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#2011.0.00006.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 10 long baseline testing data, scripts and data products. There is one ALMA execution block (ASDM) observed in the FDM observing mode. This is Band 10 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 X x X mas (milli-arcsec) There is a HCN maser in SPW 45, this is imaged in a small cube. The peak emission channel is also imaged and used for self-calibration 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 10 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 10, while the calibrator used a lower frequency, the low frequency used was Band 7. 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 7 and 10 because it is a consistent source in all the HF LBC 2021 campaign datasets of R Lep. Note that the phase calibrator was observed at Band 7, as per the B2B mode. The Check source J0423-0120 is located ~17deg from the phase calibrator is thus is not useful to 'check' the phase transfer as it is too far away, also see Maud et al 2023 ApJS Imaging was then conducted using TCLEAN. The conitnuum imaging uses auto-masking cleaning, while the very bright maser emission uses a manual mask due to the larger than anticipated flux that causes automask issues. The imaged region (size) is small as to improve imaging speed, but can be changed in the supplied scripts as required. Self-calibration was performed using the continuum first (that caused lots of flags for low SNR on long baselines), while subsequently the flags were restored and selfcal from the peak channel of the HCN maser was used (>700 Jy) R Lep continuum before selfcal: * Peak: 0.0231 Jy/bm * Flux: 0.194 Jy * Noise: 0.00084 Jy/bm * Dyn. Range: 27 * Beam: 0.0049" x 0.0047" @ -35.8 deg R Lep continuum after CONTINUUM selfcal (this causes flags to longest baselines): * Peak: 0.1705 Jy/bm * Flux: 0.242 Jy * Noise: 0.0018 Jy/bm * Dyn. Range: 95 * Beam: 0.0192" x 0.0163" @ -50.5 deg R Lep continuum before selfcal - WITH - flags from CONTINUUM selfcal process * Peak: 0.1302 Jy/bm * Flux: 0.205 Jy * Noise: 0.0020 Jy/bm * Dyn. Range: 65 * Beam: 0.0192" x 0.0163" @ -50.5 deg R Lep continuum after HCN maser selfcal (restored origional flags) * Peak: 0.0360 Jy/bm * Flux: 0.242 Jy * Noise: 0.00091 Jy/bm * Dyn. Range: 40 * Beam: 0.0053" x 0.0048" @ -26.695 deg ******************************************************* R Lep HCN maser before selfcal (restored origional flags) * Peak: 731.45 Jy/bm * Noise: 0.065 Jy/bm (away from channels with emission) ~7 to 8 Jy/bm (in channels with strong emission) * Dyn. Range: 91 (at peak emission, in peak channel) * Beam: 0.0056" x 0.0049" @ -19.4 deg R Lep HCN maser after HCN maser selfcal (restored origional flags) * Peak: 1225.49 Jy/bm * Noise: 0.064 Jy/bm (away from channels with emission) ~3.0 Jy/bm (at the peak emission channel) * Dyn. Range: 408 * Beam: 0.0055" x 0.0049" @ -25.7 deg Note: values above measured in CASA viewer with imhead output for the beam. Some images were repeatedly reprocessed with minor flag diffrences depending on the compute node running the processing and imaging for the paper, and may not match _exactly_ the documented number. E.g. continuum selfcal only images, peak of HCN maser cube post-selfcal ######################## RLep_B10_B2B_Scripts.tgz contains the calibration and imaging scripts: * uid___A002_Xf06573_X20d3.ms.scriptForCalibration.py * RLep_B10_B2B.scriptForSelfcalAndImaging.py RLep_B10_B2B_UncalibratedData.tgz contains the raw data: ASDM dataset: * uid___A002_Xf06573_X20d3 RLep_B10_B2B_CalibratedData.tgz contains the calibrated uv-data, these are BEFORE selfcal is applied, which occurs in the imaging scripts: * uid___A002_Xf06573_X20d3.ms.split.cal * uid___A002_Xf06573_X20d3.ms.split.cal.flagversions To re-create these calibrated datasets you would need to execute the calibration script (e.g uid___A002_Xf06573_X20d3.ms.scriptForCalibration.py) as provided. RLep_B10_B2B_ReferenceImages.tgz contains the continuum image products: * J0522-3627_bp.spw33_35_37_39_41_43_45_47.cont.* * J0522-3627_dgc.spw33_35_37_39_41_43_45_47.cont.* * J0423-0120_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_47.cont.I.manual.* * R_Lep_sci.spw33_35_37_39_41_43_47.cont.I.manual-contselfcal.* * R_Lep_sci.spw33_35_37_39_41_43_47.cont.I.manual-datacontselfcalflags.* * R_Lep_sci.spw33_35_37_39_41_43_47.cont.I.manual-HCNselfcal.* * R_Lep_sci.spw45.cube.I.manual-HCN.* * R_Lep_sci.spw45.cube.I.manual-HCN-HCNselfcal.* * R_Lep_sci.spw45.cube.I.manual-HCN-1415ch.* (used only for selfcal) * R_Lep_sci.spw45.cube.I.manual-HCN-1415ch-phselfcal.* (used only for selfcal) * R_Lep_sci.spw45.cube.I.manual-HCN-1415ch-phampselfcal.* (used only for selfcal) All images can be re-created by executing the imaging script (RLep_B10_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_Xf06573_X20d3.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_B10_B2B.scriptForSelfcalAndImaging.py')