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Direct estimate of cirrus noise in Herschel Hi-GAL images

Martin, P. G. and Miville-Deschênes, M.-A. and Roy, A. and Bernard, J.-P. and Molinari, S. and Billot, N. and Brunt, C. and Calzoletti, L. and DiGiorgio, A. M. and Elia, D. and Faustini, F. and Joncas, G. and Mottram, J. C. and Natoli, P. and Noriega-Crespo, A. and Paladini, R. and Robitaille, J. F. and Strafella, F. and Traficante, A. and Veneziani, M. (2010) Direct estimate of cirrus noise in Herschel Hi-GAL images. Astronomy and Astrophysics, 518 . Art. No. L105. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20101202-111113648

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Abstract

In Herschel images of the Galactic plane and many star forming regions, a major factor limiting our ability to extract faint compact sources is cirrus confusion noise, operationally defined as the “statistical error to be expected in photometric measurements due to confusion in a background of fluctuating surface brightness”. The histogram of the flux densities of extracted sources shows a distinctive faint-end cutoff below which the catalog suffers from incompleteness and the flux densities become unreliable. This empirical cutoff should be closely related to the estimated cirrus noise and we show that this is the case. We compute the cirrus noise directly, both on Herschel images from which the bright sources have been removed and on simulated images of cirrus with statistically similar fluctuations. We connect these direct estimates with those from power spectrum analysis, which has been used extensively to predict the cirrus noise and provides insight into how it depends on various statistical properties and photometric operational parameters. We report multi-wavelength power spectra of diffuse Galactic dust emission from Hi-GAL observations at 70 to 500 μm within Galactic plane fields at l = 30° and l = 59° .We find that the exponent of the power spectrum is about −3. At 250 μm, the amplitude of the power spectrum increases roughly as the square of the median brightness of the map and so the expected cirrus noise scales linearly with the median brightness. For a given region, the wavelength dependence of the amplitude can be described by the square of the spectral energy distribution (SED) of the dust emission. Generally, the confusion noise will be a worse problem at longer wavelengths, because of the combination of lower angular resolution and the rising power spectrum of cirrus toward lower spatial frequencies, but the photometric signal to noise will also depend on the relative SED of the source compared to the cirrus.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201014684DOIUNSPECIFIED
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014684&Itemid=129PublisherUNSPECIFIED
ORCID:
AuthorORCID
Martin, P. G.0000-0002-5236-3896
Roy, A.0000-0001-8127-5775
Noriega-Crespo, A.0000-0002-6296-8960
Paladini, R.0000-0002-5158-243X
Traficante, A.0000-0003-1665-6402
Additional Information:© 2010 ESO. Received 31 March 2010, Accepted 13 May 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.
Subject Keywords:ISM: structure, ISM: general, stars: formation, stars: protostars, submillimeter: ISM, infrared: ISM
Record Number:CaltechAUTHORS:20101202-111113648
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20101202-111113648
Official Citation:Direct estimate of cirrus noise in Herschel Hi-GAL images P. G. Martin, M.-A. Miville-Deschênes, A. Roy, J.-P. Bernard, S. Molinari, N. Billot, C. Brunt, L. Calzoletti, A. M. DiGiorgio, D. Elia, F. Faustini, G. Joncas, J. C. Mottram, P. Natoli, A. Noriega-Crespo, R. Paladini, J. F. Robitaille, F. Strafella, A. Traficante and M. Veneziani A&A 518 L105 (2010) DOI: 10.1051/0004-6361/201014684
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21126
Collection:CaltechAUTHORS
Deposited By: Benjamin Perez
Deposited On:02 Dec 2010 20:10
Last Modified:09 Mar 2020 13:19

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