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Herschel-HIFI water spectra of W43-MM1 (Herpin+, 2012)

hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorCHAVARRIA, L.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorVAN DER TAK, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierLeiden Observatory [Leiden]
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorVAN DISHOECK, E. F.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorJACQ, T.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBRAINE, J.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBAUDRY, Alain
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorKRISTENSEN, L.
dc.date.created2012
dc.date.issued2012-04
dc.descriptionVizieR On-line Data Catalog: J/A+A/542/A76. Originally published in: 2012A&A...542A..76H
dc.description.abstractEnData files (ASCII) of the HIFI-Herschel Space Observatory observations of 14 water lines as well as the CS(11-10) and C18O(9-8) lines toward W43-MM1. Continuum has been subtracted. Observations were performed in March, April, and October 2010 (OD 293, 295, 310, 312, 333, 338, 339, and 531). The position observed is RA=18:47:47.0, DEC=-01:54:28 J2000. The observations are part of WISH GT-KP. Data were taken simultaneously in H and V polarizations using both the acousto-optical Wide-Band Spectrometer (WBS) with a 1.1MHz resolution and the digital auto-correlator or High-Resolution Spectrometer (HRS) providing higher spectral resolution. We used the double beam switch observing mode with a throw of 3'. The HIFI receivers are double sideband with a sideband ratio close to unity. The frequencies, energy of the upper levels, system temperatures, integration times, and rms noise level at a given spectral resolution for each of the lines are provided in Table 1 of the paper. The calibration of the raw data onto the TA scale was performed by the in-orbit system (see Roelfsema et al., 2012A&A...537A..17R); and the conversion to Tmb was done using a beam efficiency given in Table 1 and a forward efficiency of 0.96. The flux scale accuracy was estimated to be 10% for bands 1 and 2, 15% for bands 3 and 4, and 20% in bands 6 and 7. Data calibration was performed in the Herschel Interactive Processing Environment version 6.0. Further analysis was done within the CLASS package. After inspection, data from the two polarizations were averaged together. Since HIFI operates in double-sideband, the measured continuum level was divided by a factor of two. (2 data files).
dc.language.isoen
dc.subject.enStars: early-type
dc.subject.enInterstellar medium
dc.subject.enSpectroscopy
dc.title.enHerschel-HIFI water spectra of W43-MM1 (Herpin+, 2012)
dc.typeAutre document
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
bordeaux.page29076
hal.identifierhal-00712453
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00712453v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.date=2012-04&rft.spage=29076&rft.epage=29076&rft.au=HERPIN,%20Fabrice&CHAVARRIA,%20L.&VAN%20DER%20TAK,%20F.&WYROWSKI,%20F.&VAN%20DISHOECK,%20E.%20F.&rft.genre=unknown


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