MACHO project 9 million star color-magnitude diagram of the large magellanic cloud

Alcock, C ; Allsman, R A ; Alves, D R ; Axelrod, T S ; Basu, A ; Becker, A C ; Bennett, D P ; Cook, K H ; Drake, A J ; Freeman, K C ; Geha, M ; Griest, K ; King,L ; Lehner, M J ; Marshall, S L ; Minniti, D ; Nelson, C ; Peterson, B A ; Popowski, P ; Pratt, M R ; Quinn, P J ; Stubbs, C W ; Sutherland, W. ; Tomaney, A B ; Vandehei, T. ; Welch, D L

Lawrence Livermore National Laboratory

关键词: Magellanic Clouds;    99 General And Miscellaneous//Mathematics, Computing, And Information Science;    Brightness;    Origin;    Luminosity;   

DOI  :  10.2172/15006433
RP-ID  :  UCRL-ID-137591
RP-ID  :  W-7405-ENG-48
RP-ID  :  15006433

美国|英语

来源: UNT Digital Library

【 摘 要 】

The authors present a 9 million star color-magnitude diagram (9M CMD) of the Large Magellanic Cloud (LMC) bar. The 9M CMD reveals a complex superposition of different age and metallicity stellar populations, with important stellar evolutionary phases occurring over three orders of magnitude in number density. First, they count the non-variable red and blue supergiants, the associated Cepheid variables, and measure the stellar effective temperatures defining the Cepheid instability strip. Lifetime predictions of stellar evolution theory are tested, with implications for the origin of low-luminosity Cepheids. The highly-evolved asymptotic giant branch (AGB) stars in the 9M CMD have a bimodal distribution in brightness, which they interpret as discrete old populations ({ge} 1 Gyr). The faint AGB sequence may be metal-poor and very old. Comparing the mean properties of giant branch and horizontal branch (HB) stars in the 9M CMD to those of clusters, they identify NGC 411 and M3 as templates for the admixture of old stellar populations in the bar. However, there are several indications that the old and metal-poor field population has a red HB morphology: the RR Lyrae variables lie preferentially on the red edge of the instability strip, the AGB-bump is very red, and the ratio of AGB-bump stars to RR Lyraes is quite large. If the HB second parameter is age, the old and metal-poor field population in the bar likely formed after the oldest LMC clusters. Lifetime predictions of stellar evolution theory lead us to associate a significant fraction of the {approx} 1 million red HB clump giants in the 9M CMD with the same old and metal-poor population producing the RR Lyraes and the AGB-bump. In this case, compared to the age-dependent luminosity predictions of stellar evolution theory, the red HB clump is too bright relative to the RR Lyraes and AGB-bump. Last, they show that the surface density profile of RR Lyraes is fit by an exponential, favoring a disk-like rather than spheroidal distribution. They conclude that the age of the LMC disk is probably similar to the age of the Galactic disk.