Isochrone Fitting of Galactic Globular Clusters—Ⅵ.High-latitude Clusters NGC 5024 (M53),NGC 5053,NGC 5272 (M3),NGC 5466,and NGC7099 (M30)  

作　　者：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 

机构地区：[1]Central(Pulkovo)Astronomical Observatory,Russian Academy of Sciences,Pulkovskoye chaussee 65/1,St.Petersburg 196140,Russia [2]Saint Petersburg State University,Universitetskij pr.28,St.Petersburg 198504,Russia [3]Special Astrophysical Observatory,Russian Academy of Sciences,369167 Nizhnij Arkhyz,Russia [4]Departamento de Astronomia,Instituto de Física,UFRGS,Av.Bento Gonçalves,9500,Porto Alegre,RS,Brazil [5]Saint Petersburg University of Aerospace Instrumentation,Bol.Morskaya ul.67A,St.Petersburg 190000,Russia [6]Department of Physics and Astronomy,Brigham Young University,N283 ESC,Provo,UT 84602,USA

出　　处：《Research in Astronomy and Astrophysics》2024年第6期170-190,共21页天文和天体物理学研究（英文版）

基　　金：financial support from the Russian Science Foundation (grant No.20-72-10052)。

摘　　要：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.

关 键 词：(stars:)Hertzsprung Russell and C-M diagrams (ISM:)dust extinction (Galaxy:)globular clusters:general (Galaxy:)globular clusters:individual(NGC 5024 NGC 5053 NGC 5272 NGC 5466 NGC7099) 

分 类 号：P154.1[天文地球—天文学]