Nguyen, H. T. and Schulz, B. and Levenson, L. and Blain, A. and Bock, J. and Cooray, A. and Dowell, C. D. and Lu, N. and Marshall, J. and Shupe, D. L. and Xu, C. K. and Zemcov, M. (2010) HerMES: The SPIRE confusion limit. Astronomy and Astrophysics, 518 . Art. No. L5. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20101202-143136718
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We report on the sensitivity of SPIRE photometers on the Herschel Space Observatory. Specifically, we measure the confusion noise from observations taken during the science demonstration phase of the Herschel Multi-tiered Extragalactic Survey. Confusion noise is defined to be the spatial variation of the sky intensity in the limit of infinite integration time, and is found to be consistent among the different fields in our survey at the level of 5.8, 6.3 and 6.8 mJy/beam at 250, 350 and 500 μm, respectively. These results, together with the measured instrument noise, may be used to estimate the integration time required for confusion limited maps, and provide a noise estimate for maps obtained by SPIRE.
|Additional Information:||© 2010 ESO. Received 31 March 2010, Accepted 20 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).|
|Subject Keywords:||space vehicules: instruments, surveys, submillimeter: diffuse background, submillimiter: galaxies|
|Official Citation:||HerMES: The SPIRE confusion limit H. T. Nguyen, B. Schulz, L. Levenson, A. Amblard, V. Arumugam, H. Aussel, T. Babbedge, A. Blain, J. Bock, A. Boselli, V. Buat, N. Castro-Rodriguez, A. Cava, P. Chanial, E. Chapin, D. L. Clements, A. Conley, L. Conversi, A. Cooray, C. D. Dowell, E. Dwek, S. Eales, D. Elbaz, M. Fox, A. Franceschini, W. Gear, J. Glenn, M. Griffin, M. Halpern, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, N. Lu, S. Madden, B. Maffei, G. Mainetti, L. Marchetti, G. Marsden, J. Marshall, B. O'Halloran, S. J. Oliver, A. Omont, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Perez Fournon, M. Pohlen, N. Rangwala, D. Rigopoulou, D. Rizzo, I. G. Roseboom, M. Rowan-Robinson, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Stevens, M. Symeonidis, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, L. Vigroux, L. Wang, R. Ward, D. Wiebe, G. Wright, C. K. Xu and M. Zemcov A&A 518 L5 (2010) DOI: 10.1051/0004-6361/201014680|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Benjamin Perez|
|Deposited On:||02 Dec 2010 23:14|
|Last Modified:||26 Dec 2012 12:42|
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