VizieR Online Data Catalog: NGC 1333-IRAS4A radio images (Taquet+, 2020)

For the SOLIS data, the IRAS4A binary system was observed in three different Setups (1, 3, and 5) with the IRAM NOEMA interferometer during several tracks in June and September 2016 (see Table 1 of Ceccarelli2017). Setup 1, 3, and 5 cover the frequency ranges from 80.8GHz to 84.4GHz, from 95.7GHz to 99.5GHz, and between 204.0 and 207.6GHz, respectively. For Setups 1 and 3, the array was used in both configurations D and C with baselines from 16m to 240m for Setup 1 and from 15m to 304m for Setup 3. For Setup 5, the array was used in configurations A and C. The phase centre is on the IRAS4A1 source, alpha(J2000)=03:29:10.5, delta(J2000)=+31:13:30.9. The bandpass was calibrated on 3C454.3 and 3C84, the absolute flux was fixed by observing MWC349, LKHA101, 2013+370, and 2007+659, and 0333+321 was used to set the gains in phase and amplitude. The final uncertainty on the absolute flux scale is less than 15%. The phase rms was less than 50 degrees, the typical precipitable water vapour (pwv) was from 4mm to 15mm, and the system temperatures ranged typically between 50 and 200K. The data were reduced using the packages CLIC and MAPPING of the GILDAS software collection. A continuum map was obtained by averaging line-free channels and self calibrating the data. The self calibration solutions were then applied to the spectral cube, which was subsequently cleaned. The resulting synthesised FWHM beam is 4.5x3.5arcsec (P.A.=27-degrees) for Setup 1, 2.2x1.9arcsec (P.A.=96-degrees) for Setup 3, and 0.9x0.7-arcsec (P.A.=47-degrees) for Setup 5. The half power primary beam is 61.4, 59.2, and 24.5arcsec for Setups 1, 3, and 5 respectively.

We used the CALYPSO data observed with the IRAM-PdBI (Maury et al., 2019A&A...621A..76M) to extract the interferometric maps from the SiO(5-4), SO(6_5-54), and OCS(8-7) transitions at 218GHz. These observations were carried out between February 2011 and February 2013 as part of the CALYPSO Large Program using the A and C configurations of the array. The synthesised FWHM beam at 1.4mm is 1.1x0.8arcsec. More details on the observational properties can be found in (Santangelo et al., 2015A&A...584A.126S).

IRAS4A was observed with the IRAM PdBI at 145 and 165 GHz on 2010 July 20, 21, August 1, 3, November 24, and 2011 March 10 in the C and D most compact configurations of the array. The baseline range of the observations is 25m-140m, allowing us to recover emission on scales from 10^-15arcsec to 2arcsec. The WIDEX backends have been used at 143.4 and 165.2GHz, providing a bandwidth of 3.6GHz each with a spectral resolution of 1.95MHz (3.5-4km/s). High-resolution narrowband backends focused on two CH₃OH lines have also been used. They provide a bandwidth of 80MHz with a spectral resolution of 0.04MHz (0.08km/s). We decreased the spectral resolution to 0.40MHz (0.8km/s) to obtain a better signal-to-noise. More details on the observational dataset can be found in Taquet et al. (2015ApJ...804...81T). PdBI observations at 225GHz were performed on 27 and 28 November 2011, on 12, 15, 21, 27 March 2012, and on 2 April 2012 in the B and C configurations of the array. The synthesised FWHM beam is 1.2"x1.0". A more detailed description of the observational setups is provided by Persson et al., 2014A&A...563A..74P. For all datasets, the amplitude calibration uncertainty is estimated to be 15-20%. Given we map relatively extended structures such as outflow lobes, we cleaned the images using the Hogbom method with natural weighting and with a mask containing all the molecular lobes to minimise artefacts in the cleaned image.

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