首页|Isochrone Fitting of Galactic Globular Clusters—Ⅵ.High-latitude Clusters NGC 5024(M53),NGC 5053,NGC 5272(M3),NGC 5466,and NGC 7099(M30)

Isochrone Fitting of Galactic Globular Clusters—Ⅵ.High-latitude Clusters NGC 5024(M53),NGC 5053,NGC 5272(M3),NGC 5466,and NGC 7099(M30)

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We fit various color-magnitude diagrams(CMDs)of the high-latitude Galactic globular clusters NGC 5024(M53),NGC 5053,NGC 5272(M3),NGC 5466,and NGC 7099(M30)by isochrones from the Dartmouth Stellar Evolution Database and Bag of Stellar Tracks and Isochrones for α-enrichment[α/Fe]=+0.4.For the CMDs,we use data sets from Hubble Space Telescope,Gaia,and other sources utilizing,at least,25 photometric filters for each cluster.We obtain the following characteristics with their statistical uncertainties for NGC 5024,NGC 5053,NGC 5272,NGC 5466,and NGC 7099,respectively:metallicities[Fe/H]=-1.93±0.02,-2.08±0.03,-1.60±0.02,-1.95±0.02,and-2.07±0.04 dex with their systematic uncertainty 0.1 dex;ages 13.00±0.11,12.70±0.11,11.63±0.07,12.15±0.11,and 12.80±0.17 Gyr with their systematic uncertainty 0.8 Gyr;distances(systematic uncertainty added)18.22±0.06±0.60,16.99±0.06±0.56,10.08±0.04±0.33,15.59±0.03±0.51,and 8.29±0.03±0.27 kpc;reddenings E(B-V)=0.023±0.004,0.017±0.004,0.023±0.004,0.023±0.003,and 0.045±0.002 mag with their systematic uncertainty 0.01 mag;extinctions Av=0.08±0.01,0.06±0.01,0.08±0.01,0.08±0.01,and 0.16±0.01 mag with their systematic uncertainty 0.03 mag,which suggest the total Galactic extinction Av=0.08 across the whole Galactic dust to extragalactic objects at the North Galactic Pole.The horizontal branch morphology difference of these clusters is explained by their different metallicity,age,mass-loss efficiency,and loss of low-mass members in the evolution of the core-collapse cluster NGC 7099 and loose clusters NGC 5053 and NGC 5466.

(stars:)Hertzsprung-Russell and C-M diagrams(ISM:)dustextinction(Galaxy:)globular clusters:general(Galaxy:)globular clusters:individual(NGC 5024,NGC 5053,NGC 5272,NGC 5466,NGC 7099)

G.A.Gontcharov、S.S.Savchenko、A.A.Marchuk、C.J.Bonatto、O.S.Ryutina、M.Yu.Khovritchev、V.B.Il'in、A.V.Mosenkov、D.M.Poliakov、A.A.Smirnov

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Central(Pulkovo)Astronomical Observatory,Russian Academy of Sciences,Pulkovskoye chaussee 65/1,St.Petersburg 196140,Russia

Saint Petersburg State University,Universitetskij pr.28,St.Petersburg 198504,Russia

Special Astrophysical Observatory,Russian Academy of Sciences,369167 Nizhnij Arkhyz,Russia

Departamento de Astronomia,Institute de Física,UFRGS,Av.Bento Gonçalves,9500,Porto Alegre,RS,Brazil

Saint Petersburg University of Aerospace Instrumentation,Bol.Morskaya ul.67A,St.Petersburg 190000,Russia

Department of Physics and Astronomy,Brigham Young University,N283 ESC,Provo,UT 84602,USA

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Russian Science FoundationThis work has made use of BaSTI and DSED web toolsFiltergraphan online data visualization tool developed at Vanderbilt University through the Vanderbilt Initiative in Dataintensive AstrophyFrist Center for Autism and Innovationresources of the Centre de Données astronomiques de Strasbourg,Strasbourgincluding the SIMBAD database,the VizieR catalog access toolX-Match serviceobservations made with the NASA/ESA Hubble Space TelescopeJet Propulsion Laboratory/California Institute of Technologydata products from the Pan-STARRS Surveysdata products from the Sloan Digital Sky Survey joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technoprocessed by the Gaia Data Processing and Analysis

20-72-10052Burger et al.2013Ochsenbein et al.2000PS1

2024

10.1088/1674-4527/ad420f

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCD
影响因子：0.406
ISSN：1674-4527
年,卷(期)：2024.24(6)