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A&A
Volume 531, July 2011
Article Number L12
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201117174
Published online 28 June 2011

© ESO, 2011

1. Introduction

The source IRAS 12556–7731 was first identified by Prusti et al. (1992) in an IRAS survey of pre-main sequence (PMS) stars in the Chamaeleon II (Cha II) cloud. The source was associated with a relatively bright (R ≈ 12 mag) off-cloud star. A later analysis of the star’s near-IR magnitudes led Larson et al. (1998) to conclude that its IR colours are more similar to those of giants than those of PMS stars. The source was then classified as a young stellar object candidate using selection criteria based on Spitzer mid-IR data (Alcalá et al. 2008), but it lacks the IR-excess (Larson et al. 1998; Alcalá et al. 2008) typical of young stars. Since lithium is efficiently destroyed by convective mixing in the interior of low-mass stars when the temperature at the bottom of the convective layer reaches about 2.5  ×  106 K, the presence of strong Li i λ6707.8 Å absorption represents an important criterion for identification of low-mass young stars. Thus, a late-type spectrum and the detection of a strong Li i λ6707.8 Å absorption in two VLT-FLAMES/Giraffe spectra, have led Spezzi et al. (2008) to assign a young stellar object nature to IRAS 12556–7731. Surprisingly, this star turned out to be over-luminous by about two orders of magnitude on the HR diagram with respect to other young stars in the Cha II cloud (Spezzi et al. 2008). This result and the conclusion by Larson et al. (1998) that IRAS 12556–7731 could be a giant star, triggered a new high-resolution spectroscopic study. We characterise the star as a lithium-rich M-type giant. Several spectroscopic studies of K-type giants in the past two decades have provided evidence of lithium enhancements in the atmosphere of these stars (Kumar et al. 2011,and references therein). We study IRAS 12556–7731 in the context of other well known lithium-rich giants and discuss possible mechanisms for its lithium enhancement.

Table 1

Physical parameters of IRAS 12556–7731.

thumbnail Fig. 1

Portion of the HARPS spectrum of IRAS 12556–7731 in the Na i D region. The M5 III best template (HD 175865) is overplotted (dotted line). A dwarf M star with nearly the same temperature (HD 173740) is also overplotted with a dashed line. The interstellar absorption components (IS) are also indicated.

2. HARPS spectroscopy

With the aim of ascertaining the nature of IRAS 12556–7731, two high-resolution (R  ~  110 000) spectra (range from 3800 Å to 6900 Å), obtained in February 2−3, 2011 with the HARPS (High Accuracy Radial velocity Planet Searcher) spectrograph at the ESO 3.6 m telescope in La Silla (Chile), were combined. The strong Li i absorption line at λ6707.8 Å was the first feature to be immediately confirmed, for which we measured an equivalent width of 550(± 10) mÅ. Likewise, the Hα line is in absorption. Overall, a number of strong molecular absorption bands, mainly of titanium oxide, can be identified, and they confirm it as a very cool object. The interstellar (IS) Na i D (λλ5890, 5996 Å) absorption components, distinguishable from the photospheric ones, are clearly detected (see Fig. 1). The narrower Na i D wings of IRAS 12556–7731 with respect to HD 173740 (see Fig. 1) definitely exclude it as a main sequence star.

The mean radial velocity of IRAS 12556–7731, as drawn from the HARPS spectra, is RV = 67.68  ±  0.02 km s-1, which is far beyond the range of the Chamaeleon region (~15  ±  2 km s-1; Covino et al. 1997). Likewise, the proper motion components of the star, μαcosδ  =   − 13.1  ±  5 mas yr-1, μδ  =  10.7  ±  5 mas yr-1, as retrieved from the PPMXL Catalog (Roeser et al. 2010), are not compatible with those of the Chamaeleon young stars (e.g., Frink et al. 1998). Therefore, we conclude that the kinematics of IRAS 12556–7731 is inconsistent with those of young stars in the Chamaeleon region and that the star is unrelated to the star-forming cloud. The detection of the interstellar Na i absorption components, for which we measure an RVIS ~ 14  ±  2 km s-1 consistent with the radial velocity of Chamaeleon, is an indication that such interstellar components can be produced by the Cha II cloud itself and that IRAS 12556–7731 must be located at a much greater distance. Because it is unrelated to the star-forming region, IRAS 12556–7731 is most likely a field giant star, far behind the Cha II cloud. This confirms the suggestion by Larson et al. (1998).

3. Physical parameters and lithium abundance

Using the combined (S/N  ≈  30) HARPS spectrum, we obtained first estimates of the physical parameters by a procedure outlined in detail in Appendix A. This procedure provides us with the best effective temperature, gravity, and metallicity by comparing the combined HARPS spectrum with template spectra of real stars with well known parameters via a χ2 minimization criterion. The derived stellar parameters come from a weighted mean of the parameters of the 50 reference stars (10 per each spectral region) that independently match the target spectrum most closely. The results are Teff  =  3460  ±  60 K, log g  =  0.6  ±  0.2, [Fe/H]  =   − 0.05  ±  0.10, and vsini  =  6.2  ±  3.0 km s-1. From the log g vs. Teff relationship by Houdashelt et al. (2000) for solar metallicity giants, we estimate log g(3500   K) ~ 0.4, in fair agreement with the value derived from the χ2 minimization.

3.1. Lithium abundance

As pointed out by Gratton & D’Antona (1989), a high value (~500 mÅ) of the λ6707.8 Å Li i line equivalent width implies that the resonance doublet should be strongly saturated and that deviations from LTE conditions may be important. This requires the use of other lithium lines. The spectral range covered by HARPS also allows us to investigate the λ6103.6 Å Li i line.

The Li abundance A(Li) was derived by spectral synthesis of the Li i 6103.6 Å line using the MOOG code (Sneden et al. 1973), which assumes LTE conditions, along with the GAIA model atmospheres (Brott & Hauschildt 2010, priv. comm.). The hyperfine line structure has been considered following the guidelines by Wahlgren (2005) to compute the atomic parameters. The atomic and molecular line lists were taken from the VALD1 database. The physical parameters derived from the χ2 minimization explained above were used as starting values for the synthesis. We let metallicity, vsini, A(Li), and microturbulence velocity ξ vary, while keeping Teff and log g fixed. The low temperature of the star makes the spectral synthesis rather difficult, because of the uncertainty on continuum determination caused by several overlapping molecular lines. The continuum was determined by a spline fit made after visually selecting regions free of absorption lines. We estimated that the uncertainty on the continuum determination, which is the main source of error on A(Li), is less than 5%. The results are shown in Fig. 2. From our best fit, we obtained values of A(Li)  =  2.4  ±  0.2, [Fe/H]  =   −0.1  ±  0.2, and vsini = 9  ±  2 km s-1 for a microturbulence velocity ξ = 0.8  ±  0.2 km s-1. The [Fe/H] and vsini values are in good agreement with those from the χ2 minimization, so average values were computed. The final adopted physical parameters are reported in Table 1.

An attempt at spectral synthesis of the lithium line at 6707.8 Å with MOOG (using the Reddy et al. 2002 line list implemented within the VALD database) resulted in large residuals (cf. Fig. 4), mainly owing to non-LTE conditions, such as the effects of over-ionization, and line asymmetry due to the convective motions, which mainly influence the λ6707.8 Å Li i line formation in very cool stars (Carlsson et al. 1994). Since the EW of this line could be measured with high accuracy, we could estimate the non-LTE Li abundance through extrapolating the curves of growth by Lind et al. (2009) to a temperature of  ~3500 K, which yield A(Li)  ~  2.5.

We thus conclude that a reliable value for the lithium abundance of IRAS 12556–7731 is A(Li)  =  2.4  ±  0.2. As a result, the low temperature and high lithium abundance of the star make IRAS 12556–7731 the coolest lithium-rich giant known to date. As shown below, our determinations of temperature and gravity place the star close to the tip of the red giant branch (RGB) on the HR diagram.

thumbnail Fig. 2

Portion of HARPS spectrum in the interval around the lithium λ6103.6 Å absorption line. The top panel shows the synthetic spectra for three values of A(Li) at fixed metallicity, while the lower one shows the synthetic spectra for three values of metallicity at fixed A(Li). The best fit is for a sligthly subsolar metallicity and A(Li) = 2.4.

4. Discussion and conclusions

The stellar parameters of IRAS 12556–7731 indicate that the star is a lithium-rich M-giant. To investigate its evolutionary status in more detail, we used the tracks and isochrones by Girardi et al. (2000) for solar metallicity stars. A comparison of the position of IRAS 12556–7731 in the log g vs. log Teff diagram (Fig. 3) showed that the physical parameters are consistent with an age  ~10 Gyr. Reasonable values for the stellar luminosity and mass at that age, which are consistent with log Teff, are log (L/L⊙)  =  2.99  ±  0.15 and M/M⊙  =  1.0  ±  0.2, respectively. The position of IRAS 12556–7731 on the HR diagram is shown in Fig. 3, along with several lithium-rich stars, as compiled by Kumar et al. (2011). Most of the known lithium-rich giants are concentrated within a luminosity range of 1.3  <  log (L/L⊙)  <  2, with only a minority having log (L/L⊙)  >  2.2. Among these luminous K-type objects, HD 39853 is the coolest one; nevertheless, IRAS 12556–7731 is about 450 K cooler, placing it among the least massive and most luminous lithium-rich giants known so far. Being close to the tip of the RGB, one should then consider three possibilities for the evolutionary stage of the star: i) giant branch ascent, i.e. H-shell burning phase; ii) AGB phase; or iii) post He-core flash. Unfortunately, the CNO abundances and the 12C/13C carbon isotopic ratios, tracers of the degree of mixing that provide further constraints on the evolutionary status, cannot be derived because the spectral range of HARPS does not include the appropriate wavelength range.

thumbnail Fig. 3

Upper panel. The log g versus log Teff diagram. The Girardi et al. (2000) isochrones for three different ages are overplotted. The black dot represents the position of IRAS 12556–7731. Lower panel. HR diagram of several Li-rich giants. The evolutionary tracks by Girardi et al. (2000) for several masses as labelled are represented with continuous lines. The lithium-rich K-type giants (Kumar et al. 2011) are over-plotted with open circles. The asterisk represents HD 39853, while the position of IRAS 12556–7731 is indicated by the big black dot.

Assuming a distance dCha   II  =  178 pc, Spezzi et al. (2008) have derived a luminosity log (L/L⊙)  ≈  1. By comparing it with the luminosity estimated above, we conclude that IRAS 12556−7731 should be located at d  ≈  1.75 kpc from the Sun. By adopting this distance and using the HARPS radial velocity and the proper motion components (cf. Sect. 2), the resulting spatial velocity components of the star in a left-handed coordinate system are (U,V,W)  =  (+30, −121, +79) km s-1, where U, V, and W are directed towards the Galactic anti-centre, the Galactic rotation direction, and the North Galactic Pole, respectively. According to the criteria of Oort (1926)2, IRAS 12556–7731 can thus be considered as a high-velocity star. The Galactic latitude, distance, and kinematics of the star imply that it most likely belongs to the old thin-disk population, consistent with its almost solar metallicity. But what is the cause of its high lithium content?

Three possible scenarions can be considered to explain the high lithium abundance observed in IRAS 12556–7731: i) the star somehow preserved the original lithium in its atmosphere; ii) lithium has been regenerated in later evolutionary stages by the Cameron-Fowler mechanism3 (Cameron & Fowler 1971); iii) lithium was enhanced by the engulfment of a brown dwarf or planetary companion.

As discussed in Fekel & Balachandran (1993), the scenario of the preservation of initial lithium in red giants is very unlikely. They also note that high lithium abundance was not revealed in a sample of 200 F-type stars with masses between 1 and 2 M⊙, just evolved off the main sequence. As they point out, if anything, lithium preservation might eventually work in stars of the early-F and A types, that are more massive than IRAS 12556–7731. As a solar mass star, the initial lithium was most likely burned during the pre-main sequence phase.

Depending on the stellar mass and luminosity, the production of lithium via the Cameron-Fowler mechanism supossedly occurs both at the RGB luminosity function bump (Charbonnel & Balachandran 2000) and during the He-core flash (Kumar et al. 2011). It is possible that lithium was synthesized in IRAS 12556–7731 by the Comeron-Fowler mechanism during the luminosity bump, but most likely it had already been destroyed as the star evolved up to the RGB. Although the Sackmann & Boothroyd (1999) model predicts that a high lithium abundance may be preserved all the way up the RGB, their parameterization requires very high mixing rates. It was assumed that rotation could provide such rates, but Palacios et al. (2006) find that a self-consistent model of rotational mixing cannot generate enough circulation to account for the mechanism working efficiently. It has been suggested (de la Reza et al. 1996) that the IR-excess observed in some lithium-rich giants may be due to a dust shell possibly also generated via the Cameron-Fowler mechanism, but for IRAS 12556–7731 there is no evidence of IR excess (Larson et al. 1998; Alcalá et al. 2008). On the other hand, it is unlikely that, assuming an AGB status for the star, lithium has been synthesized during the He-flash phase, because such a process should work for stars within a narrow mass range around 2 M⊙ (Kumar et al. 2011). A pure Cameron-Fowler mechanism should only provide 7Li, with no 6Li. An attempt at a simultaneous fit of the resonance and subordinate lithium line by including the 6Li/7Li isotopic ratio as a free parameter improves the fit of the λ6707.8 line (see Fig. 4), but there is no way to get a good fit for values of 6Li/7Li less than 0.11.

In the brown dwarf/planet engulfment scenario, the accreted matter would also result in a simultaneous enhancement of 6Li, 7Li, and Be. Unfortunately, our HARPS spectrum does not achieve the wavelength range to investigate beryllium, but the suggestion that the 6Li/7Li isotopic ratio may be as high as 0.11 would support the accretion scenario. Also, the large radius of IRAS 12556–7731 in comparison with most of the known lithum-rich giants makes the planet engulfment scenario plausible, because planet ingestion would be more likely to occur when a star evolves more in the RGB and achieves a larger radius.

Finally, in discussing the case of IRAS 12556–7731, we have to consider that its projected rotational velocity, vsini  ~  8 km s-1, is rather high in comparison with other lithium-rich giants. Several authors have argued that accretion of a planet may explain both lithium enhancement and rapid rotation in giants

(Denissenkov & Herwig 2004; Calsberg et al. 2009, 2010, and references therein). Given its physical properties, we cannot rule out that such a process has led to the lithium enhancement and rapid rotation in IRAS 12556–7731. Some rapidly rotating giants can even become magnetically active and may be detected in X-rays (Guillout et al. 2009), however IRAS 12556 − 7731 was not detected in a ROSAT pointed observation (Alcalá et al. 2000).

With the observational data available so far, we cannot be conclusive about what process dominates the lithium enhancement in IRAS 12556–7731. Perhaps several mechanisms working at different times along the RGB phase of this star have contributed to its lithium enrichment.

Online material

thumbnail Fig. 4

Comparison of the observed lithium λ6707.8 Å absorption line with synthetic MOOG spectra for three values of A(Li). The 6Li/7Li isotopic ratio has been also included as a free parameter for the fit. The inset shows the comparison of the results with and without inclusion of the 6Li/7Li ratio as a free parameter (continuous and dotted lines, respectively).

Appendix A: The ROTFIT procedure

In order to derive the astrophysical parameters of IRAS 12556 − 7731, we used a χ2 minimization procedure developed in the IDL4 environment. This procedure, which is a variation of the ROTFIT code described by Frasca et al. (2003), provides us with the best match of the observed spectrum with a grid of high-resolution spectra of real stars with well determined parameters (PASTEL catalogue, Soubiran et al. 2010) retrieved from the ELODIE archive (Moultaka et al. 2001), which is one of the largest datasets of high-resolution spectra, spanning the wavelength range 4000 − 6800 Å. Because the spectra are severely affected by molecular bands, it was difficult to perform a safe and homogeneous normalization to the local continuum for both IRAS 12556–7731 and the ELODIE templates. We thus preferred to analyse selected spectral regions, mainly around the strongest TiO bands (λλ4950, 5166, 5450, 6158, 6650, 6680 Å), normalizing the spectrum with respect to the average stellar flux in a window of  ~ 10 Å blueward of the band- head (see Fig. A.1). This allowed us to fully exploit the high sensitivity to both temperature and gravity of the molecular bands (see, e.g., Neff et al. 1995). The Na i D lines, which are very sensitive diagnostics of temperature and gravity, were selected as well (Fig. 1). At the end of this procedure, for each of the five spectral regions investigated, ten templates that best matched the HARPS spectrum of IRAS 12556–7731, based on χ2 minimization, were chosen independently, and their known astrophysical parameters were used to compute weighted average values. Such average values were adopted as astrophysical parameters for IRAS 12556−7731. The results are Teff = 3460  ±  60 K, log g = 0.6  ±  0.2 dex, [Fe/H]  =   −0.05  ±  0.10 dex, and vsini = 6.2  ±  3.0 km s-1. The errors include the 1σ standard deviation on the average and the typical errors of the PASTEL astrophysical parameters added in quadrature. The latter are  ± 50 K,  ± 0.1 dex,  ± 0.1 dex, and  ± 0.5 km s-1 for Teff, log g, [Fe/H], and vsini, respectively.

thumbnail Fig. A.1

Portions of the HARPS spectrum of IRAS 12556–7731 around three TiO bands. The M5 III best template (HD 175865) is overplotted with dotted red lines.

2

|W + 10| ≥ 30 km s-1 and/or (U2 + V2)1/2  ≥  65 km s-1.

3

Conversion of 3He to 7Li by α-capture with 7Be as a radioactive intermediary.

4

IDL (Interactive Data Language) is a registered trademark of IT Visual Information Solutions.

Acknowledgments

We thank the referee, Dr. P. Bonifacio, for his useful comments and suggestions and for information on the lithium hyperfine line structure. K.B. acknowledges financial support from the INAF Postdoctoral fellowship programme. We also thank V. Andretta, L. Belluzzi, and V. D’Orazi for discussions of hyperfine line structure.

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All Tables

Table 1

Physical parameters of IRAS 12556–7731.

In the text

All Figures

thumbnail Fig. 1

Portion of the HARPS spectrum of IRAS 12556–7731 in the Na i D region. The M5 III best template (HD 175865) is overplotted (dotted line). A dwarf M star with nearly the same temperature (HD 173740) is also overplotted with a dashed line. The interstellar absorption components (IS) are also indicated.
In the text
thumbnail Fig. 2

Portion of HARPS spectrum in the interval around the lithium λ6103.6 Å absorption line. The top panel shows the synthetic spectra for three values of A(Li) at fixed metallicity, while the lower one shows the synthetic spectra for three values of metallicity at fixed A(Li). The best fit is for a sligthly subsolar metallicity and A(Li) = 2.4.
In the text
thumbnail Fig. 3

Upper panel. The log g versus log Teff diagram. The Girardi et al. (2000) isochrones for three different ages are overplotted. The black dot represents the position of IRAS 12556–7731. Lower panel. HR diagram of several Li-rich giants. The evolutionary tracks by Girardi et al. (2000) for several masses as labelled are represented with continuous lines. The lithium-rich K-type giants (Kumar et al. 2011) are over-plotted with open circles. The asterisk represents HD 39853, while the position of IRAS 12556–7731 is indicated by the big black dot.
In the text
thumbnail Fig. 4

Comparison of the observed lithium λ6707.8 Å absorption line with synthetic MOOG spectra for three values of A(Li). The 6Li/7Li isotopic ratio has been also included as a free parameter for the fit. The inset shows the comparison of the results with and without inclusion of the 6Li/7Li ratio as a free parameter (continuous and dotted lines, respectively).
In the text
thumbnail Fig. A.1

Portions of the HARPS spectrum of IRAS 12556–7731 around three TiO bands. The M5 III best template (HD 175865) is overplotted with dotted red lines.
In the text

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