Submillimeter Number Counts From Statistical Analysis of Blast Maps

Patanchon, G.; Ade, Peter A. R.; Bock, J. J.; Chapin, Edward L.; Devlin, Mark J.; Dicker, Simon; Griffin, M.; Gundersen, Joshua O.; Halpern, M.; Hargrave, Peter Charles; Hughes, D. H.; Klein, Jeff; Marsden, G.; Mauskopf, Philip Daniel; Moncelsi, L.; Netterfield, C. B.; Olmi, L.; Pascale, Enzo; 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/707/2/1750

Cited by 99 publications

(149 citation statements)

References 62 publications

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“…There is flattening to about 20 mJy. We find very good agreement with the number counts estimated from a P(D) fluctuation analysis of the BLAST maps (Patanchon et al 2009). …”

Section: Resultssupporting

confidence: 79%

“…We have constructed input maps various from various number count models (Pearson & Khan 2009;Lagache et al 2004;Patanchon et al 2009) and models from Xu et al 2003;Lacey et al 2010). These input maps are then processed by the SPIRE photometer simulator (sps, Sibthorpe et al 2009) for observational programmes exactly the same as the real data.…”

Section: Methodsmentioning

confidence: 99%

“…This indicates that as much energy is received from galaxies after being reprocessed through dust as is received directly. It is only very recently, using BLAST, that count models have been probed using fluctuation techniques (Patanchon et al 2009) or directly (Béthermin et al 2010) at the wavelength where the background peaks.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

Oliver¹,

Wang²,

Smith³

et al. 2010

A&A

217

123

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Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ∼20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ∼15% of the infrared extra-galactic background at the wavelength near where it peaks.

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“…There is flattening to about 20 mJy. We find very good agreement with the number counts estimated from a P(D) fluctuation analysis of the BLAST maps (Patanchon et al 2009). …”

Section: Resultssupporting

confidence: 79%

Section: Methodsmentioning

confidence: 99%

See 1 more Smart Citation

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

Oliver¹,

Wang²,

Smith³

et al. 2010

A&A

217

123

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“…P(D) method allows a constraint on the faint-end counts below confusion and has been used widely in sub-mm maps since the SCUBA surveys (Hughes et al, 1998). Patanchon et al (2009) expanded the technique with a parameterized functional form for faint-end counts with knots and slopes. The number count model parameters extracted through the P(D) histogram data under such a model are correlated and these correlations need to be taken into account either when comparing faint-end P(D) counts to number count models or when using P(D) counts to distinguish cosmological models of the DSFG population.…”

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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“…Aims. We estimate the extragalactic number counts in the BLAST data, which allow a comparison with the results of the P(D) analysis of Patanchon et al (2009). Methods.…”

mentioning

confidence: 99%

Submillimeter number counts at 250 μm, 350 μm and 500 μm in BLAST data

Béthermin

Dole

Cousin

et al. 2010

A&A

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Context. The instrument BLAST (Balloon-borne Large-Aperture Submillimeter Telescope) performed the first deep and wide extragalactic survey at 250, 350 and 500 μm. The extragalactic number counts at these wavelengths are important constraints for modeling the evolution of infrared galaxies. Aims. We estimate the extragalactic number counts in the BLAST data, which allow a comparison with the results of the P(D) analysis of Patanchon et al. (2009). Methods. We use three methods to identify the submillimeter sources. 1) Blind extraction using an algorithm when the observed field is confusion-limited and another one when the observed field is instrumental-noise-limited. The photometry is computed with a new simple and quick point spread function (PSF) fitting routine (FASTPHOT). We use Monte-Carlo simulations (addition of artificial sources) to characterize the efficiency of this extraction, and correct the flux boosting and the Eddington bias. 2) Extraction using a prior. We use the Spitzer 24 μm galaxies as a prior to probe slightly fainter submillimeter flux densities. 3) A stacking analysis of the Spitzer 24 μm galaxies in the BLAST data to probe the peak of the differential submillimeter counts. Results. With the blind extraction, we reach 97 mJy, 83 mJy and 76 mJy at 250 μm, 350 μm and 500 μm respectively with a 95% completeness. With the prior extraction, we reach 76 mJy, 63 mJy, 49 mJy at 250 μm, 350 μm and 500 μm respectively. With the stacking analysis, we reach 6.2 mJy, 5.2 mJy and 3.5 mJy at 250 μm, 350 μm and 500 μm respectively. The differential submillimeter number counts are derived, and start showing a turnover at flux densities decreasing with increasing wavelength. (2009) models slightly overestimate the observed counts, but the data agree very well near the peak of the differential number counts. Models predict that the galaxy populations probed at the peak are likely z ∼ 1.8 ultra-luminous infrared galaxies.

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Submillimeter Number Counts From Statistical Analysis of Blast Maps

Cited by 99 publications

References 62 publications

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

Dusty star-forming galaxies at high redshift

Submillimeter number counts at 250 μm, 350 μm and 500 μm in BLAST data

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