A&A 404, 217-222 (2003)
J. B. Soares - E. Bica
Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil
Received 23 December 2002 / Accepted 25 March 2003
We employed J, H and photometry from the 2MASS Point Source Catalogue to study the embedded star clusters in the nebulae vdB-RN 92 and Gy 3-7, which are located in the molecular cloud Canis Majoris R1. We employed colour-colour and colour-magnitudes diagrams together with theoretical pre-main sequence isochrones to derive their fundamental parameters. Ages are based on the fraction of stars with anomalous colours, supposedly of types Herbig AeBe and T Tauri. The vdB-RN 92 cluster has an age of 5-7 Myr and the Gy 3-7 cluster 2 Myr. The average reddening values are AV=4.4 and AV=6.3, respectively for vdB-RN 92 and Gy 3-7. The distance found for vdB-RN 92 was 1.5 kpc which is, within uncertainties, compatible with previous estimates for the complex. Gy 3-7 also appears to be related to the CMaR1 complex. We conclude that CMaR1 is a very active star-forming site, now with four star clusters in early evolutionary stages.
Key words: Galaxy: open clusters and associations: individual: Gy 3-7, vdB-RN 92
IR photometry is very useful to detect sites of star formation, in particular, young clusters in nebulae or molecular clouds. In these regions many studies have revealed the presence of embedded star clusters (e.g. Hodapp 1994; Carpenter et al. 1993). Soares & Bica (2002) presented a study of two embedded star clusters in the molecular cloud complex CMaR1 using the Trapezium star cluster as a colour-magnitude diagram (CMD) template. The CMaR1 star forming region was first identified by van den Bergh (1966), as a group of stars embedded in reflection nebulosity. In the same area Clariá (1974a,b) identified an OB stellar association which appears to be a slightly evolved component of the star forming complex. Several Herbig AeBe stars occur in CMaR1. Clariá (1974b) and Shevchenko (1999) found distances of 1.15 kpc and 1.05 kpc to the association, respectively.
The CMaR1 molecular complex presents the possibility of other embedded star clusters or stellar groups. Thus it is important to further probe it with the tools of IR photometry. The reflexion nebula vdB-RN 92 was identified by van den Bergh (1966); it contains embedded stars, forming a small clustering as pointed out by himself. Gyulbudaghian (1984) identified a small nebula in CMaR1 - Gy 3-7, which was reported to contain a star cluster by Tapia et al. (1997).
According to the SIMBAD database (http://simbad.u-strasbg.fr) vdB-RN 92 includes the B1.5V star BD-11 1763, as well as the infrared source IRAS 07016-1129. Tapia et al. (1997) report young stellar objects in the range B1-B5 for Gy 3-7. The nebula also contains the infrared source IRAS 07069-1045.
The 2MASS (2 Micron All Sky Survey) Atlas and Point Source Catalogue are fundamental tools to probe the stellar content of star forming regions, and they are the result of an all-sky near infrared survey (Skrutskie et al. 1997). The effective wavelengths of the photometric bands are 1.25 m (J), 1.65 m (H) and 2.17 m (). The band is thus located slightly shortwards of the K band. The data (second incremental release) can be obtained in the web interface http://irsa.ipac.caltech.edu.
In the present study we analyse the stellar content of the nebulae vdB-RN 92 and Gy 3-7 by means of colour-colour and CMDs using the 2MASS Point Source Catalogue. In particular we verify the suggestion by van den Bergh of a clustering in the nebula vdB-RN 92. In Sect. 2 we describe the objects based on 2MASS and Digitized Sky Surveys imaging. In Sect. 3 we present the 2MASS photometric extractions in the bands . In Sect. 4 we discuss the analysis methods and the photometric diagrams of the embedded clusters in vdB-RN 92 and Gy 3-7. Finally, in Sect. 5 the concluding remarks of this work are given.
The clustering in vdB-RN 92 is located at J2000.0
band image of the region is presented in Fig. 1. A concentration of stars
occurs within a radius of 1.
|Figure 1: band 2MASS image of vdB-RN 92. Open circle indicates the object central part. Crosses indicate instrumental artifacts.|
|Figure 2: Same as Fig. 1 for Gy 3-7.|
|Figure 4: Same as Fig. 3 for Gy 3-7.|
The cluster or stellar group in Gy 3-7 is located at ) and its angular radius is . In Fig. 2 the image shows concentration of stars and some nebular emission and/or reflexion.
R band Digitized Sky Survey images http://cadcwww.dao.nrc.ca/cadcbin/getdss of vdB-RN 92 and Gy 3-7 are given in Figs. 3 and 4, respectively. The vdB-RN 92 image shows a concentrated group of bright stars standing out in a diffuse dust dominated region. The nebulous star located at NW of vdB-RN 92 is the Herbig Be star Z CMa which has a bipolar outflow (Poetzel et al. 1989). In the Gy 3-7 image what stands out is the dust refletion and/or gas emission component. Extinction estimates in the directions of the two objects can be obtained from Schlegel et al. (1998): AV = 9.5 for vdB-RN 92 and AV = 7.9 for Gy 3-7. Owing to the expected strong extinction the stellar content of the two nebulae requires IR photometry for detailed studies.
In Fig. 5 is shown a 12 m band IRAS image of CMaR1. This band is particularly sensitive to warm dust, and in turn to the presence of star formation. vdB-RN 92 corresponds to a small blob in the main body of CMaR1. Gy 3-7 corresponds to the faint blob to the east and outside the main body. The overall cloud appears to have several cores, probably caused by shock fronts.
We employed the Gator tool for Point Source Catalogue extractions, as provided in the 2MASS site. An extraction table gives for each star besides the J,H and magnitudes, the three corresponding colours, the respective errors, and J2000.0 coordinates. The 2MASS photometric errors in the present regions for each magnitude are basically the same as those presented in Soares & Bica (2002) for the regions of NGC 2327 and BRC 27. Essentially, the errors become important (0.1 mag and larger) for magnitudes fainter than . We applied a cutoff at for the stars to be studied in the colour-colour diagrams, for the sake of accuracy in their analyses. For comparison purposes we made extractions for the objects and their surrounding fields. Typical separations for objects and fields are . Table 1 condenses information on the extractions: target position and number of extracted stars for radii 1. Fields 1 to 4 are related to vdB-RN 92 and fields 5 to 8 to Gy 3-7. The numbers of stars in the cluster extractions exceed those of all fields.
The sensitivity increase of IR detectors provided new opportunities to observe and analyse the stellar content in molecular clouds. Regions of star formation contain many stars presenting IR excesses which are characteristic of very young objects. Colour-colour diagrams are a useful tool to deal with very young objects in the pre-main-sequence (PMS) stage (Carpenter et al. 1993). This method enables detections of band excesses, which originate in dust disks or envelopes of contracting objects. Large reddening values are obtained in these regions as compared to surrounding field stars.
Both vdB-RN 92 and Gy 3-7 contain dust embedded stars as revealed by reflection nebulae in the optical/near-IR and warm dust emission in the infrared (Sect. 2), probably in the stellar formation phase.
The analysis employs colour-colour diagrams and CMDs. Finally, PMS isochrones by Siess et al. (2000) are used. The empirical isochrone for an age of 1.5 Myr derived from a template cluster (Trapezium) in Soares & Bica (2002) turned out to be inappropriate for the present clusters, because they are in a later evolutionary stage.
Stars at formation stages (T Tauri and Herbig AeBe) can exhibit anomalous colours due the
created by the hot dust emission around them (Lada &
Adams 1992; Calvet et al. 1992).
colour-colour diagram we can diagnose this effect. By means of the percentage of
anomalous stars we can estimate the cluster or stellar group age, as described Lada et al. (1996).
This diagram can also give the mean reddening of the object. In the present analysis, stars with anomalous colours
were discarded from the calculation of the mean reddening.
|Name||(J2000)||(J2000)||n (r = 1)|
In Fig. 6 we show J,(J-H) CMDs of the cluster and the comparison fields 1 and 3 (Table 1). The cluster is more reddened than field 1 and slightly more reddened than field 3.
colour-colour diagram is shown in Fig. 7. The continuous curve
represents the intrinsic colours of main-sequence (MS) stars with spectral types from O3 to M5 (Schmidt-Kaler
1982). The dashed line denotes the reddened loci (Rieke & Lebofsky 1985) for a MS O3 star, while the point-dashed line is for an M5 giant.
The arrow indicates the extinction vector for AV=10. We applied a 2MASS sample cutoff at
to avoid errors larger than 0.1 mag. The figure shows a number of stars distributed along the reddening vector, and
some are little reddened and coincident with the field locus. The
mean reddening is AV = 4.4 considering only the stars along the reddening vector.
This reddening value corresponds to AJ= 1.21 and
E(J-H)=0.47. The reddening transformations employed were derived from the data in
Rieke & Lebofsky (1985) assuming
AV = 3.2E(B-V).
Some stars have
colours denoting infrared excess (below the dashed line).
The vdB-RN 92 cluster has 20% of stars with infrared excess, similarly to the IC 348 cluster (Lada & Lada 1995) implying an age of
|Figure 6: vdB-RN 92: J,(J-H) CMD of the cluster region (filled circles) and comparison fields (open diamonds). Field 1 corresponds to the left panel and field 3 to the right one. All extractions have radius 1. No cutoff was used.|
|Figure 7: vdB-RN 92: ( ) diagram for the cluster (filled circles) and comparison field 1 (open diamonds). Triangles are the four more luminous stars in the object. Reddening vector and reddening lines for M5 giant (dashed-pointed line) and O3 stars (dashed line) are shown. The continuous curve is the intrinsic distribution of spectral types. A cutoff at was used.|
|Figure 8: vdB-RN 92: J,(J-H) CMD of the cluster (filled circles) with PMS isochrones of 1 Myr (dashed line) and 7 Myr (dotted line). The ZAMS is represented by continuous line (Siess et al. 2000) and dashed-dotted line (Bertelli et al. 1994). Left panel presents the fit for the most massive star. Right panel presents the fit with AJ=1.21. Colour and magnitude errors are indicated.|
In the CMD analysis of the vdB-RN 92 cluster PMS isochrones of Siess et al. (2000) were used. These authors present isochrone grids for the range 0.1 to 7.0 and four different metallicities ( Z=0.001, 0.02, 0.03 and 0.04). For the present analyses we adopted the sollar metallicity isochrones. For more massive stars we include the Padova isochrone of 4 Myr (Bertelli et al. 1994) as complement to the Zero Age Main-Sequence (ZAMS) of Siess et al. (2000). The method of fraction of stars with infrared excess to determine ages is more appropriate than that of the isochrones, because differential reddening and age dispersion within the cluster hamper its application. Spectroscopic observations of the brightest star in vdB-RN 92 indicated spectral type B1.5 (Herbst et al. 1978). The colours and magnitudes of a B1.5 MS star (Schmidt-Kaler 1982) were used as constraint to the fit (Fig. 8 - left panel). The observed distance modulus is J-MJ= 11.16 and E(J-H)=0.11. The distance from the Sun found for vdB-RN 92 is kpc. Low mass stars cannot be described by the fit for the bright stars, suggesting differential reddening. This effect might occur due to a lower reddening in the line of sight of massive stars. In the colour-colour diagram (Fig. 7), the four brighter stars are near the locus of unreddened stars, while the faint ones are spread along the reddening lines. Between the deeply embedded phases within dust/molecular gas and an evolved cluster the interstellar material undergoes processes that certainly lead to non-isotropic dust distribution. These processes depend on the involved stellar masses. Low-mass protostars evolve much slower, release less radiative energy and drive less energetic winds (Boogert et al. 2000). The mean reddening found in the colour-colour diagram analysis was applied to the cluster CMD and the results are shown in Fig. 8 (right panel).
In Fig. 9 we show the J,(J-H) CMD for an extraction of
centered on Gy 3-7. We show equal size extractions for the comparison fields 5 and 6 (Table 1). Redder colours occur for the stars in the cluster region, suggesting larger reddening.
Note also the stronger reddening and differential reddening in Gy 3-7 as compared to vdB-RN 92 (Fig. 6).
|Figure 9: Gy 3-7: J,(J-H) CMD of the cluster region (filled circles) and comparison star fields (open diamonds). Field 5 corresponds to the left panel and field 6 to the right one. All extractions have radius 1. No magnitude cutoff was used.|
Figure 10 shows a ( ) diagram for the Gy 3-7 cluster, compared to that of field 5. A significant number of stars in the cluster present infrared excess ( - or below the dashed line). The remaining cluster stars present larger reddening values than those of the field.
The mean reddening value resulted AV = 6.3, which implies AJ=1.74 and E(J-H)=0.67. For this estimate we excluded the stars with infrared excess.
The Gy 3-7 cluster has 40% of its stars with infrared excess, a percentage slightly lower than that in the Taurus Dark Nebula (Kenyon & Hartmann 1995), suggesting an age of 2 Myr. For this calculation we minimized field contamination by discarding the stars with extinction similar to those of field stars.
In the literature two distances have been proposed to Gy 3-7. Wouterloot & Brand (1989) reported a kinematic distance of 1.41 kpc from CO observations. This distance would imply an association to CMaR1, with estimated distances in the range 1.05-1.2 kpc (Shevchenko 1999; Soares & Bica 2002). Tapia et al. (1997) suggested at least a factor two larger to explain ionizition in the nebula.
In Fig. 11 (left panel) we show a PMS fit to Gy 3-7 assuming a distance of 1.4 kpc
(Wouterloot & Brand 1989) and a reddening
E(J-H)=0.27which is appropriate to the brightest star. The latter star is located near the locus of unreddened stars
We conclude that this star is possibly a PMS around B5, hot enough (
K, Siess et al. 2000) to provide
ionization to the nebula, without the need of
a larger distance as given in Tapia et al. (1997). In Fig. 11 (right panel) we show the same plot of Fig. 11a but with a larger reddening
E(J-H)=0.67 (AJ=1.74 or AV=6.3) which is appropriate to the lower mass stars. Differential reddening is
important and several stars appear to have large (J-H) excesses denoting dust envelopes.
|Figure 10: Gy 3-7: ( ) diagram for the cluster (filled circles) and comparison field 5 (open diamonds). Triangle is the most luminous star in the object. Reference lines as in Fig. 7. A cutoff at was applied to minimize errors.|
Two embedded star clusters in CMaR1 were studied by means of 2MASS J,Hand photometry in the nebulae vdB-RN 92 and Gy 3-7. They are not massive clusters and there remains the possibility of classifying them as star clusters or stellar groups, in the sense of scarcely populated physical systems.
The vdB-RN 92 cluster diagram presents 20% of its stars with infrared excess, suggesting an age of 5-7 Myr similar to that of the IC 348 cluster (Lada & Lada 1995). The mean visible absorption is AV = 4.4. The estimated distance was kpc, where we used pre-main sequence isochrones and the most luminous star (B1.5) as constraint.
The Gy 3-7 cluster has 40% of its stars with infrared excess, implying an age of 2 Myr, likewise the Taurus Dark Nebula (Kenyon & Hartmann 1995). The mean visible absorption in Gy 3-7 is AV = 6.3, as derived from the colour-colour diagram. The kinematic distance of 1.4 kpc (Wouterloot & Brand 1989) appears to be compatible with that of the cluster, where the most luminous star (B5) is in the pre-main sequence phase, and hot enough to ionize the gas.
The results indicate that the vdB-RN 92 cluster and the Gy 3-7 cluster are in distinct evolutionary stages.
In both clusters there is evidence that the more massive stars are less reddened than low mass stars. This effect might be related to the way
which stars of different masses affect the surrounding interstellar medium.
|Figure 11: Gy 3-7: J,(J-H) CMD of the cluster (filled circles) with PMS isochrones of 1 Myr (dashed line) and 7 Myr (pointed line). The ZAMS is represented by continuous line (Siess et al. 2000) and dashed-dotted line (Bertelli et al. 1994). Left panel presents the fit for the distance found by Wouterloot & Brand (1989). Right panel presents the fit with AJ=1.74. Colour and magnitude errors are indicated.|
The CMaR1 cloud appears to be a very active site of star-formation. In addition to the overall formation in the association (Shevchenko 1999) there occur enhanced sites. These are the present two clusters and those in the nebulae NGC 2327 and BRC 27 (Soares & Bica 2002).
This publication makes use of data from the 2 Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. We employed data from the CDS database (Strasbourg). We also acknowledge support from the Brazilian Institutions CNPq and CAPES, in particular J.S. for a CNPq Ph.D. fellowship.