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Coordinates: Sky map 06h 09.1m 00s, 24° 21′ 00″
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{{short description|Open cluster in the constellation Gemini}}
{{Use dmy dates|date=April 2012}}
{{Use dmy dates|date=March 2021}}
{{Infobox open cluster
{{Infobox open cluster
| image = M35atlas.jpg
| image = [[image:M35atlas.jpg|280px]]
| caption = Credit: [[2MASS]]/[[NASA]].
| caption = Messier 35 with [[NGC 2158]] at lower right
| credit = [[2MASS]]/[[NASA]].
| name = [[Messier object|Messier]] 35
| name = [[Messier object|Messier]] 35
| class = (III2m)Open Cluster
| class = (III2m)Open Cluster
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| ra = {{RA|06|08|54.0}}<ref name=Wu2009a/>
| ra = {{RA|06|08|54.0}}<ref name=Wu2009a/>
| dec = {{DEC|+24|20|00}}<ref name=Wu2009a/>
| dec = {{DEC|+24|20|00}}<ref name=Wu2009a/>
| dist_ly = {{Convert|1186|pc|ly|lk=on|order=flip|abbr=on}}<ref name=Wu2009a/>
| dist_ly = {{Convert|912|pc|ly|lk=on|order=flip|abbr=on}}<ref name=Wu2009a/>
| appmag_v = 5.3<ref>{{cite web |url=http://www.messier.seds.org/m/m035.html |title=Messier 35 |access-date=23 July 2024 |website=SEDS Messier Catalog}}</ref>
| appmag_v = 5.1<ref name=Thompson2007/>
| size_v = 28<ref name=Thompson2007/> [[Minute of arc|arcmins]]
| size_v = 28<ref name=Thompson2007/> [[Minute of arc|arcmins]]
| mass_msol = 1,600<ref name=Bouy2015/>
| mass_msol = 1,600<ref name=Bouy2015/>
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| radius_ly = 11 ly<ref name=Stoyan/>
| radius_ly = 11 ly<ref name=Stoyan/>
| constellation = [[Gemini (constellation)|Gemini]]
| constellation = [[Gemini (constellation)|Gemini]]
| names = C 0605+243, M35, [[New General Catalogue|NGC]] 2168<ref name=SIMBAD/>
| names = M35, [[New General Catalogue|NGC]] 2168,<ref name=SIMBAD/> [[Collinder catalogue|Cr]] 82, C 0605+243
}}
}}


'''Messier 35''' or '''M35''', also known as '''NGC 2168''', is an [[open cluster]] of [[star]]s in the northern [[constellation]] of [[Gemini (constellation)|Gemini]]. It was discovered by [[Philippe Loys de Chéseaux]] around 1745 and independently discovered by [[John Bevis]] before 1750.<ref name=Thompson2007/> The cluster is scattered over an area of the sky almost the size of the [[Full Moon|full moon]] and is located {{Convert|1186|pc|ly|lk=on|order=flip|abbr=off}} from Earth.<ref name=Wu2009a/> The compact open cluster [[NGC 2158]] lies directly southwest of M35.
'''Messier 35''' or '''M35''', also known as '''NGC 2168''' or the '''Shoe-Buckle Cluster''', is a relatively close [[open cluster]] of [[star]]s in the west of [[Gemini (constellation)|Gemini]], at about the declination of the Sun when the latter is at [[June solstice]].{{efn|Hence M35 cannot be seen from the [[Antarctic Circle]]}} It was discovered by [[Philippe Loys de Chéseaux]] around 1745 and independently discovered by [[John Bevis]] before 1750.<ref name=Thompson2007/> It is scattered over part of the sky almost the size of the [[Full Moon|full moon]] and is {{Convert|912|pc|ly|lk=on|order=flip|abbr=off}} away.<ref name=Wu2009a/> The compact open cluster [[NGC 2158]] lies directly southwest of it.


Leonard & Merritt (1989) computed the mass of M35 using a [[Leonard-Merritt mass estimator|statistical technique]] based on [[proper motion]] velocities of its stars. The mass within the central 3.75 [[parsec]]s was found to be between 1600 and 3200 solar masses (95 percent confidence), consistent with the mass of a realistic stellar population within the same radius.<ref name=Leonard1989/> Bouy et al. (2015) found a mass of around {{Val|1600|fmt=commas|ul=solar mass}} within the central {{nowrap|27.5′ × 27.5′}}. There are 305 candidate members with a probability of 95% or higher, and up to 4,349 with a 50% membership probability. The cluster [[metallicity]] is given by [Fe/H] = {{Val|−0.21|0.10}}.<ref name=Bouy2015/>
Leonard & Merritt (1989) computed the mass of M35 using a [[Leonard-Merritt mass estimator|statistical technique]] based on [[proper motion]] velocities of its stars. The mass within the central {{convert|3.75|pc}} was found to be between 1600 and 3200 solar masses,{{efn|with 95 percent confidence}} consistent with the mass of a realistic stellar population within the same radius.<ref name=Leonard1989/> Bouy [[et al.]] in 2015 found a mass of around {{Val|1600|fmt=commas|ul=solar mass}} within the central {{nowrap|27.5' × 27.5[[arcminute|′]]}}. There are 305 stars that can be intrinsically shown to be extremely likely to be members,{{efn|have values that give a confidence of 95% or higher}} and up to 4,349 averaging the 50% membership probability, from the kinematic (such as [[parallax]] and [[proper motion]]) and spectral data published before 2015.<ref name=Bouy2015/> The cluster's [[metallicity]] is [Fe/H] = {{Val|−0.21|0.10}}, where &minus;1 would be ten times less metallic than the sun.<ref name=Bouy2015/>


Of 418 probable cluster members, Leiner et al. (2015) found 64 that have variable [[radial velocity|radial velocities]] and thus are [[binary star]] systems.<ref name=Leiner2015/> Four probable cluster members are [[chemically peculiar star]]s, while [[Henry Draper Catalogue|HD]]&nbsp;41995, which lies within the cluster area, shows [[emission line]]s.<ref name=Paunzen2014/> Hu et al. (2005) found 13 [[variable star]]s in the cluster field, although at least three are suspect as cluster members.<ref name=Hu2005/>
Of 418 probable members, Leiner [[et al.]] in 2015 found 64 that have variable [[radial velocity|radial velocities]] thus are [[binary star]] systems.<ref name=Leiner2015/> Four probable members are [[chemically peculiar star|chemically peculiar]]s, while [[Henry Draper Catalogue|HD]]&nbsp;41995, which in the (telescopic angular) cluster field, shows [[emission line]]s.<ref name=Paunzen2014/> Hu [[et al.]] in 2005 found 13 [[variable star]]s in the field; at least three are suspect as cluster members. To be a member means to have a gravitational tie or, if recently freed, having been created by the same event.<ref name=Hu2005/>


==References==
==See also==
* [[List of Messier objects]]

==References and footnotes==
{{reflist|refs=
{{reflist|refs=


<ref name=SIMBAD>{{cite simbad | title=M 35 | access-date=November 16, 2018 }}</ref>
<ref name=SIMBAD>{{cite simbad | title=M 35 | access-date=16 November 2018 }}</ref>


<ref name=Wu2009a>{{Cite journal | display-authors=1
<ref name=Wu2009a>{{Cite journal | display-authors=1
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| volume=399 | issue=4 | pages=2146–2164 | date=November 2009
| volume=399 | issue=4 | pages=2146–2164 | date=November 2009
| arxiv=0909.3737 | bibcode=2009MNRAS.399.2146W
| arxiv=0909.3737 | bibcode=2009MNRAS.399.2146W
| doi=10.1111/j.1365-2966.2009.15416.x }}</ref>
| doi=10.1111/j.1365-2966.2009.15416.x | doi-access=free | s2cid=6066790 }}</ref>


<ref name=Leonard1989>{{Cite journal
<ref name=Leonard1989>{{Cite journal
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| volume=575 | id=A120 | pages=6 | date=March 2015
| volume=575 | id=A120 | pages=6 | date=March 2015
| bibcode=2015A&A...575A.120B | arxiv=1501.04416
| bibcode=2015A&A...575A.120B | arxiv=1501.04416
| doi=10.1051/0004-6361/201425505 }}</ref>
| doi=10.1051/0004-6361/201425505 | s2cid=73519314 }}</ref>


<ref name=Leiner2015>{{cite journal
<ref name=Leiner2015>{{cite journal
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| journal=The Astronomical Journal
| journal=The Astronomical Journal
| volume=150 | issue=1 | id=10 | pages=18 | date=July 2015
| volume=150 | issue=1 | id=10 | pages=18 | date=July 2015
| doi=10.1088/0004-6256/150/1/10 | bibcode=2015AJ....150...10L }}</ref>
| doi=10.1088/0004-6256/150/1/10 | bibcode=2015AJ....150...10L | s2cid=123818978 }}</ref>


<ref name=Paunzen2014>{{citation
<ref name=Paunzen2014>{{citation
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| volume=564 | id=A42 | pages=8 | date=April 2014
| volume=564 | id=A42 | pages=8 | date=April 2014
| bibcode=2014A&A...564A..42P | arxiv=1403.3538
| bibcode=2014A&A...564A..42P | arxiv=1403.3538
| doi=10.1051/0004-6361/201423521 }}</ref>
| doi=10.1051/0004-6361/201423521 | s2cid=119174151 }}</ref>


<ref name=Hu2005>{{cite journal
<ref name=Hu2005>{{cite journal
Line 100: Line 105:


}}
}}
{{notelist}}


==External links==
==External links==
{{commons category}}
{{commonscat}}
* [http://www.messier.seds.org/m/m035.html Messier 35, SEDS Messier pages]
* [http://www.nightskyinfo.com/archive/m35/ M35 – Nightskyinfo.com]
* [http://www.nightskyinfo.com/archive/m35/ M35 – Nightskyinfo.com]
* {{cite web|title=M35 – Open Cluster|url=http://www.deepskyvideos.com/videos/messier/M35_open_cluster.html|work=Deep Sky Videos|publisher=[[Brady Haran]]|author=Merrifield, Michael|author2=Rothery, Roy}}
* {{cite web|title=M35 – Open Cluster|url=http://www.deepskyvideos.com/videos/messier/M35_open_cluster.html|work=Deep Sky Videos|publisher=[[Brady Haran]]|author=Merrifield, Michael|author2=Rothery, Roy}}
* {{APOD |date=19 April 2006|title=Mars and the Star Clusters}} - featured M35
* {{APOD |date=19 April 2006|title=Mars and the Star Clusters}} - featured M35
* {{WikiSky|NGC 2168}}
* {{WikiSky|NGC 2168}}



{{Sky|06|09.1|00||24|21|00|2800}}
{{Sky|06|09.1|00||24|21|00|2800}}
{{Portal bar|Astronomy|Stars|Outer space}}
{{Messier objects}}
{{Messier objects}}
{{Ngc25}}
{{Ngc25}}
{{Gemini (constellation)}}
{{Gemini (constellation)}}


{{DEFAULTSORT:Messier 35}}
[[Category:Open clusters|Messier 035]]
[[Category:Open clusters|Messier 035]]
[[Category:Gemini (constellation)|Messier 035]]
[[Category:Gemini (constellation)|Messier 035]]

Latest revision as of 06:57, 23 August 2024

Messier 35
Messier 35 with NGC 2158 at lower right
Credit: 2MASS/NASA.
Observation data (J2000 epoch)
Right ascension06h 08m 54.0s[1]
Declination+24° 20′ 00″[1]
Distance2,970 ly (912 pc)[1]
Apparent magnitude (V)5.3[2]
Apparent dimensions (V)28[3] arcmins
Physical characteristics
Mass1,600[4] M☉
Radius11 ly[5]
Estimated age175 Myr[4]
Other designationsM35, NGC 2168,[6] Cr 82, C 0605+243
Associations
ConstellationGemini
See also: Open cluster, List of open clusters

Messier 35 or M35, also known as NGC 2168 or the Shoe-Buckle Cluster, is a relatively close open cluster of stars in the west of Gemini, at about the declination of the Sun when the latter is at June solstice.[a] It was discovered by Philippe Loys de Chéseaux around 1745 and independently discovered by John Bevis before 1750.[3] It is scattered over part of the sky almost the size of the full moon and is 2,970 light-years (912 parsecs) away.[1] The compact open cluster NGC 2158 lies directly southwest of it.

Leonard & Merritt (1989) computed the mass of M35 using a statistical technique based on proper motion velocities of its stars. The mass within the central 3.75 parsecs (12.2 ly) was found to be between 1600 and 3200 solar masses,[b] consistent with the mass of a realistic stellar population within the same radius.[7] Bouy et al. in 2015 found a mass of around 1,600 M☉ within the central 27.5' × 27.5′. There are 305 stars that can be intrinsically shown to be extremely likely to be members,[c] and up to 4,349 averaging the 50% membership probability, from the kinematic (such as parallax and proper motion) and spectral data published before 2015.[4] The cluster's metallicity is [Fe/H] = −0.21±0.10, where −1 would be ten times less metallic than the sun.[4]

Of 418 probable members, Leiner et al. in 2015 found 64 that have variable radial velocities thus are binary star systems.[8] Four probable members are chemically peculiars, while HD 41995, which in the (telescopic angular) cluster field, shows emission lines.[9] Hu et al. in 2005 found 13 variable stars in the field; at least three are suspect as cluster members. To be a member means to have a gravitational tie or, if recently freed, having been created by the same event.[10]

See also

[edit]

References and footnotes

[edit]
  1. ^ a b c d Wu, Zhen-Yu; et al. (November 2009). "The orbits of open clusters in the Galaxy". Monthly Notices of the Royal Astronomical Society. 399 (4): 2146–2164. arXiv:0909.3737. Bibcode:2009MNRAS.399.2146W. doi:10.1111/j.1365-2966.2009.15416.x. S2CID 6066790.
  2. ^ "Messier 35". SEDS Messier Catalog. Retrieved 23 July 2024.
  3. ^ a b Thompson, Robert; Thompson, Barbara (2007). Illustrated Guide to Astronomical Wonders: From Novice to Master Observer. DIY science. O'Reilly Media, Inc. p. 252. ISBN 978-0596526856.
  4. ^ a b c d Bouy, H.; et al. (March 2015). "Messier 35 (NGC 2168) DANCe. I. Membership, proper motions, and multiwavelength photometry". Astronomy & Astrophysics. 575: 6. arXiv:1501.04416. Bibcode:2015A&A...575A.120B. doi:10.1051/0004-6361/201425505. S2CID 73519314. A120.
  5. ^ Stoyan, Ronald; et al. (2008). Atlas of the Messier Objects: Highlights of the Deep Sky. Cambridge University Press. p. 160. ISBN 9780521895545.
  6. ^ "M 35". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 16 November 2018.
  7. ^ Leonard, P. J. T.; Merritt, D. (1989). "The mass of the open star cluster M35 as derived from proper motions". Astrophysical Journal. 339 (1): 195–208. Bibcode:1989ApJ...339..195L. doi:10.1086/167287.
  8. ^ Leiner, E. M.; Mathieu, R. D.; Gosnell, N. M.; Geller, A. M. (July 2015). "WIYN Open Cluster Study. LXVI. Spectroscopic Binary Orbits in the Young Open Cluster M35 (NGC 2168)". The Astronomical Journal. 150 (1): 18. Bibcode:2015AJ....150...10L. doi:10.1088/0004-6256/150/1/10. S2CID 123818978. 10.
  9. ^ Paunzen, E.; et al. (April 2014), "Photoelectric search for peculiar stars in open clusters. XV. Feinstein 1, NGC 2168, NGC 2323, NGC 2437, NGC 2547, NGC 4103, NGC 6025, NGC 6633, Stock 2, and Trumpler 2", Astronomy & Astrophysics, 564: 8, arXiv:1403.3538, Bibcode:2014A&A...564A..42P, doi:10.1051/0004-6361/201423521, S2CID 119174151, A42
  10. ^ Hu, Juei-Hwa; et al. (August 2005). "Discovery of 13 New Variable Stars in the Field of the Open Cluster NGC 2168 (M35)". Chinese Journal of Astronomy and Astrophysics. 5 (4): 356–362. Bibcode:2005ChJAA...5..356H. doi:10.1088/1009-9271/5/4/003.
  1. ^ Hence M35 cannot be seen from the Antarctic Circle
  2. ^ with 95 percent confidence
  3. ^ have values that give a confidence of 95% or higher
[edit]
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