Atacama Large Millimeter/submillimeter Array (ALMA) ######################## Publications making use of these data must include the following statement in the acknowledgement: "This paper makes use of the following ALMA data:ADS/JAO.ALMA#2011.0.00009.E. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ." In addition, publications from NA authors must include the standard NRAO acknowledgement: "The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." ################################################################################### SUMMARY: This Readme file contains a description of R Lep Band 9 long baseline testing data, scripts and data products. There is one ALMA execution block (ASDM) observed in the FDM observing mode. This is Band 9 data and used Walsh Switching to provide 8 SPWs. 8x SPW use a FDM setup with 1920 channels (1.875 GHz BW) The native angular resolutions of the target image is 7 x 6 mas (milli-arcsec) There are no image cubes made as there are no _obvious_ line emission features The Calibrated Data and Reference Images provided here were produced using CASA version 6.4.1-12 ######################## COMMENTS: These are ALMA commissioning test data of the evolved star R Lep taken at Band 9 using the FDM observing mode. These are part of the High Frequency Long Baseline campaign undertaken in 2021 (HF-LBC-2021). These data were taken for new imaging capaility commissioning. The overview of this work and notes on the technical tests related to the observations of R Lep is detailed in the paper for the campaign: Asaki, Y., Maud, L.T. et al. 2023 ApJS Note there other papers related to ALMA long baselines campaign efforts. There is a single dataset for the observation. These are band-to-band (B2B) testing data, in which scheduling blocks were used to undertake similar to science-style observations. This particular B2B mode used a high frequency (for the target) of Band 9, while the calibrator used a lower frequency, the low frequency used was Band 4. A strong source, called the Differential Gain Calibration (DGC) source is observed - changing between low- and high- frequencies to solve the band offsets and facilitate the phase transfer. The bandpass is J0522-3627 which also acted as the DGC source. During calibration correct scans were selected for the purposes of BP or DGC solutions. J0522-3627 was also used for amplitude scaling at both bands 4 and 9 because it is a consistent source in all the HF LBC 2021 campaign datasets of R Lep. J0423-0120 is listed as the flux calibrator but it is not used as such due to not matching the other test data Bands. Note that the phase calibrator was observed at Band 4, as per the B2B mode. Imaging was then conducted using TCLEAN. The imaging uses auto-masking cleaning. The imaged region is small as to improve imaging speed, but can be changed in the supplied scripts as required. Self-calibration was performed using the continuum R Lep before selfcal: * Peak: 0.0264 Jy/bm * Flux: 0.111 Jy * Noise: 0.000306 Jy/bm * Dyn. Range: 86 * Beam: 0.007" x 0.006" @ -52.4 deg R Lep after selfcal (this causes flags to longest baselines): * Peak: 0.0639 Jy/bm * Flux: 0.128 Jy * Noise: 0.000305 Jy/bm * Dyn. Range: 210 * Beam: 0.011" x 0.009" @ 13.3 deg R Lep before selfcal - WITH - flags from selfcal process * Peak: 0.0529 Jy/bm * Flux: 0.111 Jy * Noise: 0.000493 Jy/bm * Dyn. Range: 107 * Beam: 0.011" x 0.009" @ 13.3 deg ######################## RLep_B9_B2B_Scripts.tgz contains the calibration and imaging scripts: * uid___A002_Xf07268_X32f0.ms.scriptForCalibration.py * RLep_B9_B2B.scriptForSelfcalAndImaging.py RLep_B9_B2B_UncalibratedData.tgz contains the raw data: ASDM dataset: * uid___A002_Xf07268_X32f0 RLep_B9_B2B_CalibratedData.tgz contains the calibrated uv-data, these are BEFORE selfcal is applied, which occurs in the imaging scripts: * uid___A002_Xf07268_X32f0.ms.split.cal * uid___A002_Xf07268_X32f0.ms.split.cal.flagversions To re-create these calibrated datasets you would need to execute the calibration script (e.g uid___A002_Xf07268_X32f0.ms.scriptForCalibration.py) as provided. RLep_B9_B2B_ReferenceImages.tgz contains the continuum image products: * JJ0522-3627_bp.spw33_35_37_39_41_43_45_47.cont.* * J0522-3627_dgc.spw33_35_37_39_41_43_45_47.cont.* * J0423-0120_flux.spw33_35_37_39_41_43_45_47.cont.* * J0438-1251_chk.spw33_35_37_39_41_43_45_47.cont.* * J0504-1512_ph.spw64_66.cont.* * J0522-3627_dgc.spw64_66.cont.* * R_Lep_sci.spw33_35_37_39_41_43_45_47.cont.I.manual.* * R_Lep_sci.spw33_35_37_39_41_43_45_47.cont.I.manual-selfcal.* * R_Lep_sci.spw33_35_37_39_41_43_45_47.cont.I.manual-dataselfcalflags.* All images can be re-created by executing the imaging script (RLep_B9_B2B.scriptForSelfcalAndImaging.py). ################################################################################### HOW TO EXECUTE THE CALIBRATION SCRIPTS (1) Put an ALMA ASDM and the corresponding calibration script in the same directory (2) In CASA 6.4.1-12 execfile('uid___A002_Xf07268_X32f0.ms.scriptForCalibration.py') HOW TO EXECUTE THE IMAGING SCRIPT (1) ensure the split.cal MS and imaging script are in the same directory (2) execfile('RLep_B9_B2B.scriptForSelfcalAndImaging.py')