Issue |
A&A
Volume 514, May 2010
|
|
---|---|---|
Article Number | A59 | |
Number of page(s) | 8 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361/200913399 | |
Published online | 20 May 2010 |
The Carina spiral feature: Strömgren-
photometry approach
II. Distances and space distribution of the O and B stars![[*]](/icons/foot_motif.png)
N. Kaltcheva - M. Scorcio
Department of Physics & Astronomy, University of Wisconsin Oshkosh, 800 Algoma Blvd., Oshkosh, WI 54901-8644, USA
Received 2 October 2009 / Accepted 29 January 2010
Abstract
Aims. In recent years a significant development has become
evident in the study of the stellar structure of the Galactic disk.
This is especially true for the 3rd Galactic quadrant, where the
stellar population was extensively investigated beyond 10 kpc,
revealing details about the warped geometry of the thin and thick disks
and outer arm. The 4th Galactic quadrant offers even better opportunity
to follow the distribution of the young stellar populace to a large
distance, since the line of sight is parallel to the largest single
segment of a spiral arm seen from our position in the Galaxy: the
Carina spiral feature. This paper further contributes to the study of
the structure of the Galactic disk in the direction of Carina field
utilizing homogeneous photometric distances of a sample of about 600
bright early-type stars seen in this direction up to 6 kpc.
Methods. The derived stellar distances are based on photometry. All O and B type stars with
data presently available are included in the study.
Results. The photometry-derived parameters allow us to study the
structure and characteristics of this segment of the Carina arm. We
find that the stellar distribution is consistent with a location of the
apparent edge of the arm at l = 287.
Toward the edge of the arm the warp of the Galactic plane can be
traced up to 6 kpc where it reaches negative 200 pc. The
field toward the edge seems to be much more complex than harboring just
one OB association, and it is likely that some of the apparent
concentrations in this field represent parts of long segments of the
edge. In the 284
-289
longitude
range an interarm space about 1 kpc wide is found beyond
850 pc from the Sun. The giant molecular clouds and open clusters
do not follow the edge of the arm as defined by the OB stars and
indicate a possible presence of an age gradient in a direction
perpendicular to the formal Galactic plane.
Key words: Galaxy: structure - stars: distances - open clusters ans associations: general
1 Introduction
The detailed structure of the Galactic spiral arms as delineated by the young stars and their groupings provides valuable information about the geometry of the thin and thick disk components. Tracing distant spiral features is, however, a complex experiment, heavily dependent on individual studies of the Galactic open clusters and OB-associations, and on the homogeny and completeness of the available catalogs. Nevertheless, in recent years significant progress has been achieved in mapping the young stellar population within the disk to great distances. Examples include a topographical study of the Galactic disk from a sample of young open clusters to a distance of 4 kpc (Alfaro et al. 1991) and a study of the vertical profile of the Carina arm (Alfaro et al. 1992). Another detailed photometric investigation of the stellar population toward the CMa over-density (Vázquez et al. 2008, and the reference therein) provides a comprehensive picture of the Local and outer spiral fragments in the third Galactic quadrant as well as of the warped geometry of the Galactic disk.
The focus of this article is the Carina section of the Milky Way,
which is still considered to be the most promising of all fields for
the optical study of a single large-scale Galactic feature (Bok 1937;
Graham 1970). Observational efforts date back more than a century to
the pioneering work of Hershel & See on the apparent stellar
clustering around Car (See 1897). At one point Carina was even
considered to be the center of our stellar system (Charlier 1916;
Trumpler 1930). Becker (1956) and Bok (1956) originally suggested
that this impressive apparent concentration of young stars is a
tangentially observed segment of a spiral arm. Graham & Lynga's
(1965) objective prism survey revealed that there are faint OB-stars
as distant as 8-10 kpc. As early radio maps would show, this
concentration is real, and not simply due to an absorption
gap. However, the interstellar extinction toward Carina is low,
allowing for observation of the structure to great distances.
Probably the first comprehensive review of the Carina star-forming
field was presented by Sher (1965), who compiled the results of the
more than eighty major papers that existed at the time. The first
mapping of the field was based on UBV photometry of a dozen open
clusters (see Sher 1965). Later Bok et al. (1970) presented the first
diagram of the structure of the field based both on clusters and field
stars. Moffat & Vogt (1975) studied about 20 major clusters in Carina
in terms of UBV
photometry. More recent photometric studies
utilizing
photometry were performed by Kaltcheva & Georgiev
(1993), Shobbrook & Lynga (1994), Kaltcheva (1998), and Kaltcheva et al. (2000). A data-base collating all
photometry available at present for O-B9 stars brighter than about
10th visual magnitude in the field of the Carina spiral
feature is presented by Kaltcheva (2003, Paper I).
Here we provide precise photometric distances for most of the
stars with complete photometry included in Kaltcheva's (2003) catalog
and use them to outline the overall structure and characteristics of
the Carina spiral feature. A detailed description of the
photometric quantities used in this photometric system can be found in
Strömgren (1966). Among the wide variety of photometric systems
available today the
photometry is arguably better suited for
the study of individual stars in terms of stellar luminosity than
any other photometric system in wide use and proven to provide
reliable stellar distances (cf. Kaltcheva & Makarov 2007).
The
derived distances and color excesses present a basis for establishing
a homogeneous distance scale for the prominent stellar groupings in the
Carina Field that will be carried out in the third paper of this
series.
2 The sample
Our sample consists of about 600 stars earlier than A0 spectral type with
available photometry listed in at least one of the HD, CPD, PPM
and LS catalogs. This excludes stars in clusters that do
not have designations in the above catalogs, like for example most of the stars
in Tr 16. The completeness of the sample over the
apparent magnitude range is discussed in detail by Kaltcheva
(2003). The limitations of the above catalogs set the magnitude limit
for the sample at about 10th visual mag. Another
restriction comes from the lack of spectral classification for the
faint stars in the above catalogs. The overall completeness of the
database (Paper I) is quite satisfactory for stars brighter than 8.5 mag,
dropping rapidly toward the fainter stars to less than 30% for the
9.5-10 visual magnitude range. However, the data-base is about
80% complete to 9.1 mag. The sample is
magnitude-limited, which poses restrictions when studying the structure of
star-forming fields. Nevertheless, the precise photometric distances
derived here present a significant improvement over the current
situation and should allow us to obtain reliable average distances for
the apparent structures and substructures in the Carina field.
Table 1 shows the completeness of the sample as a function of Galactic
longitude. The completeness is calculated in terms of number of
stars from the above mentioned catalogs that have complete photometry. The overall completeness is close to about 50%, with the
292
-294
range being an exception at a lower completeness of 36%.
Table 1: Completeness of the sample across the field.
Inspection of the redenning free
diagrams (not included
here) for the longitude ranges in Table 1 shows that half of the
stars in the sample are earlier than B5. The spectral content
of the sample is uniform over the longitude range.
3 Photometry-derived color excesses and distances
The procedure of deriving color excesses and stellar distances followed here is described in detail in Kaltcheva & Hilditch (2000) (KH hereafter). The color excesses were obtained via Crawford's (1978) calibration for luminosity class (LC) V, IV and III and via the calibration by Kilkenny & Whittet (1985) for LC II, Ib, Iab and Ia. The sample used in this article does not contain stars with [c1]>0.9 mag, and thus no stars are expected to be found outside the limits of the intrinsic color calibrations. We used R=3.2 and E(B-V) = E(b-y)/0.74 to obtain V0. The calibration of Balona & Shobbrook (1984) was utilized for all LC to derive the absolute magnitudes.
Since different calibrations are used to calculate the color excesses
for different LC types, great care was taken to resolve all cases of
suspected misclassification. To ensure as proper an LC classification as
possible, the database was divided into groups according to the LC
available in Simbad and each group was considered separately. The
reddening free [c1]/[m1] and [c1]/
diagrams (not shown here) built for each LC were used to examine for
possible LC misclassifications and for stars with H
emission. It should be mentioned, however, that the presence of
emission can complicate the photometric LC classification based on the
[c1]/
diagrams. The individual sources of spectral
classification were also considered for all cases of observed
inconsistencies.
As is well known, the largest source of error in the calculated
absolute magnitudes for early-type stars is the presence of
emission lines in the stellar spectra. In general, within a given LC,
a discrepancy between the observed
and the one calculated from the dereddened index c0 (
(c0) hereafter), may
indicate emission in the stellar spectrum, though
sometimes the effect can be due to stellar evolution. As discussed in
KH, for the brightest supergiants and all stars observed in emission,
(c0) should be used to calculate MV. A comparison of the MV values
obtained with the calculated
(c0) (MV(c0) hereafter) to the
MV values obtained via the observed
(
hereafter) can
even better indicate stars observed in emission.
Our sample contains 130 stars classified as LC II-III, III. The
photometric classification based both on [c1]/[m1] and
[c1]/
diagrams agrees with stars close to the main
sequence. Seven of these stars are located above the LC II intrinsic
color line in the [c1]/
diagram, exhibiting photometric behavior
consistent with emission. For these stars MV(c0) was adopted as a final
estimate of the absolute magnitude.
The LC III-IV, IV, V group contains 197 stars. Of these 173 were
assigned to the group because of their Simbad classification. Five
stars have
and thus felt outside the limits of the
Balona & Shobbrook (1984) calibration. For them
was
used. Nine stars appear to be emission-line stars and
was adopted as a final estimate of the absolute magnitude for them as
well. The remaining 24 stars of this group are classified in the Simbad database as LC
II, but showed a systematic disagreement between their MV(c0) and
values when treated as LC II. A close examination of
the dereddened [c1] vs.
diagram pointed to a possible LC
misclassification. Based on their photometric behavior, we adopted a
LC III for these stars and recalculated the color excess with
Crawford's (1978) calibration, which removed the systematic
difference. These stars are listed in Table 2.
In the sample are 97 stars without available LC. Inspection
of the photometric diagrams allowed those stars to be classified
as LC III-V. Among them there are 10 stars with
mag and eight emission-line stars. In both cases
was adopted.
Table 2: Stars originally classified as LC II in the Simbad data-base for which LC III was adopted.
Table 3:
Stars for which the
index calculated from
is used to obtain MV.
For stars of LC I and II the [c1]/[m1] diagram is not
informative in terms of luminosity classification, thus only the
[c1]/
diagrams were used to identify possible
mis-classifications. The sample contains eight stars classified as Ia,
Iae in the Simbad database, and that classification seems consistent
with the photometric [c1]/
diagram. Following KH, MV(c0) is adopted as a final estimate of the absolute
magnitude for all Ia
stars since
is expected to be influenced by emission
for this LC. This procedure helped to obtain reasonable estimates of
the absolute magnitude for four stars with very negative
.
The rest of the Ia stars showed good agreement between the
and MV(c0) values. Luminosity class Iab was represented by six
stars, most of which (especially HD 89714 and HD 95733) could be
classified photometrically as Ib or even LC II based on the
[c1]/
diagram. Keeping this in mind we used
for
our final estimate of the absolute magnitude of all six Iab stars. In
general there is a good agreement between
and MV(c0)for all Iab stars, with the exception of HD 96248 (-8.1 mag
vs. -5.1 mag). Luminosity class Ib contains 26 stars, of which MV(c0) was adopted for only three stars. MV(c0) was used among the 46 stars of LC Ib-II and II for
another three stars instead of
.
All stars,
for which a
index calculated from
was used to
obtain MV, are listed in Table 3. Table 4, available only
electronically via CDS, summarizes the photometry-derived information
for all 598 stars in the sample. The table contains star
identification, spectral classification found in the Simbad data-base,
the photometric quantities and the dereddened photometry and color
excess, absolute magnitudes and the calculated distances. The stars
are organized in groups according to their luminosity classes. The
expected uncertainties in MV are on the order of
0.3 for LC III-V and
0.5 for supergiants (Balona & Shobbrook 1984), which
propagate to an asymmetric uncertainty of -13% to +15% and
-21% to +26% in the derived distances, respectively.
4 Discussion
4.1 Comparisons to other surveys
It is worthwhile to compare our distance estimates to previous estimates
available in the literature. Photometric distances of two large
samples of early-type stars in Carina are published by Graham (1970)
and Shobbrook & Lynga (1994). Graham (1970) used an MV()
calibration obtained as an average of the calibrations of Fernie (1965)
and Graham (1967), and broad-band photometric estimations of reddening
to derive the distances. Shobbrook & Lynga (1994) applied the
calibration of Balona & Shobbrook (1984), but the procedure utilized
by these authors is slightly different from ours, mainly when applied
to emission-line stars. Histograms of the differences in stellar
distance in terms of ``this paper minus others''
are presented in Fig. 1. There are 98 stars in common between our
survey and that of Graham (1970). If we omit seven stars with considerable
differences, the average is
pc (the uncertainties
used throughout the text are the standard deviations, unless a
different uncertainty is mentioned). The 43 stars in common with
Shobbrook & Lynga (1994) have an average of the differences of
pc (LS 1962 and LS 2089 are omitted). On average, the
distances obtained here are smaller by 200 pc in comparison to the
previous studies. Since our procedure of using MV(c0) values
for the emission line stars should eliminate distance overestimations,
this is likely the cause of the discrepancy. The calculated
standard deviations point to a better agreement between our
results and that of Shobbrook & Lynga (1994) due to the use of the
same calibration. The bottom plot in Fig. 1 presents the structure of
the field as revealed by the stars in common with these authors. One
can notice the similar distribution of the two sets with Galactic
longitude. There are 40 stars in the Shobbrook & Lynga (1994) survey
fainter than the limiting magnitude of our survey, and thus not
included in our sample. With the relatively good agreement
in the derived distances in mind, we include these stars in the following
discussion using the distances calculated by Shobbrook & Lynga
(1994).
![]() |
Figure 1: The histograms of the differences between the photometric distances obtained here and those by Graham (1970) ( top panel) and Shobbrook & Lynga (1994) ( middle panel). The bottom panel presents a comparison of the location of the stars plotted as a function of Galactic longitude using the distances obtained here (plus symbols) and those calculated by Shobbrook & Lynga (1994) (filled symbols). The overall uncertainty in the plotted stellar distances is about 15%. |
Open with DEXTER |
![]() |
Figure 2:
Photometric distances plotted as a function of Galactic longitude for
different LC groups. In the first three plots filled dark symbols are
used for stars with
|
Open with DEXTER |
![]() |
Figure 3: Sample stars plotted in Galactic coordinates and the photometric distances and color excesses plotted as a function of the Galactic coordinates. The stars are marked with different symbols according to their LC as follows: filled squares - LC III-IV, IV, V; open triangles - LC II-III, III; open circles - the group without LC available, filled diamonds - LC Ia, Iab, Ib, II. The 40 stars from Shobbrook & Lynga (1994) are shown with open-star symbols on all diagrams. The uncertainties in the stellar distances are the same as in Fig. 2. |
Open with DEXTER |
4.2 Distribution of the stars in Galactic longitude
Figure 2 is a plot of the derived distance for each star as a function of Galactic longitude. Each LC discussed above is plotted separately. For LC II-III to V (first three diagrams) the stars with MV(c0) adopted as a final estimate of the absolute magnitude are shown with filled symbols. It can be seen that these stars do not show any systematic trend in terms of distance in comparison to the rest of the sub-samples. Luminosity class III-IV, IV, V form a main layer of 124 stars between 270 and 1400 pc at a median distance of




Figure 3 presents all sample stars plotted in Galactic coordinates, the plots
of photometric distances vs. Galactic longitude and Galactic
latitude, and the color excess vs. Galactic longitude. The solid
line on distances vs. Galactic longitude diagram is the apparent edge
of the Carina arm as derived by Graham (1970). Figure 3 supports the
conclusion of Graham (1970) that no early-type stars are found at
great distances (greater than 4 kpc for our sample) for longitudes
smaller than 286.
The location of the outer edge of the Carina arm,
as proposed by the same author, seems consistent with the structure
revealed by the present sample. For our sample, however, very few
stars are seen at large distances for longitudes greater than 291
as
well, where the completeness is less than 50%. Since for distances
greater than 3-4 kpc, the observational selection effects are severe, a
much broader and fainter sample is needed for reliable conclusions. In
the 284
-289
longitude range there is an indication of an inter-arm
space between 1 and 2 kpc that separates the relatively nearby
structure consisting mainly of III-V LC stars from the structure of
slightly more-luminous stars located beyond 2 kpc. The presence of an
inter-arm space is also supported by the gap in the color excess seen
in the fourth plot in Fig. 3. A similar feature was noticed by
Kaltcheva (1998) based on a much smaller sample. Contrarily to that, toward l=291
most of the stars are spread out in depth between 1 and
3 kpc. This is the line of sight toward the
Car OB2 association. The new larger sample confirms the previous
conclusions (Shobbrook & Lynga 1994; Kaltcheva 1998) of a grouping in this direction spread out in depth over a range larger than 1 kpc.
4.3 Distribution perpendicular to the Galactic plane
It was already demonstrated by a number of authors that spiral
arm tracers tend to lie below the Galactic plane for great distances
in the Carina direction (Graham 1970; Shobbrook & Lynga 1994 and the
references therein). Probably the most comprehensive investigation of
the Galactic warp in the southern sky that includes the Carina section
was presented by Reed (1996). His study, based on a sample of 1300 OB
stars with available UBV
photometry, found evidence of a warp
reaching -1.5 kpc at a galacto-centric distance of 15 kpc and
l=280
.
![]() |
Figure 4: Distance Z from the Galactic plane plotted against distance from the Sun for three longitude intervals. The solid line is the relation obtained by Graham (1970). The following symbols are used: plus symbols for stars of LC V-III with MV -3 mag and brighter; filled symbols for stars of LC V-III, with MV>-3 mag, open symbols for stars of LC I to II that are still close to the main sequence; and filled triangles for evolved stars of LC I to II. The 40 stars from Shobbrook & Lynga (1994) are shown with open-star symbols on the Z vs. r diagrams. The uncertainties in the stellar distances are the same as in Fig. 2. |
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As expected, in all three longitudinal intervals the stars less
luminous than -3 mag are found closer than 2 kpc in general, due to
the effect of the limiting magnitude of the survey. In the first
Galactic longitude range (284-288.6
), the majority of the intrinsically
bright stars (MV<-3) closely follow the relation proposed by Graham
(1970).
Our sample allows us to trace the outer edge of the Carina arm up to
6 kpc. At a distance of 6 kpc, the stars in the sample
show a
warp of about negative 200 pc, a value similar to the one that can
be
obtained from the plots presented by Reed (1996).
An interesting feature of the MV vs. (b-y)0 diagram for this
longitude range is the presence of very few stars in the -2 to -3 range in MV. In the Z vs. r plot, there is a clear spatial
separation of about 900-1000 pc between the intrinsically bright stars
(plus symbols) and the fainter stars (filled symbols). This feature is
also seen in the r vs. l plot (Fig. 3) and points out that an
inter-arm-like space exists between the nearby young structures and
the edge of the Carina arm within the formal Galactic plane. The
stars of LC I-II are quite spread out with no obvious concentration
along the edge. In the second longitude interval the sample still
follows the Graham's line and the warp can be traced up to 5 kpc. No
inter-arm space is obvious. There is a tendency of the evolved stars
of LC I-II to be located at and below the plane. In the third
longitude interval most of the intrinsically bright stars are located
below or above the plane and the sample does not follow the Graham's
line. Note that toward l=292 the sample is quite incomplete
and consists of mostly nearby stars. The stars located below the
formal plane are all found at longitudes larger than 293
and
indicate that the bending below the plane begins at 1.5 kpc at this
longitude.
4.4 The field between 284
-288.6
Galactic longitude
This longitudinal interval contains the outer edge of the Carina arm
parallel to the direction 287




In Fig. 5 different symbols are used to denote the apparent groups
that could be separated toward the edge based on the sample used in this subsection. The
group marked with plus-symbols (23 stars) is located at the average
coordinates l = 287.56,
b=-0.67
.
These coordinates are very
similar to those of the Car 1E group (l = 287.61
,
b = -0.68
,
at 2.64 kpc) from the list of Mel'nik
& Efremov (1995). This falls in the direction toward
Car as
well. According to the distances obtained here, these stars are spread
out between 2204 and 6404 pc, with an average of
pc.
Another apparent concentration is marked with filled squares (six
stars) at l = 287.01
and b=-0.41
and average distance of
pc. The significant spread in distance suggests that these
are not physical groups. The third apparent grouping, marked with open
triangles (16 stars) is found at l=285.83
and b=0.071
.
The
location of this group is similar to that of Car 1B at l = 285.98
,
b = 0.40
from the list of Mel'nik & Efremov (1995).
These stars are well grouped according to their individual
distances, and the density profile reveals one group at a median
distance of
(s.e.) pc.
![]() |
Figure 5:
Intrinsically bright (MV <-3 mag) stars of LC V to II in the field
between l=284 |
Open with DEXTER |
![]() |
Figure 6: Open clusters and giant molecular clouds in the field studied plotted in Galactic coordinates, and distance Z from the Galactic plane plotted against distance from Sun. Different symbols are used to mark clusters of different age, as indicated on the middle panel. The giant molecular clouds identified in the field are shown with open-star symbols. The solid line is the relation obtained by Graham (1970). |
Open with DEXTER |
Apparently this region is much more complex than harboring just one stellar association. It seems that it contains projections of stars located along the outer edge of the Carina arm. The spread of these stars along the line of sight is much more extended than the expected spread due to errors in distance determination. Ninety percent of these stars are O-type. It is highly likely that some of these apparent concentrations represent parts of long segments of the outer edge of the Carina arm.
4.5 Distribution of open clusters and giant molecular clouds toward Carina
With the aim of tracing the outer edge of the Carina
arm using different spiral structure indicators, the location of open
clusters and giant molecular clouds (GMC) are plotted in Fig. 6. The
data for the open clusters were extracted from the catalog of
Dias et al. (2003). The clusters are marked with different symbols
according to their age, as indicated on the panel. The data for the
GMC were selected from the work of Grabelsky et al. (1988). The plots provide
an impression about the Galactic stellar and molecular warp toward the
outer edge of the Carina arm. Almost all of the clusters younger than
6.8 Myr are closely associated with GMC. Interestingly, the young
clusters are all closely confined to the formal plane (b = 0), while
the clusters older than 7.6 Myr are found well below the plane for
distances greater than 1 kpc. This separation is best seen for the
field between 283
and 291
longitude and might indicate a presence of age
gradient in a direction perpendicular to the Galactic plane for this
longitude interval. The GMCs do not follow the outer edge as
delineated by Graham (1970), and the bending below the plane is much
less for these tracers than for the OB stars. The clusters also do not
convincingly follow the edge.
5 Conclusion
Precise homogeneous stellar distances and reddening were derived
for a sample of 598 O-B9-type stars in the field of the Carina spiral
feature. Photometry-derived parameters allowed us to study the
structure and characteristics of this segment of the Carina arm up to a
distance of 6 kpc. The main findings of this investigation are:
- 1.
- The distribution of the stars in this sample is consistent with the location of the apparent edge of the Carina arm as derived by Graham (1970).
- 2.
- In the 284
-289
longitude range an interarm space about 1 kpc wide was found beyond 850 pc from the Sun.
- 3.
- Toward l=291
(this is the direction of Car OB2) the young stars are spread out in depth over a range larger than 1 kpc, and the interarm space is no longer evident.
- 4.
- Toward the edge of the arm (l=287
) the warp of the Galactic plane could be traced up to 6 kpc, where it reaches negative 200 pc. Toward l=294
the sample stars do not delineate the edge of the arm any more and the bending below the plane begins at about 1500 pc from the Sun.
- 5.
- The field toward the edge of the Carina arm (this is the direction
toward
Car) seems to be much more complex than harboring just one OB association. It is likely that some of the apparent concentrations in this field represent parts of long segments of the edge of the Carina arm.
- 6.
- The distribution of the GMC and know open clusters in the field does not follow the edge of the arm as defined by the OB stars. The oldest open clusters are predominantly located below the formal plane, indicating a possible age gradient perpendicular to the formal Galactic plane.
Support for this research was provided by the National Science Foundation grant AST-0708950. N.K. acknowledges support from the SNC Endowed Professorship and the University of Wisconsin Oshkosh sabbatical program. The authors deeply thank Dr. B. Cameron Reed for helpful discussions. We are grateful to the referee Dr. Willem Jan de Wit for a number of valuable comments. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
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Footnotes
- ... B stars
- Table 4 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/514/A59
All Tables
Table 1: Completeness of the sample across the field.
Table 2: Stars originally classified as LC II in the Simbad data-base for which LC III was adopted.
Table 3:
Stars for which the
index calculated from
is used to obtain MV.
All Figures
![]() |
Figure 1: The histograms of the differences between the photometric distances obtained here and those by Graham (1970) ( top panel) and Shobbrook & Lynga (1994) ( middle panel). The bottom panel presents a comparison of the location of the stars plotted as a function of Galactic longitude using the distances obtained here (plus symbols) and those calculated by Shobbrook & Lynga (1994) (filled symbols). The overall uncertainty in the plotted stellar distances is about 15%. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Photometric distances plotted as a function of Galactic longitude for
different LC groups. In the first three plots filled dark symbols are
used for stars with
|
Open with DEXTER | |
In the text |
![]() |
Figure 3: Sample stars plotted in Galactic coordinates and the photometric distances and color excesses plotted as a function of the Galactic coordinates. The stars are marked with different symbols according to their LC as follows: filled squares - LC III-IV, IV, V; open triangles - LC II-III, III; open circles - the group without LC available, filled diamonds - LC Ia, Iab, Ib, II. The 40 stars from Shobbrook & Lynga (1994) are shown with open-star symbols on all diagrams. The uncertainties in the stellar distances are the same as in Fig. 2. |
Open with DEXTER | |
In the text |
![]() |
Figure 4: Distance Z from the Galactic plane plotted against distance from the Sun for three longitude intervals. The solid line is the relation obtained by Graham (1970). The following symbols are used: plus symbols for stars of LC V-III with MV -3 mag and brighter; filled symbols for stars of LC V-III, with MV>-3 mag, open symbols for stars of LC I to II that are still close to the main sequence; and filled triangles for evolved stars of LC I to II. The 40 stars from Shobbrook & Lynga (1994) are shown with open-star symbols on the Z vs. r diagrams. The uncertainties in the stellar distances are the same as in Fig. 2. |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Intrinsically bright (MV <-3 mag) stars of LC V to II in the field
between l=284 |
Open with DEXTER | |
In the text |
![]() |
Figure 6: Open clusters and giant molecular clouds in the field studied plotted in Galactic coordinates, and distance Z from the Galactic plane plotted against distance from Sun. Different symbols are used to mark clusters of different age, as indicated on the middle panel. The giant molecular clouds identified in the field are shown with open-star symbols. The solid line is the relation obtained by Graham (1970). |
Open with DEXTER | |
In the text |
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