{{Short description|Open cluster in the constellation Centaurus}} {{Infobox cluster | name = NGC 5460 | image = File:NGC 5460.png | caption = | credit = | epoch = [[Epoch (astronomy)#Julian years and J2000|J2000]] | constellation = [[Centaurus (constellation)|Centaurus]] | ra = {{RA|14|07|27}}<ref name="simbad">{{cite simbad| title=NGC 5460| access-date=2015-06-19}}</ref> | dec = {{DEC|-48|20|36}}<ref name="simbad"/> | dist_ly = 2,350 [[light year|ly]] | dist_pc = 720 [[parsec|pc]]<ref name="Fossati">{{cite journal|last1=Fossati|first1=L.|last2=Folsom|first2=C. P.|last3=Bagnulo|first3=S.|last4=Grunhut|first4=J. H.|last5=Kochukhov|first5=O.|last6=Landstreet|first6=J. D.|last7=Paladini|first7=C.|last8=Wade|first8=G. A.|title=A detailed spectroscopic analysis of the open cluster NGC 5460|journal=Monthly Notices of the Royal Astronomical Society|date=11 May 2011|volume=413|issue=2|pages=1132–1144|doi=10.1111/j.1365-2966.2011.18199.x|doi-access=free |arxiv = 1012.3050 |bibcode = 2011MNRAS.413.1132F |s2cid=118481509}}</ref> | appmag_v = 5.6 <ref name="simbad"/> | size_v =23'<ref name="Kharchenko2013">{{cite journal|last1=Kharchenko|first1=N. V.|last2=Piskunov|first2=A. E.|last3=Schilbach|first3=E.|last4=Röser|first4=S.|last5=Scholz|first5=R.-D.|title=Global survey of star clusters in the Milky Way|journal=Astronomy & Astrophysics|date=3 October 2013|volume=558|pages=A53|doi=10.1051/0004-6361/201322302|url=ftp://cdsarc.u-strasbg.fr/pub/cats/J/A%2BA/558/A53/catalog.dat|arxiv = 1308.5822 |bibcode = 2013A&A...558A..53K |archive-url=https://web.archive.org/web/20200312135436/ftp://cdsarc.u-strasbg.fr/pub/cats/J/A+A/558/A53/catalog.dat|archive-date=2020-03-12|url-status=dead|s2cid=118548517}}</ref> | mass_msol = 505<ref name=Piskunov2008>{{cite journal|last1=Piskunov|first1=A. E.|last2=Schilbach|first2=E.|last3=Kharchenko|first3=N. V.|last4=Röser|first4=S.|last5=Scholz|first5=R.-D.|title=Tidal radii and masses of open clusters|journal=Astronomy & Astrophysics|date=6 November 2007|volume=477|issue=1|pages=165–172|doi=10.1051/0004-6361:20078525|url=ftp://cdsarc.u-strasbg.fr/pub/cats/J/A%2BA/477/165/table.dat|bibcode = 2008A&A...477..165P |archive-url=https://web.archive.org/web/20200310213712/ftp://cdsarc.u-strasbg.fr/pub/cats/J/A+A/477/165/table.dat|archive-date=2020-03-10|url-status=dead|doi-access=free}}</ref> | age = 160 million years<ref name="Fossati"/> | notes = | names = Collinder 280, Melotte 123 }} '''NGC 5460''' is an [[open cluster]] in the constellation [[Centaurus (constellation)|Centaurus]]. It is a bright but loose cluster of intermediate age located approximately 2,300 light years away from Earth. It is located nearly 2 degrees east-southeast of [[Zeta Centauri]].<ref name=OMeara/>
== Observation history == [[File:NGC 5460 map.png|thumb|left|The location of NGC 5460]] NGC 5460 was discovered by [[James Dunlop]] in 1826. He described it on May 7, 1826 as "a curiously curved line of small stars, of nearly equal magnitudes; two stars of 7th magnitude to the east" and added it to his catalog as number 431. [[John Herschel]] described as "a region of large bright stars of 8, 9... etc. magnitude; a very coarse cluster" and added it to General Catalogue as No. 3555. In the [[New General Catalogue]] it is described as "very large, very little concentrated, stars 8th magnitude and fainter".<ref name=OMeara>{{cite book|last1=O'Meara|first1=Stephen James|title=Deep-Sky Companions: Southern Gems|date=2013|publisher=[[Cambridge University Press]]|isbn=9781107015012|pages=266–268|url=https://books.google.com/books?id=S5QIEKns33sC&pg=PA264|language=en|bibcode=2013dcsg.book.....O}}</ref>
== Characteristics == NGC 5460 is a loose open cluster, of [[Robert Julius Trumpler#Trumpler Classification for open star clusters|Trumpler type II3m]]. There are 272 probable member stars within the angular radius of the cluster and 96 within the central part of the cluster. The tidal radius of the cluster is 4.1 - 8.2 parsecs (13 - 26 light years) and represents the average outer limit of NGC 5460, beyond which a star is unlikely to remain gravitationally bound to the cluster core.<ref name="Kharchenko2013">{{cite journal|last1=Kharchenko|first1=N. V.|last2=Piskunov|first2=A. E.|last3=Schilbach|first3=E.|last4=Röser|first4=S.|last5=Scholz|first5=R.-D.|title=Global survey of star clusters in the Milky Way|journal=Astronomy & Astrophysics|date=3 October 2013|volume=558|pages=A53|doi=10.1051/0004-6361/201322302|url=ftp://cdsarc.u-strasbg.fr/pub/cats/J/A%2BA/558/A53/catalog.dat|arxiv = 1308.5822 |bibcode = 2013A&A...558A..53K |archive-url=https://web.archive.org/web/20200312135436/ftp://cdsarc.u-strasbg.fr/pub/cats/J/A+A/558/A53/catalog.dat|archive-date=2020-03-12|url-status=dead|s2cid=118548517}}</ref>
A photometric study by Barrado and Byrne in 1995 studied 353 stars near the core of the cluster and identified 25 members and 27 possible members. They estimated the age of the cluster to be 110 mys and its distance to be 740 pc and identified three stars, members and possible members, as [[variable star|variable]].<ref name=Barrado/> A spectrographic study of the cluster by Fossati et al. (2011) estimated the distance of the cluster to be 720 ± 50 pc, its age log t=8.2 ± 0.1 and the mean radial velocity −17.9 ± 5.2 km/s. The [[metallicity]] of the cluster is slightly higher than the solar one (Z = 0.013).<ref name="Fossati"/>
The brightest of the members is HD 123226 (mag. 8.98, B8),<ref name=Barrado>{{cite journal|last1=Barrado|first1=D.|last2=Byrne|first2=P. B.|title=BV(RI)_KC_ CCD photometry of the core of the young open cluster, NGC 5460|journal=Astronomy and Astrophysics Supplement|date=June 1995|volume=111|page=275|url=https://ui.adsabs.harvard.edu/?#abs/1995A%26AS..111..275B|language=en|bibcode = 1995A&AS..111..275B }}</ref> which is also the hottest star of the cluster.<ref name="Fossati"/> One more star, HD 122983, (mag. 9.77, B9.5IV/V) has been found to be variable, with period 3.4 days.<ref>{{Cite FTP |last1=Paunzen|first1=E.|last2=Hensberge|first2=H.|last3=Maitzen|first3=H. M.|last4=Netopil|first4=M.|last5=Trigilio|first5=C.|last6=Fossati|first6=L.|last7=Heiter|first7=U.|last8=Pranka|first8=M.|title=A photometric long-term study of chemically peculiar stars in open clusters|date=26 November 2010|volume=525|pages=A16|doi=10.1051/0004-6361/200913789|url=ftp://cdsarc.u-strasbg.fr/pub/cats/J/A%2BA/525/A16/stars.v00|arxiv = 1012.0149 |bibcode = 2011A&A...525A..16P |server=Astronomy & Astrophysics|url-status=dead|s2cid=15373925}}</ref> It is a [[Chemically peculiar star|He-weak star]]. Other chemically peculiar stars within the cluster are HD 123182 (He-weak star of an unclear type, mag. 9.88, spectral type B9), and UCAC 11105038 (mag. 11.59, A8). Also, the hotter component of the HD 123225 system may be an HgMn star.<ref name="Fossati"/>
== References == {{reflist}}
== External links == {{commonscat}} {{wikiSky}}
{{Catalogs|NGC=5160|Collinder=280}} {{Stars of Centaurus}} {{Ngc55}}
{{DEFAULTSORT:NGC 5460}} [[Category:NGC objects|5460]] [[Category:Centaurus]] [[Category:Open clusters]]