# Energetic feedback and 26Al from massive stars and their supernovae in the Carina region

R. Voss, P. Martin, R. Diehl, J. S. Vink, D. H. Hartmann, T. Preibisch

► To cite this version:

R. Voss, P. Martin, R. Diehl, J. S. Vink, D. H. Hartmann, et al., Energetic feedback and 26Al from massive stars and their supernovae in the Carina region. Astronomy and Astrophysics - A&A, 2012, 539, 10.1051/0004-6361/201118209. insu-03612449

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# Energetic feedback and $^{26}$Al from massive stars and their supernovae in the Carina region

R. Voss$^{1}$, P. Martin$^{2}$, R. Diehl$^{3}$, J. S. Vink$^{4}$, D. H. Hartmann$^{5}$, and T. Preibisch$^{6}$

Received 5 October 2011 / Accepted 3 January 2012

## ABSTRACT

**Aims.** We study the populations of massive stars in the Carina region and their energetic feedback and ejection of $^{26}$Al.

**Methods.** We did a census of the stellar populations in young stellar clusters within a few degrees of the Carina nebula. For each star we estimated the mass, based on the spectral type and the host cluster age. We used population synthesis to calculate the energetic feedback and ejection of $^{26}$Al from the winds of the massive stars and their supernova explosions. We used 7 years of INTEGRAL observations to measure the $^{26}$Al signal from the region.

**Results.** The INTEGRAL $^{26}$Al signal is not significant with a best-fit value of ~1.5 ± 1.0 × 10⁻⁵ ph cm⁻² s⁻¹, approximately half of the published Compton Gamma Ray Observatory (CGRO) result, but in agreement with the latest CGRO estimates. Our analysis of the stellar populations in the young clusters leads to an expected signal of ~half the observed value, but the results are consistent within 2σ. We find that the fraction of $^{26}$Al ejected in Wolf-Rayet winds is high, and the observed signal is unlikely to be caused by $^{26}$Al ejected in supernovae alone, indicating a strong wind ejection of $^{26}$Al. Due to the lack of prominent O stars, regions with ages ≥10 Myr are often neglected in studies of OB associations. We find that in the Carina region such clusters contribute significantly to the stellar mass and the energetics of the region.

**Key words.** stars: abundances – ISM: abundances – stars: winds, outflows – stars: early-type – gamma rays: ISM

## 1. introduction

Feedback from massive stars plays a crucial role in the formation of stars and in shaping the surrounding inter-stellar medium (ISM). We developed a new population synthesis tool to study the feedback from populations of massive stars in OB associations (Voss et al. 2009). In Voss et al. (2010) we applied the population synthesis to the nearby Orion region and found good agreement with observations of the region. However, the population of massive stars in Orion is not large enough to provide strong constraints on the feedback models. For this it is necessary to study a larger population that includes very high-mass stars (~100 $M_{\odot}$).

The Carina region hosts a large population of very young massive stars at a distance of 2.3 ± 0.1 kpc (Allen & Hillier 1993; Walborn 1995; Smith 2002), including 72 of spectral type O (Smith 2006; Cappa et al. 2008), six Wolf-Rayet (WR) stars (van der Hucht 2001), one luminous blue variable (LBV; η Carinae), and three evolved red supergiants (Feinstein et al. 1980; Feinstein 1981). The total stellar mass is estimated to be ~3.7 × 10⁴ $M_{\odot}$ (Preibisch et al. 2011c), and the total mass of the surrounding gas and dust is ~2.8 × 10⁵ $M_{\odot}$ (Preibisch et al. 2011b). The majority of the young stars reside in the Carina nebula (summarized in Smith 2006), but the surrounding region hosts a large number of smaller open clusters with a wider range of stellar ages. While the stellar populations have been studied

in the most prominent of these (NGC3293; NGC 3324; Evans et al. 2005; Cappa et al. 2008), many of the smaller clusters have never been investigated in detail.

The content of massive stars in the Carina region is intermediate between the population of relatively well-studied small star-forming regions, such as Orion and Sco-Cen, and more distant superclusters, where single regions such as 30 Doradus, hosting ~1000 O-stars, can affect the energetics and chemistry of their host galaxies. Therefore the Carina region is useful for the study of massive stars and as feedback from massive stars, and important for understanding how the feedback mechanisms scale with the size/mass of the region. The population is similar to the Cygnus OB2 association hosting 80 (Hanson 2003) stars of type O, which was the goal of a recent study similar to ours (Martin et al. 2009, 2010).

The radioactive isotope $^{26}$Al is ejected from massive stars through their winds and supernova explosions (Prantzos & Diehl 1996). It is therefore intimately related to the energy feedback from massive stars. It has a mean lifetime of ~1 Myr and is traced by the γ-ray decay line at 1808.63 keV, observable by γ-ray observatories such as the COMPTEL instrument aboard the CGRO and the SPI instrument aboard INTEGRAL.

In the light of the uncertainties in the modelling of massive stars, it is necessary to perform multi-wavelength consistency checks, encompassing the different aspects of feedback provided by massive star clusters. In this paper we discuss the ejection of

<footnote>$^{1}$ Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
e-mail: rvoss@science.ru.nl</footnote>

<footnote>$^{2}$ Institut de Planétologie et d'Astrophysique de Grenoble, BP 53, 38041 Grenoble Cedex 9, France</footnote>

<footnote>$^{3}$ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany</footnote>

<footnote>$^{4}$ Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland, UK</footnote>

<footnote>$^{5}$ Department of Physics and Astronomy, Clemson University, Kinard Lab of Physics, Clemson, SC 29634-0978, USA</footnote>

<footnote>$^{6}$ Universitäts-Sternwarte München, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 München, Germany</footnote>
²⁶Al and the injection of energy into the ISM from the massive star population in the Carina region. This is complementary to the modelling and observations of the energy and UV balance studied by Smith (2006) and Smith & Brooks (2007). The comparison between the theoretical models and the observables is important, both for understanding crucial parts of stellar evolution, in particular mass-loss rates, nucleosynthesis, and supernova explosions, and for understanding issues related to the ISM, such as star-formation and feedback mechanisms. A new generation of stellar models (Meynet & Maeder 2005; Palacios et al. 2005; Limongi & Chieffi 2006) has improved observations of stellar populations in star-forming regions, and the advent of the INTEGRAL observatory providing new ²⁶Al observations has allowed progress on the subject: Voss et al. (2010) studied the variations between different models of massive stars, in particular the effects of rotation and the strength of wind mass-loss on the radio-active tracers and the energetics of star-forming regions. The individual nearby star-forming regions Sco-Cen (Diehl et al. 2010), Orion (Voss et al. 2010), and Cygnus (Martin et al. 2009, 2010) have been studied in detail and good agreement has been found between theory and the observations.

## 2. Observations of ²⁶Al from the Carina region

### 2.1. CGRO results

The ²⁶Al signal from the Carina region was discussed by Knödlseder et al. (1996), based on a measured flux of $3.2 \times 10^{-5}$ ph s⁻¹ cm⁻² (with statistical and systematic uncertainties of $0.8 \times 10^{-5}$ and $0.1 \times 10^{-5}$, respectively). Their analysis showed that the signal is seen only from within two degrees of the Carina nebula direction, although an origin from a larger region extending up to six degrees would also be consistent with the measurements. A subsequent analysis of the full CGRO database revised flux values down to $1.1-2.2 \times 10^{-5}$ ph s⁻¹ cm⁻² (with ~20% statistical error Plüschke 2001). This signal corresponds to 0.005–0.010 $M_\odot$ of ²⁶Al at the distance of the Carina nebula. An origin from foreground stellar groups and from AGB stars is implausible, and background groups would have to be exceptionally active to explain the flux (see Knödlseder et al. 1996, for a discussion). Here we use INTEGRAL observations for a new measurement of ²⁶Al from the Carina region, and use a population synthesis approach (Voss et al. 2009) to compare them to expectations.

### 2.2. INTEGRAL data analysis

We used INTEGRAL data taken between revolution 19 and 855 of the satellite. This corresponds to a total effective exposure of 17.6 Ms on Carina, defined as a circular region with radius of 40° centred on $(l, b) = (285.0°, 0.0°)$. The methodology developed in Martin et al. (2009) to extract the 1809 keV signal from Cygnus was again used for the present study. The reader is referred to their work for more details about data preparation, instrumental background modelling, and other technical aspects. We searched for emission in the 1806–1812 keV band over the 245°–325° longitude range, using two different methods.

The first was a point-source scan, where we try to account for the data by fitting an instrumental background model and a sky model consisting of a single point source. The operation is repeated for a grid of positions covering the whole Carina region. From this analysis, however, no significant excess emission was detected in the Carina region around $(l, b) = (287.0°, 0.0°)$, where the main massive star clusters are located. Significant

<table><caption>**Table 1.** Open clusters in our study.</caption><thead><tr><th>Cluster</th><th>Number of O stars</th><th>Age Myr</th><th>Distance kpc</th></tr></thead><tbody><tr><td>Bochum 10</td><td>1</td><td>7</td><td>2.3</td></tr><tr><td>Bochum 11</td><td>5</td><td>2</td><td>2.3</td></tr><tr><td>Loden 153</td><td>1</td><td>5.5</td><td>2.7</td></tr><tr><td>NGC 3293</td><td>0</td><td>10</td><td>2.7</td></tr><tr><td>NGC 3324</td><td>3</td><td>2.5</td><td>3.0</td></tr><tr><td>Trumpler 14</td><td>9</td><td>1</td><td>2.3</td></tr><tr><td>Trumpler 15</td><td>6</td><td>6</td><td>2.3</td></tr><tr><td>Trumpler 16</td><td>43</td><td>2.5</td><td>2.3</td></tr></tbody></table>

emission appears beyond $l = 305°$, as we move towards the Galactic ridge, which dominates the allsky 1809 keV emission. As a comparison, we did the same for the Cygnus region and found strong emission around $(l, b) = (80.0°, 0.0°)$, consistent with the dedicated analysis exposed in Martin et al. (2009). (While the exposure is similar for both regions, Cygnus hosts almost twice the number of O-stars, and is nearer.) Figure 1 shows the maximum likelihood ratio maps obtained for the Carina and Cygnus regions.

We then determined the 1809 keV flux from the Carina region more quantitatively by fitting to the data extended sky models to the data that better describe the expected ²⁶Al decay emission from a conglomerate of star clusters. We used a 2D Gaussian intensity distribution of various sizes and tried two different positions for these. The first is $(l, b) = (287.6°, -0.6°)$, the position of Trumpler 16, the richest cluster in terms of O stars, and the second is $(l, b) = (285.8°, 0.1°)$, which is the position of NGC3293, which is the cluster with the largest number of past supernovae (as extrapolated from its present-day IMF, see below). In that way, we tested two scenarios: one in which the ²⁶Al content of the Carina region is assumed to be fed mostly by the WR-winds of present-day massive stars, and one in which it is assumed to result mostly from past supernovae. Fluxes in the range 1.0–1.5×10⁻⁵ ph s⁻¹ cm⁻² are obtained, with typical statistical uncertainties of $1.0 \times 10^{-5}$ ph s⁻¹ cm⁻². Combining information from both CGRO and INTEGRAL apparently points to a 1809 keV flux from the Carina region, in the range 1–2 × 10⁻⁵ ph s⁻¹ cm⁻², corresponding to a ²⁶Al mass of $4–9 \times 10^{-3} M_\odot$.

## 3. Analysis of the stellar populations

To compute the amount of ²⁶Al in the observed region, it is necessary to understand the stellar content of the region, and how star formation developed in the past ~10 Myr. In our analysis we include the region considered by Knödlseder et al. (1996) to be the emitting region, which is a region approximately centred on the Carina nebula, with a radius of ~2.8°. This includes the Carina nebula itself, but also some clusters that are distant enough from this to not be linked directly to it by dynamics. In our main analysis we only consider clusters with a distance below ~3 kpc, but a possible contribution from the background is discussed in Sect. 4.

The population of massive stars in clusters belonging to the Carina nebula was presented in Smith (2006), and we adopt their stellar classifications and cluster ages (noting that ages of such young clusters are always very uncertain) and assume that the study is complete for the O stars. In addition we include the three supergiants listed in Feinstein et al. (1980) and Feinstein (1981). For NGC 3324 and NGC 3293, we used Cappa et al. (2008) and Evans et al. (2005), respectively, with the addition
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Maximum likelihood ratio (MLR) maps built from a point-source scan of the regions of Cygnus (top panel) and Carina (bottom panel). The colour coding ranges from MLR ~ 0 (black) to MLR ~ 40 (red).</figcaption></figure>

of a red supergiant from Carraro & Patat (2001). Other clusters were found to be too old or small to contribute significantly to the observed $^{26}$Al signal, e.g. Loden 165, NGC 3114, VdB Hagen 99, and Bochum 9 (Carraro & Patat 2001; Patat & Carraro 2001). Additional WR stars that are found outside the main clusters were taken from van der Hucht (2001). Table 1 summarizes basic information about the clusters being considered. Recent studies have shown that there is a significant population of OB stars obscured by dust from the Carina region itself (e.g. Povich et al. 2011). We discuss this population in Sect. 5.2.

To use this information it is necessary to derive the stellar masses from the spectral types. We do this separately for the main sequence stars and for the evolved stars. As in Voss et al. (2010) we find the temperature and luminosity of the stellar spectral types of O stars from the line-blanketed models of Martins et al. (2005), using their observational scale. The masses were then found by comparing them to the rotating stellar models of Meynet & Maeder (2005). In Voss et al. (2010) we compared the masses found from this method to the spectroscopic masses and found agreement, and a similar result was found by Weidner & Vink (2010). Figure 2 compares the properties of the observed stars to isochrones from four different sets of stellar models. The analysis above was repeated for each of the sets, and the differences were found to be negligible compared to the uncertainties of our results. We used a similar approach for the most massive B-stars, where we took the extrapolation of the Martins et al. (2005) luminosities presented in Smith (2006), together with the effective temperatures of Zorec et al. (2009).

The luminosities are only available for B-stars of luminosity classes III and V. Luminosities for class IV were found by logarithmic interpolation between class III and V. B-stars of luminosity class I and II were assumed to be near the end of the main sequence, so were not included in this analysis. These stars were included as evolved stars in the analysis below.

It is not possible to derive the masses of evolved stars with this method. Instead we made crude estimates of the initial mass of these stars based on the ages of the clusters. This was done by assuming that the mass of the evolved stars must be above the most massive main sequence star in the host cluster and below the mass for which the stellar lifetime is equal to the age of the cluster. The list of evolved stars is given in Table 2. Some of the WR stars are not associated with clusters. We do not attempt to derive their ages, and the uncertainties resulting from these objects are discussed in Sect. 4.

### 3.1. Initial mass function

The set of initial masses can be used to derive an initial mass function (IMF) for the region. The IMF of Trumpler 16 was previously derived by Massey & Johnson (1993), who found it to be consistent with a single power law with a slope of $\Gamma = 1.3 \pm 0.2$ above 15 $M_{\odot}$, where $dN/dM = M^{-\Gamma-1}$ (the Salpeter slope is $\Gamma = 1.35$). The stellar content of the group has been revised several times since then; in particular, many binary components have been resolved, and the stellar evolutionary and atmosphere models have changed significantly. Furthermore, Massey & Johnson (1993) assumed Gaussian statistics despite having bins with very few counts. We therefore provide a new fit to the IMF, by fitting a single power law to the initial stellar masses using maximum likelihood fitting.

Each of the clusters with a population large enough to achieve a meaningful fit were fitted individually, assuming that all stars above 15 $M_{\odot}$ have been identified. The results are given in Table 3. Clearly they are all consistent with the Salpeter (1955) mass function, but only Trumpler 16 provides relatively good statistics. A combined sample consisting of all the stars in the clusters that samples the complete 15–120 $M_{\odot}$ range yields a very similar result to the fit from Trumpler 16 alone. We also performed a combined fit to all the clusters, with an upper limit of 40 $M_{\odot}$ (to avoid incompleteness corrections). Interestingly this yields a relatively shallow slope. However, the narrower range means that this is relatively strongly affected by systematic errors on the stellar masses, as well as a possible incompleteness of the sample at masses ~15 $M_{\odot}$, and it is not clear that the result should be trusted. To understand the dependence on these effects we have performed the fits with a higher completeness mass of 25 $M_{\odot}$, yielding very similar results to the Salpeter (1955) mass function.

In a recent survey of Trumpler 15, Wang et al. (2011) found a lack of massive stars (>20 $M_{\odot}$) by extrapolating observations of stars of lower masses. Using the Kroupa (2001) mass function, they find that there should be ~11 stars, whereas they claim that none are observed. They conclude that either it is an anomaly of the IMF or, alternatively, that all stars above 20 $M_{\odot}$ have already exploded, which would indicate an age above 10 Myr, older than what is normally assumed for this cluster. In contrast to their results, our analysis finds that there are six stars in this cluster with masses above 20 $M_{\odot}$ and that with an age of ~6 Myr, approximately three supernova have exploded, which agrees with the results at lower stellar masses. We believe that the discrepancy is the result of Wang et al. (2011) underestimating the masses of stars with early-type spectra.
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** The O stars in the four groups richest in O stars. The solid lines correspond to stellar tracks, and the dashed lines are isochrones with a separation of 2 Myr. The stellar models are from Meynet et al. (1997) (upper left), Limongi & Chieffi (2006) (upper right), Schaller et al. (1992) (lower left), and Meynet & Maeder (2005) (lower right). As our analysis only allows a limited set of discrete values, many of the points contain multiple stars.</figcaption></figure>

Feinstein (1995) summed up the total masses of the observed stars in the individual clusters. With the updated stellar populations we improve these estimates. We furthermore take the completeness limits and the contribution from exploded stars into account to compare the *initial* stellar content of the individual groups. Our results show that TR 16 is still the dominant group, but that the older group (~10 Myr) NGC 3293, which is often neglected due to the lack of O stars, has previously hosted a decent population of these (~10 stars are expected to have exploded as supernovae in this association). Assuming the Salpeter (1955) mass function, the Carina region hosts around three to four times as many stars as the closer Orion region (Voss et al. 2010). This is lower than what is expected from the observed number of O-stars (a factor of ~12), due to the somewhat higher age (5–6 Myr) of the bulk of the stars in Orion.

We furthermore used the Salpeter (1955) IMF to estimate the relative sizes of the open clusters, by extrapolating the number of stars in the observed mass ranges of the individual clusters. Estimates of the initial numbers of stars (>15 $M_\odot$) are given in Table 3, together with the estimated number of SNe that have already exploded. While the young clusters (<3.5 Myr) clearly

dominate visually (and in terms of how well studied they are), especially the clusters that are part of the extended Carina nebula, they only comprise half of the star formation within the past ~10 Myr.

## 4. $^{26}$Al

The amount of $^{26}$Al found from different analyses of CGRO and INTEGRAL data is in the range 0.004–0.009 $M_\odot$. Even the lower estimates are significantly higher than the highest expected mass emitted by a single object. The possibility of a much lower mass ejected by a foreground object was dismissed by Knödlseder et al. (1996). The current understanding that $^{26}$Al is almost exclusively being ejected by massive stars further limits the possibility of confusing foreground objects, thanks to the completeness of the detection of nearby massive stars. The background of the Carina complex is less well understood, but clearly hosts young clusters with massive stars; for example, the massive young cluster Westerlund 2 is within our field, at a distance of 8 kpc (Rauw et al. 2007). However, most of these are at large distances (at least twice the distance of the Carina nebula).
<table><caption>**Table 2.** Evolved stars in the Carina region.</caption><thead><tr><th>Name</th><th>Type</th><th>Cluster</th><th>Initial mass<br>M<sub>☉</sub></th><th><sup>26</sup>Al<br>(10<sup>-4</sup> M<sub>☉</sub>)</th></tr></thead><tbody><tr><td>HD 92809</td><td>WC6</td><td>Bochum 10</td><td>~30</td><td>0.3–1.5</td></tr><tr><td>HD 92964</td><td>B2 Ia</td><td>Bochum 10</td><td>~30</td><td>0.0–0.3</td></tr><tr><td>HD 92852</td><td>K1/3 III</td><td>Bochum 10</td><td>~30</td><td>0.0–0.3</td></tr><tr><td>Evans 3293-001</td><td>B0 Iab</td><td>NGC 3293</td><td>~20</td><td>0.0–0.1</td></tr><tr><td>Evans 3293-002</td><td>B0.7 Ib</td><td>NGC 3293</td><td>~20</td><td>0.0–0.1</td></tr><tr><td>Feinstein CPD 3502</td><td>M1.5 Iab-Ib</td><td>NGC 3293</td><td>~20</td><td>0.0–0.1</td></tr><tr><td>HD 93129Aa</td><td>O2 If</td><td>Trumpler 14</td><td>80–120</td><td>0.0–4.0</td></tr><tr><td>η Car</td><td>LBV</td><td>Trumpler 16</td><td>80–120</td><td>0.0–4.0</td></tr><tr><td>HD 93162</td><td>WN6ha</td><td>Trumpler 16</td><td>80–120</td><td>2.0–8.0</td></tr><tr><td>HD 93131</td><td>WN6ha</td><td>Trumpler 16</td><td>80–120</td><td>2.0–8.0</td></tr><tr><td>HD 92740A</td><td>WN7ha</td><td>Trumpler 16</td><td>80–120</td><td>2.0–8.0</td></tr><tr><td>Hucht WR27</td><td>WC6</td><td>Field (2.5)</td><td>—</td><td>—</td></tr><tr><td>HD 94546</td><td>WN4</td><td>Field (4.05)</td><td>—</td><td>—</td></tr><tr><td>Hucht WR31a</td><td>WN11h</td><td>Field (8.0)</td><td>—</td><td>—</td></tr><tr><td>HD 90657</td><td>WN5</td><td>Field (3.88)</td><td>—</td><td>—</td></tr><tr><td>HD 95435</td><td>WC5</td><td>Field (6.11)</td><td>—</td><td>—</td></tr><tr><td>Hucht WR21a</td><td>WN6</td><td>Field (?)</td><td>—</td><td>—</td></tr></tbody></table>

**Notes.** Stars without HD designations are labelled by the name of the first author of the publication in which they appear (see Sect. 3), followed by the name given in that publication. The initial masses are estimated by the maximum mass of stars still present in a population with the age of the host cluster. The ejected amount of <sup>26</sup>Al is found from the stellar tracks at the given mass. The range is over all WR-phases for WR-stars, and until the onset of the WR-winds for non-WR stars.

<table><caption>**Table 3.** Best-fit IMF of open clusters in our study.</caption><thead><tr><th>Cluster</th><th>IMF (&gt;15 M<sub>☉</sub>)<br>Γ<sup>1</sup></th><th>IMF (&gt;25 M<sub>☉</sub>)<br>Γ<sup>1</sup></th><th>Mass range</th><th>No. of stars</th><th>Supernovae</th><th>Total No. (&gt;15 M<sub>☉</sub>)</th></tr></thead><tbody><tr><td>Bochum 10</td><td>—</td><td>—</td><td>15–32</td><td>5</td><td>2.34</td><td>7.34</td></tr><tr><td>Bochum 11</td><td>1.8<sup>+1.1</sup><sub>-0.9</sub></td><td>—</td><td>15–120</td><td>6</td><td>0</td><td>6</td></tr><tr><td>Loden 153</td><td>—</td><td>—</td><td>15–45</td><td>2</td><td>0.43</td><td>2.43</td></tr><tr><td>NGC 3293</td><td>—</td><td>—</td><td>15–22</td><td>23</td><td>20.5</td><td>53.5</td></tr><tr><td>NGC 3324</td><td>1.4<sup>+1.3</sup><sub>-1.1</sub></td><td>—</td><td>15–120</td><td>3</td><td>0</td><td>3</td></tr><tr><td>Trumpler 14</td><td>1.3<sup>+0.6</sup><sub>-0.6</sub></td><td>—</td><td>15–120</td><td>13</td><td>0</td><td>13</td></tr><tr><td>Trumpler 15</td><td>—</td><td>—</td><td>15–40</td><td>11</td><td>3.08</td><td>14.08</td></tr><tr><td>Trumpler 16</td><td>1.2<sup>+0.3</sup><sub>-0.3</sub></td><td>1.3<sup>+0.5</sup><sub>-0.5</sub></td><td>15–120</td><td>54</td><td>0</td><td>54</td></tr><tr><td>All young<sup>2</sup></td><td>1.2<sup>+0.3</sup><sub>-0.2</sub></td><td>1.2<sup>+0.5</sup><sub>-0.4</sub></td><td>15–120</td><td>76</td><td>0</td><td>76</td></tr><tr><td>All<sup>3</sup></td><td>0.6<sup>+0.5</sup><sub>-0.4</sub></td><td>1.3<sup>+0.4</sup><sub>-0.4</sub></td><td>—</td><td>—</td><td>26.35</td><td>153.35</td></tr></tbody></table>

**Notes.** The upper limits on the mass ranges were estimated by the age of the host clusters. The number of stars inside the mass ranges were extrapolated using the Salpeter IMF to find the number of supernovae and the total number of initial stars. <sup>(1)</sup> Slope of a single power-law fit. <sup>(2)</sup> Clusters young enough that no supernova explosions are believed to have occurred. <sup>(3)</sup> Clusters with maximum stellar masses ≥40 M<sub>☉</sub> fitted in the 15–40 M<sub>☉</sub> range.

Within our search radius, Westerlund 2 is the only cluster with a content of young stars that can be compared to Trumpler 16. The background can therefore only contribute a modest fraction of the observed signal.

To investigate the origin of the observed <sup>26</sup>Al signal, we divided the stars into three categories:

- main sequence (O) stars;

- exploded stars (SNe);

- evolved (WR and supergiant) stars;

and explored their contributions separately. We ignored the population of stars of spectral type B or later, as their wind contribution is negligible and their lifetimes are long enough that they have not yet gone supernova.

**<sup>26</sup>Al from O stars:** The initial stellar masses and current ages of the 66 O-stars with spectral types of O3 or later were estimated above. From following the wind ejection and radioactive

decay of <sup>26</sup>Al along the stellar tracks, we can associate a <sup>26</sup>Al mass to each cluster along its evolution. The sum is found to be 5 × 10<sup>-5</sup> M<sub>☉</sub>. While the average ages of the stars are fairly stable using the isochrone fitting, the individual ages are not very reliable, and the ages of the few most massive stars are quite important for the result. We therefore calculated an upper limit to the O-star contribution by assuming that all the O-stars are just about to evolve off the main sequence. This is the maximum age of the O-stars as they will change spectral type after this. This assumption gives an upper limit of 1.5 × 10<sup>-3</sup> M<sub>☉</sub>. In this estimate the contribution from the O2 star in Tr 14, as well as from η Carinae, was ignored. They are included in the discussion of the evolved stars instead.

**<sup>26</sup>Al from supernovae:** We use our estimate of the number of supernova explosions in each cluster (see Table 3), together with the population synthesis tool described in Voss et al. (2009, 2010) to estimate the contribution from exploded stars to the
observed <sup>26</sup>Al. For each cluster the expected contribution and the error on the estimate is calculated using Monte Carlo simulations. In each simulation, the number of exploded stars is chosen from a Poissonian distribution with the mean values given in Table 3, and the masses of the stars are chosen randomly from the Salpeter (1955) mass function. The lower mass limit of the IMF is given by the stellar track with the lowest initial mass that has a lifetime shorter than the current age of the cluster. The ejection of <sup>26</sup>Al from the winds and supernovae is followed while taking the radioactive decay into account. This gives an estimate of $9_{-4}^{+5} \times 10^{-4} M_{\odot}$ of <sup>26</sup>Al from the supernova yields and $3 \pm 2 \times 10^{-4} M_{\odot}$ from the preceding winds of the exploded stars.

**<sup>26</sup>Al from evolved stars:** The final contribution to the <sup>26</sup>Al signal comes from the winds of the evolved stars. In Table 2 we list the evolved stars that we have identified inside the region. The cluster association of each evolved star is listed. A number of WR stars in the catalogue of van der Hucht (2001) have no cluster association and are listed as field sources, with the photometric distances given by the catalogue (only WR stars with estimated distances below 10 kpc are included in our list). The initial masses of the evolved cluster stars were assumed to be close to the maximum initial stellar mass given the age of the clusters. For each star we have identified stars in our stellar isochrones with similar initial masses and evolutionary states (spectral types) and used these to estimate the possible range of <sup>26</sup>Al masses present in the ISM. These are also listed in Table 2. The field WR stars are more problematic, since their distances are unreliable, and there is no stellar population through which their approximate age can be deduced. However, owing to the slope of the IMF and the shorter lifetimes of massive stars, most of them probably correspond to relatively low (for WR stars) initial masses of (25–40 $M_{\odot}$). Because there is no foreground population of massive stars that they can belong to, most of them must be located behind the Carina nebula. This is consistent with their estimated distances (however uncertain), so their contribution is unlikely to be significant. From Table 2, it can be seen that the total mass of <sup>26</sup>Al from all the evolved stars is unlikely to exceed $3 \times 10^{-3} M_{\odot}$. The most realistic estimate range is $1.5–2.0 \times 10^{-3} M_{\odot}$.

**Population synthesis:** For comparison we computed the expectation of <sup>26</sup>Al from the entire region using population synthesis (Voss et al. 2009), with the cluster ages from Table 1 and total star-numbers from Table 3. Each cluster was assumed to have a Gaussian age spread with $\sigma = 0.5$ Myr. We used the model that gives the highest <sup>26</sup>Al yields, with rotating stellar evolution models from Meynet & Maeder (2005) and supernova yields from Limongi & Chieffi (2006). The results are shown in the top panel of Fig. 3. Also shown as the range between the two horizontal dashed lines is the most likely observed <sup>26</sup>Al signal. As discussed in Sect. 2 the range should not be taken as a statistical confidence interval, due to the poorly constrained systematic effects of the different ways to measure the signal. The population synthesis model predicts that the signal is divided roughly evenly between the wind and the supernova contributions. This is mainly because the population synthesis model predicts a lower wind contribution than what is found from the observed stars. However, this is consistent within the 90% variance caused by the sampling of the population of massive stars (see discussion in Voss et al. 2009). It is therefore just an effect of the actual realization of the population of massive stars, which yields

a higher wind contribution to the <sup>26</sup>Al than an average cluster (with the same properties). Also the slope of the time-profile is relatively steep, and it is therefore clear that small errors in the estimates of the cluster ages (especially of the youngest clusters) can have a relatively large influence on the conclusions from the population synthesis.

In the middle panel of Fig. 3 we show the energy injected into the ISM from the stars, predicted by the population synthesis. The total output can be seen to have risen to $\ge 2 \times 10^{38}$ erg s<sup>-1</sup> about 10 Myr ago, and then slowly increased to the current output of $\sim 5–6 \times 10^{38}$ erg s<sup>-1</sup>. The energy budget of the associations in the Carina Complex was studied by Smith (2006) and Smith & Brooks (2007), who found the stellar wind output to be $\sim 2 \times 10^{38}$ erg s<sup>-1</sup>. This result did not take supernova contributions into account, and did not include NGC 3293. When doing so, their results are in good agreement with our population synthesis. They also estimated the mechanical energy needed to create the superbubble surrounding the region to be $8 \times 10^{51}$ erg. This corresponds to $\sim 5 \times 10^{37}$ erg s<sup>-1</sup>, assuming a constant power over the past 5 Myr. We multiply this by a factor of 10 to account for the observations from other regions showing that only a fraction of ~10–20% of the kinetic energy goes into the expansion of the bubble (e.g. Brown et al. 1995; Cooper et al. 2004). From the middle panel of Fig. 3, it is evident that this estimate is in good agreement with the expectations, arguing for a similar energy efficiency of creating the superbubble in the Carina region. Our population synthesis predictions for the emission of hydrogen ionized UV photons are shown in the lower panel of Fig. 3. The UV emission was also studied by Smith & Brooks (2007). They find a rate just below $10^{51}$ s<sup>-1</sup>, in good agreement with our population synthesis model. From observations of the radio continuum, they deduced that the ISM around the Carina region absorbs $\sim 7 \times 10^{50}$ ph s<sup>-1</sup> of UV radiation, which we use as the observational estimate in Fig. 3. The remaining ~25% of the flux leaks out of the region.

# 5. Discussion

## 5.1. Comparison with other young associations

Other regions have been investigated recently. Population synthesis models of the regions Orion (Voss et al. 2010), Cygnus (Martin et al. 2009, 2010), and Sco-Cen (Diehl et al. 2010) were found to be consistent with observations. Similar to the results presented above, the analysis of both Orion and Cygnus supports theoretical models with high <sup>26</sup>Al ejection from the WR-winds of the massive stars. However, due to the high statistical fluctuations of the <sup>26</sup>Al output from individual regions, caused by the random sampling of the IMF, each result is of low significance (<2σ).

An interesting aspect of comparing different regions is the differences in their star formation histories. In Orion and Sco-Cen the <sup>26</sup>Al output is dominated by populations of stars with ages >5 Myr, where the ejection from supernova explosions is most important. More than 50% of the <sup>26</sup>Al in these regions is expected to be emitted by the supernovae. Therefore these observations alone could not be used to distinguish between models with strong wind ejection, as all the <sup>26</sup>Al could be emitted by supernovae if their yields were enhanced by a factor of $\le 2$. The situation is different in the Carina and Cygnus regions. In Carina we have estimated that only ~20% of the signal comes from supernovae, and also in Cygnus the wind contribution dominates (Martin et al. 2009, 2010). An increase in the supernova ejection by a factor of ~5 would be needed to explain the signal with
$^{26}$Al from supernovae alone, but this is not consistent with the observations of Orion and Sco-Cen. It is therefore clear that the $^{26}$Al signals observed from Carina and Cygnus are not due to supernova ejecta alone, so a strong wind ejection component is necessary. This is therefore the strongest evidence of $^{26}$Al ejection in WR-winds to date.

## 5.2. Possible explanations for the high $^{26}$Al signal

We have shown above that the most likely observed $^{26}$Al signal is higher than the theoretical predictions, even for the models with the strongest wind ejection. Here we discuss possible effects that were not taken into account in our analysis:

**Hidden stars:** Recent results have shown that the population of OB stars in the Carina region has been underestimated by a factor of ~50% (Povich et al. 2011). The extra OB stars are found outside the clusters discussed above with some of them being in recently identified clusters and the rest distributed between them. The reason these stars were not identified before is the large absorbing column in front of them, caused by molecular clouds in their local environment. The average visual extinction of the OB candidates of Povich et al. (2011) is $A_V = 5.8$, and the most absorbed candidates have an extinction $A_V > 30$. As $^{26}$Al is observed with γ-rays, it is not affected by extinction, and the hidden population can therefore provide a significant contribution to the signal. However, we believe that the hidden population contributes less than expected from the number of OB stars. The large absorbing columns indicate that many of the stars are still inside or near their parent molecular clouds. For example the Treasury Chest cluster is estimated to be younger than 1 Myr (Smith et al. 2005). Groups of stars with the age where the $^{26}$Al signal is strongest (3–10 Myr) provide enough kinetic energy and UV radiation to ionize/disperse nearby clouds, and are therefore much less likely to be obscured. On the other hand, some of the OB stars could be located behind other clouds. In the Cygnus region, this is for example the case of Cygnus OB2, which is heavily obscured, but contributes significantly to the $^{26}$Al signal (Martin et al. 2009, 2010). In Cygnus the contribution from a diffuse population of massive stars was estimated to be ~33%. From the discussion above we believe that $^{26}$Al from stars outside clusters and in hidden clusters that were not taken into account in our analysis does contribute to the signal, but with less than 33% (corresponding to the fraction of hidden massive stars) of the total signal.

**Nucleosynthesis uncertainties:** There are large uncertainties in the modelling of supernova explosions (Woosley et al. 1995; Limongi & Chieffi 2006). Furthermore, the uncertainties in the nuclear reaction rates responsible for the formation of $^{26}$Al ejected in the supernova explosions lead to uncertainties of a factor ~3 (Iliadis et al. 2011). Both could explain the results, if only the Carina region was observed. However, as discussed above, the observations of the Sco-Cen and Orion regions contradict strongly enhanced supernova yields. The nuclear reaction rates responsible for producing $^{26}$Al ejected in stellar winds are much better constrained (Iliadis et al. 2011), and the strong signal can therefore not be explained by the uncertainties of these.

**Binaries:** The yields from close binaries are challenging to quantify (Langer et al. 1998). Such systems experience mass transfer episodes, which can lead to enhanced mass loss and

mixing and early exposure and ejection of chemically enriched layers of the stars. Furthermore, tidal forces affect their rotation and mixing. This can in principle lead to very high enhancement factors. However, the enhancement in binaries is concentrated in very few particular systems. Large enhancements in a few systems would lead to high fluctuations in the $^{26}$Al signal over the sky, which are not seen. We therefore conclude that while enhanced systems might explain a modest difference between the theoretical models and the observations, most of the $^{26}$Al is being ejected by “normal” stars.

**Very massive stars:** There is growing evidence that stars can initially be more massive than the limit of 120 $M_\odot$ assumed in our study (Figer 2005; Koen 2006; Crowther et al. 2010; Bestenlehner et al. 2011), and many stars are born in multiple systems can both increase the yields significantly. Indeed, both have been invoked to explain properties of stars in the Carina nebula, in particular $\eta$ Carinae. The $^{26}$Al yields of stars with masses above 120 $M_\odot$ have not been studied. However, the yields of stellar models increase relatively strongly with initial mass, and it is therefore likely that initially very massive stars can yield several times the amount of $^{26}$Al given by our most massive stellar model. Similar to the binaries, Large enhancements in a few stars would lead to high fluctuations in the $^{26}$Al signal over the sky, which are not seen, so we believe that the possible contribution from such very massive stars must be modest.

## 5.3. Implications for stellar evolution

The effects discussed above are likely to be minor. It is possible that a combination of these effects are enough to account for the observed $^{26}$Al signal being higher than the highest theoretical model, including both a large wind and a large supernova contribution. We therefore do not find that the apparent discrepancy calls for significant changes in the modelling of massive stars. However, only ~20% of the signal can be explained by $^{26}$Al ejected by supernova explosions. As discussed above in Sect. 5.1, the observations of other regions do not allow the supernova yields to be raised by a factor of a few, so our results therefore support a strong wind ejection.

Despite the downwards revision of the mass-loss rates in the latest stellar evolutionary models (Vink et al. 2000; Meynet & Maeder 2005), the integrated mass loss has not decreased significantly, and the $^{26}$Al ejection has actually increased (Palacios et al. 2005). This is due to the effects of rotation that makes the stars spend a longer time in states with high mass loss rates, and the meridional circulation is increased, lifting $^{26}$Al to the surface. A further downwards revision of the wind mass loss rates (as suggested by e.g. Fullerton et al. 2006) would reduce the wind yields significantly, and our analysis might therefore be evidence against such a downwards revision (see also the discussion in Voss et al. 2010). Similarly, non-rotating models with current wind mass-loss prescriptions have low wind ejection of $^{26}$Al, and our results are therefore in support of rotational effects being significant.

## 5.4. Conclusions

We have studied the population of massive stars in the Carina region. Our analysis of the ejection of kinetic energy into the ISM and the emission of ionizing UV radiation and our results agree with previous theoretical estimates and observational results. $^{26}$Al is an important tracer of massive star evolution and
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Population synthesis model of the Carina region, for a combined population of stars from all the stellar clusters with the ages given in Table 1 and numbers of stars given in Table 3. Time zero corresponds to the current time. The *upper panel* shows the mass of <sup>26</sup>Al in the ISM of the Carina region, the *middle panel* shows the mechanical power ejected into the ISM from the massive stars, and the *lower panel* shows the emitted flux of hydrogen ionizing photons (>13.6 eV). The solid lines show the total output from the stellar population, the dashed line shows the output from the winds, and the dotted line shows the output from supernova explosions. The grey shaded areas show the 1σ deviations of the total output caused by random sampling of the IMF. The horizontal dashed lines indicate estimates based on observations, as discussed in the population synthesis part of Sect. 4.</figcaption></figure>

of the interaction between massive stars and their surroundings. We have constrained the <sup>26</sup>Al signal from the region around the Carina nebula, and shown that it is consistent with coming from the populations of massive stars in this region. Our results show that most ~80% of the <sup>26</sup>Al was ejected by the winds of massive stars. This result strongly favours rotating stellar evolutionary models and disagrees with the suggested further reductions of the mass-loss rates due to clumping beyond what is included in the latest generation of models.

***Acknowledgements.*** This research is supported by NWO Vidi grant 016.093.305. P.M. acknowledges support from the European Community

via contract ERC-StG-200911. Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states.

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