NGC 663

{{short description|Open star cluster in the constellation Cassiopeia}}

{{Infobox cluster

| name = NGC 663

| image = 250px

| caption= NGC 663 in Cassiopeia

| constellation = Cassiopeia

| epoch = J2000

| class = -

| ra = 01^h 46.0^m

| dec = +61° 15{{prime}}

| dist_ly = 6,850 ly

| dist_pc = 2,100 pc

| appmag_v = 7.1

| size_v = 16.0{{prime}}

| mass_kg =

| mass_msol =

| radius_ly =

| v_hb =

| age =

| notes =

| names = Caldwell 10, Cr 20, Lawnmower Cluster

}}

File:NGC663 - Open Cluster in Cassopeia.jpg]]

NGC 663 (also known as Caldwell 10) is a young open cluster located 6,850 light years from Earth in the constellation of Cassiopeia. It has an estimated 400 stars and spans about a quarter of a degree across the sky. It can reportedly be detected with the unaided eye, although a telescope is recommended for best viewing. The brightest members of the cluster can be viewed with binoculars. Although the listed visual magnitude is 7.1, several observers have reported higher estimates.

{{cite book

| last=O'Meara | first=S. J.

| date=2002

| title=The Caldwell objects, Deep-sky companions

| publisher=Cambridge University Press

| pages=50–51

| isbn=978-0-521-82796-6

}}

After adjusting for reddening due to interstellar dust, the distance modulus is estimated as 11.6 magnitudes. It is located about 2,100 parsecs distant with an estimated age of 20–25 million years.

{{cite journal

| author=Pigulski, A.

| author2=Kopacki, G.

| author3=Kolaczkowski, Z.

| date=2001

| title=The young open cluster NGC 663 and its Be stars

| journal=Astronomy & Astrophysics

| volume=376 | issue=1 | pages=144–153

| bibcode=2001A&A...376..144P

| doi=10.1051/0004-6361:20010974

| doi-access=free

}} This means that stars of spectral class B2 or higher (in the sense of higher mass), are reaching the end of their main sequence lifespan.

{{cite journal

| author=Marco, A.

| author2=Negueruela, I.

| author3=Motch, C.

| date=2007

| title=Blue Stragglers, Be Stars and X-ray Binaries in Open Clusters

| journal=ASP Conference Series

| volume=361 |pages=388

| bibcode=2007ASPC..361..388M

}} This cluster appears to be located in front of a molecular cloud, although the two are not physically associated. This cloud has the effect of blocking background stars from the visual image of the cluster as it lies at a distance of 300 parsecs.

{{cite journal

| author=Phelps, Randy L.

| author2=Janes, Kenneth A.

| date=1993

| title=Young open clusters as probes of the star-formation process. 2: Mass and luminosity functions of young open clusters

| journal=Astronomical Journal

| volume=106 | issue=5 | pages=1870–1884

| bibcode=1993AJ....106.1870P

| doi=10.1086/116772

}}

This cluster is of interest because of the high number of Be stars, with a total of about 24 discovered. These are spectral class B stars that show prominent emission lines of hydrogen in their spectrum. Most of the Be stars in the cluster lie between spectral class B0 and B3. A candidate member of the cluster, LS I +61° 235, is a Be star with an X-ray binary component that has a period of about three years.{{cite journal

| author=Reig, P.

| display-authors=4

| author2=Fabregat, J.

| author3=Coe, M. J.

| author4=Roche, P.

| author5=Chakrabarty, D.

| author6=Negueruela, I.

| author7=Steele, I.

| date=1997

| title=The Be/X-ray binary LS I +61 235/RX J0146.9+6121: physical parameters and V/R variability

| url=http://aa.springer.de/papers/7322001/2300183.pdf

| journal=Astronomy and Astrophysics

| volume=322

| issue=1

| pages=183–192

| bibcode=1997A&A...322..183R

| access-date=2012-04-17

| archive-url=https://web.archive.org/web/20160304050941/http://aa.springer.de/papers/7322001/2300183.pdf

| archive-date=2016-03-04

| url-status=dead

}} There are at least five blue stragglers in the cluster. These are stars that formed by the merger of two other stars. Two of the cluster's star systems are likely eclipsing binaries with periods of 0.6 and 1.03 days.

{{cite journal

| last=Pietrzynski | first=G.

| date=1996

| title=Variable Stars in the Young Open Cluster NGC 663

| journal=Acta Astronomica

| volume=46 | pages=357–360

| bibcode=1996AcA....46..357P

}} NGC 663 also has two red supergiant stars, both located on its periphery{{cite journal

| author=Mermilliod, J. C.

| author2=Mayor, M.

| author3=Udry, S.

| title=Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters

| journal=Astronomy & Astrophysics

| volume=485

| issue=1

| pages=303–314

| date=2008

| doi=10.1051/0004-6361:200809664

| bibcode=2008A&A...485..303M| citeseerx=10.1.1.30.7545}}{{cite journal

| author=Pandey, A. K.

| display-authors=4

| author2=Upadhyay, K.

| author3=Ogura, K.

| author4=Sagar, Ram

| author5=Mohan, V.

| author6=Mito, H.

| author7=Bhatt, H. C.

| author8=Bhatt, B. C.

| title=Stellar contents of two young open clusters: NGC 663 and 654

| journal=Monthly Notices of the Royal Astronomical Society

| volume=358

| issue=4

| pages=1290–1308

| date=2005

| doi=10.1111/j.1365-2966.2005.08784.x

| bibcode=2005MNRAS.358.1290P| doi-access=free

}}

The star cluster is assumed to form part of the stellar association Cassiopeia OB8, that is located in the Perseus Arm of the Milky Way, along with the open clusters M103, NGC 654, NGC 659, and some supergiant stars scattered between them, all of them having similar ages and distances.{{cite journal

| author=Negueruela, I.

| author2=González-Fernández, C.

| author3=Marco, A.

| author4=Clark, J. S.

| title=A massive association around the obscured open cluster RSGC3

| journal=Astronomy & Astrophysics

| volume=528

| pages=A59

| date=2011

| doi=10.1051/0004-6361/201016102

| bibcode=2011A&A...528A..59N|arxiv = 1102.0028 | s2cid=53517711

}}{{cite journal

| author=Humphreys, R. M.

| title=Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way.

| journal=Astrophysical Journal Supplement Series

| volume=38

| pages=309–350 | date=1978

| doi=10.1086/190559

| bibcode=1978ApJS...38..309H}}

Recent ultraviolet observations from the AstroSat satellite revealed that many of the Be stars in NGC 663 have hot, compact helium-burning subdwarf OB (sdOB) companions, making up about 70% of the Be star population in the cluster. This discovery provides strong evidence that binary interactions, involving mass transfer and stripping of one star to form an sdOB companion, play a key role in the formation and evolution of Be stars in young clusters like NGC 663.{{cite journal |title=AstroSat/UVIT Study of NGC 663: First detection of Be+sdOB systems in a young star cluster |last1=Nedhath |first1=Sneha |last2=Rani |first2=Sharmila |last3=Subramaniam |first3=Annapurni |last4=Pancino |first4=Elena |journal=Astronomy & Astrophysics |date=2025 |volume=699 |pages=L1 |doi=10.1051/0004-6361/202555495 |arxiv=2506.08126 }}