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III/242     ISO Astrophysical Spectroscopic Database  (Jourdain de Muizon, 2005)

ISO Astrophysical Spectroscopic Database Jourdain de Muizon Marie <(Test version, Oct. 2005) >
ADC_Keywords: Spectra, infrared Mission_Name: ISO Keywords: Infrared ; Spectroscopy ; Planets ; Protostars; Stars ; Interstellar Medium ; Galaxies Description: This database will eventually contain all the published infrared lines observed by ISO, the Infrared Space Observatory. At this stage only a few percent of the total content is included but it is increasing steadily. Thus what is presented at this stage is a beta-version of the final product. ISO - the Infrared Space Observatory - was operational during about 28 months, between November 1995 and May 1998, until its cooling fluid (liquid helium) burnt out (Kessler et al. 1996A&A...315L..27K). It was the first far-infrared satellite equipped with two medium and high resolution spectrometers, SWS (Short Wavelength Spectrometer, 2.38-45.2µm, de Graauw et al. 1996A&A...315L..49D) and LWS (Long Wavelength Spectrometer, 43-197µm, Clegg et al. 1996A&A...315L..38C). Both spectrometers could be operated in grating or Fabry-Perot mode. In addition, the two other ISO instruments also provided spectroscopic data: ISOCAM (the ISO Camera, Cesarsky et al. 1996A&A...315L..32C) had a CVF (Circular Variable Filter) mode in 3 bands covering the range 2.3-17.3µm, and ISOPHOT (The Imaging Photo-Polarimeter, Lemke et al. 1996A&A...315L..64L) had a dual grating spectrometer (PHOT-S) with resolving power of order 90 in two bands (2.5-4.9µm and 5.8-11.6µm). Detailed information about ISO and its four ISO instruments can be found in "The ISO Handbook" available on-line at The novelty, the richness and the unicity of the ISO spectroscopic data is what motivated us in compiling this data in a systematic and homogeneous way in order to make it available to the whole astronomical community. No other past, current or foreseen space project will overwrite this data, hence the importance of this compilation. In addition, queries on the database content will be a useful tool for the preparation of follow-up observations with other space, airborne or ground-based observatories such as Herschel, SOFIA, ALMA, VLT and more. In this early version, the database is very incomplete. It contains about 3000 lines which represents only a few percent of the total. Each observed and published ISO spectroscopic line corresponds to a physical line in IASD with up to 39 parameter/information fields. The description of the various columns is given below. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file iasd.dat 972 3015 The ISO Astrophysical Spectroscopic Database
See also: VI/111 : ISO Observation Log (ISO Data Centre, 2004) Byte-by-byte Description of file: iasd.dat
Bytes Format Units Label Explanations
2- 9 I8 --- TDT Number that identifies an ISO observation in ISO log (Cat. VI/111) 10 A1 --- --- [0] 12- 13 I2 h RAh Actual Pointing Right Ascension J2000 (hours) (1) 14 A1 --- --- [:] 15- 16 I2 min RAm Actual Pointing Right Ascension J2000 (minutes) 17 A1 --- --- [:] 18- 22 F5.2 s RAs Actual Pointing Right Ascension J2000 (seconds) 24 A1 --- DE- Actual Pointing Declination J2000 (sign) 25- 26 I2 deg DEd Actual Pointing Declination J2000 (degrees) (1) 27 A1 --- --- [:] 28- 29 I2 arcmin DEm Actual Pointing Declination J2000 (minutes) 30 A1 --- --- [:] 31- 35 F5.2 arcsec DEs Actual Pointing Declination J2000 (seconds) 37- 38 I2 d Obs.D Start day/time of observation (UTC) 40- 42 A3 "month" Obs.M Start day/time of observation (UTC) 44- 47 I4 yr Obs.Y Start day/time of observation (UTC) 49- 50 I2 h Obs.h Start day/time of observation (UTC) 51 A1 --- --- [:] 52- 53 I2 min Obs.m Start day/time of observation (UTC) 54 A1 --- --- [:] 55- 56 I2 s Obs.s Start day/time of observation (UTC) 58- 60 A3 --- AOT Astronomical Observing Template number (4) 63- 78 A16 --- Target Target Name, as given by the observer 94-120 A27 --- Name2 Another Source Name from Simbad (5) 125-151 A27 --- Name3 Another Source Name from Simbad 156-181 A26 --- Name4 Another Source Name from Simbad 187-216 A30 --- Type1 Source Type, generally from Simbad 218-247 A30 --- Type2 Another Source Type 249-256 A8 --- Mode Observing mode, specifies the observing mode within the AOT, if applicable (6) 264 A1 --- Ext [PE] Source Extent: "P" for point source, "E" for extended source 299 A1 --- sp [LFB] Spectral Line Type (2) 322-327 F6.2 um cLambda Central Wavelength, in micron 331-340 F10.3 GHz Freq Frequency, in GHz 346-354 F9.4 cm-1 sigma Wavenumber, in inverse centimeter 356-358 A3 --- EmA "ABS" for absorption, "EM" for emission 369-375 F7.2 --- FWHM ? Line Width (FWHM) as given in the article 377-380 A4 --- x_FWHM Line Width Unit as given in the relevant article 404-408 I5 --- R Resolving Power (λ/deltaλ) 410-421 A12 --- Apert Instrument aperture, taken from the ISO Handbook 443-450 E8.3 W/m2 Flux ? Line/Feature Flux as given in the relevant article, converted to W/m2 461-468 E8.2 cm-2 nH ? Column Density as given in the relevant article 487-493 F7.2 --- S/N ? Signal-to-Noise Ratio, given or calculated from the relevant article 495-505 E11.4 --- pInt ? Line Peak Intensity as given in the relevant article, expressed in x_pInt units 512-519 A8 --- x_pInt Peak Intensity Unit (see pInt) 551-554 F4.2 --- L/C ? Line to Continuum Ratio, from the relevant article (7) 560-563 F4.2 mag Op ? Opacity, in case of an absorption feature 565-569 A5 --- Phase Physical phase of the observed specie e.g. GAS, SOLID, SOL/G, DUST 571 I1 --- Det [1,3] Detection Flag: 3 = quantitative detection, 2 = qualitative detection, 1 = upper limit 586-617 A32 --- Element The chemical component responsible for the relevant spectral line 619-650 A32 --- Trans The electronic, or vibration, rotation, ... transition of the line 666-671 F6.2 um tLambda ? Nominal laboratory or theoretical wavelength of the line, in micron 682-691 F10.3 GHz tFreq ? Nominal laboratory or theoretical frequency of the line, in GHz 704-712 F9.4 cm-1 tSigma ? Nominal laboratory or theoretical wavenumber of the line, in inverse centimeter 714-732 A19 --- Bibcode The reference code of the article (3) 734-972 A239 --- Comment Additonal useful information or parameters which could not fit in any of the other columns
Note (1): in most cases the ISO position except in case of a map Note (2): mode is "L" for spectral line, "F" for spectral feature, "B" for molecular band Note (3): the 19-digit code from which the data in this line has been taken, as given in the Astrophysical Data System and in Simbad ( Note (4): Each AOT name refers to a specific observation configuration with the relevant instrument. It is composed of a letter (C for ISO_CAM, S for ISO_SWS, L for ISO_LWS and P for ISO_PHOT) and a number. IASD includes all the AOT names of SWS (S01, S02, S06, S07 and S99) and of LWS (L01, L02, L03 and L04), but only one AOT name of CAM (C04, for CAM spectrophotometric mode) and one of PHOT (P40, for PHOT-S, the grating spectrometer of ISOPHOT). Note (5): Another source name, equally of more famous than the "Target" name given by the observer, often the IRAS Name, or the "target" name corrected in case the observer had entered it wrongly. This name comes from Simbad. Note (6): An IDA observational parameter which adds a precision to the AOT name. For example, it can be "pointing" of "raster" for LWS AOT names and "Speed1", "Speed2", "Speed3", or "Speed4" for SWS AOT names. Note (7): Line-to-continuum ratio, either as given by the authors of the relevant article, or calculated if the peak of the line and the corresponding continuum flux densities are given in a table or in a figure.
History: The essential of this catalog and documentation was prepared by Marie JOURDAIN de MUIZON. Send your comments to:
(End) Francois Ochsenbein [CDS] 18-Oct-2005
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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