Astron. J., 117, 1313-1331 (1999/March-0)
The variable stars and blue horizontal branch of the metal-rich globular cluster NGC 6441.
LAYDEN A.C., RITTER L.A., WELCH D.L. and WEBB T.M.A.
Abstract (from CDS):
We present time-series VI photometry of the metal-rich ([Fe/H]=-0.53) globular cluster NGC 6441. Our color-magnitude diagram shows that the extended blue horizontal branch seen in Hubble Space Telescope data exists in the outermost reaches of the cluster. About 17% of the horizontal-branch stars lie blueward and brightward of the red clump. The red clump itself slopes nearly parallel to the reddening vector. A component of this slope is due to differential reddening, but part is intrinsic. The blue horizontal-branch stars are more centrally concentrated than the red clump stars, suggesting mass segregation and a possible binary origin for the blue horizontal-branch stars. We have discovered ∼50 new variable stars near NGC 6441, among them eight or more RR Lyrae stars that are highly probable cluster members. Comprehensive period searches over the range 0.2-1.0 days yielded unusually long periods (0.5-0.9 days) for the fundamental pulsators compared with field RR Lyrae of the same metallicity. Three similar long-period RR Lyrae are known in other metal-rich globular clusters. With over 10 examples in hand, it seems that a distinct subclass of long-period, metal-rich RR Lyrae stars is emerging. It appears that these stars have the same intrinsic colors as normal RR Lyrae. Using the minimum-light color of the RR Lyrae, we determine the mean cluster reddening to be E(B-V)=0.45±0.03 mag, with a significant variation in reddening across the face of the cluster. The observed properties of the horizontal-branch stars are in reasonable agreement with recent models that invoke deep mixing to enhance the atmospheric helium abundance, while they conflict with models that assume high initial helium abundance. The light curves of the c-type RR Lyrae seem to have unusually long rise times and sharp minima. Reproducing these light curves in stellar pulsation models may provide another means of constraining the physical variables responsible for the anomalous blue horizontal-branch extension and sloped red clump observed in NGC 6441.
Stars: Color-Magnitude Diagrams - Galaxy: Globular Clusters: Individual: NGC Number: NGC 6441 - Stars: Variables: RR Lyrae Variable - Stars: Horizontal-Branch - Stars: Variables: General
VizieR on-line data:
<Available at CDS (J/AJ/117/1313): table1.dat var.dat table6.dat notes.dat>
Table 1: Cl* NGC 6441 LRW NNNNN N=16011. Tables 2-4: Cl* NGC 6441 Saw VNN (Nos V13-V50). Table 5: Cl* NGC 6441 LRW SN (Nos S1-S9).
Table 5 : data for SV2 (Cl* NGC 6441 LRW S2) are: X=536 Y=1057 <V≥17. 22 <V-I≥1.03
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