2013A&A...556A.116W


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.18CET05:51:22

2013A&A...556A.116W - Astronomy and Astrophysics, volume 556A, 116-116 (2013/8-1)

Observing extended sources with the Herschel SPIRE Fourier transform spectrometer.

WU R., POLEHAMPTON E.T., ETXALUZE M., MAKIWA G., NAYLOR D.A., SALJI C., SWINYARD B.M., FERLET M., VAN DER WIEL M.H.D., SMITH A.J., FULTON T., GRIFFIN M.J., BALUTEAU J.-P., BENIELLI D., GLENN J., HOPWOOD R., IMHOF P., LIM T., LU N., PANUZZO P., PEARSON C., SIDHER S. and VALTCHANOV I.

Abstract (from CDS):

The Spectral and Photometric Imaging Receiver (SPIRE) on the European Space Agency's Herschel Space Observatory utilizes a pioneering design for its imaging spectrometer in the form of a Fourier Transform Spectrometer (FTS). The standard FTS data reduction and calibration schemes are aimed at objects with either a spatial extent that is much larger than the beam size or a source that can be approximated as a point source within the beam. However, when sources are of intermediate spatial extent, neither of these calibrations schemes is appropriate and both the spatial response of the instrument and the source's light profile must be taken into account and the coupling between them explicitly derived. To that end, we derive the necessary corrections using an observed spectrum of a fully extended source with the beam profile and considering the source's light profile. We apply the derived correction to several observations of planets and compare the corrected spectra with their spectral models to study the beam coupling efficiency of the instrument in the case of partially extended sources. We find that we can apply these correction factors for sources with angular sizes up to θD∼17". We demonstrate how the angular size of an extended source can be estimated using the difference between the subspectra observed at the overlap bandwidth of the two frequency channels in the spectrometer, at 959<ν<989GHz. Using this technique on an observation of Saturn, we estimate a size of 17.2'', which is 3% larger than its true size on the day of observation. Finally, we show the results of the correction applied on observations of a nearby galaxy, M82, and the compact core of a Galactic molecular cloud, Sgr B2.

Abstract Copyright:

Journal keyword(s): instrumentation: spectrographs - methods: analytical - methods: data analysis - techniques: spectroscopic

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 946 0
2 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 702 0
3 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5272 6
4 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2187 2
5 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11246 0
6 NAME Sgr B2 (North) Rad 17 47 20.2 -28 22 21           ~ 504 1
7 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1879 1
8 NAME Sgr B2 (South) HII 17 47 20.430 -28 23 45.06           ~ 84 0
9 NAME Sgr B2 Main Rad 17 47 20.5 -28 23 06           ~ 327 1

    Equat.    Gal    SGal    Ecl

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2020.02.18-05:51:22

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