2015MNRAS.449.2274H


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.21CEST15:54:34

2015MNRAS.449.2274H - Mon. Not. R. Astron. Soc., 449, 2274-2303 (2015/May-3)

Systematic characterization of the Herschel SPIRE Fourier Transform Spectrometer.

HOPWOOD R., POLEHAMPTON E.T., VALTCHANOV I., SWINYARD B.M., FULTON T., LU N., MARCHILI N., VAN DER WIEL M.H.D., BENIELLI D., IMHOF P., BALUTEAU J.-P., PEARSON C., CLEMENTS D.L., GRIFFIN M.J., LIM T.L., MAKIWA G., NAYLOR D.A., NOBLE G., PUGA E. and SPENCER L.D.

Abstract (from CDS):

A systematic programme of calibration observations was carried out to monitor the performance of the Spectral and Photometric Imaging REceiver (SPIRE) Fourier Transform Spectrometer (FTS) instrument on board the Herschel Space Observatory. Observations of planets (including the prime point-source calibrator, Uranus), asteroids, line sources, dark sky and cross-calibration sources were made in order to monitor repeatability and sensitivity, and to improve FTS calibration. We present a complete analysis of the full set of calibration observations and use them to assess the performance of the FTS. Particular care is taken to understand and separate out the effect of pointing uncertainties, including the position of the internal beam steering mirror for sparse observations in the early part of the mission. The repeatability of spectral-line centre positions is <5 km/s, for lines with signal-to-noise ratios >40, corresponding to <0.5-2.0 percent of a resolution element. For spectral-line flux, the repeatability is better than 6 percent, which improves to 1-2 percent for spectra corrected for pointing offsets. The continuum repeatability is 4.4 percent for the SPIRE Long Wavelength spectrometer (SLW) band and 13.6 percent for the SPIRE Short Wavelength spectrometer (SSW) band, which reduces to ∼ 1 percent once the data have been corrected for pointing offsets. Observations of dark sky were used to assess the sensitivity and the systematic offset in the continuum, both of which were found to be consistent across the FTS-detector arrays. The average point-source calibrated sensitivity for the centre detectors is 0.20 and 0.21Jy [1σ; 1 h], for SLW and SSW. The average continuum offset is 0.40Jy for the SLW band and 0.28Jy for the SSW band.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): instrumentation: spectrographs - methods: data analysis - space vehicles: instruments

VizieR on-line data: <Available at CDS (J/MNRAS/449/2274): tableb.dat>

Simbad objects: 13

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Number of rows : 13

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 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1445 0
2 V* IK Tau Mi* 03 53 28.8884898148 +11 24 21.865959095 16.99 17.03 13.39 7.29 3.20 M7-11 578 0
3 V* R Dor AB* 04 36 45.59127 -62 04 37.7974 7.84 6.98 5.40 2.71 -0.44 M8III:e 289 0
4 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 958 0
5 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 727 0
6 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 1005 0
7 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2154 0
8 HD 302821 sg* 10 23 19.4807452802 -59 32 04.680572222   10.59 9.17     A7Ie 75 1
9 V* W Hya Mi* 13 49 02.0018313132 -28 22 03.532006894   8.97 7.70     M7.5-9e 603 0
10 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 759 1
11 NAME NEP reg 18 00 00.000 +66 33 38.55           ~ 260 0
12 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 833 1
13 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2333 1

    Equat.    Gal    SGal    Ecl

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2020.10.21-15:54:34

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