A Comprehensive Study of Five Intermediate-age Pismis (2,3,7,12,15) Clusters Using Photometric and Astrometric Data from Gaia EDR3

被引:5
作者
Bisht, D. [1 ]
Zhu, Qingfeng [1 ]
Elsanhoury, W. H. [2 ,3 ]
Yadav, R. K. S. [4 ]
Rangwal, Geeta [5 ]
Sariya, Devesh P. [6 ,7 ]
Durgapal, Alok [8 ]
Jiang, Ing-Guey [6 ,7 ]
机构
[1] Univ Sci & Technol China, Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China
[2] Natl Res Inst Astron & Geophys NRIAG, Astron Dept, Cairo 11421, Egypt
[3] Northern Border Univ, Fac Sci & Arts, Phys Dept, Turaif Branch, Ar Ar, Saudi Arabia
[4] Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India
[5] Indian Inst Astrophys, Koramangala 2 Block, Bangalore 560034, Karnataka, India
[6] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan
[7] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan
[8] Kumaun Univ, Ctr Adv Study, Dept Phys, DSB Campus, Naini Tal 263002, India
关键词
INITIAL MASS FUNCTION; PROPER MOTIONS; STAR-FORMATION; RADIAL-VELOCITIES; MEMBERSHIP; CATALOG; EVOLUTION; SIMULATIONS; DISTANCES; REGION;
D O I
10.3847/1538-3881/ac8cf4
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Open clusters are groups of stars that form simultaneously; hence, these are excellent probes to test theories of star formation, stellar evolution, and dynamics in the Milky Way disk. We carry out a detailed photometric and kinematic study of five poorly studied intermediate-age open clusters, Pismis 2 (Pi 2), Pismis 3 (Pi 3), Pismis 7 (Pi 7), Pismis 12 (Pi 12), and Pismis 15 (Pi 15), using the Gaia EDR3 database. By estimating the membership probabilities of stars, we recognized 635, 1488, 535, 368, and 494 most probable members for these clusters by using proper-motion and parallax data taken from Gaia EDR3. The radial density profiles of cluster members provide cluster radii of 4.' 5-6.' 5 for these clusters. Their ages range from 0.9 to 2.5 Gyr, and distances range, using parallax, from 2.15 to 5.10 kpc. The overall mass function slopes for main-sequence stars are found as 0.27 +/- 0.16 (for 1.0-1.6 M (circle dot) stars), 0.86 +/- 0.27 (for 1.0-2.1 M (circle dot) stars), 1.08 +/- 0.32 (for 1.0-2.2 M (circle dot) stars), 0.89 +/- 0.38 (for 1.0-2.2 M (circle dot) stars), and 1.07 +/- 0.28 (for 1.0-2.1 M (circle dot) stars) for clusters Pi 2, Pi 3, Pi 7, Pi 12, and Pi 15. Our obtained values of slopes are flatter in comparison with Salpeter's value (x = 1.35) within uncertainty. The present study demonstrates that all these Pismis clusters are dynamically relaxed. We found that these objects follow a circular path around the Galactic center. We compute these clusters' apex coordinates (A, D) and other kinematic parameters.
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页数:17
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