Blast: Resolving the Cosmic Submillimeter Background

Marsden, G.; Ade, Peter A. R.; Bock, J. J.; Chapin, Edward L.; Devlin, Mark J.; Dicker, Simon; Griffin, Matthew Joseph; Gundersen, Joshua O.; Halpern, M.; Hargrave, Peter Charles; Hughes, D. H.; Klein, Jeff; Mauskopf, Philip Daniel; Magnelli, B.; Moncelsi, L.; Netterfield, C. B.; Ngo, Henry; Olmi, L.; Pascale, Enzo; Patanchon, G.; Rex, M.; Scott, D.; Semisch, Christopher; Thomas, Nicholas E.; Truch, Matthew D. P.; Tucker, C.; Tucker, Gregory S.; Viero, Marco P.; Wiebe, Donald

doi:10.1088/0004-637x/707/2/1729

Cited by 167 publications

(203 citation statements)

References 51 publications

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“…Despite recent successes in attributing most of the extragalactic background light at submillimetre wavelengths to known galaxy populations through stacking analyses [15][16][17] , we have not individually detected the faint galaxies that are responsible for more than 85% of the total extragalactic intensity at these wavelengths 18 . The faint star-forming galaxies are expected to trace the large-scale structure of the Universe, especially in models where galaxy formation and evolution is closely connected to dark matter halos.…”

mentioning

confidence: 71%

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Amblard

Cooray

Serra

et al. 2011

Nature

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104

187

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The extragalactic background light at far-infrared wavelengths 1-3 originates from opticallyfaint, dusty, star-forming galaxies in the universe with star-formation rates at the level of a few hundred solar masses per year 4 . Due to the relatively poor spatial resolution of farinfrared telescopes 5, 6 , the faint sub-millimetre galaxies are challenging to study individually. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations 7-10 . A previous attempt 11 at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model 12 . Here we report a clear detection of the excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350, and 500 µm. From this excess, we find that submillimetre galaxies are located in dark matter halos with a minimum mass of log[M min /M ⊙ ] = 11.5 +0.7 −0.2 at 350 µm. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the universe 13 , and is lower than that predicted by semi-analytical models for galaxy formation 14 .Despite recent successes in attributing most of the extragalactic background light at submillimetre wavelengths to known galaxy populations through stacking analyses 15-17 , we have not individually detected the faint galaxies that are responsible for more than 85% of the total extragalactic intensity at these wavelengths 18 . The faint star-forming galaxies are expected to trace the large-scale structure of the Universe, especially in models where galaxy formation and evolution is closely connected to dark matter halos. While not individually detected in low resolution observations, the clustering of galaxies is expected to leave a distinct signature in the total intensity variations at sub-millimetre wavelengths. The amplitude of the power spectrum of intensity vari-2 ations as a function of the angular scale provides details on the redshift distribution and the dark matter halo mass scale of dusty, star-forming galaxies in the universe 7 .For this analysis, we used data from the Herschel Multi-tiered Extra-galactic survey (HerMES 18 ), taken with the Spectral and Photometric Imaging Receiver (SPIRE 19 ) onboard the Herschel Space Observatory 20 , during the Science Demonstration Phase (SDP) of Herschel. The data are composed of a wide 218 ′ by 218 ′ area in the Lockman Hole complemented by a narrow, but very deep (30 repeated scans), map of the Great Observatories Origins Deep Survey (GOODS) North field covering 30 ′ by 30 ′ . These fields have been very well studied at other wavelengths and they are known to have a low Galactic dust density, making it easier to distinguish the extragalactic component we wish to study. The observing time to complete each of the two fields was about 13.5 hours, observing simultaneously at 250, 350, and 500 µm.To limit the influence of a few ...

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mentioning

confidence: 71%

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Amblard

Cooray

Serra

et al. 2011

Nature

Self Cite

104

187

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“…In surveying 455 deg 2 in the 2008 ACT Southern Survey to ∼0.03 Jy, it has also contributed somewhat to the study of DSFGs (e.g. Marsden et al, 2013), although perhaps not as much as its later counterpart, South Pole Telescope.…”

Section: Atacama Cosmology Telescope [Act] 2007-presentmentioning

confidence: 99%

“…Note that Béthermin et al (2012b) use a stacking analysis of 24µm-emittors (similar to the methodology outlined by Marsden et al, 2009;Pascale et al, 2009, used for analysis of BLAST data) using Herschel data to recover the FIRAS CIB and estimate the underlying redshift distribution of 250µm, 350µm, and 500µm sources. The resulting estimates to number counts (extrapolated well beyond the nominal Herschel confusion limit) held up to more recent results from Scuba-2 (Chen et al, 2013a;Geach et al, 2013;Casey et al, 2013).…”

Section: The Cosmic Infrared Background and P(d) Analysismentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…In this work we apply the same methodology discussed in B17: we use stacking (see Dole et al 2006;Marsden et al 2009;Béthermin et al 2012, and references therein) to reduce the noise/background, since it is expected to fluctuate around the mean with positive and negative values, and enhance the signal we want to study, correspondingly.…”

Section: Stackingmentioning

confidence: 99%

Statistics of the fractional polarization of extragalactic dusty sources in Planck HFI maps

Bonavera

González‐Nuevo

Marco

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We estimate the average fractional polarisation at 143, 217 and 353 GHz of a sample of 4697 extragalactic dusty sources by applying stacking technique. The sample is selected from the second version of the Planck Catalogue of Compact Sources at 857 GHz, avoiding the region inside the Planck Galactic mask (f sky ∼ 60 per cent). We recover values for the mean fractional polarisation at 217 and 353 GHz of (3.10±0.75) per cent and (3.65 ± 0.66) per cent, respectively, whereas at 143 GHz we give a tentative value of (3.52 ± 2.48) per cent. We discuss the possible origin of the measured polarisation, comparing our new estimates with those previously obtained from a sample of radio sources.We test different distribution functions and we conclude that the fractional polarisation of dusty sources is well described by a log-normal distribution, as determined in the radio band studies. For this distribution we estimate µ 217GHz = 0.3 ± 0.5 (that would correspond to a median fractional polarisation of Π med = (1.3 ± 0.7) per cent) and µ 353GHz = 0.7 ± 0.4 (Π med = (2.0 ± 0.8) per cent), σ 217GHz = 1.3 ± 0.2 and σ 353GHz = 1.1 ± 0.2. With these values we estimate the source number counts in polarisation and the contribution given by these sources to the CMB B-mode angular power spectrum at 217, 353, 600 and 800 GHz. We conclude that extragalactic dusty sources might be an important contaminant for the primordial B-mode at frequencies > 217 GHz.

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Blast: Resolving the Cosmic Submillimeter Background

Cited by 167 publications

References 51 publications

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Dusty star-forming galaxies at high redshift

Statistics of the fractional polarization of extragalactic dusty sources in Planck HFI maps

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