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Technical reports

The following list of IRAM technical Reports contains reports from IRAM Grenoble or Granada on various topics (technical / informatical / physical / …) written in English and PDF format.

  • 2024-1: Planet brightness temperatures in ASTRO V1.0 (2024), J. Boissier (IRAM Grenoble), J. Pety (IRAM Grenoble, Observatoire de Paris), S. Bardeau (IRAM Grenoble)
    Keywords: GILDAS\ASTRO, IRAM instruments, Planet models, Flux Calibration
    Abstract: Planets are used as primary flux calibrator for both IRAM observatories. Planet brightness temperatures in ASTRO were not updated since their first implementation. The accuracy of the planet models have greatly improved over the past years to about 5% absolute accuracy, rendering it important to update ASTRO. We present in this report the comparison of the current implementation of planet brightness temperature in ASTRO to the results of more advanced models. We describe how we implement new models in ASTRO and what could be the impact on IRAM instrument calibration.
  • 2017-1 : Observational examples of spectral line calibration at the 30m telescope with MRTCAL and MIRA V1.0 (2017), C. Marka (IRAM Granada), J. Pety (IRAM Grenoble, Observatoire de Paris), S. Bardeau (IRAM Grenoble), A. Sievers (IRAM Granada).
    Keywords: MRTCAL, MIRA, 30m calibration
    Abstract: Since February 2017, MRTCAL has replaced MIRA as the software for spectral line data calibration (except polarimetry and continuum) at the 30m-Telescope. Slight changes in the calibrated spectra are expected, for example in form of an improved calibration accuracy at the edges of the atmospheric windows as result of the narrower calibration bandwidth used by MRTCAL (20MHz by default, compared to up to about 1.35 GHz for MIRA). This report demonstrates the practical performances of MRTCAL by a systematic comparison of observations calibrated with both softwares.
  • 2016-2 : Gridding spectra with CLASS V1.1 (2018), S. Bardeau (IRAM Grenoble) and J. Pety (IRAM Grenoble, LERMA, Observatoire de Paris).
    Keywords: Gridding, Transposition, Memory, Large files
    Abstract: In the sep16a CLASS release, the internal code of the XY MAP command was refurbished to ensure that datasets larger than the available RAM memory can be processed by slicing the data in intervals of channels. The command is now also able to read direct or transposed input XY tables and/or to write direct (LMV) or transposed (VLM) output cubes. The latter feature is useful to easily reimport data when a 2nd step of baselining is desired on the gridded data cube. The online help was upgradeed accordingly (see in particular the output of LAS> HELP XY MAP MEMORY). This memo describes how the gridding is performed in CLASS, from the collection of spectra to the spectral cube. It focuses on the file access effciency, memory consumption, and how the user choices can impact them.
  • 2016-1 : MAPPING for NOEMA: Concepts and Usage V1.1 (2016), S. Guilloteau (LAB Bordeaux).
    Keywords: Imaging, Data processing
    Abstract: With the advent of ALMA and NOEMA, the interferometers deliver much larger data sets than initially anticipated for GILDAS software. This document describes new facilities in MAPPING to handle 1) Mosaics and 2) Wide bandwidth data sets, and a proposed new (simpler) way of using MAPPING.
  • 2015-4 : Introducing Associated Arrays in CLASS V1.0 (2016), S. Bardeau (IRAM Grenoble), J. Pety (IRAM Grenoble, Observatoire de Paris).
    Keywords: CLASS Data Format
    Abstract: The concept of Associated Arrays is being added in the CLASS data format. It is an additional section that will store a set of data arrays whose spectral axis matches the brightness spectral axis, i.e., one-to-one channel correspondence. At start, this will be used in two contexts. For Herschel/HIFI, it will store a logical array of blanked channels and a logical array to define the channels where the lines appear (see IRAM Memo 2015-3). At some point, it will be used at the IRAM-30m to store the results of the calibration scans, i.e., the sky counts in the <b>RY</b> array and the hot/cold counts, and the receiver, system, and calibration temperatures in a set of Associated Arrays. This document introduces the detailed specifications of the concept of an Associated Array, its implementation/integration in CLASS, and it gives an example of use, namely how to baseline a spectra using a LINE associated array to define the baseline windows. The specifications of the Associated Arrays is foreseen to evolve following feedback from its use at IRAM and elsewhere.
  • 2015-3 : Importing Herschel-FITS into CLASS V1.0 (2015), S. Bardeau (IRAM Grenoble), D.Teyssier (ESAC Madrid), D. Rabois (IRAP Toulouse), J. Pety (IRAM Grenoble, Observatoire de Paris).
    Keywords: CLASS Data Format
    Abstract: Herschel/HIFI data were already readable by CLASS after conversion into specific FITS file by the HiClass task from HIPE. These FITS files are however not the ones served by the Herschel Science Archive as result of the standard data processing. The CLASS community thus requested the possibility to fill Herschel/HIFI archive science products directly into CLASS. In a nutshell, the new filler automatically recognizes the Herschel/HIFI FITS level 2.0 and 2.5. The standard CLASS sections (General, Position, Spectroscopy, Calibration) are filled from the FITS header parameters. A dedicated Herschel section is added to the CLASS Data Format in order to attach HIFI specific metadata. The data are filled as one or several CLASS spectra depending of the FITS level and/or context (On-The-Fly, spectral survey, etc). The associated FLAG and LINE arrays are filled as associated arrays (new CLASS feature documented in a separate memo) to each spectrum data. This memo describes all these points in details.

 

  • 2015-1 : Extended support of sky spherical coordinates in CLASS V1.0 (2015), S. Bardeau (IRAM Grenoble), J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris).
    Keywords: Coordinates, (re)Projection, CLASS Data Format
    Abstract: Up to now, CLASS only supported natively the radio projection of the sky spherical coordinates. The main limitation of the radio projection is the absence of support of a projection angle. This could imply some approximation in the handling of On-The-Fly data with rotated scanning directions. CLASS now supports all the projections already supported in the GILDAS kernel, i.e., none (unprojected spherical coordinates), gnomonic, orthographic, azimuthal, stereographic, lambert, aito
    , radio, and sfl. This required the introduction of the MODIFY PROJECTION command, the modi
    fication of the MODIFY POSITION command, and the modi
    cation of the position header section in the CLASS Data Format. This memo describes all this in detail.

 

  • 2014-1 : CLASS Data Fillers V1.2 (2016), S. Bardeau (IRAM Grenoble), J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris).
    Keywords: Data Format, CLASS
    Abstract: CLASS is the program of the GILDAS suite dedicated to the data reduction and analysis of heterodyne instruments at cm and (sub-)mm single-dish telescopes. It is used by the IRAM-30m, APEX, SOFIA/GREAT, Herschel/HIFI, YEBES, E
    ffelsberg. Because of tremendous improvement of the heterodyne spectrometer, the CLASS data format is evolving again after years of stability. To help non-IRAM telescope to cope with these changes, the CLASS team is now providing fillers to the Class Data Format writers. Three different possibilities are given: 1) A procedure using the SIC intepreter; 2) A Fortran program linked to the CLASS library; And 3) a Python script using a dedicated Python module. This document describes how those 3 APIs can be used and examples are provided in the appendices.

 

  • 2013-3 : CLASSIC Application Programming Interface V1.0 (2015), S. Bardeau (IRAM Grenoble) , V. Pietu (IRAM Grenoble), J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris).
    Keywords: Data Format, CLASS, CLIC
    Abstract: We describe in details the Application Programming Interface of the CLASSIC Library, provided by GILDAS.

 

  • 2013-2 : CLASSIC Data Container V1.0 (2013), S. Bardeau (IRAM Grenoble) , V. Pietu (IRAM Grenoble), J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris).
    Keywords: Data Format, CLASS, CLIC
    Abstract: The CLASS/CLIC Data Format are digital formats used to describe single-dish/interferometric radio-astronomy data. They can be described in two layers: 1) a CLASSIC Data Container, which is generic enough to store many kinds of data, typically several observations which gather observational parameters with actual data, and 2) the CLASS/CLIC Data Format itself, which make a particular use of the CLASSIC Data Container. The size of the datasets produced by the IRAM instruments experience a tremendous increase (because of multi-beam receivers, wide bandwidth receivers, spectrometers with thousands of channels, and/or new observing mode like the interferometric on-the-fly). This implied that the CLASS/CLIC Data Format were reaching common limits in the size of data which could be stored. To solve these issues, the CLASSIC Data Container standard was revised. This documents aims to describe the new standard. A companion document describes the GILDAS library which implements this standard and which is now used by CLASS and CLIC.

 

  • 2013-1 : Improvement of the IRAM 30m telescope beam pattern V8.2 (2013), Carsten Kramer (IRAM Granada), Juan Penalver (IRAM Granada), and Albert Greve (IRAM Grenoble).
    Keywords: IRAM 30-M, Beam pattern, Reflector surface
    Abstract: Numerous revious publications on the subject, see reference section in the report.

 

  • 2011-4 : Description of the spectral axis handling in CLASS  V1.2 (2019), J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris) , S. Bardeau (IRAM Grenoble) .
    Keywords: CLASS, Spectral information in observations
    Abstract: An observer is interested by the physical properties (line frequencies, velocity of the gas) of a source in its own reference frame. However, the observations happen in a different frame, namely the topocentric frame for ground-based observations. This implies a change of frame to infer the physical properties in the source frame from the measured frequencies in the measurement frame. This memo tries to explain the different interpretation of the spectral axis, the additional subtleties related to heterodyne receivers in radio-astronomy, the current description of the spectral axis handling in CLASS, and the impact of various short-comings that happen for historical reasons.

 

  • 2011-3 : CLASS User Section V1.0 (2011), S. Bardeau (IRAM Grenoble) , J. Pety (IRAM Grenoble; LERMA, Observatoire de Paris) , S. Guilloteau (LAB, Observatoire de Bordeaux).
    Keywords: CLASS, Data headers, User-defined information
    Abstract: CLASS is a state-of-the-art GILDAS software for reduction and analysis of (sub)–millimeter spectroscopic data. Up to now, the CLASS data format could only describe a predetermined number of parameters in the observation headers, these parameters being grouped in 17 sections (e.g. the general, spectroscopic or calibration sections). However, the possibility to add telescope-specific information to the CLASS data format was requested several time. Instead of introducing a per-telescope specific and fixed section, we thus decided to introduce a new flexible section, named User Section. This document describes the functionalities available to the end-users as well as the implementation steps which must be developed by the section owner.

 

  • 2011-2 : WIFISYN: The GILDAS implementation of a new wide-field synthesis algorithm V0.1 (2011), J. Pety (IRAM Grenoble, Observatoire de Paris), N. Rodriguez-Fernandez (IRAM Grenoble).
    Keywords: Wide-field synthesis, Mosaics, Interferometric imaging
    Abstract: The usual way to image wide-field interferometric observations is known as mosaicking. Different variants of mosaicking exist (e.g. Cornwell, 1988; Sault et al., 1996), including an interesting recent implementation of mosaicking in the uv plane (Golap et al., priv. comm.). Pety & Rodriguez-Fernandez (2010) revisited the theory of wide-field imaging to propose a different algorithm to image interferometric wide-field observations, based on the well-known Ekers & Rots’ scheme. This algorithm is named wide-field synthesis because it explicitely synthesizes the wide-field spatial frequencies throughout the uv plane. This memo describes the current state of the implementation of this algorithm in a new package, named WIFISYN, of the GILDAS software suite.

 

  • 2011-1 : Preparing GILDAS for large datasets. I – GREG 2011  V1.3 (2011), S. Bardeau (IRAM Grenoble), E. Reynier (IRAM Grenoble), J. Pety (IRAM Grenoble, Observatoire de Paris).
    Keywords: Multi-threading, Multi-windowing, the GIMP ToolKit (GTK+), Portable Network Graphics (PNG)
    Abstract: The size of the datasets produced by the IRAM instruments experience a tremendeous increase (because of multi-beam receivers, wide bandwidth receivers, spectrometers with thousands of channels, and/or new observing mode like the interferometric on-the-fly). Visualizing these datasets in a fluent way is a challenge, which requires the best use of the available hardware and operating systems (multi-cores processors and multi-window environments). This prompted a large rewriting of the part of the GILDAS kernel (known as GTV) in charge of the interface between the plotting facilities and the system. The main guidelines of this rewriting were 1) the backward compatibility when possible, 2) the use of modern standards as the multi-threading or the GTK+ toolkit, 3) the factorization of the source code for different OS (Linux, Mac OSX and MS Windows), 4) the implementation of new facilities like a PNG output or an interactive lens. This document thoroughly describes the improvements for the end-users and the programmers.

 

  • 2010-3 : Polarimetry with EMIR / XPOL  V1.0 (2010), H. Wiesemeyer (IRAM Granada, on sabbatical leave at MPIfR) and C. Thum (IRAM Grenoble).
    Keywords: IRAM 30-m, Heterodyne, Polarimetry, EMIR, XPOL
    Abstract: Following the installation of the new EMIR receiver in spring 2009, the XPOL observing mode needed to be adapted and the consequences for polarization observations to be investigated. Here we report on test measurements made at 90 and 230 GHz. XPOL now works at these EMIR bands with lower on–axis instrumental polarization than before. Sidelobe levels are however not significantly reduced, with the consequence that observations of extended sources still demand special care. Commissioning of XPOL in the E150 and E330 bands remains to be done.

 

  • 2010-2 : IRAM-30m MAMBO time / sensitivity estimator  V1.0 (2010), J. Pety (IRAM Grenoble,  Observatoire de Paris), G. Quintana-Lacaci (IRAM Granada), R. Zylka (IRAM Grenoble), S. Bardeau (IRAM Grenoble), E. Reynier (IRAM Grenoble).
    Keywords: IRAM 30-m, Bolometer, MAMBO
    Abstract: This memo describes the equations used in the IRAM-30m MAMBO time/sensitivity estimator available in the GILDAS / ASTRO program.

 

  • 2010-1 : IRAM-30m HERA time/sensitivity estimator V1.0 (2010), J. Pety (IRAM, Observatoire de Paris), M. Gonzalez (IRAM Granada), S. Bardeau (IRAM) and E. Reynier (IRAM).
    Keywords:  IRAM-30m, Multibeam, HERA
    Abstract: This memo describes the equations used in the IRAM-30m HERA time/sensitivity estimator available on the IRAM-30m web page. A large part of the memo aims at describing the peculiarities of time/sensitivity estimation of the On-The-Fly observing mode with a multi-pixel like HERA. It explains how to generalize the equations of the single pixel case, so that the same code can be used in both cases (single and multi-pixel).

 

  • 2009-6 : Read-write optimization in CLASS  V1.0 (2009), S. Bardeau (IRAM), J. Pety (IRAM, Observatoire de Paris) and S. Guilloteau (LAB Observatoire de Bordeaux).
    Keywords: On-The-Fly, CLASS file format, Data rate, User and system times
    Abstract: CLASS is a GILDAS software for reduction and analysis of (sub){millimeter spectroscopic data. It is daily used to reduce spectra acquired with the IRAM 30m telescope. CLASS is currently used in many other facilities (e.g. CSO, HHT, Effelsberg) and it is considered for use by Herschel/HIFI. CLASS history started in 1983. As a consequence, it was written in FORTRAN 77 and tailored to reduce pointed observations.
    When CLASS was re-written in Fortran 90, it was decided to split On-The-Fly spectra into one observation each (see IRAM memo 2005-1). This eases spectra handling from the user side, but, of course, multiplies the number of observations in a single file (typically by a factor ~1000). The increasing number of observations (especially with the OTF acquisition schemes) and number of channels of the back-ends produces larger and larger files. CLASS has thus been revised with new file types and optimized with a faster algorithm in order to ensure a maximal data rate from the software side. We will expose here this new algorithm, and show that the major limitation for writing CLASS large files is currently on the hardware side.

 

  • 2009-5 : Comparison of ATM versions: Impact on the calibration of IRAM instruments  V1.0 (2009), J. Pety (IRAM, Observatoire de Paris), S. Bardeau (IRAM) and E. Reynier (IRAM).
    Keywords: ATM, Atmospherical model, Radiative transport
    Abstract: Since its first introduction into GILDAS in 1985, the ATM modelling program completely changed. With the advent of large bandwidth receivers and submillimeter receivers, it is time to upgrade the version of ATM used in GILDAS to calibrate IRAM instruments. This memo tries to assess the impact of changing the atmospheric model on the calibration of IRAM instruments. After a short description 1) of the single-dish calibration, 2) of ATM 2009 and 3) the GILDAS interface to ATM 1985 and ATM 2009, an in-depth comparison of the results obtained with ATM 1985 and ATM 2009 is described. From this study, we expect slight variations of the calibration results when swapping from ATM 1985 to ATM 2009.

 

  • 2009-4 : Averaging spectra with CLASS  V1.0 (2009), S. Bardeau (IRAM), J. Pety (IRAM, Observatoire de Paris).
    Keywords: AVERAGE, ACCUMULATE, Resampling, Weighting, Concatenation
    Abstract: CLASS90 (hereafter CLASS) provides a set of commands capable to average two or more spectra. They provide many averaging modes, presented hereafter in this document. The different modes often imply to perform internally and silently some important computations, namely resampling and weighted average. Combining these operations at the same time may imply some non-trivial effects described here. On October 2008, it appeared that some particular combinations of the tunable modes were not behaving as expected (either in CLASS90 and in CLASS77). A complete cleaning and factorization of the algorithm was performed, associated to exhaustive tests of all combinations. A test suite was also provided to check the output of each commands and modes. Following this maintenance of the code, and the use of these capabilities to concatenate the new EMIR spectra, it was decided to write this document in order to keep a trace of all the methods applied. This was also the occasion to investigate deeply in the code and to examine the effects which can occur during all the possible processings.

 

  • 2009-3 : A simulator of interferometric On-the-fly observations V1.0 (2009), N. Rodriguez-Fernandez (IRAM), Frederic Gueth (IRAM), Jerome Pety (IRAM).
    Keywords: Interferometric wide-field imaging, On-the-fly observing, Simulations
    Abstract: We have developed a simulator of interferometric on-the-fly observations in the framework of our research on image synthesis for mosaics observed in the on-the-fly (OTF) mode, in which the interferometer takes data at the same time that the antennas move continuously across the source. This simulation tool has been developed on the basis of the IRAM/GILDAS ALMA+ACA simulator (Pety, Gueth & Guilloteau 2001).

 

  • 2009 – 2 : Imaging of interferometric On-The-Fly observations (I): context and discussion of possible methods  V1.0 (2009), N. Rodriguez-Fernandez (IRAM), Jerome Pety (IRAM, Observatoire de Paris), Frederic Gueth (IRAM).
    Keywords: Interferometric wide-field imaging, On-the-fly observing
    Abstract: We discuss the measurement equation for interferometric observations of fields larger than the primary beam of the antennas, both for standard “pointed” mosaics and for mosaics observed in on-the-fly (OTF) mode. The main advantages of using the OTF mode are a gain of observing time and a higher homogeneity of the dataset. OTF mosaicing is similar to classical stop-and-go mosaicing but the effective beam when observing OTF is not exactly the primary beam of the antennas. We show that the effective beam is similar to the primary beam when the scanning rate is better than Nyquist. We review different techniques to image and deconvolve mosaic data, in particular the Ekers & Rots 1979 (ER79) scheme, which consist in Fourier transforming the visibility function with respect to the scanning coordinate. We discuss how to implement an OTF-optimized imaging algorithm to deal with the mosaic data as a whole based on the ER79 scheme. Finally we discuss observing time and mosaic size constrains for OTF observations.

 

  • 2009-1 : IRAM-30m EMIR time/sensitivity estimator  V1.1 (2010), J.Pety (IRAM Grenoble, Observatoire de Paris).
    Keywords: IRAM 30-m – EMIR – Proposal preparation – Time estimator.
    Abstract: This memo describes the equations used in the IRAM-30m EMIR time/sensitivity estimator available in the GILDAS/ASTRO program. A large part of the memo aims at deriving sensitivity estimate for the case of On-The-Fly observations, which is not clearly documented elsewhere (to our knowledge). Numerical values of the different parameters used in the time/sensitivity estimator are grouped in appendix A.
    V1.0 (2009)

 

  • 2008-2 : Single-dish observation and processing to produce the short-spacing information for a millimeter interferometer   V1.0 (2008), N.J. Rodriguez-Fernandez (IRAM), J. Pety (IRAM, Observatoire de Paris), F. Gueth (IRAM).
    Keywords: Interferometric wide-field imaging, Short-spacings.
    Abstract: Adding the short-spacing information filtered out by (sub)-millimeter interferometers is crucial to obtain good images of wide fields (observed in stop-and-go or on-the-fly mode). In this memo we discuss how to obtain the short-spacing information with single-dish data using the pseudo-visibility method. We have computed the natural weights of the pseudo-visibilities from the noise in the single-dish map. We also discuss 1) the relative weights of the single-dish and interferometric data, 2) how the relative weight equation transform into relative integration time and 3) severals ways of weighting the pseudo-visibilities. Finally, we discuss the addition of the short-spacings in practice (e.g. single-dish artifacts, field-of-view,…).

 

  • 2008-1 : Test Observations of CLOUDSAT  V1.0 (2008), D. Morris (IRAM Grenoble), G. Butin (IRAM Grenoble), N. Marcelino (IRAM Granada).
    Keywords: IRAM 30m telescope, Cloudsat, Receivers, Satellite interference
    Abstract: Test observations to assess the risk of interference due to Cloudsat emissions were made at the IRAM 30m telescope in July 2006. The telescope was pointed at various offsets from the predicted culmination of Cloudsat and short integrations were made. A simple axially symmetric model of the antenna sidelobe patterns was used to predict an upper limit to the expected signal. Although interference in the shared band was detected, it is of short duration. In routine astronomical observations its impact can be reduced by telescope pointing restrictions during staellite transits and by avoiding observations when the satellite is near the zenith. The loss of observing time will be small. In this special case (time)sharing between Radioastronomy and an active service is feasible at the price of some loss in observing time. This is possible because only one fast moving satellite with excellent sidelobes in angle and frequency is active.

 

  • 2005-1 : CLASS evolution: I. Improved OFT support  V1.0 (2005), P. Hily-Blant (IRAM Grenoble), J.Pety (IRAM Grenoble, LERMA Paris), S. Guilloteau (L3AB, Obs. de Bordeaux).
    Keywords: CLASS, single-dish telescope software, OTF
    Abstract: : CLASS is a GILDAS software for reduction and analysis of (sub)-millimeter spectroscopic data. It is daily used to reduce spectra acquired with the IRAM 30m telescope. CLASS is currently used in many other facilities (e.g. CSO, HHT, Effelsberg) and it is considered for use by Herschel/HIFI. CLASS history started in 1983. As a consequence, it was written in FORTRAN 77 and tailored to reduce pointed observations. On-The-Fly support was added in the 90s but it showed limitations as the quantity of OTF data increased quickly. One year ago, we decided to fully rewrite CLASS in FORTRAN 90 with the 3 following goals: 1) clarifying satisfying features with backward compatibility in mind, 2) improving code readability to simplify maintenance and 3) easing reduction of large OTF data sets. This memo is describing the current state of affair with a particular emphasis on changes in the program behavior. Future foreseen changes (linked to the increase of receiver instantaneous bandwidth like an improved conversion from frequency to velocity axis) will be described in a future memo.

 

  • 2005-0 : Thoughts about polarization calibration with the next generation receivers at Plateau de Bure V1.0 (2005), H. Wiesemeyer (IRAM Grenoble).
    Keywords: Polarimetry, Leakage terms, Crossed-band polarization calibration
    Abstract: With the next generation receivers, the Plateau de Bure interferometer will be able to simultaneously measure all four Stokes parameters. The interferometer can be optimized for the detection of either linear or circular polarization. In both cases, the weakness of the polarization of all bandpass and phase calibrators requires calibration schemes that are more involved than the usual mode. Time estimates are given.

 

  • 2003-4 : Case for interoperability as an ALMA off-line model  V1.0 (2003), J. Pety (Obs. de Paris/IRAM Grenoble), F. Gueth (IRAM Grenoble), S. Guilloteau (ESO/IRAM Grenoble), P. Teuben (U. Maryland), M. Wright (RAL, U.C. Berkeley).
    Keywords: Interoperability, Offline, Software, Science, Calibration
    Abstract: In this memo we argue that interoperability between the existing radio-interferometry packages provides a fast, robust, flexible, complete, and user-friendly data reduction package for ALMA. We discuss our first steps toward interoperation with MIRIAD and GILDAS using python as a command line interface.

 

  • 2003-3 : Complementarity of the AIPS++, GILDAS and MIRIAD packages as seen from evaluations for ALMA off-line processing V1.0 (2003), J. Pety (Obs. de Paris/IRAM Grenoble), F. Gueth (IRAM Grenoble), S. Guilloteau (ESO/IRAM Grenoble), P. Teuben (U. Maryland), M. Wright (RAL, U.C. Berkeley).
    Keywords: Requirements, Offline, Software, Science, Calibration
    Abstract: In this memo, we analyze the results of the audit of the AIPS++, and of evaluations of GILDAS and MIRIAD packages for compliance with the ALMA Offline Data Processing Requirements. These evaluations/audit show that about 2/3 of the SSR Requirements are fulfilled by each data reduction package, and almost 90% are fulfilled if we use existing software from all three packages.

 

  • 2003-2 : Evaluation of the GILDAS Package for ALMA Off-line Data Processing  V1.0 (2003), F. Gueth (IRAM Grenoble), S. Guilloteau (ESO/IRAM Grenoble), R. Lucas (IRAM Grenoble), J. Pety (Obs. de Paris/IRAM Grenoble), M. Wright (RAL, U.C. Berkeley).
    Keywords: Requirements, Offline, Software, Science, Calibration
    Abstract: This memo presents the evaluation of the GILDAS package for compliance with the ALMA off-line data processing requirements (ALMA-SW Memo 18). This evaluation follows exactly the same template that was used for the AIPS++ audit.

 

  • 2003-1 : Evaluation of the MIRIAD Package for ALMA Off-line Data Processing V1.0 (2003), M. Wright (RAL, U.C. Berkeley), P. Teuben (U. Maryland), J. Pety (Obs. de Paris/IRAM Grenoble).
    Keywords: Requirements, Offline, Software, Science, Calibration
    Abstract: This memo presents an evaluation of the MIRIAD package for compliance with the ALMA off-line data processing requirements (ALMA-SW Memo 18). This evaluation follows exactly the same template that was used for the AIPS++ audit.

 

  • 2001-1 : A Calibration Scheme for the IF Polarimeter using the Coherence Matrix Formulation V1.02 (2001), H. Wiesemeyer (IRAM Grenoble).
    Keywords: Polarimetry, Calibration, Stokes parameters, IF polarimeter, Jomes matrices, Coherence matrix
    Abstract: A calibration scheme for the IF polarimeter at the MRT is worked out using Jones matrices and the quantum-mechanical density operator (the coherence matrix in classical theory). It is shown that the proposed calculus combines the advantages of Jones calculus and Mueller matrices.