NGC 5927

{{Short description|Globular cluster in the constellation Lupus}}

{{Infobox globular cluster

| name = NGC 5927

| class = VIII

| image = 250px

| caption = The globular cluster NGC 5927 imaged by the Hubble Space Telescope

| credit =

| epoch = J2000

| constellation = Lupus

| ra = {{RA|15|28|00.69}}{{cite simbad|title=NGC 5927|access-date=8 January 2017}}

| dec = {{DEC|-50|40|22.9}}

| dist_ly = 25.1 kly
(7.7 kpc)

| appmag_v = 8.86

| size_v =

| mass_msol =

| radius_arcminsec = 6.0' x 6.0'{{cite web|title=NGC 5927|url=http://spider.seds.org/spider/MWGC/n5927.html|access-date=8 January 2016}}

| v_hb =

| metal_fe = -0.49{{cite web|title=A Galactic Globular Clusters Database: NGC 5927|url=http://gclusters.altervista.org/cluster_4.php?ggc=NGC+5927|access-date=8 January 2017}}

| metal_z =

| age =

| notes =

| names = GCl 35, GCRV 5278 E, VDBH 173

}}

NGC 5927 is a globular cluster in the constellation Lupus. NGC 5927 has a diameter of about 12 arcminutes and an apparent magnitude of +8.86. Its Shapley–Sawyer Concentration Class is VIII, and it contains stars of magnitude 15 and dimmer.

The globular cluster was discovered by the astronomer James Dunlop in 1826 and was also observed in 1834 by John Herschel.{{Cite web|title=New General Catalog Objects: NGC 5900 - 5949|url=https://cseligman.com/text/atlas/ngc59.htm#5927|access-date=2021-03-11|website=cseligman.com}}

NGC 5927 is relatively metal-rich for a globular cluster, and may have multiple generations of stars.{{citation|arxiv=1802.07314|year=2018|title=On the Chemical Abundances of Miras in Clusters: V1 in the Metal-rich Globular NGC 5927|doi=10.3847/2041-8213/aab100 |last1=d'Orazi |first1=V. |last2=Magurno |first2=D. |last3=Bono |first3=G. |last4=Matsunaga |first4=N. |last5=Braga |first5=V. F. |last6=Elgueta |first6=S. S. |last7=Fukue |first7=K. |last8=Hamano |first8=S. |last9=Inno |first9=L. |last10=Kobayashi |first10=N. |last11=Kondo |first11=S. |last12=Monelli |first12=M. |last13=Nonino |first13=M. |last14=Przybilla |first14=N. |last15=Sameshima |first15=H. |last16=Saviane |first16=I. |last17=Taniguchi |first17=D. |last18=Thevenin |first18=F. |last19=Urbaneja-Perez |first19=M. |last20=Watase |first20=A. |last21=Arai |first21=A. |last22=Bergemann |first22=M. |last23=Buonanno |first23=R. |last24=Dall'Ora |first24=M. |last25=Da Silva |first25=R. |last26=Fabrizio |first26=M. |last27=Ferraro |first27=I. |last28=Fiorentino |first28=G. |last29=Francois |first29=P. |last30=Gilmozzi |first30=R. |journal=The Astrophysical Journal |volume=855 |issue=1 |pages=L9 |bibcode=2018ApJ...855L...9D |s2cid=119375515 |display-authors=1 |doi-access=free }}