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CLASS evolution: I. Improved OTF support5. class90 for beta testersCLASS evolution: I. Improved OTF support5. class90 for beta testers• ANALYSE\TABLE creates a table containing the offsets, weights and intensities of all the dumpedspectra. A check of the consistency of the observations in the current index is performed at thisstep, if not already done before.• MAP\XY_MAP grids the dumped spectra from the table to an lmv cube. An image of the associatedweights is also produced for further processing like optimal combination of several data cubes.• Moreover, all the plotting capabilities of GREG program has been imported inside CLASS so thatthe user can directly visualize the data cube of the gridded spectra. For instance, Fig. 8 has beenobtained with the following sequence of commands:LAS90> file in 12co21-newfmt.30mLAS90> findLAS90> table 12co21 newLAS90> xy_map 12co21LAS90> let name 12co21LAS90> let type lmvLAS90> go viewThe “go view” scripts enables interactive visualization of a spectra cube. Channel maps may beproduced through the go bit command and position-velocity diagrams through the go xv and govy commands.tel-00726959, version 1 - 31 Aug 20124.4 PLAIT algorithmThe PLAIT algorithm “combine” two spectra cubes resulting from OTF observation with orthogonal scanningdirections into a single spectra cube. It works in the Fourier plane and it reduces the striping dueto receiver and atmospheric instabilities which inevitably show up in OTF maps. A version of this algorithmhas been implemented as a GILDAS task named PLAIT from a previous version by C.Nieten (itselfelaborated on original ideas from the NOD2 package).5 CLASS90 for beta testersThe current default version of CLASS is CLASS77. Soon enough, the default version will swap toCLASS90, i.e. users will have access directly to CLASS90 when calling CLASS from the shell prompt.There will be a warning that this is a new CLASS with modified features and that the old CLASS isstill available through the CLASS77 name in case of a problem with CLASS90. CLASS77 will stayabout one year after the swap to ensure good stability of CLASS90. However, no support will be givenanymore to CLASS77.Before the swap happens, you can become beta testers of CLASS90 if you are interested by the newfeatures. Beta testers should be able to quickly get bug fixes in their version. We thus recommend theyuse anonymous CVS in the following way:1 shell-prompt> export CVSROOT=:pserver:anonymous@netsrv1.iram.fr:/CVS/GILDAS2 shell-prompt> cvs co -r feb06 -d gildas-src-feb06 gildas3 shell-prompt> cd gildas-src-feb064 shell-prompt> source admin/gildas-env.sh5 shell-prompt> make6 shell-prompt> make install7 shell-prompt> cd packages/class908 shell-prompt> cvs up -r class90-stable9 shell-prompt> make cleanCLASS evolution: I. Improved OTF support10 shell-prompt> make11 shell-prompt> make install165. class90 for beta testersLine 1 and 2 create a directory name gildas-src-feb06 with the feb06 “stable” monthly release. Lines3 to 6 are the standard way to install GILDAS. As CLASS90 is evolving quickly, the CLASS90version shipped in a GILDAS monthly release may be unstable. We thus recommend that you go to theCLASS90 directory (line 7), update it to a “stable” version (line 8), compile and install it (lines 9 to 11).Beta testers also refer to the manual which is being fully updated. Bug reports and suggestions ofimprovements should be send to gildas@iram.fr. We will try to fix bugs quickly. We will considerthe feasibility of all suggestions on longer timescales. When a bug is fixed, here are the steps to updateCLASS90:1 shell-prompt> export CVSROOT=:pserver:anonymous@netsrv1.iram.fr:/CVS/GILDAS2 shell-prompt> cd gildas-src-feb063 shell-prompt> source admin/gildas-env.sh4 shell-prompt> cd packages/class905 shell-prompt> cvs up -r class90-stable6 shell-prompt> make7 shell-prompt> make installLine 5 is the line which will update the class90 directory. Be sure to type it only in thegildas-src-feb06/packages/class90 directory to ensure that only CLASS90 is updated because nothingensure that other parts of GILDAS are “stable” between 2 monthly releases.Have fun!Figure 8: Screen-shot of result of the go view command. The top,left panel is the channel map correspondingto velocity shown as a vertical red line in the top,right panel. The top,right panel displays thespectrum at the position localized on the top,right panel. The bottom,left panel shows the line emissionintegrated over the velocity range appearing in yellow on the bottom,right panel. This last panel displaysthe spectrum averaged over the whole map. go view is an interactive command with many more features.Please, type h to display the complete help.1718
A&A 526, A47 (2011)DOI: 10.1051/0004-6361/201015487c○ ESO 2010Astronomy&AstrophysicsWeeds: a CLASS extension for the analysis of millimeterand sub-millimeter spectral surveysS. Maret 1 , P. Hily-Blant 1 ,J.Pety 2,3 , S. Bardeau 2 , and E. Reynier 21 Laboratoire d’Astrophysique de Grenoble, Observatoire de Grenoble, Université Joseph Fourier, CNRS, UMR 571 Grenoble,Francee-mail: sebastien.maret@obs.ujf-grenoble.fr2 Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d’Hères, France3 LERMA, UMR 8112, CNRS and Observatoire de Paris, 61 avenue de l’Observatoire, 75014 Paris, FranceReceived 28 July 2010 / Accepted 6 December 2010ABSTRACTtel-00726959, version 1 - 31 Aug 2012The advent of large instantaneous bandwidth receivers and high spectral resolution spectrometers on (sub-)millimeter telescopes hasopened up the possibilities for unbiased spectral surveys. Because of the large amount of data they contain, any analysis of thesesurveys requires dedicated software tools. Here we present an extension of the widely used CLASS software that we developed tothat purpose. This extension, named Weeds, allows for searches in atomic and molecular lines databases (e.g. JPL or CDMS) thatmay be accessed over the internet using a virtual observatory (VO) compliant protocol. The package permits a quick navigationacross a spectral survey to search for lines of a given species. Weeds is also capable of modeling a spectrum, as often needed forline identification. We expect that Weeds will be useful for analyzing and interpreting the spectral surveys that will be done with theHIFI instrument onboard Herschel, but also observations carried-out with ground based millimeter and sub-millimeter telescopes andinterferometers, such as IRAM-30 m and Plateau de Bure, CARMA, SMA, eVLA, and ALMA.Key words. ISM: molecules – ISM: lines and bands – line: identification – methods: data analysis – virtual observatory tools1. IntroductionA spectral survey consists in a series of spectra covering a significantspectral domain. At (sub-)millimeter wavelengths, a spectralsurvey typically covers several tens of GHz. Spectral surveysare generally referred to as unbiased if they provide a completecoverage with a uniform sensitivity. As such, they allow for acomplete census of the species emitting in that band, and sometimesfor discovery of new interstellar species. In addition, becausea given band often contains many transitions of the samespecies, the simultaneous analysis of all these lines providesstringent constraints on the physical conditions in the emittinggas, such as the density and temperature. Therefore spectral surveysare very useful for characterizing both the chemical compositionand physical condition in the observed objects.Ever since the pioneering work of Johansson et al. (1984),who carried-out an unbiased spectral survey of the Orion KLstar-forming region and IRC +10216 carbon-rich star between72 and 91 GHz with the Onsala telescope, many spectral surveyshave been carried-out at millimeter and sub-millimeterwavelengths using ground-based telescopes (see Herbst &van Dishoeck 2009, for a review). Because of the limited sensitivityof the instruments available at that time, early spectralsurveys were targeted at bright star-forming regions, such asOrion KL and Sgr B2 in the millimeter range. Thanks to the increasingsensitivity of heterodyne receivers and the availabilityof sub-millimeter telescopes, these surveys were later extendedto higher frequencies (e.g. Schilke et al. 1997, 2001; Comitoet al. 2005) and carried-out towards fainter young stellar objects(e.g. NGC 1333 IRAS4 or IRAS16292-2422; Blake et al. 1994;van Dishoeck et al. 1995; Blake et al. 1995). A few spectralsurveys have been carried with millimeter and sub-millimeterinterferometers, such as OVRO or the SMA (e.g. Blake et al.1996; Beuther et al. 2006). The HIFI instrument (de Graauwet al. 2010) onboard the Herschel space observatory (Pilbrattet al. 2010) now allows for a complete coverage of the almostunexplored 480–1250 and 1410–1910 GHz frequency bands. Itslarge spectral coverage – up to 4 GHz instantaneous bandwidth– and unprecedented sensitivity in this frequency range enableastronomers to carry-out spectral surveys over almost 1.5 THzdown to the line confusion limit in a few tens of hours. The firstspectral surveys with this instrument have already given spectacularresults (Bergin et al. 2010; Ceccarelli et al. 2010). Amongthese, we can cite the richness of the Orion BN-KL spectrum observedat THz frequencies (see Fig. 2, Bergin et al. 2010)orthediscovery of ND in IRAS16293-2422 (Bacmann et al. 2010).Current developments in (sub-)millimeter instruments includean increase in the instantaneous bandwidth of the detectiondevices. During the past decade, the instantaneous bandwidth oftunable heterodyne receivers has increased by more than an orderof magnitude, now routinely reaching ∼10 GHz. Other technologies(e.g. HEMT, FCRAO and IRAM) have already providedseveral tens of GHz, although it is still unclear whetherthe sensitivity of these receivers can match that of SIS receivers.This increase in bandwidth has been accomplished in parallelwith the advent of digital spectrometers (autocorrelators, fastFourier transform), the versatility of which allow the coverage ofsuch bandwidth with a spectral resolution down to a few hundredkHz. As a result, unbiased spectral surveys of the 3 mm atmosphericwindow (ν = 80−117 GHz) can be done with the IRAM-30 m telescope in ∼10 h, with a 2 mK noise at 1σ in 2 MHz(∼6 kms −1 ) spectral channels. The ALMA interferometer willalso permits coverage of large frequency windows, providingspectral cubes with up to 8 GHz bandwidth (Wootten 2008).Article published by EDP Sciences A47, page 1 of 5
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UNIVERSITÉ PIERRE ET MARIE CURIEHA
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Table des matières1 Rapport de sou
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Rapport après soutenanceHabilitati
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Chapitre 2Curriculum vitaetel-00726
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2.7 ANIMATION ET DIFFUSION DE LA CU
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2.8 PARCOURS 131992-1993 ÉCOLE NOR
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Chapitre 3Copyright: IRAM/PdBIIntro
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4.2 ETUDES DIRECTES EN ÉMISSION 19
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4.4 LA LUMINOSITY CO PAR MOLÉCULE
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356 E. Falgarone et al.: Extreme ve
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A&A 518, A45 (2010)1001010⌠⌡ τ
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A&A 518, A45 (2010)Table E.2. Data
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A&A 541, A58 (2012)0.08 0.10.20.12
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A&A 541, A58 (2012)Jenkins, E. B.,
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A&A 541, A58 (2012)Galactic Latitud
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5.2 UNE PHYSIQUE BIEN CONTRAINTE ET
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5.3 PERSPECTIVES : DES RELEVÉS DE
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A&A 435, 885-899 (2005)DOI: 10.1051
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J. Pety et al.: Are PAHs precursors
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WIFISYNA. implementation planWIFISY
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8.3 PERSPECTIVES 227tel-00726959, v
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3 REQUIREMENTS 44 CHANGES FOR END-U
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5 CHANGES FOR PROGRAMMERS 125 CHANG
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A EXHAUSTIVE DESCRIPTION OF THE CHA
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Chapitre 9Copyright: Stéphane Guis
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Contribution de l'Action Spécique
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Articles publiés dans des revues
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ARTICLES PUBLIÉS DANS DES REVUES
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Mémos IRAM et ALMAtel-00726959, ve
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Actes de colloques nationaux et int
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ACTES DE COLLOQUES NATIONAUX ET INT
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