Date and Time of the Query: 2019-06-18 T13:09:35 PDT
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Notes for object MESSIER 016

1 note(s) found in NED.

1. 2006A&A...457..265D
Re:NGC 6611
For NGC6611, because of the highly variable reddening across the field, it
was not possible to use a similar method to that for NGC3293 and NGC4755.
From Hillenbrand et al. (1993), we can identify 22 stars with spectral
types earlier than B3, which are likely cluster members but for which we
do not have spectroscopy. All but one of these are classified as B0.5V-B3V
and we have adopted effective temperature estimates based on the data in
Table 1. The other target is BD-13deg4912,which was classified as B2.5I,
and for this we have adopted T_eff_ = 16 500 K (Crowther et al. 2006).
Masses were then calculated following the same procedure as discussed in
Sect. 3.5.
We have also estimated effective temperatures, luminosities and
masses for likely cluster members in the Hillenbrand et al. sample without
spectral types by calculating Q, and using the Q . T_ef_f relation of
Massey et al. (1989). None of these targets had masses above 7 M_sun_ and
hence it is reasonable to assume that the combination of our spectroscopy
and that of Hillenbrand et al. is virtually complete above 7 M_sun_. In
Fig. 7 we plot the IMF for NGC6611 and determine a slope of Gamma = .1.5
+- 0.1, which is slightly steeper than the value of Gamma = .1.1 +- 0.3 of
Hillenbrand et al., but is consistent with a Salpeter type value and again
similar to our other clusters and those in the Massey et al. (1995)

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