# A New Galactic Wolf-Rayet Star in Centaurus

Authors: A. Roman-Lopes
Journal: ISRN Astronomy and Astrophysics
 (2011)

---

## Abstract

I communicate the detection of a new Galactic Wolf-Rayet star (WR60a) in Centaurus. The H- and
K-band spectra of WR60a show strong carbon near-infrared emission lines, characteristic of Wolf-Rayet stars of the
WC5-7 subtype. Adopting mean absolute magnitudeMK and mean intrinsic (J-KS) and (H-KS) colours, it was found that WR60a suffers a mean visual extinction of 3.8±1.3 magnitudes, being located at a probable heliocentric
distance of 5.2±0.8 Kpc, which for the related Galactic longitude (l=312) puts this star probably in the Carina-Sagittarius arm at about 5.9 kpc from the Galactic center. I searched for clusters in the vicinity of WR60a
and in principle found no previously known clusters in a search radius region of several tens arcminutes. The detection of a
well-isolated WR star induced us to seek for some still unknown cluster, somewhere in the vicinity of WR60a. From
inspection of 5.8 μm and 8.0 μm Spitzer/IRAC GLIMPSE images of the region around the new WR star,
strong mid-infrared extended emission at about 13.5 arcmin south-west of WR60a was found.
The study of the H-KS colour
distribution of point sources associated with the extended emission reveals the presence of a new Galactic cluster
candidate probably formed by at least 85 stars.


---

## Body

## 1. Introduction

Despite the important role that WR stars probably play in shaping both Galactic structure and chemical evolution, the total number of WR stars in the Milk Way is still an open issue. Shara et al. [1] and Van Der Hucht. [2] estimate a number between 1000 and 2500 WR stars to be located within the Galaxy, which compared to the about 300 known Galactic WR stars [3] indicates that, up to date, there still a large number of such stars to be discovered in our Galaxy. One reason for this comes from the fact that dust obscuration makes hard to observe WR stars in the optical window through the entire Galactic plane. On the other hand, infrared observations can provide the means for finding a significant fraction of the remaining population of obscured Galactic WR stars. Indeed, in the near-infrared (NIR) window, H and K band spectroscopy may be used to properly identify and classify the new Galactic WR stars, accordingly to the known WC, WN, and WO subtypes [4–6].In this work, I report the discovery of a new Wolf-Rayet star in Centaurus through the detection of its NIR carbon and He emission lines, using ESO-NTT-SOFI archival spectroscopic data. In Section2, I describe the observational data and the data reduction procedures, in Section 3, I present the results, and in Section 4, it is presented a summary of the work.


## 2. Observational Data and ReductionProcedures

### 2.1. Photometric Parameters of the Newly-Identified WR Star

Coordinates and photometric parameters for the new WR star are shown in Table1. The near-IR photometric data were taken from the Two-Micron All Sky Survey 2MASS, [7] using the NASA/IPAC Infrared Science Archive (http://irsa.ipac.caltech.edu/applications/BabyGator/), while the V-band photometry was obtained from the Naval Observatory Merged Astronomical Dataset (NOMAD) (http://www.nofs.navy.mil/data/fchpix/vo_nofs.html). The star was named WR60a, following the common practice to giving numbers to Galactic WR stars in RA order, with further additions between integers from Van Der Hucht [2, 3]. A 2MASS KS band finding chart for this object is presented in Figure 1.Table 1
Some photometric parameters of the WR60a star. The near-IR photometric data were taken from the Two-Micron All Sky Survey (2MASS) using the NASA/IPAC Infrared Science Archive, while theV-band photometry was obtained from the Naval Observatory Merged Astronomical Dataset (NOMAD). For the derived spectral type, visual extinction, and heliocentric distance, see the text.
IDRADecVJHKsSp typeAV (mag)d (Kpc)(J2000)(J2000)WR60a14:06:03.61−60:27:29.515.3510.8410.129.39WC5-73.8±1.35.2±0.8Figure 1
The 4 arcmin × 4 arcmin 2MASSKS band finding chart for the newlydiscovered Wolf-Rayet star WR60a. North is to the top, East to the left.


### 2.2. Near-Infrared Spectroscopic Observations

In this work, I used ESO archival data (http://archive.eso.org/eso/eso_archive_main.html) obtained with the SofI instrument [8], coupled to the 3.6 m NTT telescope. The spectra were taken as part of the ESO program 075.D-0210(A) (PI A.P. Marston and collaborators), with the targets being selected according to the technique presented by Hadfield et al. [9]. A summary of the spectroscopic dataset is presented in Table 2.Table 2
Summary of the NTT/SofI dataset used in this work.
Date2005-06-23TelescopeNTTInstrumentSofIGrismGRSlit (arcsec)0.6×290Resolution1000Coverage (μm)1.53–2.52Seeing (arcsec)1-2


### 2.3. Data Reduction

The raw spectra were reduced following the NIR reduction procedures presented by Roman-Lopes [10], shortly described here. The two-dimensional frames were sky subtracted for each pair of images taken at the two nod positions A and B, followed by division of the resultant image by a master flat. The multiple exposures were combined, followed by one-dimensional extraction of the spectra. Thereafter, wavelength calibration was applied using the sky lines; the typical error (1-σ) for this calibration was ~21 Å. Telluric atmospheric correction done using H- and K-band spectra of A and B type stars completed the reduction process.


## 2.1. Photometric Parameters of the Newly-Identified WR Star

Coordinates and photometric parameters for the new WR star are shown in Table1. The near-IR photometric data were taken from the Two-Micron All Sky Survey 2MASS, [7] using the NASA/IPAC Infrared Science Archive (http://irsa.ipac.caltech.edu/applications/BabyGator/), while the V-band photometry was obtained from the Naval Observatory Merged Astronomical Dataset (NOMAD) (http://www.nofs.navy.mil/data/fchpix/vo_nofs.html). The star was named WR60a, following the common practice to giving numbers to Galactic WR stars in RA order, with further additions between integers from Van Der Hucht [2, 3]. A 2MASS KS band finding chart for this object is presented in Figure 1.Table 1
Some photometric parameters of the WR60a star. The near-IR photometric data were taken from the Two-Micron All Sky Survey (2MASS) using the NASA/IPAC Infrared Science Archive, while theV-band photometry was obtained from the Naval Observatory Merged Astronomical Dataset (NOMAD). For the derived spectral type, visual extinction, and heliocentric distance, see the text.
IDRADecVJHKsSp typeAV (mag)d (Kpc)(J2000)(J2000)WR60a14:06:03.61−60:27:29.515.3510.8410.129.39WC5-73.8±1.35.2±0.8Figure 1
The 4 arcmin × 4 arcmin 2MASSKS band finding chart for the newlydiscovered Wolf-Rayet star WR60a. North is to the top, East to the left.


## 2.2. Near-Infrared Spectroscopic Observations

In this work, I used ESO archival data (http://archive.eso.org/eso/eso_archive_main.html) obtained with the SofI instrument [8], coupled to the 3.6 m NTT telescope. The spectra were taken as part of the ESO program 075.D-0210(A) (PI A.P. Marston and collaborators), with the targets being selected according to the technique presented by Hadfield et al. [9]. A summary of the spectroscopic dataset is presented in Table 2.Table 2
Summary of the NTT/SofI dataset used in this work.
Date2005-06-23TelescopeNTTInstrumentSofIGrismGRSlit (arcsec)0.6×290Resolution1000Coverage (μm)1.53–2.52Seeing (arcsec)1-2


## 2.3. Data Reduction

The raw spectra were reduced following the NIR reduction procedures presented by Roman-Lopes [10], shortly described here. The two-dimensional frames were sky subtracted for each pair of images taken at the two nod positions A and B, followed by division of the resultant image by a master flat. The multiple exposures were combined, followed by one-dimensional extraction of the spectra. Thereafter, wavelength calibration was applied using the sky lines; the typical error (1-σ) for this calibration was ~21 Å. Telluric atmospheric correction done using H- and K-band spectra of A and B type stars completed the reduction process.


## 3. Results

### 3.1. TheH- and K-Band Spectra of WR60a

TheH- and K-band spectra of WR60a are shown in Figure 2, with the main helium and carbon emission lines identified by labels. From an inspection of the this figure, we can see that the carbon emission lines are very strong, with the most prominent being the CIv line at 2.076 μm. On the other hand, from a comparison of the WR60a K-band spectrum with those from the spectral atlas of WRs stars of Figer et al. [11], we might conclude that this new WR star is probably of the WC5-7 subtype. Indeed, from the ratio (3.7) of the CIv 2.076 μm and CIII 2.110 μm equivalent widths (EWs), one can get the same conclusion [12].The continuum normalizedH- and K-band spectra of the new Wolf-Rayet star WR60a.
(a)(b)


#### 3.1.1. A Probable Nondusty WC Star

Late-type WC stars sometimes are surrounded by circumstellar dust (which is believed to be produced by interaction with an OB binary companion), whose thermal emission may contribute to the underlying NIR continuum. As can be noticed in Figure2, the K-band carbon lines of WR60a do not seem to suffer such effect in its underlying continuum. In one hand, the observed NIR colours of WR60a are compatible with that for a WC5-7 WR star ((J-KS)0=0.62,(H-KS)0=0.58—[12]), reddened by 3.8±1.3 mag in the V band [13]. On the other hand, the absence of reduced line strengths in principle can not be used to discard the presence of a line-of-sight/binary early-type companion since relatively short period late-type WC binaries like γ Vel (WC8+O) are known not to form dust.


#### 3.1.2. Heliocentric Distance to WR60a

Despite quantitative analysis of the newly discovered WR star is beyond the scope of this work, from the derived spectral type and associated NIR photometry, it is possible to obtain an estimate for the heliocentric distance to WR60a, considering the extinction law for NIR bands derived by Indebetouw et al. [13] and following the procedure described by Mauerhan et al. [6]. I used the mean values for absolute K-band magnitude (MK=-4.59) and J-KS and H-KS colours (0.62 and 0.58, resp.) taken from Crowther et al. [12]. It was found a mean heliocentric distance of 5.2±0.8 kpc, which puts this WR star at about 5.9 kpc from the Galactic center, probably in the Carina-Sagittarius arm.


### 3.2. Cluster Candidates and Other WR Stars in the Vicinity of WR60a

I searched for cataloged clusters in the vicinity of WR60a and found no known clusters around it in a region of tens of arcminutes. In fact, the first known cluster is DBS2003 #135 [14] with coordinates 14:08:42, −61:10:36 and located at about 47 arcmin from the new WR star. Also from a search in the clusters candidate list of Mercer et al. [15], the closest one is their number #43 (α= 14:00:28, δ= −60:59:15—J2000) that is located at about 52 arcmin from WR60a.The presence of a well-isolated WR star naturally generates the question about the WR60a parental cluster candidate. In fact, the presence of such kind of star strongly suggests the existence of some nearby unknown stellar cluster. In order to address this question, I performed a visual search through 2MASS and Spitzer/IRAC images of the region towards the new WR star. I found no indication for the presence of clusters from a visual inspection of the 2MASS images. However, from the 5.8μm and 8.0 μm Spitzer/IRAC images, it can be noticed the presence of strong extended emission, south-west of WR60a. In Figure 3, I present a false-color image made using the 4.5 μm, 5.8 μm, and 8.0 μm Spitzer/IRAC images of this Galactic sector, taken by the GLIMPSE survey. There, it is clearly seen the presence of several filamentary structures distributed perpendicularly to the Galactic plane and extending at least to b~1.1. On the other hand, an inspection of the filamentary region indicates the existence of an apparent concentration of near- to mid-infrared point sources around the coordinates (J2000) 14:05:05.42, −60:31:22.9, and 14:05:35.07, −60:40:30.5 (hereafter named cluster candidate #1 and cluster candidate #2—see Figure 3), both located at angular distances of 8 arcmin and 13.5 arcmin, respectively, from WR60a.Figure 3
The Spitzer/IRAC 4.5μm (blue), 5.8 μm (green), and 8.0 μm (red) false-color image of the region around WR60a.Finally, I also searched for other known Wolf-Rayet stars in the vicinity of WR60a; however, only two were found at angular distances greater than a degree! HD121194 (WC7) with coordinates 13:55:48.1, −61:09:50 (J2000) and SSTGLMCG313.8558+00.6489 (WN6) with coordinates 14:21:23.15, −60:18:04.1 (J2000).


#### 3.2.1. Known Astrophysical Sources Possibly Associated to the Cluster Candidates #1 and #2

Using the SIMBAD Astronomical Database, I took a look in the literature for astrophysical sources around the central coordinates of both cluster candidates and found no sources related to the cluster candidate #1. On the other hand, for the cluster candidate #2, there are two objects found at about 3 arcmin from its assigned coordinates. The first measuring about 1.7 arcmin × 1.1 arcmin is the bright nebula named GN J1405.9–6040 (14:05:58.53, −60:40:14.4 (J2000)), cataloged by kronberger et al. [16] from inspection of DSS-2 blue and red images. The second is the dark nebula SDC G311.862+0.854 (14:05:28.32, −60:43:37 (J2000)), which was cataloged by Peretto and Fuller [17] in a work aimed to identify Galactic infrared dark clouds (IRDCs), using Spitzer GLIMPSE and MIPSGAL data. The relative positions of this objects are indicated in Figure 3. It is interesting to notice that both nebula are placed at the border of the region assigned to the cluster candidate #2, which may be indication of ongoing star formation within the host molecular clouds. However, only the detection of extended mid-infrared emission is not enough to properly support the assumption of the presence of a cluster of stars there. In the next section, it is presented some results that favor this assumption for the cluster candidate #2.


#### 3.2.2. NIR Colour Study of the Stellar Population Associated to the Cluster Candidates #1 and #2

The detailed study of the stellar population associated with the two cluster candidates identified in the previous section is out of the scope of this work. However, even a simple analyses of the NIR colour distributions can provide additional clues to support (or not) the idea of existence of clusters of stars associated with the two selected regions in Figure3. In this sense, it was analyzed the H-KS colour distributions of point sources from three delimited areas, labeled cluster candidate #1, cluster candidate #2, and control field, the last centered at coordinates (J2000) 14:06:06.57, −60:28:46.2 and assumed to be mainly compound by Galactic field stars (with the obvious exception of WR60a). The study was done using the 2MASS H- and KS-band photometry of sources present in the three selected regions, considering circular fields of 4 arcmin radius (as illustrated in Figure 3 by the white large circles). The results are shown in Figure 4. From these diagrams, we can see that the stellar population in the direction of the cluster candidate #1 is mainly formed by Galactic field stars. In fact, its N(H-KS)×H-KS diagram presents an excess of field sources in the colour range 0.25≤H-KS≤0.75(91±32) that is fully compensated by the excess of cluster #1 sources in the range 0.75≤H-KS≤1.0(81±14). On the other hand, the N(H-KS)×H-KS diagram for sources in the cluster candidate #2 region clearly indicates an excess of objects with H-KS colours greater than 0.75 mag. Indeed, the number of extra sources found in the control region in the colour range 0.5≤H-Ks≤0.75(80±25) is much less than that computed for the colour range 0.75≤H-KS≤1.25(165±18). From this results, I can crudly estimate the number of probable members of the cluster candidate #2 at 85±31. Considering that the photometric completeness of the 2MASS survey in the H and KS bands restricts the analyses mainly to the more luminous sources, the true number of cluster members probably is greater than the inferred here. Of course, new further spectrophotometric studies are necessary to properly constrain the cluster population in this part of the Galaxy.TheH-KS colours histograms for the 2MASS sources detected in the direction of the two cluster candidates, together with that obtained from the control field (see Figure 3).
(a)(b)


## 3.1. TheH- and K-Band Spectra of WR60a

TheH- and K-band spectra of WR60a are shown in Figure 2, with the main helium and carbon emission lines identified by labels. From an inspection of the this figure, we can see that the carbon emission lines are very strong, with the most prominent being the CIv line at 2.076 μm. On the other hand, from a comparison of the WR60a K-band spectrum with those from the spectral atlas of WRs stars of Figer et al. [11], we might conclude that this new WR star is probably of the WC5-7 subtype. Indeed, from the ratio (3.7) of the CIv 2.076 μm and CIII 2.110 μm equivalent widths (EWs), one can get the same conclusion [12].The continuum normalizedH- and K-band spectra of the new Wolf-Rayet star WR60a.
(a)(b)


### 3.1.1. A Probable Nondusty WC Star

Late-type WC stars sometimes are surrounded by circumstellar dust (which is believed to be produced by interaction with an OB binary companion), whose thermal emission may contribute to the underlying NIR continuum. As can be noticed in Figure2, the K-band carbon lines of WR60a do not seem to suffer such effect in its underlying continuum. In one hand, the observed NIR colours of WR60a are compatible with that for a WC5-7 WR star ((J-KS)0=0.62,(H-KS)0=0.58—[12]), reddened by 3.8±1.3 mag in the V band [13]. On the other hand, the absence of reduced line strengths in principle can not be used to discard the presence of a line-of-sight/binary early-type companion since relatively short period late-type WC binaries like γ Vel (WC8+O) are known not to form dust.


### 3.1.2. Heliocentric Distance to WR60a

Despite quantitative analysis of the newly discovered WR star is beyond the scope of this work, from the derived spectral type and associated NIR photometry, it is possible to obtain an estimate for the heliocentric distance to WR60a, considering the extinction law for NIR bands derived by Indebetouw et al. [13] and following the procedure described by Mauerhan et al. [6]. I used the mean values for absolute K-band magnitude (MK=-4.59) and J-KS and H-KS colours (0.62 and 0.58, resp.) taken from Crowther et al. [12]. It was found a mean heliocentric distance of 5.2±0.8 kpc, which puts this WR star at about 5.9 kpc from the Galactic center, probably in the Carina-Sagittarius arm.


## 3.1.1. A Probable Nondusty WC Star

Late-type WC stars sometimes are surrounded by circumstellar dust (which is believed to be produced by interaction with an OB binary companion), whose thermal emission may contribute to the underlying NIR continuum. As can be noticed in Figure2, the K-band carbon lines of WR60a do not seem to suffer such effect in its underlying continuum. In one hand, the observed NIR colours of WR60a are compatible with that for a WC5-7 WR star ((J-KS)0=0.62,(H-KS)0=0.58—[12]), reddened by 3.8±1.3 mag in the V band [13]. On the other hand, the absence of reduced line strengths in principle can not be used to discard the presence of a line-of-sight/binary early-type companion since relatively short period late-type WC binaries like γ Vel (WC8+O) are known not to form dust.


## 3.1.2. Heliocentric Distance to WR60a

Despite quantitative analysis of the newly discovered WR star is beyond the scope of this work, from the derived spectral type and associated NIR photometry, it is possible to obtain an estimate for the heliocentric distance to WR60a, considering the extinction law for NIR bands derived by Indebetouw et al. [13] and following the procedure described by Mauerhan et al. [6]. I used the mean values for absolute K-band magnitude (MK=-4.59) and J-KS and H-KS colours (0.62 and 0.58, resp.) taken from Crowther et al. [12]. It was found a mean heliocentric distance of 5.2±0.8 kpc, which puts this WR star at about 5.9 kpc from the Galactic center, probably in the Carina-Sagittarius arm.


## 3.2. Cluster Candidates and Other WR Stars in the Vicinity of WR60a

I searched for cataloged clusters in the vicinity of WR60a and found no known clusters around it in a region of tens of arcminutes. In fact, the first known cluster is DBS2003 #135 [14] with coordinates 14:08:42, −61:10:36 and located at about 47 arcmin from the new WR star. Also from a search in the clusters candidate list of Mercer et al. [15], the closest one is their number #43 (α= 14:00:28, δ= −60:59:15—J2000) that is located at about 52 arcmin from WR60a.The presence of a well-isolated WR star naturally generates the question about the WR60a parental cluster candidate. In fact, the presence of such kind of star strongly suggests the existence of some nearby unknown stellar cluster. In order to address this question, I performed a visual search through 2MASS and Spitzer/IRAC images of the region towards the new WR star. I found no indication for the presence of clusters from a visual inspection of the 2MASS images. However, from the 5.8μm and 8.0 μm Spitzer/IRAC images, it can be noticed the presence of strong extended emission, south-west of WR60a. In Figure 3, I present a false-color image made using the 4.5 μm, 5.8 μm, and 8.0 μm Spitzer/IRAC images of this Galactic sector, taken by the GLIMPSE survey. There, it is clearly seen the presence of several filamentary structures distributed perpendicularly to the Galactic plane and extending at least to b~1.1. On the other hand, an inspection of the filamentary region indicates the existence of an apparent concentration of near- to mid-infrared point sources around the coordinates (J2000) 14:05:05.42, −60:31:22.9, and 14:05:35.07, −60:40:30.5 (hereafter named cluster candidate #1 and cluster candidate #2—see Figure 3), both located at angular distances of 8 arcmin and 13.5 arcmin, respectively, from WR60a.Figure 3
The Spitzer/IRAC 4.5μm (blue), 5.8 μm (green), and 8.0 μm (red) false-color image of the region around WR60a.Finally, I also searched for other known Wolf-Rayet stars in the vicinity of WR60a; however, only two were found at angular distances greater than a degree! HD121194 (WC7) with coordinates 13:55:48.1, −61:09:50 (J2000) and SSTGLMCG313.8558+00.6489 (WN6) with coordinates 14:21:23.15, −60:18:04.1 (J2000).


### 3.2.1. Known Astrophysical Sources Possibly Associated to the Cluster Candidates #1 and #2

Using the SIMBAD Astronomical Database, I took a look in the literature for astrophysical sources around the central coordinates of both cluster candidates and found no sources related to the cluster candidate #1. On the other hand, for the cluster candidate #2, there are two objects found at about 3 arcmin from its assigned coordinates. The first measuring about 1.7 arcmin × 1.1 arcmin is the bright nebula named GN J1405.9–6040 (14:05:58.53, −60:40:14.4 (J2000)), cataloged by kronberger et al. [16] from inspection of DSS-2 blue and red images. The second is the dark nebula SDC G311.862+0.854 (14:05:28.32, −60:43:37 (J2000)), which was cataloged by Peretto and Fuller [17] in a work aimed to identify Galactic infrared dark clouds (IRDCs), using Spitzer GLIMPSE and MIPSGAL data. The relative positions of this objects are indicated in Figure 3. It is interesting to notice that both nebula are placed at the border of the region assigned to the cluster candidate #2, which may be indication of ongoing star formation within the host molecular clouds. However, only the detection of extended mid-infrared emission is not enough to properly support the assumption of the presence of a cluster of stars there. In the next section, it is presented some results that favor this assumption for the cluster candidate #2.


### 3.2.2. NIR Colour Study of the Stellar Population Associated to the Cluster Candidates #1 and #2

The detailed study of the stellar population associated with the two cluster candidates identified in the previous section is out of the scope of this work. However, even a simple analyses of the NIR colour distributions can provide additional clues to support (or not) the idea of existence of clusters of stars associated with the two selected regions in Figure3. In this sense, it was analyzed the H-KS colour distributions of point sources from three delimited areas, labeled cluster candidate #1, cluster candidate #2, and control field, the last centered at coordinates (J2000) 14:06:06.57, −60:28:46.2 and assumed to be mainly compound by Galactic field stars (with the obvious exception of WR60a). The study was done using the 2MASS H- and KS-band photometry of sources present in the three selected regions, considering circular fields of 4 arcmin radius (as illustrated in Figure 3 by the white large circles). The results are shown in Figure 4. From these diagrams, we can see that the stellar population in the direction of the cluster candidate #1 is mainly formed by Galactic field stars. In fact, its N(H-KS)×H-KS diagram presents an excess of field sources in the colour range 0.25≤H-KS≤0.75(91±32) that is fully compensated by the excess of cluster #1 sources in the range 0.75≤H-KS≤1.0(81±14). On the other hand, the N(H-KS)×H-KS diagram for sources in the cluster candidate #2 region clearly indicates an excess of objects with H-KS colours greater than 0.75 mag. Indeed, the number of extra sources found in the control region in the colour range 0.5≤H-Ks≤0.75(80±25) is much less than that computed for the colour range 0.75≤H-KS≤1.25(165±18). From this results, I can crudly estimate the number of probable members of the cluster candidate #2 at 85±31. Considering that the photometric completeness of the 2MASS survey in the H and KS bands restricts the analyses mainly to the more luminous sources, the true number of cluster members probably is greater than the inferred here. Of course, new further spectrophotometric studies are necessary to properly constrain the cluster population in this part of the Galaxy.TheH-KS colours histograms for the 2MASS sources detected in the direction of the two cluster candidates, together with that obtained from the control field (see Figure 3).
(a)(b)


## 3.2.1. Known Astrophysical Sources Possibly Associated to the Cluster Candidates #1 and #2

Using the SIMBAD Astronomical Database, I took a look in the literature for astrophysical sources around the central coordinates of both cluster candidates and found no sources related to the cluster candidate #1. On the other hand, for the cluster candidate #2, there are two objects found at about 3 arcmin from its assigned coordinates. The first measuring about 1.7 arcmin × 1.1 arcmin is the bright nebula named GN J1405.9–6040 (14:05:58.53, −60:40:14.4 (J2000)), cataloged by kronberger et al. [16] from inspection of DSS-2 blue and red images. The second is the dark nebula SDC G311.862+0.854 (14:05:28.32, −60:43:37 (J2000)), which was cataloged by Peretto and Fuller [17] in a work aimed to identify Galactic infrared dark clouds (IRDCs), using Spitzer GLIMPSE and MIPSGAL data. The relative positions of this objects are indicated in Figure 3. It is interesting to notice that both nebula are placed at the border of the region assigned to the cluster candidate #2, which may be indication of ongoing star formation within the host molecular clouds. However, only the detection of extended mid-infrared emission is not enough to properly support the assumption of the presence of a cluster of stars there. In the next section, it is presented some results that favor this assumption for the cluster candidate #2.


## 3.2.2. NIR Colour Study of the Stellar Population Associated to the Cluster Candidates #1 and #2

The detailed study of the stellar population associated with the two cluster candidates identified in the previous section is out of the scope of this work. However, even a simple analyses of the NIR colour distributions can provide additional clues to support (or not) the idea of existence of clusters of stars associated with the two selected regions in Figure3. In this sense, it was analyzed the H-KS colour distributions of point sources from three delimited areas, labeled cluster candidate #1, cluster candidate #2, and control field, the last centered at coordinates (J2000) 14:06:06.57, −60:28:46.2 and assumed to be mainly compound by Galactic field stars (with the obvious exception of WR60a). The study was done using the 2MASS H- and KS-band photometry of sources present in the three selected regions, considering circular fields of 4 arcmin radius (as illustrated in Figure 3 by the white large circles). The results are shown in Figure 4. From these diagrams, we can see that the stellar population in the direction of the cluster candidate #1 is mainly formed by Galactic field stars. In fact, its N(H-KS)×H-KS diagram presents an excess of field sources in the colour range 0.25≤H-KS≤0.75(91±32) that is fully compensated by the excess of cluster #1 sources in the range 0.75≤H-KS≤1.0(81±14). On the other hand, the N(H-KS)×H-KS diagram for sources in the cluster candidate #2 region clearly indicates an excess of objects with H-KS colours greater than 0.75 mag. Indeed, the number of extra sources found in the control region in the colour range 0.5≤H-Ks≤0.75(80±25) is much less than that computed for the colour range 0.75≤H-KS≤1.25(165±18). From this results, I can crudly estimate the number of probable members of the cluster candidate #2 at 85±31. Considering that the photometric completeness of the 2MASS survey in the H and KS bands restricts the analyses mainly to the more luminous sources, the true number of cluster members probably is greater than the inferred here. Of course, new further spectrophotometric studies are necessary to properly constrain the cluster population in this part of the Galaxy.TheH-KS colours histograms for the 2MASS sources detected in the direction of the two cluster candidates, together with that obtained from the control field (see Figure 3).
(a)(b)


## 4. Summary

In this work, the detection of a new Galactic Wolf-Rayet star in the direction of Centaurus is reported. TheH- and K-band spectra of WR60a indicate that the star probably belongs to the WC5-7 subtype. From the derived spectral type and associated NIR photometry, it was computed a probable heliocentric distance of 5.2±0.8 Kpc, which for the related Galactic longitude (l=312) puts this WR star at about 5.9 kpc from the Galactic center, probably in the Carina-Sagittarius arm.I searched for clusters in the vicinity of WR60a and in principle found no known cataloged clusters in a radius search region of several tens of arcminutes. On the other hand, I also searched for other known Wolf-Rayet stars in the vicinity of WR60a, with no detections inside a one-degree search radius!The detection of a well-isolated WR star naturally leaved us to seek for some still unknown cluster, somewhere in the vicinity of WR60a. From visual inspection of 5.8μm and 8.0 μm Spitzer/IRAC GLIMPSE images of the region around the new WR star, it was found strong mid-infrared extended emission produced by filamentary structures oriented perpendicularly to the Galactic plane. The study of the the H-KS colour distributions of point sources associated with the extended emission indicates the presence of a new Galactic cluster candidate (central coordinates (J2000) 14:05:35.07, −60:40:30.5) placed at about 13.5 arcmin south-west of WR60a, for which I estimate a lower limit of 85±31 cluster members.



---

*Source: 632850-2011-09-14.xml*