We shall just have to get used to calling the HII region "Markarian 71" (or one of its other names) since it is not N2363 as we've thought all these years."

⚫
Within the region known as Mrk 71, there are two [[super star clusters]] (SSC) which are named 'A' and 'B' or 'Knot A' and 'Knot B'.{{cite journal| author1=R.M. Gonzalez-Delgado| author2=E. Perez| author3=G. Tenorio-Tagle| display-authors=etal| title=Violent star formation in NGC 2363| journal=The Astrophysical Journal| date=1994| volume=437| pages=239–261| bibcode=1994ApJ...437..239G| doi=10.1086/174992| hdl=10486/13452| url=https://repositorio.uam.es/bitstream/10486/13452/1/63308_63308.pdf| hdl-access=free}}
Other names for the above components include: NGC 2366-I, NGC 2366-II, NGC 2366-III, NGC2366-A, NGC 2366-B, NGC 2366-C, NGC 2363-A, NGC 2363-B.
Other names for the above components include: NGC 2366-I, NGC 2366-II, NGC 2366-III, NGC2366-A, NGC 2366-B, NGC 2366-C, NGC 2363-A, NGC 2363-B. NGC 2366 is an outlying member of the [[M81 Group]].{{Cite journal

NGC 2366 is an outlying member of the [[M81 Group]].{{Cite journal
|last1=Karachentsev|first1=I.D.
|last1=Karachentsev|first1=I.D.
|last2=Sharina|first2=M.E.
|last2=Sharina|first2=M.E.
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Within Mrk 71 there are two super star clusters which will be referred to as Mrk 71 knot A (Knot A) and Mrk 71 knot B (Knot B).
Within Mrk 71 there are two super star clusters which will be referred to as Mrk 71 knot A (Knot A) and Mrk 71 knot B (Knot B).


⚫
'''Knot A''' has total stellar mass of approximately {{val|1.3–1.4|e=5}} [[solar mass]]es. The absence of [[Wolf-Rayet stars]] in its spectra might well indicate that its age is no more than 3 Myrs, while an age of less than 1 Myr is given in a study by Drissen et al. 2000.{{cite journal| author1=L. Drissen| author2=J.-R. Roy| author3=C. Robert| author4=D. Devost| author5=R. Doyon| title=The Star Formation History of the Starburst Region NGC 2363 and its Surroundings| journal=The Astronomical Journal| date=2000| volume=119| issue=22| pages=688–704| arxiv=astro-ph/9910476| bibcode=2000AJ....119..688D| doi=10.1086/301204| s2cid=119372867}}> Knot A hosts a massive, enshrouded SSC, in which no stellar features have been confirmed and that is still in its natal cloud. Knot A might well contain 'very massive stars' (VMS), which are O-type supergiants of 150–300 solar masses. These have short lifespans of 1–3 Myr and have been suggested as a reason why there are extreme stellar temperatures.>
'''Knot A''' has total stellar mass of approximately 1.3–1.4 x 10^5 [[solar mass]]es.

⚫
The absence of [[Wolf-Rayet stars]] in its spectra might well indicate that its age is no more than 3 Myrs, while an age of less than 1 Myr is given in a study by Drissen et al. 2000.{{cite journal| author1=L. Drissen| author2=J.-R. Roy| author3=C. Robert| author4=D. Devost| author5=R. Doyon| title=The Star Formation History of the Starburst Region NGC 2363 and its Surroundings| journal=The Astronomical Journal| date=2000| volume=119| issue=22| pages=688–704| arxiv=astro-ph/9910476| bibcode=2000AJ....119..688D| doi=10.1086/301204| s2cid=119372867}}

Knot A hosts a massive, enshrouded SSC in which no stellar features have been confirmed and that is still in its natal cloud.

⚫
The hydrogen alpha luminosity measurement for Mrk 71, of which 90% is produced by Knot A, is given as 8.4 x 10^39 ergs/s in a study by James et al. 2016.{{cite journal| author1=B.L. James| author2=M. Auger| author3=A. Valois| author4=D. Calzetti|author4-link= Daniela Calzetti | author5=L. Kewley| title=Resolving Ionization and Metallicity on Parsec Scales across Mrk 71 with HST-WFC3| journal=The Astrophysical Journal| date=January 2016| volume=816| issue=1| pages=40| arxiv=1510.02447| bibcode=2016ApJ...816...40J| doi=10.3847/0004-637X/816/1/40| s2cid=118671054| doi-access=free}}

Knot A might well contain 'very massive stars' (VMS), which are O-type supergiants of 150–300 solar masses. These have short lifespans of 1–3 Myr and have been suggested as a reason why there are extreme stellar temperatures.

'''Knot B''' has a lower mass of 1.5 x 10^4 solar masses and an estimated age of 3–5 Myrs.


⚫
The hydrogen alpha luminosity measurement for Mrk 71, of which 90% is produced by Knot A, is given as {{val|8.4|e=39|u=ergs/s}} in a study by James et al. 2016.{{cite journal| author1=B.L. James| author2=M. Auger| author3=A. Valois| author4=D. Calzetti|author4-link= Daniela Calzetti | author5=L. Kewley| title=Resolving Ionization and Metallicity on Parsec Scales across Mrk 71 with HST-WFC3| journal=The Astrophysical Journal| date=January 2016| volume=816| issue=1| pages=40| arxiv=1510.02447| bibcode=2016ApJ...816...40J| doi=10.3847/0004-637X/816/1/40| s2cid=118671054| doi-access=free}}
UV spectral synthesis leads to the conclusion that there are approximately 800 B and 40 O stars present.


Studies indicate that there might be up to 8 Wolf–Rayet stars present, which would set the age between 3–5 Myrs.{{cite journal| author1=K.R. Sokal| author2=K.E. Johnson| author3=R. Indebetouw| author4=P. Massey|
'''Knot B''' has a lower mass of {{val|1.5|e=4}} solar masses and an estimated age of 3–5 Myrs. UV spectral synthesis leads to the conclusion that there are approximately 800 B and 40 O stars present. Studies indicate that there might be up to 8 Wolf–Rayet stars present, which would set the age between 3–5 Myrs.{{cite journal| author1=K.R. Sokal| author2=K.E. Johnson| author3=R. Indebetouw| author4=P. Massey|
title=The Prevalence and Impact of Wolf–Rayet Stars in Emerging Massive Star Clusters| journal=The Astrophysical Journal|
title=The Prevalence and Impact of Wolf–Rayet Stars in Emerging Massive Star Clusters| journal=The Astrophysical Journal|date=August 2016| volume=826| issue=2| pages=194| arxiv=1605.08044| bibcode=2016ApJ...826..194S| doi=10.3847/0004-637X/826/2/194| s2cid=118517910| doi-access=free}}
date=August 2016| volume=826| issue=2| pages=194| arxiv=1605.08044| bibcode=2016ApJ...826..194S| doi=10.3847/0004-637X/826/2/194| s2cid=118517910| doi-access=free}}


A [[superbubble]] appears to have been generated with strong shell morphology to the east and a blow-out region to the north, with expansion velocities of approximately 20 km/s. This is consistent with the substantial mechanical feedback generated by a massive, somewhat evolved SSC.
A [[superbubble]] appears to have been generated with strong shell morphology to the east and a blow-out region to the north, with expansion velocities of approximately 20 km/s. This is consistent with the substantial mechanical feedback generated by a massive, somewhat evolved SSC.
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