查看“Star cluster group”的源代码

== Discussions ==
=== 2015 ===

==== 2015.06.23 ====
<i> Li: 星團 IMF </i>

PADOVA isochrone test

<i> Zhong: M35 Proper Motion </i>

PM+Spatial --> high prob. mem. comp. with LAMOST RV. (need phot info. to support the results)

==== 2015.06.18 ====
<i> Lin: 跟中央大學談的合作事項。</i>

1. PTF 在星團中的變星 -- 饒兆聰，楊庭彰  (造父變星、RR Ly)

2. NGC752 科學文章 -- 陳文屏 (蒸發、潮汐的成員，動力自行成員、金屬豐度)

3. 星團中的 Brown Dwarfs -- 陳文屏 

==== 2015.06.08 ====
<i> Lin: 說明用密度找PS1星團，分析距離年齡的方法。 </i>

整理出[[star cluster catalog]]以及[[Be star catalog]]。

<i> Zhong: LAMOST在星團中的觀測還不足。 </i>

<i> Li: 學習Chi-square fitting方法。 </i>

== Star Clusters ==
=== in LAMOST ===

=== in APGOEE ===

=== in Pan-STARRS ===

=== in 2MASS ===

=== in Kepler ===

== Catalogs ==
=== open clusters ===

=== globular clusters ===

=== variable stars ===
 Star cluster sample from (186) Dias et al. 2002[http://vizier.china-vo.org/viz-bin/VizieR-3?-source=B/ocl&-out.max=20&-out.add=_r&-out.add=_RAJ,_DEJ&-sort=_r] and (320) Kharchenko et al. 2013. [http://vizier.china-vo.org/viz-bin/VizieR?-source=J/A+A/558/A53&-to=3] with age > 10^9 years and 0 < Dec < 80 deg.

=== be stars ===
==== NGC 663 ====
 
 SEARCHING FOR Be STARS IN THE OPEN CLUSTER NGC 663[http://adsabs.harvard.edu/abs/2015AJ....149...43Y]
 ABSTRACT
 We present Be star candidates in the open cluster NGC663, identified by Hα imaging 
 photometry with the Palomar Transient Factory Survey, as a pilot program to investigate 
 how the Be star phenomena, the emission spectra, extended circumstellar envelopes, 
 and fast rotation, correlate with massive stellar evolution. Stellar membership of the 
 candidates was verified by 2MASS magnitudes and colors and by proper motions (PMs).  
 We discover four new Be stars and exclude one known Be star from being a member due 
 to its inconsistent PMs. The fraction of Be stars to member stars [N(Be)/N(members)] in 
 NGC663 is 3.5%. The spectral type of the 34 Be stars in NGC663 shows bimodal peaks 
 at B0–B2 and B5–B7, which is consistent with the statistics in most star clusters. 
 Additionally, we also discover 23 emission-line stars of different types, including 
 non-member Be stars, dwarfs, and giants.

=== brown dwarfs ===

== bookmarks ==

 Local Group Astrostatistics Conference http://dept.astro.lsa.umich.edu/lgastrostatistics/

[[Category:Internal]]