The CHESS survey of the L1157-B1 shock: the dissociative jet shock as revealed by Herschel–PACS††thanks: Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Key Words.:stars: formation - ISM: individual objects: L1157 - ISM: molecules - ISM: jets and outflows
Outflows generated by protostars heavily affect the kinematics and chemistry of the hosting molecular cloud through strong shocks that enhance the abundance of some molecules. L1157 is the prototype of chemically active outflows, and a strong shock, called B1, is taking place in its blue lobe between the precessing jet and the hosting cloud. We present the Herschel-PACS 55–210 m spectra of the L1157-B1 shock, showing emission lines from CO, HO, OH, and [O i]. The spatial resolution of the PACS spectrometer allows us to map the warm gas traced by far-infrared (FIR) lines with unprecedented detail. The rotational diagram of the high- CO lines indicates high-excitation conditions ( 210 10 K). We used a radiative transfer code to model the hot CO gas emission observed with PACS and in the CO (13–12) and (10–9) lines measured by Herschel-HIFI. We derive 200800 K and cm. The CO emission comes from a region of about 7 located at the rear of the bow shock where the [O i] and OH emission also originate. Comparison with shock models shows that the bright [O i] and OH emissions trace a dissociative J-type shock, which is also supported by a previous detection of [FeII] at the same position. The inferred mass-flux is consistent with the “reverse” shock where the jet is impacting on the L1157-B1 bow shock. The same shock may contribute significantly to the high- CO emission.
Shocks from protostellar outflows heat and compress the surrounding medium, triggering chemical processes that enrich the chemical composition of the environment of young stars (see e.g. Bachiller et al., 2001). Although outflows and shocks have been studied since the eighties, we are still far from a clear understanding of the interaction between the jet/outflow and the ambient cloud. In particular, studies based on the Infrared Space Observatory (ISO) data have shown that the atomic and molecular lines emitted in the FIR range significantly contribute to the cooling of the shocked material in outflows. However, because of the large ISO beam (80) only information averaged along a large part of the outflow lobe could be inferred, and a mixture of both continuous C-type and dissociative J-type shocks has been suggested to be responsible for the excitation of the observed FIR lines (e.g. Giannini et al., 2001; Flower & Gusdorf, 2009).
In the outflow powered by the L1157-mm Class 0 protostar at a distance of 250 pc (Looney et al., 2007), more than 20 species have been detected in the southern, blue-shifted lobe (Bachiller et al., 2001; Arce et al., 2008). The brightest shock, B1, has been extensively observed in several molecular species at millimetre (Gueth et al., 1996, 1998; Benedettini et al., 2007; Codella et al., 2009), near-infrared (Nisini et al., 2010a) and FIR wavelengths (Giannini et al., 2001; Nisini et al., 2010b), revealing a complex structure with various shock tracers peaking at different positions. Previous modelling concluded that a (possibly non-stationary) C-type shock is taking place in B1 (Gusdorf et al., 2008; Neufeld et al., 2009; Viti et al., 2011).
Because of its chemical richness, L1157-B1 was selected to be observed with the HIFI (de Graauw et al., 2010) and PACS (Poglitsch et al., 2010) spectrometers on board Herschel (Pilbratt et al., 2010), as part of the Chemical Herschel Survey of Star forming regions (CHESS) Key Program (Ceccarelli et al., 2010). The first results obtained by HIFI confirm the chemical richness of B1 (Codella et al., 2010), including the first detection of HCl in shocked gas (Codella et al., 2011). They also reveal a high-velocity gas with higher HO abundance and excitation conditions than the bulk of the emission, and tracing a more compact region within B1 (Lefloch et al., 2010).
In this letter we present the PACS spectra of L1157-B1, focusing our analysis on the high- CO, OH and [O i] lines with the aim of investigating the high-excitation gas component. The HO lines will be analysed in a forthcoming paper.
2 Observations and data reduction
The range spectroscopy mode of the PACS instrument was used to obtain the full range spectrum towards L1157-B1 (RA(J2000) = 2039102, Dec(J2000) = +6801105). Two observations were carried out on May 25, 2010, covering the spectral ranges 55–95.2m and 101.2–210 m. The resolving power ranges between 1000 and 4000, depending on wavelength and order. The PACS field of view (FOV) of 47 47 is composed of 55 spatial pixels (spaxels) providing a spatial sampling of 94/spaxel, with a position angle of 6183. Our observations were carried out in staring mode, i.e. our maps are not Nyquist-sampled with respect to the point spread function (PSF). The data were reduced with the HIPE111HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, The NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. v5.0 package. The flux calibration was performed by calculating the ratio between the source flux and the telescope background, and subsequently multiplying by the spectrum of Neptune. This procedure gives a flux accuracy of about 10% shortwards of 190 m, while at longer wavelengths the flux calibration is much more uncertain, which caused us to exclude the CO (13–12) line at 200.25 m in the analysis. Post-pipeline reduction steps were performed to extract the spectrum of each of the 25 spaxels, to calculate the line fluxes with a Gaussian fitting of the line profile and to produce line intensity maps.
|(m)||(10 W m/spaxel)|
This line is affected by a large flux calibration error and it is not considered in the analysis.
Table 1 lists the line fluxes of the analysed species, namely CO, OH and [O i], detected at the centre of the FOV (the nominal position of B1) and towards the PACS emission peak, located at offset (5, 7) with respect to the centre of the FOV. The spectra of these two spaxels are shown in Figs. 6 and 7. The spectral range between 161.5 m and 190.2 m was observed in the two observations; the fluxes of the lines detected in both scans generally agree within the errors and in any case never differ by more than 20%, therefore we consider the averaged value in the following analysis.
Figure 1 presents the maps of the CO lines from (14–13) to (22–21). The emission peaks towards spaxel (5,7), with an elongation towards south-east. The deconvolved full with at half maximum (FWHM) size of the CO peak, estimated by subtracting in quadrature the FWHM of the PSF, ranges between 5and 10 depending on wavelength, with a mean value of 7, hence marginally resolved in these observations. The emission from [O i] and OH peaks in the same spaxel as high- CO. In Fig. 2 we show the CO (14–13) and [O i] 63 m PACS maps superimposed on tracers of postshock gas such as SiO (2–1) (Gueth et al., 1998) and CHCN (8–7) (Codella et al., 2009) observed with the Plateau de Bure at a resolution of 3. While both SiO and CHCN trace an extended bow shock at the tip of the outflow cavity traced by CO (1–0) (Gueth et al., 1996), it is clear that high- CO, OH and [O i] are peaking in a different region, at the rear of this bow shock. On the other hand, [O i], OH and high- CO lines correlate well with the [Fe ii] at 26 m (Neufeld et al., 2009), the H ro-vibrational line 1-0 S(1) (Caratti o Garatti et al., 2006) that traces hot gas (2500 K) as well as with the pure H rotational lines tracing gas at temperatures between 200 and 1400 K (Nisini et al., 2010a). This indicates that the FIR PACS lines trace a more compact and more excited region than the bulk of the B1 bow shock, most probably the “jet-shock” where the jet powered by the protostar is impacting on the internal cavity wall.
3.2 Physical conditions in the high- CO emitting gas
In order to look for possible spatial gradients of the physical conditions in the CO gas, we calculated the excitation temperatures, which gives a lower limit to the kinetic temperature if the gas is not in local thermodynamic equilibrium (LTE). To correct for the different beam sizes, we convolved all CO line maps to the resolution of the transition with the longest wavelength, i.e. 131 (PSF at 186 m) and then extracted the fluxes at the position of each spaxel. The fluxes for spaxels (5,7) and (0,0) are reported in Table 2. We then constructed the corresponding rotation diagrams for each spaxel, as illustrated in Fig. 3 for three positions. The CO lines in B1 are optically thin for 9, as indicated by the CO lines detected with HIFI (Lefloch et al., 2012), thus the slope of the diagram gives directly 1/. We find a similar excitation temperature K at all positions, indicating that the excitation conditions are fairly uniform, although at offset (9,2) the excitation temperature is slightly higher, 241 K. In fact, a secondary peak of H1-0 S(1) is observed at this position (see Fig. 2) where Nisini et al. (2010a), from the H lines, derived a temperature about 100 K higher than at the CO peak. The total column density of CO averaged over 131, assuming LTE, ranges from 210 cm at (9,2) to 610 cm at (5,7).
Constraints on the kinetic temperature and density of the CO gas were obtained using the radiative transfer code RADEX (Van der Tak et al., 2007) in a plane-parallel geometry. We used the collisional rate coefficients with H of Yang et al. (2010) and built a grid of models with density between 10 cm and 10 cm and temperature between 10 K and 10 K. In Fig. 4 the region of minimum is shown as a function of density and temperature for the CO peak at (5,7). The best fit is obtained for 210 cm and =1080 K, but other fits at lower temperatures combined with higher densities are also possible (see Fig. 9), including the LTE solution.
Additional constraints on physical conditions are provided by the CO lines observed with HIFI towards the (0,0) position that, as shown by the rotational diagram, has the same excitation condition of offset (5,7). Indeed, line profiles in CO (16–15) and CO (13–12) reveal a specific spectral shape for the excited CO component dominating the PACS range (Lefloch et al., 2012). Its flux contribution to CO (10–9) can then be extracted and scaled to 131 by assuming the same spatial distribution as for CO (16–15). The simultaneous fitting of the HIFI and PACS fluxes clearly excludes low-density / high-temperature solutions (Fig. 4 right panel). The best fit now has =580 K and =210 cm but still with a wide range of acceptable parameters, 2001100 K for cm (Fig. 8).
Tighter limits come from the comparison of the CO column density at (-5”,7”) inferred from RADEX fits with the H column density at the same position and temperature derived from Spitzer data (Nisini et al., 2010a), averaged over the same beam. We find that the ratio (CO)/(H) is (0.3–2) for the best CO fits at of 200 and 580 K, respectively. In contrast, the CO relative abundance increases to unphysically high values for 800 K. This clearly favours dense and moderately warm gas (200800 K, and cm). From these best-fit models we calculate a total cooling of (CO) = 0.004 L at the CO peak and an intrinsic CO column density (CO)= 210 cm, assuming the size of 7 derived from PACS maps.
3.3 [O i] and OH lines: Evidence for a dissociative jet-shock
In the left panel of Fig. 5, the surface brightness of the [O i]145m line (obtained using an upper limit to the size of 7) is compared with shock-model predictions from Flower & Pineau des Forêts (2010). The [O i]145/63 line ratio indicates that both lines are optically thin, but we used the [O i]145m line for this comparison, because the 63m line may be affected by foreground absorption, as usually found by ISO (Liseau et al., 2006). Evidently only dissociative J-type shocks, with velocity km s for =210 cm and km s for =210 cm, can match the observed [O i]145m brightness. Non-dissociative shocks (of both J- and C-type) underpredict this line by at least two orders of magnitude. This conclusion is also supported by the detection of [Fe ii] at 26 m and [S i] at 25 m (Neufeld et al., 2009) at the [O i] peak; the iron and sulfur fine structure lines are excited only in dissociative shocks. In particular, the [O i]/ [S i] observed intensity ratio is consistent with both lines originating from a J-shock with the same conditions as inferred above (Hollenbach & McKee, 1989). The same models underpredict the [O i]/[Fe ii] but this is likely because the iron is partially depleted on grains. Shock models reproducing the [O i] brightness predict a ratio of CO to [O i] total luminosity within a factor of a few of the observed one (see Fig. 5 right panel), therefore the dissociative J-shock traced by [O i] may also contribute to the high- CO emission.
The sum of the three OH doublets at 79 m, 84 m, and 119 m (see Table 3) amounts to three times the [O i]145m line, consistent with both species tracing the same dissociative J-shock (Hollenbach & McKee, 1989). Moreover, the ratio of OH to CO luminosity is an order of magnitude higher than predicted for C-shocks (Kaufman & Neufeld, 1996). Indeed, in C-shock all oxygen not locked in CO is converted in water, while in dissociative J-shocks the presence of FUV photons produced at the shock front delays the full conversion of free oxygen into water and maintains a significant abundance of OH. Interestingly, both the relative intensities of the OH doublets in L1157-B1 and the ratios of each OH doublet to [O i]145m and to , are very similar to those observed much closer to low-mass protostars (Wampfler et al., 2010; Herczeg et al., 2011). This suggests that, OH may not be excited by infrared pumping, but predominantly by dissociative J-shocks in outflows far away as well as close to the source.
In dissociative J-type shocks, the [O i]63m luminosity is proportional to the mass flux into the shock, which is close to the wind mass-flux in a slow moving wind-shock (Hollenbach, 1985). Considering the total flux of the [O i]63m line in the PACS FOV ( W/m), we derive ([O i]63m) = 0.002 and ([O i])= 210 Myr in the blue lobe. We may compare this value to independent estimate derived from the momentum and age of the blue outflow lobe traced by CO (1–0) by Bachiller et al. (2001). Rescaling the value these authors derived for a distance of 440 pc to our adopted distance of 250 pc, we infer (CO) = 6 Myr under the assumption of outflow-wind momentum conservation and wind velocity of 100 km s. Given the large uncertainties in the outflow age (Downes & Cabrit, 2007) and possible self-absorption in the [O i]63m line, the two estimates are consistent and agree reasonably well with a jet-driven shock accelerating the outflow as the main excitation mechanism of [O i] in B1.
In the Herschel-PACS spectrum of the B1 shocked region of the L1157 outflow, emission lines from CO, HO, OH and [O i] have been detected. The analysis of the high- CO lines with a radiative transfer code has allowed us to constrain the physical conditions of the warm (200 K) and dense ( cm) gas. The spatial resolution of PACS, unprecedented at FIR wavelengths, has shown that CO, OH and [O i] all surprisingly peak at the rear of the bow shock, where others tracers of J-type shocks such as ro-vibrational H and [Fe ii] were also detected. The intensity of the bright [O i] lines clearly indicates for the first time that a dissociative “reverse” wind-shock is the dominant exciting mechanism of these lines. The (CO) and (OH) are also consistent with a J-type shock. Our analysis reveals that the C-shock previously found in B1 appears to give only a minor contribution to the emission of [OI], OH, and high- CO lines detected in the PACS spectra.
Acknowledgements.PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain)
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In Fig. 6 and 7 we show the PACS spectra at the centre of the FOV (the nominal position of B1) RA(J2000) = 2039102, Dec(J2000) = +6801105 and towards the PACS emission peak, at position RA(J2000) = 203993, Dec(J2000) = +6801178, located at offset (5; 7) with respect to the centre of the FOV.
In Table 2 we list the fluxes at offset (0,0) and (5,7) extracted from the line maps convolved at the diffraction size of the CO transition at the highest wavelength, i.e. 131 (PSF at 186 m). They were obtained by multiplying the line surface brightness by an area of 1.133 131, and were used for the rotational diagram and the RADEX modelling, assuming the same source area.
|Line||Flux offset (5,7)||Flux offset (0,0)|
|(m)||(10 W cm)||(10 W cm)|
In Table 3 we list the fluxes of the OH lines measured at offset (5,7). Since the OH lines were detected only in one spaxel, we applied the flux correction for a point source that takes into account the size of the PSF.
In Fig. 8 we show the comparison between the CO line fluxes at the centre of the PACS FOV, offset (0,0), and three models: the best-fit model obtained considering only the PACS lines ( 14) with 210 cm and 1080 K; the best-fit model obtained considering also the HIFI CO (13–12) and (10–9) lines with 210 cm and 580 K and the LTE model with kinetic temperature equal to the excitation temperature derived from the rotational diagram, with 210 cm and 207 K. In Fig. 9 the same models are shown compared to the CO line fluxes at the peak of the CO emission, i.e. offset (5,7).