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A&A
Volume 572, December 2014
Article Number A56
Number of page(s) 7
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201424534
Published online 27 November 2014

© ESO, 2014

1. Introduction

The HII region N113 is located in the central part of the Large Magellanic Cloud (LMC). It hosts two H2O masers, of which one is the most intense maser of the Magellanic Clouds (Whiteoak & Gardner 1986; Lazendic et al. 2002; Imai et al. 2013), and an OH maser (Brooks & Whiteoak 1997). This region is associated with a clumpy molecular cloud (Seale et al. 2012) that is active in star formation. Three young stellar clusters, NGC 1874, NGC 1876, and NGC 1877, are related to N113 (Bica et al. 1992) and several young stellar objects (YSOs) have been found embedded in the molecular gas associated with this HII region (Gruendl & Chu 2009; Seale et al. 2009; Sewiło et al. 2010; Seale et al. 2012; Carlson et al. 2012).

One of the main motivations of molecular observational studies towards different regions in the LMC (e.g. Johansson et al. 1994) is to study a low-metallicity interstellar medium (ISM), whose physical conditions may resemble those that existed in the early Milky Way and that therefore can shed light on the primeval processes of star formation. The molecular cloud associated with N113 is one of the richest in the LMC and has been studied often, presenting observations with different resolutions and sensitivities of many molecular lines (Wong et al. 2006; Wang et al. 2009, and references therein). However, most of the molecular lines observed towards N113 cover the frequency range 85−270 GHz (see Chin et al. 1997; Wang et al. 2009). Only three lines were successfully observed at higher frequencies: 13CO and 12CO J = 3 − 2 at 330.56 and 345.79 GHz, respectively, and HCO+J = 4 − 3 at 356.73 GHz. Thus, a survey and study of molecular lines at the 345 GHz window (324−372 GHz) is required for a more complete understanding of the chemistry and excitation conditions of the region. To do this, we used the Atacama Submillimeter Telescope Experiment (ASTE) to map N113 in the 13CO J = 3 − 2 transition and to observe 16 molecular lines within the 345 GHz window towards its centre.

thumbnail Fig. 1

Left: three-colour image where the 8, 24, and 70 μm emission obtained from the IRAC and MIPS cameras of the Spitzer Space Telescope (from SAGE Spitzer; Meixner et al. 2006) are presented in blue, green, and red, respectively. The black box shows the region mapped in the 13CO J = 3 − 2 line with an angular resolution of 22′′. Right: zoom-in of the mapped region (white box). The colour code is the same as in the left image, but the scales are different. The red contours correspond to the 13CO J = 3 − 2 emission integrated between 230 and 245 km s-1 with levels of 2.5, 4.0, 6.0, and 8.0 K km s-1. The FWHM beam size of the observations is included in the bottom right corner of the region. The black circle corresponds to the position where the 16 molecular lines were observed as single pointings.

2. Observations and data reduction

The molecular observations were performed between July and August 2010 with the 10 m ASTE telescope (Ezawa et al. 2004). We used the CATS345 GHz band receiver, a two single-band SIS receiver, which is remotely tunable in the LO frequency range of 324−372 GHz. The XF digital spectrometer was set to a bandwidth and spectral resolution of 128 MHz and 125 kHz. The spectral velocity resolution was 0.11 km s-1 and the half-power beamwidth (HPBW) was 22′′ at 345 GHz. The system temperature varied from Tsys = 150 to 250 K and the main beam efficiency was ηmb ~ 0.65.

The data were reduced with NEWSTAR1 and the spectra processed using the XSpec software package2. The spectra were Hanning-smoothed to improve the signal-to-noise ratio, and in some cases a boxcar smoothing was as applied as well. Polynomials between first and third order were used for baseline fitting.

Table 1

Observed molecular lines towards N113.

Several molecular lines in the 345 GHz window were observed towards the centre of N113 at RA = 05h13m19.5s, Dec =−69° 22′ 37.9′′, J2000 as single pointings (black circle in Fig. 1-right). In Table 1 we list the observed molecular lines and integration times; they indicate whether the detection was positive or not. Additionally, we mapped a 2.́5 × 2.́5 region centred on RA = 05h13m20s, Dec = −69°22′35.5′′, J2000 in the 13CO J = 3 − 2 line (white square in Fig. 1-right). This observation was performed in on-the-fly mapping mode and achieved an angular sampling of 6′′.

3. Results and discussion

3.1. Molecular cloud

Figure 1 (left) is a three-colour image of the mid/far-IR emission in the N113 area where the mapped region in the 13CO J = 3 − 2 line is indicated with a black square. Figure 1 (right) shows a zoom-in of the mapped region with a different colour scale, which allows identifying some point-like sources in the IR emission. The 13CO J = 3 − 2 emission integrated between 230 and 245 km s-1 is presented in contours and shows that the curved and elongated morphology of the molecular cloud agrees well with the IR emission. The surveyed area is populated by 18 O and early-B stars (both on the main sequence and evolved), most of them with spectral types derived via UBV photometric data (Wilcots 1994). A few have spectroscopic observations as a mid-OV star (target s1 in the Wilcots study), sources BI 104 and BI 105 observed by Massey et al. (1995) that are B0.5V and O7V stars, and the more widely studied supergiant star, HD269217, which is of type B2[e] (e.g. Kastner et al. 2010). The main concentration of high-mass YSOs (Seale et al. 2012) and intermediate-mass YSO candidates (Carlson et al. 2012) are located in projection along the CO emission, a configuration commonly found in massive star-forming regions (e.g. Povich et al. 2009; Book et al. 2009; Chen et al. 2010). The three conspicuous IR sources observed in Fig. 1 (right) that appear over the molecular concentration, marked as IR1, IR2, and IR3, are coincident with the compact radio continuum sources detected by Brooks & Whiteoak (1997) and with three YSOs (from south-east to north-west: 051325.09-692245.1, 051321.43-692241.5, and 051317.69-692225.0) catalogued by Seale et al. (2012) and Carlson et al. (2012). As discussed in Wong et al. (2006), these sources might be young ionizing stars that affect the molecular gas and probably contribute to the birth of new stars.

The morphology and velocity distribution of the molecular gas related to N113 is shown in Fig. 2, where the 13CO J = 3 − 2 emission is presented in a series of channel maps in the range of 231−242 km s-1, integrated in steps of 1 km s-1. The curved and elongated molecular cloud is resolved into two clumps, one located towards the north-west and peaking at 233 km s-1, the other one slightly eastwards of the centre of the surveyed region, peaking at 236 km s-1.

thumbnail Fig. 2

Integrated velocity channel maps of the 13CO J = 3 − 2 emission every 1 km s-1. The greyscale is displayed at the top of the first panel and is in K km s-1, the contour levels are 0.3, 0.7, 1, 2, and 2.5 K km s-1.

To roughly estimate the molecular mass, we assumed local thermodynamic equilibrium (LTE). We calculated the excitation temperature from Tex(3→2)=16.59Kln[1+16.59K/(Tmax(12CO)+0.036K)],\begin{equation} T_{\rm ex}(3 \rightarrow 2) = \frac{16.59~{\rm K}}{{\rm ln}[1 + 16.59~{\rm K}/(T_{\rm max}(^{12}{\rm CO}) + 0.036~{\rm K})]}, \label{eq1} \end{equation}(1)where Tmax(12CO) is the 12CO peak temperature towards the centre of the region, obtaining Tex ~ 20 K. We derived the 12CO and 13CO optical depths, τ12 and τ13, using (e.g. Scoville et al. 1986) 12Tmb13Tmb=1−exp(−τ12)1−exp(−τ12/X),\begin{eqnarray} \frac{^{12}{\rm T}_{\rm mb}}{^{13}{\rm T}_{\rm mb}} = \frac{1-\exp(-\tau_{12})}{1-\exp(-\tau_{12}/X)}, \label{eq2} \end{eqnarray}(2)where Tmb12\hbox{$^{12}T_{\rm mb}$} and Tmb13\hbox{$^{13}T_{\rm mb}$} are the peak temperatures of the 12CO and 13CO J = 3 − 2 lines at the centre of the region, and X = 50 is the assumed isotope abundance ratio (Wang et al. 2009). The result is τ12 ~ 9.5 and τ13 ~ 0.2, which indicates that the 13CO J = 3 − 2 line is optically thin. Thus, we estimated its column density from N=8.28×1013e15.87TexTex+0.881−e-15.87Tex1J(Tex)−J(TBG)∫Tmbdv\begin{equation} {N} = 8.28 \times 10^{13}~e^{\frac{15.87}{T_{\rm ex}}}\frac{T_{\rm ex}+0.88}{1-e^{\frac{-15.87}{T_{\rm ex}}}} \frac{1}{J(T_{\rm ex})-J(T_{\rm BG})} \int{{T_{\rm mb} ~{\rm d}v}} \label{eq3} \end{equation}(3)with J(T)=hν/kexp(hνkT)−1·\begin{equation} J(T) = \frac{h\nu/k}{\exp(\frac{h\nu}{kT}) - 1}\cdot \label{eq4} \end{equation}(4)To obtain the molecular hydrogen column density N(H2) we assumed an abundance ratio of [H2/13CO] = 1.8 × 106, estimated by Garay et al. (2002) towards the giant molecular complex No. 37 in the LMC. Almost the same value has been obtained for N159W (Heikkilä et al. 1999), which like N113 is associated with a prominent star-forming region. Finally, the mass was derived from M=μmH∑i[D2ΩiNi(H2)],\begin{equation} {M} = \mu~m_{{\rm H}} \sum_{i}{\left[D^{2}~\Omega_{i}~{N_{\it i}({\rm H}_{2}}) \right]}, \label{eq5} \end{equation}(5)where Ω is the solid angle subtended by the beam size, D is the distance (50 kpc), mH is the hydrogen mass, and μ is the mean molecular weight, assumed to be 2.8 by taking into account a relative helium abundance of 25%. We summed over all beam positions of the molecular structure displayed in contours in Fig. 1 (right panel). The obtained mass is about 1 × 104M⊙, which is somewhat lower than the 8.2 × 104M⊙ estimated by Wong et al. (2006) from the 12CO J = 1 − 0 line using a standard Galactic CO to H2 conversion factor (NH2/ICO = 2.0 × 1020 cm-2 (K km s-1)-1). This discrepancy probably arises because the 13CO J = 3 − 2 and the 12CO J = 1 − 0 map different extensions of the molecular cloud; alternatively the Galactic CO to H2 conversion factor used by Wong et al. might not be appropriate for N113.

From the average of the 13CO J = 3 − 2 emission towards the molecular structure we obtain an averaged spectrum with Δv = 5.3 km s-1. We roughly approximated the molecular cloud with a spherical shape of radius 35′′ (R = 8.8 pc) and considered a density profile of ρ ∝ r-1. From this we estimated the virial mass according to MacLaren et al. (1988), MvirM⊙=190(Rpc)(Δvkms-1)2,\begin{equation} \frac{M_{\rm vir}}{M_{\odot}} = 190 \left( \frac{R}{\rm pc} \right) \left( \frac{\Delta v}{\rm km~s^{-1}} \right)^2, \label{eq6} \end{equation}(6)which gives ~ 4.5 × 104M⊙.

thumbnail Fig. 3

500 μm emission obtained from SPIRE in the Herschel Space Observatory (from Herschel HERITAGE; Meixner et al. 2010, 2013) with the same 13CO J = 3 − 2 contours as shown in Fig. 1 (right). The FWHM beam size of the molecular observations is included in the top left corner. The angular resolution of the SPIRE image is about 36′′.

Additionally, we estimated the mass of gas of the N113 cloud from the continuum emission at the far-infrared regime arising from the dust. To do so we obtained the integrated flux of the continuum emission at 500 μm using the calibrated level 2 PLW SPIRE image extracted from the Herschel Data Archive (ObsID:1342202224). Figure 3 displays the 500 μm emission with contours of the 13CO J = 3 − 2, showing that both emissions are very similar in morphology and size. From the radiative transfer equation and assuming an optically thin medium we estimated the gas mass in the cloud as Mgas=SλD2κd(λ)xdBλ(Td),\begin{equation} M_{\rm gas}=\frac{S_{\lambda} D^2}{\kappa_{\rm d}(\lambda) x_{\rm d} B_{\lambda}(T_{\rm d})}, \label{eq7} \end{equation}(7)where Sλ, D, κd(λ), xd, and Bλ(Td) are the integrated flux at 500 μm, the distance, the dust absorption coefficient, the dust-to-gas mass ratio, and the Planck law at the Td dust temperature, respectively. We considered the obtained integrated flux at 500 μm to be of about 50 Jy, a distance of 50 kpc, κd(500 μm) = 1.14 for the LMC (Weingartner & Draine 2001), a Td of about 24 K, and xd = 1.7 × 10-3 (Verdugo et al. 2011) and derived a gas mass of about 7 × 103M⊙. This value is almost two orders of magnitude lower than the mass estimated by Wang et al. (2009) from the 1.2 mm dust continuum. The Mvir/Mgas ratio is higher than unity, as found in several clouds in N11 (Herrera et al. 2013), a bright HII region in the LMC hosting several star clusters.

3.2. Molecular lines

In Figs. 4 and 5 we present the spectra of the molecular lines that were successfully observed towards the position indicated with a black circle in Fig. 1 (right). Figure 4 shows the CO isotopologues and Fig. 5 the emission of the detected rarer lines. The line parameters given in Table 2 were obtained from single-component Gaussian fits. All the spectra have signals well above the 3σ, except for the C18O J = 3 − 2 line, for which the signal is evident but the noise is high. The HNC and HCN lines are detected for the first time towards N113 in the J = 4 − 3 transition. On the other side, the CS J = 7 − 6 line was tentatively detected by Wang et al. (2009), and we confirm its detection here. Our CS central velocity and Δv agree, within the errors, with the previous tentative detection. Taking into account that the critical density of the HCN J = 4 − 3 line is about 108 cm-3 (Takakuwa et al. 2007), we conclude that we observe a high-density molecular clump, which agrees with the conspicuity of the CS J = 7 − 6 line, which also is a tracer of high-density gas.

thumbnail Fig. 4

CO isotopologues obtained towards the centre of N113. The rms noise levels of each spectrum are 80, 35, and 30 mK, respectively, and the channel spacings are about 0.2 km s-1 for 12CO and 13CO, and 0.4 km s-1 for C18O.

thumbnail Fig. 5

Spectra of CS J = 7 − 6 and HCO+, HCN, and HNC J = 4 − 3 obtained towards the centre of N113. The rms noise levels of each spectrum are 14, 90, 20, and 13 mK, respectively, and the channel spacings are about 0.2 km s-1 for CS, HCO+, and HNC, and 1.2 km s-1 for HCN.

Table 2

Line parameters for the molecular lines presented in Figs. 4 and 5.

thumbnail Fig. 6

Spectrum in the frequency range 349.30−349.43 GHz. The arrows indicate the frequencies at which molecular emission lines are expected according to the NIST data base (see Table 3). The rms noise is about 6 mK and the channel spacing is about 0.5 MHz.

Figure 6 shows the obtained spectrum in the frequency range 349.30−349.43 GHz, which is populated by several lines and fine-structure components of C2H and CH3CN. The frequencies at which molecular emission lines are expected according to the NIST data base3 are indicated in the figure and listed in Table 3. In the spectrum presented in Fig. 6 two peaks can be distinguished that are most likely due to the C2H (4–3) fine-structure transitions. The peak centred on 349.342 GHz is composed of two C2H blended hyperfine lines and probably of one line of the CH3CN 19–18 transition. The other peak, centred on 349.403 GHz, is also composed of two C2H blended hyperfine lines. Chin et al. (1997) and Wang et al. (2009) have reported the detection of C2H (1−0) J = 3/2 − 1/2F = 2 − 1 and 1−0 lines towards N113, and here we present the first detection of C2H (4−3) towards this region. It is not possible to confirm the detection of the CH3CN 19(4)−18(4) line, which is probably blended in the peak centred on 349.345 GHz. In addition the non-detection of the CH3CN 18−17 line, a lower transition, also suggests a non-detection for the J = 19 − 18 transition.

Table 3

Molecular lines within the 349.30−349.43 GHz range.

Beuther et al. (2008) observed C2H (4–3) towards a Galactic sample of star-forming regions in different evolutionary stages, including infrared dust clouds (IRDCs), high-mass protostellar objects (HMPOs), and ultracompact HII regions (UCHIIs). They found that the C2H lines are detected independently of the evolutionary stage of the sources, but the UCHIIs regions exhibit line widths in both C2H (4−3) main peaks that are significantly broader than the others objects (on average about 5.5 km s-1). Assuming that the peaks in the spectrum of Fig. 6 are due exclusively to emission of C2H, and converting the frequency into velocity, we measured the FWHM of the two peaks to be 6.8 and 6.4 km s-1, which indicates that both are broad lines like those measured by Beuther et al. (2008) towards UCHIIs. This result agrees with the presence of the compact radio continuum sources detected by Brooks & Whiteoak (1997) in N113. Furthermore, the position at which the molecular lines were observed in this study lies between the two most intense continuum sources in the study of Wong et al. (2006) (sources 2 and 3; IR2 and IR3 in Fig. 1-right). The authors have estimated that the equivalent of one or two O6 stars is needed to produce the measured fluxes in the radio continuum (at 24 and 86 GHz) towards source 2, which, as discussed in their study, are probably young ionizing stars that affect the molecular gas. The C2H can be formed and/or replenished after destruction in earlier stages in PDRs through C2H2 + hν → C2H + H. The neutral-neutral reaction CH2 + C → C2H + H can also produce C2H, where the precursor carbon atom is formed through the photodissociation of CO (Miettinen 2014, and references therein). Therefore, we suggest that the chemistry involving this radical in N113 is similar to the chemistry in Galactic PDRs.

The observed integrated intensity ratios are listed in Table 4 for the lines presented in Table 2, together with a comparison with ratios obtained using the J = 1−0 transitions from Chin et al. (1997) and Wang et al. (2009) for the transitions indicated in the table. Our results agree with the ratios obtained from lower transitions, except for the ratios of HCO+/HCN and HNC/HCO+. The HCO+/HCN ratio is higher than unity, as was found in several Magellanic giant molecular clouds, suggesting that the ion abundance is higher than in Galactic clouds, where this ratio was found to be lower than unity (Stacey et al. 1991; Chin et al. 1997). This must be due to higher UV fields in the Magellanic environments. Additionally, the low nitrogen abundance in the LMC (e.g. Hunter et al. 2007; Bekki & Tsujimoto 2010) can also contribute to the increment of the HCO+/HCN ratio. Furthermore, it seems that the HCO+/HCN ratio increases for increasing rotational transitions, which suggests that the physical conditions in N113 may favour the excitation of the HCO+ higher transitions more efficiently than those of HCN. If the HCO+ and HCN emission occur in the same region, the increment in the HCO+/HCN ratio with the rotational transitions may reflect different critical densities, with HCN being selectively de-excited at higher transitions. Even though the Eu/kB factor is similar in both molecular species, their critical densities vary between different Ju − Jl transitions (ncrit(HCN)/ncrit(HCO+) ~5−7 for J = 1−0, 3–2, and 4–3; Papadopoulos 2007). Similar cases of this HCO+/HCN ratio behaviour were found towards the Galactic NGC 1333-IRAS 2A outflow (Jørgensen et al. 2004) and towards the nuclear region of M82 (Seaquist & Frayer 2000). The HCN/HNC ratio is higher than unity in the J = 4−3 line, as is the case for the lower transitions, which supports the prediction by Chin et al. (1997) that the ratio would be high in warm gas that is subject to strong UV heating, but approaches unity in cloud cores. Wang et al. (2009) also pointed out that HCN/HNC ratio higher than unity may indicate a PDR scenario, which agrees with the C2H chemistry discussed above.

Table 4

Integrated intensity ratios towards N113.

thumbnail Fig. 7

Radex calculations for the HCN J = 4 − 3 and 3–2 lines for kinetic temperatures of 20, 50, and 100 K. The results for HCN J = 1 − 0 are included for comparison with Wang et al. (2009).

Using the derived HCN J = 4 − 3 parameters listed in Table 2 and the HCN J = 3 − 2 and J = 1 − 0 parameters presented in Wang et al. (2009), we performed a non-LTE study of this molecular species using the code RADEX (van der Tak et al. 2007). This code uses the mean escape probability approximation for the radiative transfer equation. As in Wang et al. (2009), we corrected for beam dilution by calculating Tmb′=\hbox{$T_{\rm mb}^{\prime} =$}Tmb/ηbf, with ηbf=θs2/(θs2+θb2)\hbox{$\eta_{\rm bf} = \theta_{\rm s}^{2}/(\theta_{\rm s}^{2} + \theta_{\rm b}^{2})$}, where θb and θs are the beam and the source size. Following Wang et al., a source size of 40′′ was assumed. Then we ran the RADEX code using the measured Δv to fit Tmb′\hbox{$T_{\rm mb}^{\prime}$} for each transition. Figure 7 shows the RADEX calculations for the HCN, displaying the expected H2 density and N(HCN) pairs that correspond to a given Tmb′\hbox{$T_{\rm mb}^{\prime}$} and 4−3/3−2 intensity ratio. The calculations were made for kinetic temperatures of 20, 50, and 100 K, as in previous studies (see Wang et al. 2009 and references therein). The results from the J = 4 − 3 and J = 3 − 2 lines are presented in Table 5. The results from the J = 3 − 2 and J = 1 − 0 lines are similar to those obtained by Wang et al. (2009), that is, a density of several 105 cm-3, and N(HCN) of about 1 × 1013 cm-2. Thus we conclude that the HCN column density ranges from 1.4 × 1012 to about 1 × 1013 cm-2, and the density varies from some 105 to a few 107 cm-3. Our results confirm that the HCN emission arises from a very high density region in N113. The density of this region ranges between the HCO+ and HCN J = 4−3 critical densities, which explains the dependency of the HCO+/HCN ratio on the rotational transitions discussed above.

Table 5

Radex results from the HCN 4–3 and 3–2 lines.

4. Summary

The HII region N113 is located in the central part of the Large Magellanic Cloud (LMC) with an associated molecular cloud that is very rich in molecular species. Most of the molecular lines observed to date cover the frequency range 85–270 GHz, which means that a survey at higher frequencies in the 345 GHz window is required for a more complete understanding of the chemistry and excitation conditions of the region. To do this, we mapped a region of \hbox{$2\farcm5 \times 2\farcm5$} centred on N113 using the Atacama Submillimeter Telescope Experiment in the 13CO J = 3 − 2 line with an angular and spectral resolution of 22′′ and 0.11 km s-1, and observed 16 molecular lines as single pointings towards its centre. The main results are summarized as follows:

  • (1)

    The molecular cloud associated with N113 mapped in the 13COJ = 3 − 2 line shows a curved and elongated morphology that agrees well with the IR emission. From this line we estimated LTE and virial masses for the molecular cloud of about 1 × 104 and 4.5 × 104M⊙, respectively. Additionally, from the dust continuum emission at 500 μm we obtained a gas mass of about 7 × 103M⊙.

  • (2)

    Towards the centre of the N113 molecular cloud we detected emission from 12CO, 13CO, C18O (3–2), HCN, HNC, HCO+, C2H (4–3), and CS (7–6); this is the first reported detection of HCN, HNC, and C2H in the J = 4 − 3 line from this region. We confirmed the detection of CS (7–6), which was previously tentatively detected. The detection of HCN (4–3) and CS (7–6) reveals a very high density region.

  • (3)

    The observed C2H (4–3) presents two peaks due to its fine-structure transitions. We suggest that the chemistry involving C2H in N113 is similar to the chemistry in Galactic PDRs.

  • (4)

    We found that the HCN/HNC ratio is higher than unity in the J = 4 − 3 line, as is the case for lower transitions, supporting the prediction that this ratio would be high in warm gas that is subject to strong UV heating, which in turn indicates a PDR scenario, which agrees with our finding of broad C2H lines. Additionally, we found that HCO+/HCN ratio increases with increasing rotational transitions, showing different critical densities for the two molecular species.

  • (5)

    Using the parameters derived from our HCN J = 4 − 3 observation and previous results from HCN J = 3 − 2 and J = 1 − 0, we performed a non-LTE study of this molecule. Our results confirm that the HCN emission arises from a very high density region in N113, with densities ranging between some 105 and 107 cm-3.

1

Reduction software based on AIPS developed at NRAO, extended to treat single-dish data with a graphical user interface (GUI).

2

XSpec is a spectral line reduction package for astronomy that has been developed by Per Bergman at Onsala Space Observatory.

Acknowledgments

We thank the anonymous referee for her/his helpful comments and corrections. The ASTE project is led by Nobeyama Radio Observatory (NRO), a branch of National Astronomical Observatory of Japan (NAOJ), in collaboration with University of Chile, and Japanese institutes including University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University, Hokkaido University, and the Joetsu University of Education. S.P. and M.O. are members of the Carrera del investigador científico of CONICET, Argentina. This work was partially supported by grants awarded by CONICET, ANPCYT and UBA (UBACyT) from Argentina. M.R. wishes to acknowledge support from CONICYT through FONDECYT grant No. 1140839.

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All Tables

Table 1

Observed molecular lines towards N113.

In the text
Table 2

Line parameters for the molecular lines presented in Figs. 4 and 5.

In the text
Table 3

Molecular lines within the 349.30−349.43 GHz range.

In the text
Table 4

Integrated intensity ratios towards N113.

In the text
Table 5

Radex results from the HCN 4–3 and 3–2 lines.

In the text

All Figures

thumbnail Fig. 1

Left: three-colour image where the 8, 24, and 70 μm emission obtained from the IRAC and MIPS cameras of the Spitzer Space Telescope (from SAGE Spitzer; Meixner et al. 2006) are presented in blue, green, and red, respectively. The black box shows the region mapped in the 13CO J = 3 − 2 line with an angular resolution of 22′′. Right: zoom-in of the mapped region (white box). The colour code is the same as in the left image, but the scales are different. The red contours correspond to the 13CO J = 3 − 2 emission integrated between 230 and 245 km s-1 with levels of 2.5, 4.0, 6.0, and 8.0 K km s-1. The FWHM beam size of the observations is included in the bottom right corner of the region. The black circle corresponds to the position where the 16 molecular lines were observed as single pointings.
In the text
thumbnail Fig. 2

Integrated velocity channel maps of the 13CO J = 3 − 2 emission every 1 km s-1. The greyscale is displayed at the top of the first panel and is in K km s-1, the contour levels are 0.3, 0.7, 1, 2, and 2.5 K km s-1.
In the text
thumbnail Fig. 3

500 μm emission obtained from SPIRE in the Herschel Space Observatory (from Herschel HERITAGE; Meixner et al. 2010, 2013) with the same 13CO J = 3 − 2 contours as shown in Fig. 1 (right). The FWHM beam size of the molecular observations is included in the top left corner. The angular resolution of the SPIRE image is about 36′′.

In the text
thumbnail Fig. 4

CO isotopologues obtained towards the centre of N113. The rms noise levels of each spectrum are 80, 35, and 30 mK, respectively, and the channel spacings are about 0.2 km s-1 for 12CO and 13CO, and 0.4 km s-1 for C18O.
In the text
thumbnail Fig. 5

Spectra of CS J = 7 − 6 and HCO+, HCN, and HNC J = 4 − 3 obtained towards the centre of N113. The rms noise levels of each spectrum are 14, 90, 20, and 13 mK, respectively, and the channel spacings are about 0.2 km s-1 for CS, HCO+, and HNC, and 1.2 km s-1 for HCN.
In the text
thumbnail Fig. 6

Spectrum in the frequency range 349.30−349.43 GHz. The arrows indicate the frequencies at which molecular emission lines are expected according to the NIST data base (see Table 3). The rms noise is about 6 mK and the channel spacing is about 0.5 MHz.
In the text
thumbnail Fig. 7

Radex calculations for the HCN J = 4 − 3 and 3–2 lines for kinetic temperatures of 20, 50, and 100 K. The results for HCN J = 1 − 0 are included for comparison with Wang et al. (2009).

In the text

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