BLAST: RESOLVING THE COSMIC SUBMILLIMETER BACKGROUND

By G. Marsden, Peter A. R. Ade, J. Bock, E. Chapin, M. Devlin, S. Dicker, M. Griffin, J. Gundersen, Mark Halpern, P. Hargrave and 19 more. 2009

144 citations recorded by the source corpus.

The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) has made 1 deg2, deep, confusion-limited maps at three different bands, centered on the Great Observatories Origins Deep Survey South Field. By calculating the covariance of these maps with catalogs of 24 μm sources from the Far-Infrared Deep Extragalactic Legacy Survey, we have determined that the total submillimeter intensities are 8.60 ± 0.59, 4.93 ± 0.34, and 2.27 ± 0.20 nW m−2 sr−1 at 250, 350, and 500 μm, respectively. These numbers are more precise than previous estimates of the cosmic infrared background (CIB) and are consistent with 24 μm-selected galaxies generating the full intensity of the CIB. We find that the fraction of the CIB that originates from sources at z ⩾ 1.2 increases with wavelength, with 60% from high-redshift sources at 500 μm. At all BLAST wavelengths, the relative intensity of high-z sources is higher for 24 μm-faint sources than that for 24 μm-bright sources. Galaxies identified as active galactic nuclei (AGNs) by their Infrared Array Camera colors are 1.6–2.6 times brighter than the average population at 250–500 μm, consistent with what is found for X-ray-selected AGNs. BzK-selected galaxies are found to be moderately brighter than typical 24 μm-selected galaxies in the BLAST bands. These data provide high-precision constraints for models of the evolution of the number density and intensity of star-forming galaxies at high redshift.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3360d097e7f393119a2324344823c04bcb8b3029

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Citations in the corpus

• The Herschel Multi-tiered Extragalactic Survey: HerMES (2012, background): “It appears that a large fraction of the 24 µm sources can be statistically detected at longer wavelengths (e.g. Marsden et al. 2009).”
• Building the cosmic infrared background brick by brick with Herschel/PEP. ⋆ (2011, background): “It is possible to recover part of this information by performing stacking of sources from deep r data (typically at shorter wavelengths, e.g. Dole et al. 2006; Marsden et al. 2009; Béthermin et al. 2010a).”
• A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “The CIB signal originates in DSFGs over a large range in redshift (Lagache et al. 2005; Marsden et al. 2009; Casey et al. 2014).”
• A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, background): “Cosmic Infrared Background The CIB is produced by thermal emission from DSFGs over a very broad range in redshift (Lagache et al. 2005; 10 Marsden et al. 2009).”
• THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, methodology): “We thus apply the Marsden et al. (2009) method to perform our stacking, which takes the mean of pixels centered on sources in the beam-smoothed map.”
• MODELING THE EXTRAGALACTIC BACKGROUND LIGHT FROM STARS AND DUST (2009, methodology): “Their infrared component, however, considerable overpredicts the 250 µm measurements from BLAST (Marsden et al. 2009) and COBE (Fixsen et al. 1998).”
• A deep ALMA image of the Hubble Ultra Deep Field (2016, unknown): “…15% of the known far-infrared/mm background (Fixsen et al. 1998; Scott et al. 2012; Geach et al. 2013), and attempts to complete our inventory of obscured star formation have had to rely on stacking experiments (e.g. Peacock et al. 2000; Marsden et al. 2009; Geach et al. 2013; Coppin et al. 2015).”
• Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, unknown): “The Marsden et al. (2009) limits are very stringent.”
• HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background (2012, methodology): “Several methods can be used (e.g. Dole et al. 2006, Marsden et al. 2009, see the discussion in Vieira et al. in prep.).”
• SIMULATIONS OF THE MICROWAVE SKY (2009, result): “This is consistent with BLAST observations (Marsden et al. 2009; Devlin et al. 2009), which indicate that most, and perhaps all, of the CIB is generated by infrared sources.”
• The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, background): “More specifically, it can be shown that the mean stacked value corresponds to the covariance between the input source catalog and the map (Marsden et al. 2009).”
• AN IMPRINT OF MOLECULAR CLOUD MAGNETIZATION IN THE MORPHOLOGY OF THE DUST POLARIZED EMISSION (2013, background): “Estimations made using nominal values of the sensitivity of BLASTPol (Marsden et al. 2009) in a 50 hours observation of a 1 square degree region indicate that polarization errors of 0.5% or less can be achieved in regions which densities ∼ 2.38×1022 NH cm −2, where the HRO show the change of the rel”
• COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE (2011, background): “Dusty galaxies (CIB) The CIB is produced by thermal emission from dusty star-forming galaxies (DSFGs) over a very broad range in redshift (Lagache et al. 2005; Marsden et al. 2009).”