F. Levrier (LERMA - ENS) J. Pety (LERMA - IRAM Grenoble) P. Salomé (LERMA - Observatoire de Paris) STAR FORMAT meeting, Heidelberg, 4-5 may 2010 Making.

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Presentation transcript:

F. Levrier (LERMA - ENS) J. Pety (LERMA - IRAM Grenoble) P. Salomé (LERMA - Observatoire de Paris) STAR FORMAT meeting, Heidelberg, 4-5 may 2010 Making ALMA observations of MHD simulations

The ALMA Simulator in GILDAS An ALMA / ALMA Compact Array (ACA) / Single Dish imaging simulator Detailed description in ALMA memo 398 (Pety, Gueth, Guilloteau) Developed for studying the impact of ACA on wide-field imaging capabilities Scientific preparation of ALMA (e.g. Wolf et al.) Included in GILDAS’ MAPPING software F90 routines SIC procedures Widget interface 1. Inputs Source position and size : mosaicing Model brightness distribution Array configuration Frequency (only continuum) Type of observation (ALMA + ACA + Single Dish) 2. Visibilities Cover from source position, array configuration and time range Beam from antenna size Source-calibrator loop Possibility to add pointing errors, atmospheric phase noise, calibration errors 3. Imaging Calibration (standard, fast switching, water vapor radiometry) Deconvolution (Standard CLEAN based methods) Input and output comparison

Main windowConfigurationObservation Graphical User Interface a

Antenna positions on the ground for 8 configurations Up-to-date ALMA configurations Thanks to J. Pety and A. Wooten 28 configurations From 90 m to 9.5 km radius CASA to GILDAS format conversion

ALMA simulator on MHD simulations RAMSESRaw FITS GILDAS (FITS) IDL Python Input FITS Subset Distance Brightness temperature Sky position Input GDFOutput GDFOutput FITS GILDAS (FITS) GILDAS (ALMA) Raw model field Physical model 100 pc

ALMA only Smoothed inputSimulated observation DifferenceFidelity Examples of simulated observations Smoothed inputSimulated observation DifferenceFidelity ALMA + Single Dish Flux recovered : 48%Flux recovered : 73% Fidelity image = input model / difference Inverse of relative error In practice, lowest values of difference are truncated

Simulations for different configurations ALMA only ALMA + Single Dish #8#11#15 Spatial frequency filtering Flux loss Importance of single-dish measurements Original field

ALMA simulator for STARFORMAT Current status of batch mode Shell script Input file ! parameter parameter parameter value value value Initialization file Default parameter values GILDAS procedure file GILDAS routines Proposed evolution Python script Command line arguments Initialization file Default parameter values GILDAS routines User supplied parameter values Suppresses extra layer Simplifies development of web service Possible mutualization with CASA (Ian Heywood) [] Runs one per line in the input file Runs single

Example batch simulation : line mapping Raw 3D FITS GILDAS (FITS) Python Input “PPV” FITS Input 3D GDF Output “PPV” FITS GILDAS (FITS) Split (GILDAS) { N x Input 2D GDF Input file (frequencies) } N x Output 2D GDF GILDAS (ALMA) Concatenate (GILDAS) Output 3D GDF Develop comparison measures