The very bright SCUBA galaxy count: looking for SCUBA galaxies with the Mexican hat wavelet

Barnard, V. E.; Vielva, P.; Pierce-Price, D.; Blain, A. W.; Barreiro, R. B.; Richer, J. S.; Qualtrough, C. J.

doi:10.1111/j.1365-2966.2004.07985.x

Cited by 33 publications

(42 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Scuba-2 850µm data from Casey et al (2013) and Chen et al (2013b) are also plotted, the latter including the lens field work of Chen et al (2013a). The Cowie et al (2002) results do not quote uncertainties and the Barnard et al (2004) results represent upper limits on number counts at very high flux densities, covering larger areas than the nominal Scuba survey. The work of Blain et al (1999), Smail et al (2002), Cowie et al (2002), Knudsen et al (2008) and Chen et al (2013a) used gravitational lensing in cluster fields to survey flux densities <1 mJy.…”

Section: Number Countsmentioning

confidence: 99%

“…Figure 12 illustrates both 850-870µm number counts (from Scuba, Laboca, Scuba-2, and ALMA Blain et al, 1999;Scott et al, 2002;Chapman et al, 2002;Cowie et al, 2002;Borys et al, 2003;Webb et al, 2003;Barnard et al, 2004;Coppin et al, 2006;Scott et al, 2006;Knudsen et al, 2008;Beelen et al, 2008;Weiß et al, 2009a;Karim et al, 2013;Casey et al, 2013;Chen et al, 2013a) and 450-500µm (from Scuba, Herschel and Scuba-2 Smail et al, 2002;Oliver et al, 2010;Clements et al, 2010;Béthermin et al, 2012b;Geach et al, 2013;Casey et al, 2013;Chen et al, 2013a). Figure 13 illustrates other infrared and submillimeter number counts in the literature in direct units, from 70µm Béthermin et al, 2010a;Berta et al, 2011), 100µm (Héraudeau et al, 2004;Rodighiero & Franceschini, 2004;Kawara et al, 2004;Berta et al, 2011;Magnelli et al, 2013b), 160µm Kawara et al, 2004;Béthermin et al, 2010a;Berta et al, 2011;Magnelli et al, 2013b), 250µm and 350µm Chen+13 (850) Casey+13 (850 Figure 12: Differential submillimeter number counts at 850µm/870µm (left) and 450-500 µm (right).…”

Section: Number Countsmentioning

confidence: 99%

“…Figure 13 illustrates other infrared and submillimeter number counts in the literature in direct units, from 70µm Béthermin et al, 2010a;Berta et al, 2011), 100µm (Héraudeau et al, 2004;Rodighiero & Franceschini, 2004;Kawara et al, 2004;Berta et al, 2011;Magnelli et al, 2013b), 160µm Kawara et al, 2004;Béthermin et al, 2010a;Berta et al, 2011;Magnelli et al, 2013b), 250µm and 350µm Chen+13 (850) Casey+13 (850 Figure 12: Differential submillimeter number counts at 850µm/870µm (left) and 450-500 µm (right). The 850µm and 870µm number counts come the initial Scuba surveys Scott et al, 2002;Chapman et al, 2002;Cowie et al, 2002;Borys et al, 2003;Webb et al, 2003;Barnard et al, 2004;Coppin et al, 2006;Scott et al, 2006;Knudsen et al, 2008, , shown in brown, dark red, red, dark orange, orange, dark gold yellow, light green, green, dark teal, and teal respectively). Data from Beelen et al (2008), Weiß et al (2009a), and Karim et al (2013) are taken at 870µm rather than 850µm, the two former from Laboca and the latter from interferometric ALMA data.…”

Section: Number Countsmentioning

confidence: 99%

See 2 more Smart Citations

Dusty star-forming galaxies at high redshift

2014

View full text Add to dashboard Cite

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.

show abstract

Section: Number Countsmentioning

confidence: 99%

Section: Number Countsmentioning

confidence: 99%

Section: Number Countsmentioning

confidence: 99%

See 1 more Smart Citation

Dusty star-forming galaxies at high redshift

2014

View full text Add to dashboard Cite

show abstract

“…Candidate sources are identified by finding peaks after a Mexican Hat Wavelet type convolution (MHW, hereafter; see, e.g., Barnard et al 2004) is applied to all five SPIRE/PACS maps. Initial candidate lists from 70, 160 and 250 μm are then found and fluxes at all three bands extracted by fitting a compact Gaussian profile to the source.…”

Section: Source and Flux Extraction In The Spire/pacs Mapsmentioning

confidence: 99%

On the shape of the mass-function of dense clumps in the Hi-GAL fields

Olmi

Anglés-Alcázar

Elia

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Stars form in dense, dusty clumps of molecular clouds, but little is known about their origin and evolution. In particular, the relationship between the mass distribution of these clumps (also known as the clump mass function or CMF) and the stellar initial mass function (IMF), is still poorly understood. Aims. To discern the "true" shape of the CMF and to better understand how the CMF may evolve toward the IMF, large samples of bona-fide pre-and proto-stellar clumps are required. The sensitive observations of the Herschel Space Observatory (HSO) are now allowing us to look at large clump populations in various clouds with different physical conditions. Methods. We analyze two fields in the Galactic plane mapped by HSO during its science demonstration phase (SDP), as part of the more complete and unbiased Herschel infrared GALactic Plane Survey (Hi-GAL). These fields underwent a source-extraction and flux-estimation pipeline, which allowed us to obtain a sample with thousands of clumps. Starless and proto-stellar clumps were separated using both color and positional criteria to find those coincident with MIPS 24 μm sources. We describe the probability density functions of the power-law and lognormal models that were used to fit the CMFs. For the lognormal model we applied several statistical techniques to the data and compared their results. Results. The CMFs of the two SDP fields show very similar shapes, but very different mass scales. This similarity is confirmed by the values of the best-fit parameters of either the power-law or lognormal model. The power-law model leads to almost identical CMF slopes, whereas the lognormal model shows that the CMFs have similar widths. Conclusions. The similar CMF shape but different mass scale represents an evidence that the overall process of star formation in the two regions is very different. When comparing with the IMF, we find that the width of the IMF is narrower than the measured widths of the CMF in the two SDP fields. This may suggest that an additional mass selection occurs in later stages of gravitational collapse.

show abstract

“…Finally, we would like to point out that the MHW has been used for the detection of objects in X-ray images [22,23] and, more recently, in SCUBA [6,53] and Boomerang data [21].…”

Section: The Mexican Hat Waveletmentioning

confidence: 99%

Techniques for Compact Source Extraction in CMB Maps

Barreiro

2008

Data Analysis in Cosmology

View full text Add to dashboard Cite

The detection of compact sources embedded in a background is a very common problem in many fields of Astronomy. In these lecture notes we present a review of different techniques developed for the detection and extraction of compact sources, with a especial focus on their application to the field of the cosmic microwave background radiation. In particular, we will consider the detection of extragalactic point sources and the thermal and kinematic Sunyaev-Zeldovich effects from clusters of galaxies.

show abstract

The very bright SCUBA galaxy count: looking for SCUBA galaxies with the Mexican hat wavelet

Cited by 33 publications

References 42 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

On the shape of the mass-function of dense clumps in the Hi-GAL fields

Techniques for Compact Source Extraction in CMB Maps

Contact Info

Product

Resources

About