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Top panels : (A) Observed infrared emission towards VLA1, (B) VLA4 and (C) the Cohen-Schwartz star (CS star). The spectra for VLA4 and the CS star correspond to those obtained with a POFV of 3 arcsec while for VLA1+VLA2 we show the spectra observed in both CVFs. Note the emission through the three infrared windows. Panel (D) shows the observed infrared emission around VLA1+VLA2 with a PFOV of 3 arcsec. (E) Optical17 image [SII 6717/31 E] of the central HH1-2 region (colors) with a superposition (contours) of the IR emission detected with the LW2 filter of ISOCAM. The positions of the VLA1 & 2 &4 sources are indicated by white filled circles. The position towards which we have discovered the three infrared windows is indicated by a black filled square and coincides, within the astrometric errors, with that of VLA1+VLA2 objects; the red circle indicates the PFOV the infrared observations (6 arcsec). (F) Optical image (same as before) with the contours of the continuum emission at 1.3 mm (1300 mm as observed with the 30-m IRAM radiotelescope). The contours are between 0.04 and 0.4 Jy/beam and show the presence of a core centered on VLA1+VLA2 surrounded by an extended envelope indicating the Class 0 nature of the powering engine of the HH1-2 system (see text). (G,H,I) Optical image (as above) with the corresponding infrared emission in the 5.3 and 6.6 mm windows minus the adjacent continuum (G); the total continuum emission between 5 and 7 mm (H), and the total continuum emission between 13 and 14 mm (I). In these three figures the emission of the source VLA4 has been removed by fitting the ISOCAM PSF to the CVF spectra. Image credit: Science journal
Last Update: 31 August 2019
23-Sep-2020 07:41 UT

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