古老疏散星團柏克萊17成員星的選取

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雷拉(Mikhaela Leia A. Gallardo) 查詢紙本館藏

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論文名稱

古老疏散星團柏克萊17成員星的選取
(Determining Membership Candidates for Aged Open Cluster Berkeley 17)

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摘要(中)

柏克萊17 是位於距離太陽大約2700秒差距的疏散星團，其是銀河系中最古老的開放星團之一。其年齡約為一百億年、[Fe/H]金屬豐度值為0.33 dex、有着數量龐大的藍離散星、顯著的水平分支，使其相似於球狀星團。這星團外型因為其被潮汐力的影響而整體形成拉長的形狀。在以前對於核心-尾部的形態分析當中發現大質量恆星的數量超越小質量恆星的數量。這則可以說明了質量層化在此星團的影響，而其中大質量成員“下沉”到核心，低質量成員佔據更大的外圍空間，造成這個現象的主要成因目前還不清楚。然而其中一個可能成因是來自於星團其獨特位置: 接近英仙旋臂進而產生的潮汐力影響。這論文使用了來自於PS1、2MASS、ALLWISE和GAIA EDR3的多波段資料來作測光分析，並提供了可以找出最有可能是這在瓦解中的星團內的成員星，及其光譜型態和其當下的演化階段的資訊。
利用視差及自行的資料我們可以去除掉一半的已知候選成員星，而藍離散星的數量從21個減少至12個。利用LAMOST的光譜資料我們得到[Fe/H]金屬豐度的值為-0.75 dex。根據這星團相對於銀河系運動的狀態可以看出柏克萊 17受到英仙旋臂的顯著影響，因為它的運動方向與銀河自轉方向相反並朝向銀河中心。

摘要(英)

oindent Berkeley 17, located at a heliocentric distance of 2700 pc, is among the oldest Galactic open
clusters. The cluster is noted to resemble globular clusters for its ~10 Gyr age, [Fe/H] of -0.33
subsolar metallicity, excessive number of blue stragglers, and a prominent horizontal branch. The
cluster displays an elongated shape due to a tail and anti-tail. In previous analysis of its core-tail
morphology, massive stars outnumber less massive ones. This indicated the effect of dynamical
mass segregation, where massive members ′sink′ to the core, while the low-mass members occupy
larger volumes. The cause of this phenomenon is unclear, however, one possible tidal source is the
Perseus arm, where distinct field population of Berkeley 17 is attributed to. Multi-wavelength
photometry and astrometry from PS1, 2MASS, AllWISE, and GAIA EDR3 were processed to gain
the disintegrating cluster’s highest-probable members and their spectral types, as well as current
stage in dynamical evolution.

Almost half of the previously known members are removed due to parallax and proper motion, also reducing the blue straggler population from 21 to 12. LAMOST spectrosocpy returned a near solar metallicity at [Fe/H] = -0.175 dex. Galactic motion also suggests that Berkeley 17 is heavily affected by the Perseus arm due to its motion against the Galactic rotation and towards the Galactic center.

關鍵字(中)

★ 散星

關鍵字(英)

論文目次

Abstract vi
Acknowledgements viii
List of Figures xi
List of Tables xii
1 Introduction 1
1.1 Star Clusters and Disintegration . . . . . . . . . . . . . . . . . . . . . . . 1
1.2 Berkeley 17 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3
1.3 Motivation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3
2 Archival Data 5
2.1 Photometry . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5
2.2 Proper Motion and Distance . . . . . . . . . . . . . . . . . . . . . . . . . 6
3 Membership Determination 7
3.1 Clusterix . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
3.2 DBSCAN . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8
3.3 Adapting previous filtering method . . . . . . . . . . . . . . . . . . . . . 9
3.4 Compilation of results . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10
4 Members of Berkeley 17 13
4.1 Evolved Members . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13
4.2 Blue Stragglers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17
4.3 Comparison to previously known members . . . . . . . . . . . . . . . . . 17
ix
4.4 Spectral type based on photometry . . . . . . . . . . . . . . . . . . . . . 18
4.5 Additional Spectroscopic Data . . . . . . . . . . . . . . . . . . . . . . . . 19
4.6 Location and motion of Be17 in the galaxy . . . . . . . . . . . . . . . . . 21
5 Summary 24
A Members of Berkeley 17 25
A.1 Members of Be17 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26
A.2 Blue Stragglers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 37

參考文獻

Ahumada J. A., Lapasset E., 2007, AAP, 463, 789
Bailer-Jones C. A. L., Rybizki J., Fouesneau M., Demleitner M., Andrae R., 2021, AJ,
161, 147
Balaguer-Núñez L., et al., 2020, MNRAS, 492, 5811
Bhattacharya S., Mishra I., Vaidya K., Chen W. P., 2017, ApJ, 847, 138
Bhattacharya S., Vaidya K., Chen W. P., Beccari G., 2019, AAP, 624, A26
Bragaglia A., Tosi M., Andreuzzi G., Marconi G., 2006, MNRAS, 368, 1971
Bressan A., Marigo P., Girardi L., Salasnich B., Dal Cero C., Rubele S., Nanni A., 2012,
MNRAS, 427, 127
Cabrera-Cano J., Alfaro E. J., 1990, AAP, 235, 94
Cánovas H., et al., 2019, , 626, A80
Cardelli J. A., Clayton G. C., Mathis J. S., 1989, ApJ, 345, 245
Carraro G., Geisler D., Villanova S., Frinchaboy P. M., Majewski S. R., 2007, AAP,
476, 217
Chambers K. C., et al., 2016, arXiv e-prints, p. arXiv:1612.05560
Chen W. P., Chen C. W., Shu C. G., 2004, AJ, 128, 2306
Chen W. P., Bhattacharya S., Mishra I., Vaidya K., Lalchand B., 2017, in Journal of
Physics Conference Series. p. 012093, doi:10.1088/1742-6596/869/1/012093
Clarke C. J., Bonnell I. A., Hillenbrand L. A., 2000, in Mannings V., Boss A. P., Russell
S. S., eds, Protostars and Planets IV. p. 151 (arXiv:astro-ph/9903323)
Cutri R. M., et al., 2013, Explanatory Supplement to the AllWISE Data Release Products, Explanatory Supplement to the AllWISE Data Release Products
Ester M., Kriegel H.-P., Sander J., Xu X., 1996. AAAI Press, pp 226–231
Friel E. D., 1995, ARA&A, 33, 381
Friel E. D., Janes K. A., Tavarez M., Scott J., Katsanis R., Lotz J., Hong L., Miller N.,
2002, AJ, 124, 2693
39

Galadi-Enriquez D., Jordi C., Trullols E., 1998, AAP, 337, 125
Green G. M., Schlafly E., Zucker C., Speagle J. S., Finkbeiner D., 2019, ApJ, 887, 93
Hayes C. R., Friel E. D., 2014, AJ, 147, 69
Hills J. G., Day C. A., 1976, ApL, 17, 87
Hodapp K. W., Siegmund W. A., Kaiser N., Chambers K. C., Laux U., Morgan J.,
Mannery E., 2004, in Oschmann Jacobus M. J., ed., Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 5489, Ground-based Telescopes.
pp 667–678, doi:10.1117/12.550179
Kaluzny J., 1994, AcA, 44, 247
Kharchenko N. V., Piskunov A. E., Schilbach E., Röser S., Scholz R. D., 2013, AAP,
558, A53
Kruijssen J. M. D., 2012, MNRAS, 426, 3008
Krumholz M. R., McKee C. F., Bland-Hawthorn J., 2019, ARA&A, 57, 227
Krusberg Z. A. C., Chaboyer B., 2006, AJ, 131, 1565
Lada C. J., Lada E. A., 2003, ARA&A, 41, 57
Lindegren L., et al., 2021, AAP, 649, A2
Luo A. L., et al., 2015, Research in Astronomy and Astrophysics, 15, 1095
Magnier E. A., et al., 2013, ApJs, 205, 20
Mainzer A., et al., 2011, ApJ, 743, 156
Mathieu R. D., 1984, ApJ, 284, 643
McCrea W. H., 1964, MNRAS, 128, 147
Phelps R. L., 1997, ApJ, 483, 826
Phelps R. L., Janes K. A., Montgomery K. A., 1994, AJ, 107, 1079
Reid M. J., et al., 2014, ApJ, 783, 130
Reid M. J., et al., 2019, ApJ, 885, 131
Riello M., et al., 2021, AAP, 649, A3
Salaris M., Weiss A., Percival S. M., 2004, AAP, 414, 163
Sandage A. R., 1953, AJ, 58, 61
Scott J. E., Friel E. D., Janes K. A., 1995, AJ, 109, 1706
Skrutskie M. F., et al., 2006, AJ, 131, 1163

Skrzypek N., Warren S. J., Faherty J. K., Mortlock D. J., Burgasser A. J., Hewett P. C.,
2015, AAP, 574, A78
Spitzer Lyman J., Harm R., 1958, ApJ, 127, 544
Tang S.-Y., et al., 2019, ApJ, 877, 12
Tonry J. L., et al., 2012, ApJ, 750, 99
Wright E. L., et al., 2010, AJ, 140, 1868
Xu Y., Reid M. J., Zheng X. W., Menten K. M., 2006, Science, 311, 54
Yen S. X., Reffert S., Schilbach E., Röser S., Kharchenko N. V., Piskunov A. E., 2018,
AAP, 615, A12
Zhang Y., Tang S.-Y., Chen W. P., Pang X., Liu J. Z., 2020, ApJ, 889, 99
Zuckerman B., Song I., 2004, ARA&A, 42, 685

指導教授

饒兆聰(Chow-Choong Ngeow)

審核日期

2021-10-27

推文