2024-03-28T15:51:37Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/26172022-10-10T10:57:12Zcom_10261_135com_10261_4col_10261_388
The ISO LWS high resolution spectral survey towards Sagittarius B2
Polehampton, Edward T.
Baluteau, Jean-Paul
Swinyard, Bruce M.
Goicoechea, Javier R.
Brown, John M.
White, Glenn J.
Cernicharo, José
Grundy, Timothy W.
Line: identification
Surveys
ISM: individual: Sagittarius B2
ISM: lines and bands
ISM: molecules
Infrared: ISM
Accepted for publication in MNRAS.
A full spectral survey was carried out towards the Giant Molecular Cloud complex, Sagittarius B2 (Sgr B2), using the ISO Long Wavelength Spectrometer Fabry-Perot mode. This provided complete wavelength coverage in the range 47-196 um (6.38-1.53 THz) with a spectral resolution of 30-40 km/s. This is an unique dataset covering wavelengths inaccessible from the ground. It is an extremely important region of the spectrum as it contains both the peak of the thermal emission from dust, and crucial spectral lines of key atomic (OI, CII, OIII, NII and NIII) and molecular species (NH3, NH2, NH, H2O, OH, H3O+, CH, CH2, C3, HF and H2D+). In total, 95 spectral lines have been identified and 11 features with absorption depth greater than 3 sigma remain unassigned. Most of the molecular lines are seen in absorption against the strong continuum, whereas the atomic and ionic lines appear in emission (except for absorption in the OI 63 um and CII 158 um lines). Sgr B2 is located close to the Galactic Centre and so many of the features also show a broad absorption profile due to material located along the line of sight. A full description of the survey dataset is given with an overview of each detected species and final line lists for both assigned and unassigned features.
JRG was supported by an individual Marie Curie fellowship, contract MEIF-CT-2005-515340.
Peer reviewed
2007-12-27T09:53:04Z
2007-12-27T09:53:04Z
2007-02-27
preprint
http://purl.org/coar/resource_type/c_816b
arXiv:astro-ph/0702725v1
Monthly Notices of the Royal Astronomical Society (MNRAS) 377, 3 (2007), 1122-1150.
1365-2966
http://hdl.handle.net/10261/2617
10.1111/j.1365-2966.2007.11669.x
en
Preprint
open
835401 bytes
application/pdf
Blackwell Publishing