IRIS: A New Generation of IRAS Maps

By M. Miville-Deschênes, G. Lagache. 2004

390 citations recorded by the source corpus.

The Infrared Astronomical Satellite (IRAS) had a tremendous impact on many areas of modern astrophysics. In particular, it revealed the ubiquity of infrared cirrus that are a spectacular manifestation of the interstellar medium complexity but also an important foreground for observational cosmology. With the forthcoming Planck satellite there is a need for all-sky complementary data sets with arcminute resolution that can bring informations on specific foreground emissions that contaminate the cosmic microwave background radiation. With its ∼4′ resolution matching perfectly the high-frequency bands of Planck, IRAS is a natural data set to study the variations of dust properties at all scales. But the latest version of the images delivered by the IRAS team (the ISSA plates) suffer from calibration, zero level, and striping problems that can preclude its use, especially at 12 and 25 μm. In this paper we present how we proceeded to solve each of these problems and enhance significantly the general quality of the ISSA plates in the four bands (12, 25, 60, and 100 μm). This new generation of IRAS images, called IRIS, benefits from a better zodiacal light subtraction, from a calibration and zero level compatible with DIRBE, and from a better destriping. At 100 μm the IRIS product is also a significant improvement from the Schlegel et al. maps. IRIS keeps the full ISSA resolution, it includes well-calibrated point sources, and the diffuse emission calibration at scales smaller than 1° was corrected for the variation of the IRAS detector responsivity with scale and brightness. The uncertainty on the IRIS calibration and zero level is dominated by the uncertainty on the DIRBE calibration and on the accuracy of the zodiacal light model.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7d1ba85d5c6ed29e8589ac3bc5588dc0b32f8743

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Citations in the corpus

A full sky, low foreground, high resolution CMB map from WMAP (2008, methodology): “For this reason, in the present work, we improve on dust removal by using, as an additional measurement, the IRIS 100 micron dust template obtained from a combination of DIRBE and IRAS maps (Miville-Deschênes & Lagache 2005).”
The COMPLETE Survey of Star-Forming Regions: Phase I Data (2006, methodology): “IRIS6 images (Miville-Deschênes & Lagache 2005) of 60 and 100µm flux density were obtained for the two regions.”
Characterizing precursors to stellar clusters with Herschel (2011, methodology): “We compared the Herschel-SPIRE and PACS data with the predictions of a model provided by the Planck collaboration (Planck Core-Team, priv. comm.) and constrained on the Planck and IRIS data (Miville-Deschênes & Lagache 2005).”
Planckintermediate results (2016, methodology): “We explicitly use the Improved Reprocessing of the IRAS Survey maps (IRIS3, Miville-Deschênes & Lagache 2005), for which artefacts such as zero level, calibration, striping, and residual zodiacal light have been corrected.”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, methodology): “8 (CIB, [2], the cross-correlation between tSZ and CIB (tSZ-CIB, negative at 150 GHz, [3], and Galactic cirrus ([47]).”
The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data (2013, methodology): “Following Hajian et al. (2012) we perform a multicomponent ﬁt to the auto-power spectrum of the IRIS map after application of the dust mask described above.”
Planck2013 results. XXVIII. ThePlanckCatalogue of Compact Sources (2013, methodology): “A catalogue was extracted from the IRIS 100 µm map (MivilleDeschênes & Lagache 2005) using the MHW2 pipeline, and that is used as the neighbouring channel above 857 GHz.”
The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, positive): “To determine the amplitude and spectrum of the residual component we cross correlate with the IRIS map (Miville-Deschˆenes & Lagache 2005) as described in detail in Das et al. (2013).”
Planck 2013 results. XI. All-sky model of thermal dust emission (2013, methodology): “Miville-Deschênes & Lagache (2005) used the DIRBE 100 µm map from which ZE was removed by the DIRBE team, using the model of Kelsall et al. (1998).”
Planck2015 results: XXVI. The SecondPlanckCatalogue of Compact Sources (2015, positive): “A catalogue was extracted from the IRIS 100 µm map (Miville-Deschênes & Lagache 2005) using the MHW2 pipeline, and used as the neighbouring channel above 857 GHz.”
SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW (2011, methodology): “Previous SMC infrared surveys have been done with IRAS at a resolution of ∼4′ for 12, 25, 60, and 100 µm (Schwering & Israel 1989; Miville-Deschênes & Lagache 2005), with the Infrared Space Observatory (ISO) at a resolution of 2′ at 170 µm (Wilke et al. 2003), and with MSX at a resolution of 18′′…”
Planck 2015 results: XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation (2015, positive): “We use the reprocessed IRAS maps, IRIS (Improved Reprocessing of the IRAS Survey, Miville-Deschênes & Lagache 2005) in the HEALPix pixelization scheme.”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, methodology): “The IRIS effective FWHM is about 4.3′ (Miville-Deschênes & Lagache 2005).”
Planck 2015 results. I. Overview of products and scientific results (2015, methodology): “As was done in 2013, in Planck Collaboration X (2015) we establish a single parametric model of the microwave sky, accounting simultaneously for all significant diffuse astrophysical components and relevant instrumental effects using the Bayesian Commander analysis framework (Eriksen et al.”