New Wolf-Rayet stars in Circinus

# Discovery of two Galactic Wolf-Rayet stars in Circinus

A. Roman-Lopes
Physics Department - Universidad de La Serena - Cisternas, 1200 - La Serena - Chile
roman@dfuls.cl
###### Abstract

I report the discovery of two new Galactic Wolf-Rayet stars in Circinus via detection of their C, N and He Near-Infrared emission lines, using ESO-NTT-SOFI archival data. The H- and K-band spectra of WR67a and WR67b, indicate that they are Wolf-Rayet stars of WN6h and WC8 sub-types, respectively. WR67a presents a weak-lined spectrum probably reminiscent of young hydrogen rich main-sequence stars such as WR25 in Car OB1 and HD97950 in NGC3603. Indeed, this conclusion is reinforced by the close morphological match of the WR67a H- and K-band spectra with that for WR21a, a known extremely massive binary system. WR67b is probably a non-dusty WC8 Wolf-Rayet star that has a estimated heliocentric distance of 2.70.9 kpc, which for its Galactic coordinates, puts the star probably in the near portion of the Scutum-Centaurus arm.

###### keywords:
Stars: Wolf-Rayet; Infrared: stars
pagerange: Discovery of two Galactic Wolf-Rayet stars in CircinusLABEL:lastpagepubyear: 2010

## 1 Introduction

Very massive stars are key actors in the energy balance and chemical evolution of the Galaxy. Their powerful winds, massive outflows and expanding Hii regions inject large quantity of momentum and energetic ultraviolet (UV) photons into the Galactic interstellar medium (ISM). Wolf-Rayet (WR) stars, the chemically evolved descendants of the most massive O type stars, have been suggested as possible precursors of core-collapse supernovae of types Ib and Ic (Hadfield et al., 2007). As consequence, they are the main generators of alpha elements (such C, N, O, etc) and due to their short life time (considering the age of the Galaxy), they quickly enrich (through supernova explosions) the ISM with large quantity of heavy elements (Crowther, 2007).

Despite the dominant role that WR stars probably play in shaping both, the Galactic structure and its chemical evolution, the total number of WR stars and their spatial distribution in the Milk Way is still an open issue. Shara et al. (1999); van der Hucht (2001) estimate a number between 1000-2500 WR stars to be located within the Galaxy. The last census on the Wolf-Rayet Galactic population was made by van der Hucht (2006), which computed 298 as the known WR stars in the Galaxy. I searched in the literature for new discoveries (see Table 1), and found that up to date, approximately 100 new Galactic members were discovered. The total number of 395 known Galactic WR stars suggest that we still have a large number of such stars to be discovered in the Galaxy. One reason for this issue, comes from the fact that dust obscuration makes impossible to observe such stars in the optical window through the entire Galactic plane. In this sense, 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 (Eenens et al., 1991; Crowther & Smith, 1996; Indebetouw et al., 2005).

In this paper I report two newly-discovered Wolf-Rayet stars in Circinus via detection of their NIR C, N and He emission lines, using ESO-NTT-SOFI archival data. In section 2 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 ESO archival data and reduction procedure

In this work I used ESO archival spectroscopic data obtained with the SofI instrument (Son of ISAAC - Moorwood, Cuby & Lidman 1998, 1998), coupled to the 3.6m 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 accordingly the technique presented by Hadfield et al. (2007). A summary of the spectroscopic dataset is presented in Table 2.

The raw frames were reduced following the NIR reduction procedures presented by Roman-Lopes (2009), and briefly describe 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 obtained using the IDENTIFY/DISPCOR IRAF tasks applied to a set of OH sky line spectra (each with about 35 sky lines in the range 15500A-23000A). The typical error (1-) for this calibration process is estimated as 20 Å, which corresponds to half of the mean FWHM of the OH lines in the mentioned spectral range. Telluric atmospheric corrections were done using H- and K-band spectra of B type stars. The photospheric absorption lines present in the high signal-to-noise telluric spectra, were subtracted from a careful fitting (from the use of Voigt and Lorentz profiles) to the hydrogen and helium absorption lines (the He absorption lines are sometimes seem at 1.70m and 2.11m in case of earliest B-type stars), and respective adjacent continuum. This method works fine in case of moderate to early B-type stars because the hydrogen lines are not too strong, thus enabling a good determination of the adjacent continuum. On the other hand, the strong telluric absorption bands below about 1.55m make difficult the use of this method for lines below this wavelength.

## 3 Results and Discussion

### 3.1 Photometric parameters of the newly-identified Wolf-Rayet stars

Coordinates and photometric parameters for the newly discovered Wolf-Rayet stars are shown in Table 3. The near- to mid-IR photometric data were taken from the NASA/IPAC infrared science archive, while the B- and V-band photometry were obtained from the Naval Observatory Merged Astronomical Dataset (NOMAD). The stars were named WR67a and WR67b, following the common practice of to give numbers to Galactic WR stars in RA order, with further additions between integers from van der Hucht (2001), being done by adding a, b, c, etc.

### 3.2 NIR Spectral Classification

From the NTT-SofI H- and K-band spectra, I derived spectral types for the two new WR stars, using the NIR classification scheme proposed by Crowther et al. (2006).

#### 3.2.1 The WN Wolf-Rayet star

In Figure 1 I present the telluric corrected (continuum normalized) H- and K-band spectra of the WR67a star, together with the H- and K-band ESO archival spectra for WR21a, a well known massive Galactic binary star (Niemela et al., 2008). The strongest features are those corresponding to the blend of H and He emission lines at 1.736m and 2.167m, as well as, the Hei+Niii and Heii emission lines at 2.115m and 2.189m, respectively. I can also point out the presence of a less intense emission line due to Nv at 2.100m. From a quickly inspection of the WR67a NIR spectra, one can infer that it is probably a WR of the nitrogen sub-type. The list with the main detected lines and corresponding equivalent line widths is presented in Table 4.

We can see that WR67a has the Nv 2.100 m emission line in its K-band spectrum, which suggest a subtype earlier than WN7 (Crowther et al., 2006). Also, from the observed ratios of the Nv (2.100m) to Hei+Niii (2.115m), and Heii (2.189m) to Heii+Br (2.167m) equivalent widths (0.25 and 0.46, respectively), a WN6 subtype could be derived (Crowther et al., 2006). However, strong lined WN6 stars typically possess EW(HeII 2.189) of about 100Å, while weak lined WN6 stars possess EW(HeII 2.189) of about 50Å(e.g. Crowther & Smith 1996), versus 3.9Å, a value an order of magnitude lower than that expected for the weak-lined case.

Such kind of weak-lined spectrum as that for WR67a, is reminiscent of young hydrogen rich main-sequence WN6h stars such as HD93162 (WR25) in Car OB1 and HD97950 in NGC3603, that appear mimicking the spectral appearance of WR stars, due to their high-luminosities drive dense and fast winds (Grafener & Hamann, 2008). Indeed, this conclusion is reinforced by the close morphological match of the WR67a H- and K-band spectra with that for WR21a (see Figure 1), an extremely massive binary system (O3f/WN6ha + early O) for which Niemela et al. (2008) estimated M(WN6)>87M and M(O)>53M.

On the other hand, it is also possible to propose an alternative scenario in which WR67a is in reality a much lower mass weak-lined WN star, which has an emission line spectra diluted by the presence of a binary/line-of-sight companion. In this sense, further UV and optical spectroscopic survey are necessary to properly address this question.

#### 3.2.2 The WC Wolf-Rayet star

In Figure 2 I present the H- and K-band spectra of the WR67b star, with the main emission lines indicated by labels. From a qualitative inspection of the spectra, one can immediately conclude that WR67b is a carbon type WR star, as evidenced by the broad and strong Carbon emission lines at 2.076m (Civ) and 2.113m (Ciii). In Table 5 I present a summary of the main detected emission lines together with the corresponding equivalent widths.

Using the observed ratio of the Civ (2.076m) and Ciii (2.113m) equivalent widths (Table 5), and the NIR classification scheme for carbon WR stars summarized in Table 6 of Crowther et al. (2006), one can conclude that WR67b is a WR star of WC8 subtype. Late-type WC stars sometimes are surrounded by circumstellar hot dust whose thermal emission may contribute to the underlying NIR continuum. The observed NIR colours of WR67b are compatible with those for a non-dusty WC8 type WR star (J-H=0.05, H-K=0.38 - Crowther et al. (2006)), reddened by about 7-10 magnitudes in the V band. Also, the carbon lines detected in the K-band spectrum of WR67b (Figure 2), do not seem to be ”diluted” by continuum emission from circumstellar hot dust or by the presence of a line-of-sight companion. However, 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 Vel (WC8+O), are known not to form dust.

#### 3.2.3 Reddening and distance

Despite quantitative analysis of the two newly-discovered WR stars is beyond the scope of this work, from the derived spectral types and related NIR photometry, I computed mean values for reddening and heliocentric distances to each new WR star, using the intrinsic colours and absolute magnitudes given by Crowther et al. (2006, 2010), considering the extinction law for NIR bands derived by Indebetouw et al. (2005). For WR67a I used the average of the (J-K) intrinsic colours for WR10 (WN5h) and WR78 (WN7h), while the absolute M magnitude was computed from the average of the values from Table 4 presented by Crowther et al. (2010), considering an associated uncertainty of 0.5 magnitudes. The results are shown in Table 6.

For WR67a I computed distances and reddening taking into account the two scenarios mentioned in Section 3.2.1. In the first, the WN star is assumed to belongs to the WN6h sub-type for which M=-6.95 and (J-K)=0.06, while in the the second situation a WN6(weak) star for which M=-4.41 and (J-K)=0.18 is considered. When WR67a is considered a WN6h star, the resulting distance values is quite different than that for WR67b, as expected considering the remarkable difference between the luminosities of the two objects. In fact, while the WR67b star has a computed heliocentric distance of 2.70.9 kpc, which for Galactic coordinates G321.4 -0.4, puts it in the near side of the Scutum-Centaurus arm, WR67a (Galactic coordinates G321.1 -0.5) has a computed heliocentric distance of 10.52.1 kpc, which places it probably in the other side of the Galaxy, just at the far portion of the Scutum-Centaurus arm. On the other hand, in a scenario where one consider WR67a as a weak-lined WN star in which its emission line spectra seems diluted by the presence of a binary/line-of-sight companion, a much lower heliocentric distance of 3.4 kpc is found.

I searched for stellar clusters close to WR67a and WR67b, and found that they are located at about 10 arcsec and 15 arcmin, respectively, from the centre of the cluster candidate MCM2005b #60 (Mercer et al., 2005), that has central coordinates =15:16:36 and =-58:10:07 (J2000), which however is not obviously seem in the 2MASS K-band image. However, from the GLIMPSE 3.6m and 8.0m images of the field around WR67a (Figure 3), one can notice the presence of several point like sources (mainly in the 3.6m image) inside a cavity delineated by the hot dust extended emission, with WR67a being one of the most prominent. Also from the GLIMPSE m image of the region around the newly-discovered WN star, it can be seem the hot dust extended emission nicely tracing what seems to be the effects of a powerful stellar wind into the surrounding nebula. Indeed, WR67a appears as the unique point source placed near the centre of the cavity that is seem in the m image, which is probably associated to a Galactic Hii region detected by the H 109/H 110 radio recombination line survey performed by Caswell & Haynes (1987). Their source #143 (G321.1 -0.55), measuring about 3 arcmin 3 arcmin, has coordinates 15:16:36.3 -58:12:10 (J2000). It presents a flux density of 8.5 Jy at 5 GHz, and a radial velocity of -56 km/s, measured from the associated hydrogen recombination lines. From the use of the Galactic rotation curve, they computed far and near heliocentric distances of 11.6 kpc and 3.9 kpc, respectively. Interesting, both values are similar to those obtained in this work when WR67a is considered to be a WN6h (10.52.1 kpc) and a WN6(weak) (3.4 kpc) type WR star, respectively.

## 4 Summary

In this work I report the discovery of two new Galactic Wolf-Rayet stars in the direction of Circinus. The analysis of their ESO-NTT-SOFI H- and K-band spectra, indicate that WR67a and WR67b are WR stars belonging to the WN and WC types, respectively.

WR67a presents a weak-lined spectrum reminiscent of young hydrogen rich main-sequence WN6h stars such as HD93162 (WR25) in Car OB1 and HD97950 in NGC3603, which due to their high-luminosities drive dense and fast winds, appear mimicking the spectral appearance of WR stars. In one hand, this assumption is reinforced by the close morphological match of the WR67a H- and K-band spectra with that for WR21a, an extremely massive binary system (O3f/WN6ha + early O) for which Niemela et al. (2008) estimated M(WN6)>87M and M(O)>53M. In this case, an heliocentric distance of 10.52.1 kpc is computed, placing WR67a in the other side of the Galaxy, probably in the far portion of the Scutum-Centaurus arm. On the other hand, if we consider an alternative scenario where WR67a is supposed to be a weak-lined WN star showing an emission line spectra diluted by the presence of a binary/line-of-sight companion, a much lower heliocentric distance of 3.4 kpc is found.

WR67b is a WC8 Wolf-Rayet star probably placed at an heliocentric distance of 2.70.9 kpc, which for Galactic coordinates G321.4 -0.4, puts it probably at the near portion of the Scutum-Centaurus arm. Late-type WC stars sometimes are surrounded by circumstellar hot dust, but the observed NIR colours of WR67b seems to be compatible with those for a non-dusty WC8 type WR star reddened by about 7-10 magnitudes in the V band. Indeed, its K-band carbon lines do not seem to be ”diluted” by the presence of a line-of-sight companion. However, 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 (e.g. like Vel (WC8+O)), are known not to form dust.

## References

• Barniske (2008) Barniske, A., Oskinova, L. M., Hamann, W.-R. 2008, A&A, 486, 971
• Caswell & Haynes (1987) Caswell, J. L., Haynes, R. F. 1987, A&A, 171, 261
• Crowther & Smith (1996) Crowther, P.A. & Smith, L.J. 1996, A&A, 305, 541
• Crowther & Smith (1997) Crowther, P.A. & Smith, L.J. 1997, A&A, 320, 500
• Crowther et al. (2006) Crowther, Paul A., Hadfield, L. J., Clark, J.S., Negueruela, I., Vacca, W.D., 2006, MNRAS, 372, 1407
• Crowther (2007) Crowther, Paul A. 2007, MNRAS, 376, 248
• Crowther et al. (2010) Crowther, Paul A.,O. Schnurr, R. Hirschi, N. Yusof, R. J. Parker, S. P. Goodwin, H. A. Kassim 2010, MNRAS, in press, arXiv:1007.3284v1
• Crowther & Dessart (1998) Crowther, Paul A., Dessart, L. 1998, MNRAS, 296, 622
• Eenens et al. (1991) Eenens, P.R.J., Williams, P.M., Wade, R. 1991, MNRAS, 252, 300
• Figer, MacLean & Najarro (1997) Figer, D.F., McLean, I.S., Najarro, F. 1997, ApJ, 486, 420
• Grafener & Hamann (2008) Grafener, G.; Hamann, W.-R. 2008, A&A, 482, 945
• Gvaramadze et al. (2009) Gvaramadze, V. V.; Fabrika, S.; Hamann, W.-R.; Sholukhova, O.; Valeev, A. F.; Goranskij, V. P.; Cherepashchuk, A. M.; Bomans, D. J.; Oskinova, L. M. 2009, MNRAS, 400, 524
• Gvaramadze et al. (2010a) Gvaramadze, V. V.; Kniazev, A. Y.; Hamann, W.-R.; Berdnikov, L. N.; Fabrika, S.; Valeev, A. F. 2010a, MNRAS, 403, 760
• Hadfield et al. (2007) Hadfield, L. J., van Dyk, S. D., Morris, P. W., Smith, J. D., Marston, A. P., Peterson, D. E. 2007, MNRAS, 376, 248
• Hamann et al. (2006) Hamann, W.-R., Grafener, G., Liermann A. 2006, A&A, 457, 1015
• Indebetouw et al. (2005) Indebetouw, R., Mathis, J. S., Babler, B. L., Meade, M. R., Watson, C., Whitney, B. A., Wolff, M. J., Wolfire, M. G., Cohen, M., Bania, T. M., and 10 coauthors 2005, ApJ, 619, 931
• Maeder & Meynet (1994) Maeder, A., Meynet, G. 1994. A&A, 287, 803
• Mauerhan et al. (2010) Mauerhan, J. C.; Muno, M. P.; Morris, M. R.; Stolovy, S. R.; Cotera, A. 2010, ApJ, 710, 706
• Mercer et al. (2005) Mercer E.P., Clemens D.P., Meade M.R., Babler B.L., Indebetouw R., Whitney B.A., Watson, C., and 12 more authors, 2005, ApJ, 635, 560
• Meynet & Maeder (2005) Meynet, G. & Maeder, A., 2005 A&A, 429, 581
• Son of ISAAC - Moorwood, Cuby & Lidman 1998 (1998) Moorwood, A., Cuby, J.G., Lidman, C. 1998, Msngr, 91, 9M
• Niemela et al. (2008) Niemela V. S., Gamen R. C., Barba R. H., Fernandez Lejus E., Benaglia P., Solivella G. R., Reig P., Coe M. J., 2008, MNRAS,389, 1447
• Roman-Lopes (2009) Roman-Lopes, A. 2009, MNRAS, 398, 1368
• Schaerer & Vacca (1998) Schaerer, D., Vacca, W.D., 1998 ApJ, 497, 618
• Shara et al. (1999) Shara, Michael M., Moffat, Anthony F. J., Smith, Lindsey F., Niemela, Virpi S., Potter, Michael, Lamontagne, Robert 1999, AJ, 118, 390
• Shara et al. (2009) Shara, Michael M.; Moffat, Anthony F. J. 2009, AJ, 138, 402
• van der Hucht (2001) van der Hucht, K. A. 2001, NewAR, 45, 135
• van der Hucht (2006) van der Hucht, K. A. 2006, A&A, 458, 453
• Wachter et al. (2010) Wachter, Stefanie; Mauerhan, Jon C.; Van Dyk, Schuyler D.; Hoard, D. W.; Kafka, Stella; Morris, Patrick W. 2010, AJ, 139, 2330
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