NGC 5662

{{Short description|Open cluster in the constellation Centaurus}}

{{Infobox cluster

| name = NGC 5662

| image = File:NGC 5662 DSS.jpg

| caption = NGC 5662 imaged by DSS

| credit =

| type = Open Cluster

| epoch = J2000

| constellation = Centaurus

| ra = {{RA|14|35|37}}

{{cite simbad

| title=NGC 5662

| access-date=2015-06-19

}}

| dec = {{DEC|-56|37|06}}

| dist_ly = 2,170 ly

| dist_pc = 666 pc[https://webda.physics.muni.cz/cgi-bin/ocl_page.cgi?dirname=ngc5662 WEBDA: NGC 5662]

| appmag_v = 5.5

| size_v =12'

| mass_msol = 348{{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 |doi-access=free}}

| age = 93 million years

| notes =

| names = Melotte 127, Colinder 284, vdBH 162

}}

NGC 5662 is an open cluster in the constellation Centaurus. It was discovered by Nicolas Louis de Lacaille on May 17, 1752 from South Africa.{{cite journal

| title=The search for the nebulae - VI

| last=Jones | first=K. G.

| journal=Journal of the British Astronomical Association

| volume=79 | pages=213–222 | date=March 1969

| bibcode=1969JBAA...79..213J

}} James Dunlop observed it on July 10, 1826 from Parramatta, Australia and added it to his catalog as No. 342.

It is a rich cluster (Trumpler class II3r), with 295 stars according to Haug (1978) and 280 according with Archinal, Hynes (2003).{{cite web|last1=Kronberg|first1=Christine|last2=Frommert|first2=Hartmut|title=NGC 5662|url=http://messier.seds.org/xtra/ngc/n5662.html|website=messier.seds.org}} One of its members, V Centauri, is a cepheid variable. Despite its large distance from the cluster centre, it has high likelihood of being a member of it.{{cite journal|last1=Anderson|first1=Richard I.|last2=Eyer|first2=Laurent|last3=Mowlavi|first3=Nami|title=Cepheids in open clusters: an 8D all-sky census|journal=Monthly Notices of the Royal Astronomical Society|date=July 2013|volume=434|issue=3|pages=2238–2261|doi=10.1093/mnras/stt1160|doi-access=free |arxiv = 1212.5119 |bibcode = 2013MNRAS.434.2238A }}

The tidal radius of the cluster is 6.4 - 12.4 parsecs (21 - 40 light years) and represents the average outer limit of NGC 5662, beyond which a star is unlikely to remain gravitationally bound to the cluster core.