2. Observations and results
L1448-mm ( = , = 30o 33 35) was observed with the LWS (Long Wavelength Spectrometer, Clegg et al. 1996) and SWS (Short Wavelength Spectrometer, de Graauw et al. 1996) on the ISO satellite. In Fig. 1 the apertures of the two instruments are superimposed on a 2.12 µm map of L1448 to show the region covered by the observations.
2.1. LWS observations
A low resolution (R 300) spectrum of the source extending from 45 to 197 µm was obtained with the LWS during revolution 653 (August 30, 1997). The spectrum was oversampled by a factor of four and each spectral sample had 10 s integration, for a total integration time of 4265 s. The raw data were reduced and calibrated using version 7 of the LWS pipeline, which resulted in an absolute intensity calibration within 30% (Swinyard et al. 1996). Post-pipeline processing included the removal of spurious signals resulting from cosmic ray impacts, and averaging of the various grating scans from each detector. The line fluxes, obtained from gaussian fitting to the spectral profiles, are listed in Table 1, where the associated errors refer to the rms noise of the local baseline. We show in Fig. 2 the global spectrum obtained by merging together the sub-spectra obtained from the ten LWS detectors just to give an idea of the relative contribution of the line emission with respect to the underline continuum, while a detailed account for the FIR continuum emission of the mm source will be given elsewhere (Nisini et al. 1999, Paper II).
Table 1. Emission lines measured with LWS toward L1448-mm
Fig. 3 shows the continuum subtracted (by second order polynomial fitting) spectrum from 50 to 190 µm while in Fig. 4 the [OI ] 63µm line is plotted. The spectrum appears extremely rich in rotational lines of both carbon monoxide and water vapour. All the CO transitions with J from 14 (the lowest transition observable with the LWS, at 186 µm) to 21 were detected. The J=22 line is not seen to a 3 level of 7 10-20 W cm-2, but the J=25 line at 104.5 µm is clearly detected with a S/N of about 5. The J=23, 24 and 26 lines are blended with strong H2O transitions which have a FWHM slightly broader than the instrumental resolution element of 0.6 µm. An attempt to deblend with a two gaussian fit was made for the J=26 and J=24 lines, which are separated from the adjacent p-H2O 220-111 and o-H2O 221-110 lines by about 0.5 and 0.6 µm. The CO J=23 at 113.46 µm is however too close to the o-H2O 414-303 line (at 113.54 µm) to permit a meaningful deblending. The fact that the observed line peaks at 113.65 µm suggests however that most of the flux can be attributed to the water line.
Water lines are observed in both the ortho and para form; almost all the backbone lines up to excitation temperatures of about 500 K are present, plus most of the strongest transitions which fall in the LWS spectral range (see Fig. 6). In addition to CO and water, the OH fundamental at 119 µm (a blend of the four low-lying transitions of the 3/2 ladder) is also observed. An upper limit to the 99 µm line of OH 5/2-3/2 was set by attempting to deblend it from the nearby o-H2O 505-414 line at 99.5 µm. The [CII ] 158µm and [OI ] 63µm lines are the only atomic emission lines present in the spectrum.
2.2. SWS observations
The SWS was used in the AOT SWS02 mode to scan the H2 pure rotational lines from S(1) to S(7) and the [SiII ] 35µm line with a resolution ranging from 1000 to 2000. The beam sizes of these observations (obtained during revolution 814, on February 6, 1998) are 14"20" for the lines from S(3) to S(7), 14"27" for the S(1), S(2) and 20"27" for [SiII ].
Each line was integrated for a total time of 200 s. The data were reprocessed through the SWS pipeline version 6; systematic flux errors due to the SWS calibration uncertainties are estimated to be about 30% (Schaeidt et al. 1996). Of the scanned lines, only the H2 S(3), S(4) and S(5) were detected and their spectrum is shown in Fig. 5. The measured and upper limits fluxes are reported in Table 2.
Table 2. Emission lines measured with SWS towards L1448-mm
© European Southern Observatory (ESO) 1999
Online publication: October 4, 1999