A&A 373, 153-158 (2001)
DOI: 10.1051/0004-6361:20010577
E. Paunzen1,2 - H. M. Maitzen1
1 - Institut für Astronomie der Universität Wien,
Türkenschanzstr. 17, 1180 Wien, Austria
2 - Zentraler Informatikdienst der Universität Wien,
Universitätsstr. 7, 1010 Wien, Austria
Received 20 February 2001 / Accepted 20 April 2001
Abstract
High accurate photometric data in the three filter, narrow-band
-system for five open clusters
(NGC 2489, NGC 2567, NGC 2658, NGC 5281 and NGC 6208) are presented
permitting one
to detect apparent chemically peculiar stars. The ages and distances
are wide spread to improve the statistics of peculiar stars in
our Milky Way. A total of 235 stars within these clusters have been observed.
We have detected ten apparent peculiar objects
(six with significant positive and four with negative
-values) in four
open clusters. Although three of them within the boundaries of
NGC 2567 are probably not members of this cluster.
Since no Strömgren
data are available from the literature,
Johnson UBV photometry was used to test and calibrate our photometric data.
The results from a comparison of both systems are excellent.
Key words: stars: chemically peculiar - stars: early-type - techniques: photometric - open clusters and associations: general
We continue our search for chemically peculiar objects of the
upper Main Sequence using the three filter -system
(Maitzen 1976) and applying the CCD technique. The first paper
of this series (Bayer et al. 2000, Paper I hereafter) presented
the characteristics of the telescopes, instrumentation, filters and the
reduction processes which were used.
Another five open clusters (NGC 2489, NGC 2567, NGC 2658, NGC 5281 and NGC 6208) with distances from 1000 to 3800pc and ages from 0.01 to 1Gyr have been investigated. A broad variety of distances and ages brings us closer to find a possible correlation of the apparent number of chemically peculiar depending on these parameters.
In addition to (g1-y) measurements, Johnson (B-V) values from the literature were
used to derive -values. Color-magnitude diagrams are shown
for all five open clusters in Fig. 1.
In total, we detected six objects with significant positive -values
and four with negative ones. Three of the latter found in NGC 2567
are most probably not members of the cluster but background stars.
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Figure 1: V versus (g1-y) and a versus (g1-y) for NGC 2489 (left upper panel), NGC 2567 (right upper panel), NGC 2658 (left middle panel), NGC 5281 (right middle panel), NGC 6208 (left lower panel). Filled circles indicate apparent peculiar stars whereas open circles are non-peculiar objects. The solid line is the normality line whereas the dotted lines are the confidence intervals corresponding to 99.9 %. The error bars for each individual objects are the mean errors. The measurement errors of V are much smaller than the symbols and have been omitted. |
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Observations of the five open clusters were performed with the Bochum 61cm (ESO-La Silla) as well as the Helen-Sawyer-Hogg 61cm telescope (UTSO-Las Campanas Observatory) in 1995. The instrumentation and filters used are described in Paper I. The observing log is listed in Table 1.
The basic reductions (bias-subtraction, dark-correction, flat-fielding) were carried out within standard IRAF routines. For all frames we have applied a point-spread-function-fitting within the IRAF task DAOPHOT (Stetson 1987). Photometry of each frame was performed separately and the measurements were then averaged and weighted by their individual photometric error.
In Paper I, we compared our photometric indices with results from
published Strömgren
photometry. The situation
for the five open clusters presented here is different. None of them
has yet been investigated, to our knowledge, via Strömgren
photometry.
However, Johnson UBV photometry is available for all of them
and has been used to test and calibrate our photometric data.
The normality lines were, therefore, independently derived for
(g1-y) and (B-V), respectively. We have only taken published (B-V) values
for this analysis and not tried to transform (g1-y) values
in the corresponding system. There are several reasons for this.
Firstly, most of the data are based on photographic plates
resulting in larger uncertainties. An unknown error is introduced by
unresolved visual binaries not taken into account by the photometry.
From a statistical point of view, the "mixture'' of different
data sets will give misleading results. A comparison of the
-values for both systems results in an excellent agreement.
There are only a few exceptions which are discussed in the relevant
sections.
However, for the peculiar objects reported in this paper without
(B-V) values from the literature, a heuristic transformation
of measured (g1-y) values was applied. Starting with a list
of all stars observed in both systems, objects which deviate more than
5
from a preliminary linear least square fit were rejected.
A final least square fit gives a correlation of (g1-y) with respect
to (B-V). These "calibrated'' values were only used to have an estimate
of the temperature range for the apparent peculiar objects
(Table 2) found. No other attempt to use these values was done.
For the calibration of our y measurements we have used published V observations. A linear fit always resulted in an excellent correlation with a negligible regression coefficient. The only exception are the data for NGC 6208. This is probable caused by our larger errors as well as those in the measurements of Lindoff (1972).
Candidate peculiar stars in all five clusters were
selected if their mean -values are 3
(taking the standard
deviation of the photometry) outside the corresponding confidence intervals
of the normality line. If available, we have also checked the apparent
peculiarity of
using (B-V) from the literature. In overall,
the
-values for both systems are in excellent agreement
shows confidence for the detected apparent peculiar stars.
Cluster | Site | Nights | #
![]() |
#
![]() |
#y |
NGC 2489 | ESO | 3 | 3 | 4 | 3 |
UTSO | 1 | 1 | 1 | 1 | |
NGC 2567 | ESO | 4 | 5 | 7 | 5 |
NGC 2658 | ESO | 3 | 4 | 5 | 3 |
UTSO | 1 | 1 | 1 | 1 | |
NGC 5281 | ESO | 4 | 10 | 13 | 9 |
NGC 6208 | ESO | 2 | 3 | 4 | 5 |
Table 2 lists our observed open clusters and
their characteristics from the literature (Lyngå 1987
and the references listed in the corresponding sections). Further, the
number of observed stars, the number of individual
frames (Table 1) the regression coefficients for all relevant
transformations and normality lines are listed. In addition, the
described peculiar
objects with their -values and apparent (B-V)0 values as well
as the 3
detection limit are given.
The finding charts of our open clusters are shown in Fig. 1. The size of the symbols are inversely proportional to the apparent visual magnitudes of the objects in the sense that larger symbols denote brighter objects.
Name | NGC 2489 | NGC 2567 | NGC 2658 | NGC 5281 | NGC 6208 |
Name | C0754-299 | C0816-304 | C0841-324 | C1343-626 | C1645-537 |
l/b | 247/-1 | 250/+3 | 255/+6 | 309/-1 | 334/-6 |
E(B-V) | 0.40 | 0.13 | 0.40 | 0.26 | 0.18 |
d[pc] | 1450 | 1600 | 3800 | 1300 | 1000 |
logt | 8.45 | 8.43 | 8.50 | 7.04 | 9.00 |
Tr-type | I 2 m | II 2 m | I 2 r | I 3 m | III 2 r |
n(obj) | 59 | 50 | 55 | 30 | 41 |
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+0.032/-0.18 | -0.065/+0.41 | +0.043/+0.01 | +0.049/+0.00 | |
+0.052/-0.11 | -0.062/+0.55 | +0.026/+0.03 | |||
-0.061/+0.04 | -0.097/+0.70 | ||||
+0.031/+0.46 | |||||
![]() |
-8.16/0.997 | -8.34/1.005 | -8.17/0.995 | -8.56/1.013 | -6.67/0.916 |
![]() |
0.754/0.217 | 0.904/0.381 | 0.740/0.181 | 0.735/0.285 | 0.822/0.228 |
![]() |
0.618/0.056 | 0.627/0.130 | 0.640/0.093 | 0.532/0.096 | 0.674/0.054 |
3![]() |
0.013 | 0.021 | 0.010 | 0.006 | 0.018 |
n(frames) | 13 | 17 | 15 | 32 | 12 |
The complete tables with all data for the individual cluster stars are available
both from SIMBAD (via anonymous ftp)
or upon request from the first author. These tables include the cross
identification of objects from the literature, the observed (g1-y) and
a values with their corresponding errors, V magnitudes,
the (B-V) values from the literature and
-values derived from the normality lines of (g1-y) and
(B-V), respectively.
Table 3 lists the apparent peculiar stars found within our investigation. The individual objects are discussed in more detail in the following subsections.
The V versus (g1-y) and a versus (g1-y) diagrams for all five open clusters are shown in Fig. 1. Furthermore, the normality lines and the confidence intervals corresponding to 99.9% are plotted. Filled circles indicate the apparent peculiar objects.
Lindoff & Johansson (1968) used photographic plates to investigate this rather rich open cluster at a distance of about 1450pc from the Sun. The earliest members found have spectral types of about B8. The Johnson UBV measurements of Ramsay & Pollacco (1992) were also used for our analysis. Figure 1 shows a well defined Main Sequence with objects down to 15.5mag.
The normality lines based on both (B-V) and (g1-y), respectively,
are given as:
NGC 2567 was the subject of a detailed investigation by Clariá & Lapasset (1986). They presented photoelectric Johnson UBV photometry for 164 objects brighter than 14.6mag. Further photometry was published by Lindoff (1968) and Ramsay & Pollacco (1992). This open cluster is the most extensively investigated of our five targets.
Several red giants have been found to be members of NGC 2567. Two of them
were also observed by us (Fig. 1). Furthermore, the turn off
point for this cluster is nicely visible (earliest spectral type of about B8).
The Main Sequence consists of late-type B, A and F stars. Clariá & Lapasset
(1986) found no evidence for differential reddening across the cluster. They
derived a distance of 1620pc from the Sun as well as 420pc above the
Galactic plane. The latter is probably incorrect because a
Galactic latitude of +3
and the given distance from the Sun,
a distance of only 85pc above the Galactic plane has been calculated.
The metallicity was found to be nearly solar.
The normality lines based on both (B-V) and (g1-y), respectively,
are given as:
Cluster | No1 | No2 | X | Y | V | a | ![]() |
(g1-y) |
![]() |
![]() |
(B-V) | ![]() |
NGC 2489 | ||||||||||||
24 | 2 | 225.5 | 241.8 | 13.00 | 0.575 | 0.003 | -0.511 | 0.007 | -0.068 | 0.44 | -0.066 | |
39 | 58 | 267.5 | 521.3 | 12.58 | 0.690 | 0.002 | -0.532 | 0.003 | +0.052 | 0.29 | +0.056 | |
54 | 40 | 380.9 | 349.9 | 12.64 | 0.667 | 0.004 | -0.546 | 0.003 | +0.032 | 0.22 | +0.037 | |
57 | 43 | 422.3 | 49.1 | 14.33 | 0.694 | 0.003 | -0.418 | 0.003 | +0.031 | 0.86 | +0.028 | |
NGC 2567 | ||||||||||||
2 | 20.5 | 441.8 | 15.34 | 0.641 | 0.003 | -0.437 | 0.013 | -0.097 | ||||
4 | 38.8 | 283.0 | 15.08 | 0.657 | 0.003 | -0.487 | 0.007 | -0.062 | ||||
16 | 3 | 129.0 | 215.4 | 15.67 | 0.643 | 0.003 | -0.515 | 0.007 | -0.065 | 0.56 | -0.057 | |
NGC 2658 | ||||||||||||
26 | 33 | 165.5 | 236.0 | 15.31 | 0.664 | 0.002 | -0.562 | 0.004 | +0.026 | 0.43 | +0.020 | |
53 | 80 | 342.3 | 310.8 | 15.98 | 0.674 | 0.005 | -0.551 | 0.004 | +0.034 | 0.41 | +0.032 | |
NGC 5281 | ||||||||||||
24 | 322.2 | 179.0 | 13.09 | 0.604 | 0.006 | -0.631 | 0.008 | +0.049 |
Col. 1: Cluster name.
Col. 2: Notation sorted after X and Y, respectively (Fig. 1).
Col. 3: Notation according to Lindoff & Johansson (1968; NGC 2489),
Ramsay & Pollacco (1992; NGC 2567, NGC 2658).
Cols. 4, 5: X and Y coordinates in the finding charts (Fig. 1).
Col. 6: Visual magnitude.
Cols. 7, 8: mean a-index and its standard deviation.
Cols. 9, 10: mean (g1-y) value and its standard deviation.
Col. 11: Deviation from cluster line
a0=a+b
using the
corresponding constants as listed in Table 2.
Col. 12: (B-V) from the literature.
Col. 13: Deviation from cluster line
a0=a+b
using the
corresponding constants as listed in Table 2.
With a distance of about 3800pc, NGC 2658 is the most distant
open cluster investigated in the -system so far.
Johnson UBV colors were taken from Ramsay & Pollacco (1992).
Note that they mixed up Nos. 70 and 119 in their finding chart.
No other appropriate publication was found in the literature.
However, the apparent reddening and, hence, the resulting distance and age
of this cluster from Ramsay & Pollacco (1992) are controversial.
Lyngå (1987) lists
E(B-V)=+0.04 mag, r=2000 pc,
logt=9.15 and an earliest spectral type of about F8.
Since Ramsay & Pollacco (1992) derived
E(B-V)=+0.40 mag,
the distance and age as given in Table 2 are implied.
We are confident that the latter values are correct because of the
results from the Q-method (Golay 1974). Ramsay & Pollacco (1992)
list 38 members of this cluster together with their (B-V) and (U-B)colors based on CCD observations. These objects have spectral types from late
B to mid A type
(according to the Q-method) making the values given in Lyngå (1987)
highly improbable. Furthermore, the results from the -photometry
support these findings. Taking a distance of 3800pc, we derive a distance
of about 400pc above the Galactic plane.
The color-magnitude diagram (Fig. 1) shows a well
defined Main Sequence with objects going down to V16.5mag.
No significant differential reddening was found for this cluster.
The normality lines based on both (B-V) and (g1-y), respectively,
are given as:
The detection of two chemically peculiar objects in such a distant open cluster lends confidence to investigate the incidence of such objects depending on different metallicities in our Milky Way in the near future.
A sequence of 11 B-type stars of this open cluster was observed by
Moffat & Vogt (1973). The earliest bright star found has a spectral
type of about B5. We have used their photoelectric measurements to
derive the normality lines based on (B-V). Together with the one
of (g1-y), they are given as:
Lindoff (1972) already pointed out that this old open cluster lies in a
dense region, 100pc above the Galactic plane. This makes it rather
difficult to investigate its membership and astrophysical properties.
He finds that only half of the objects in the innermost 12
are true members of NGC 6208.
The color-magnitude diagram shown in Fig. 1 coincides very well with the one given by Lindoff (1972). It already shows the rather broad and poorly defined Main Sequence of this cluster.
The normality lines based on both (B-V) and (g1-y), respectively,
are given as:
In the second paper of our series on CCD
photometry of
open clusters, we presented high accurate data of five open
clusters (NGC 2489, NGC 2567, NGC 2658, NGC 5281 and NGC 6208) for
more than 230 objects. For none of these clusters differential reddening was found
to play an important role.
Overall we have detected ten apparent peculiar objects.
But three are probably not members of the corresponding
cluster. The results of the individual clusters follow:
Acknowledgements
We are indebted to an anonymous referee for helpful comments. This work benefitted from the financial contributions of the City of Vienna (Hochschuljubiläumsstiftung project: Wiener Zweikanalphotometer). Use was made of the SIMBAD database, operated at CDS, Strasbourg, France and the WEBDA database, operated at the Institute of Astronomy of the University of Lausanne.
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Figure 1: Finding charts for NGC 2489 (left upper panel), NGC 2567 (right upper panel), NGC 2658 (left middle panel), NGC 5281 (right middle panel), NGC 6208 (left lower panel). North is to the right and west is upwards; 1 pixel=0.5''. The sizes of the open circles are inverse proportional to the V-magnitudes taken from Tables 4 to 8 in the sense that larger open circles denote brighter objects. |
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