The Detection of a Population of Submillimeter-Bright, Strongly Lensed Galaxies

Negrello, M.; Hopwood, R.; Zotti, G. de; Cooray, Asantha; Verma, Aprajita; Bock, J. J.; Frayer, D. T.; Gurwell, M. A.; Omont, A.; Neri, R.; Dannerbauer, H.; Leeuw, L. L.; Barton, Elizabeth J.; Cooke, Jeff; Kim, S.; Cunha, Elisabete da; Rodighiero, G.; Cox, P.; Bonfield, D. G.; Jarvis, M. J.; Serjeant, S.; Ivison, R. J.; Dye, S.; Aretxaga, I.; Hughes, D. H.; Ibar, E.; Bertoldi, F.; Valtchanov, I.; Eales, Stephen Anthony; Dunne, L.; Driver, Simon P.; Auld, Robbie Richard; Buttiglione, S.; Cava, A.; Grady, C. A.; Clements, D. L.; Dariush, Aliakbar; Fritz, J.; Hill, D. T.; Hornbeck, Jeremy; Kelvin, Lee S.; Lagache, G.; López‐Caniego, M.; González‐Nuevo, J.; Maddox, S.; Pascale, Enzo; Pohlen, M.; Rigby, E. E.; Robotham, Aaron S. G.; Simpson, Chris; Smith, D. J. B.; Temi, P.; Thompson, M. A.; Woodgate, B. E.; York, Donald G.; Aguirre, James E.; Beelen, A.; Blain, A. W.; Baker, A. J.; Birkinshaw, Mark; Blundell, R.; Bradford, C. M.; Burgarella, D.; Danese, L.; Dunlop, James; Fleuren, S.; Glenn, J.; Harris, A. I.; Kamenetzky, J.; Lupu, Roxana; Maddalena, R. J.; Madore, Barry F.; Maloney, Philip R.; Matsuhara, Hideo; Michaowski, M. J.; Murphy, E. J.; Naylor, B. J.; Nguyen, Hien; Popescu, Cristina; Rawlings, Steve; Rigopoulou, D.; Scott, Douglas; Scott, K. S.; Seibert, Mark; Smail, Ian; Tuffs, R.; Vieira, J. D.; Werf, P. P. van der; Žmuidzinas, J.

doi:10.1126/science.1193420

Cited by 395 publications

(531 citation statements)

References 42 publications

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“…The selection is especially easy since the lensed sources are the brightest sources in the submm maps, and only basic spectral filtering for radio-bright blazars is needed to find the lensed DSFGs in millimeter maps. Negrello et al (2010) demonstrated through multi-wavelength follow-up observations of the first five Herschel-selected DSFGs with S 500 > 100 mJy at 500µm, after accounting for nearby spiral galaxies and radio-bright blazars, are all gravitationally lensed (Fig. 34).…”

Section: Lensed Dsfgsmentioning

confidence: 99%

“…In this context, gravitational lensing has played a critical role because the spatial enhancement associated with magnification provides a way to investigate the internal structure of distant, faint galaxies to levels unattainable with the current generation of instrumentation for typical DSFGs. A second important fact here is that large samples of gravitationally lensed galaxies can be efficiently selected by searching for bright sources in wide area submillimeter surveys (Blain, 1996;Perrotta et al, 2002;Negrello et al, 2007Negrello et al, , 2010Hezaveh & Holder, 2011;Wardlow et al, 2013). While the early submm surveys were limited to smaller sky areas, the advent of wide-field surveys, especially with Herschel and SPT, at sub/millimeter wavelengths have allowed detections of large samples of lensed DSFGs that can be followed up with a host of radio and submm/mm-wave interferometers.…”

Section: Detailed Studies Of Individual Dusty Star-forming Galaxiesmentioning

confidence: 99%

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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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Section: Lensed Dsfgsmentioning

confidence: 99%

Section: Detailed Studies Of Individual Dusty Star-forming Galaxiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…Now, Herschel (Pilbratt et al 2010) has found that lensing is significant for some of the brightest submm sources, with surveys such as H-ATLAS and HerMES (Herschel Multi-tiered Extragalactic Survey) turning up a population of sources which are boosted enough that they can be studied in great detail in follow-up observations (e.g. Negrello et al 2010;Wardlow et al 2013). How-E-mail: todd@phas.ubc.ca ever, the limited resolution of Herschel, and of non-interferometric ground-based observatories such as the JCMT, means that the effects of source blending are a cause of uncertainty in interpreting the results (e.g.…”

Section: Introductionmentioning

confidence: 99%

Disentangling a group of lensed submm galaxies at z∼ 2.9

Mackenzie¹,

Scott²,

Smail³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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MS 0451.6−0305 is a rich galaxy cluster whose strong lensing is particularly prominent at submm wavelengths. We combine new SCUBA-2 data with imaging from Herschel SPIRE and PACS and HST in order to try to understand the nature of the sources being lensed. In the region of the "giant submm arc," we uncover seven multiply imaged galaxies (up from the previously known three), of which six are found to be at a redshift of z ∼ 2.9, and possibly constitute an interacting system. Using a novel forward-modelling approach, we are able to simultaneously deblend and fit SEDs to the individual galaxies that contribute to the giant submm arc, constraining their dust temperatures, far infrared luminosities and star formation rates. The submm arc first identified by SCUBA can now be seen to be composed of at least five distinct sources, four of these within the galaxy group at z ∼ 2.9. The total unlensed luminosity for this galaxy group is (3.1 ± 0.3) × 10 12 L , which gives an unlensed star formation rate of (450 ± 50) M yr −1 . From the properties of this system, we see no evidence of evolution towards lower temperatures in the dust temperature versus far-infrared luminosity relation for high redshift galaxies.

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“…It is true that a significant fraction of IRAS hyperluminous infrared galaxies are lensed (Rowan-Robinson & Wang 2010 estimate the lensed percentage to be 10-30%). Negrello et al (2010) show 5 lensed galaxies from the Herschel-Atlas survey. They estimate that a significant fraction (50%?)…”

Section: Submillimetre Galaxiesmentioning

confidence: 99%

Panchromatic radiation from galaxies as a probe of galaxy formation and evolution

Rowan-Robinson

2011

Proc. IAU

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Abstract. I review work on modelling the infrared and submillimetre SEDs of galaxies. The underlying physical assumptions are discussed and spherically symmetric, axisymmetric, and 3-dimensional radiative transfer codes are reviewed. Models for galaxies with Spitzer IRS data and for galaxies in the Herschel-Hermes survey are discussed. Searches for high redshift infrared and submillimetre galaxies, the star formation history, the evolution of dust extinction, and constraints from source-counts, are briefly discussed.Keywords. infrared galaxies, radiative transfer, star formation Early work on radiative transfer models for infrared sourcesDuring the 1960s and early 1970s very simplistic models began to be developed for infrared sources associated with circumstellar dust shells, HII regions and star-forming regions. These models assumed that the dust grain density n(r) and temperature T(r) have a power-law dependence on radius r and that the dust is optically thin. Scattering was neglected and so the emission was simply calculated as a sum of n(r)Q ν B ν (T (r)), integrated over r.The first complete solution of the spherically symmetric radiative transfer problem for an optically thick dust cloud was by Leung (1975). He used detailed grain properties and carried out a full solution of the moment equations, including anisotropic scattering. The grain temperature was solved for by assuming radiative balance. Yorke & Krugel (1977) modelled the dynamical evolution of an HII region, including the interaction between gas and dust. Radiative transfer was approximated by diffusion. These two papers marked a tremendous step forward in the quality of models for infrared sources. To take advantage of numerical techniques which had been used in modelling stellar atmospheres, Leung essentially assumed that the radiation field is isotropic through most of the cloud (the Eddington approximation).Rowan-Robinson (1980) carried out a numerical solution of the full radiative transfer equation. The intensity, I ν (θ, r), was calculated throughout the cloud using a grid of values in ν, r, θ. This showed that the Eddington approximation is a poor assumption throughout a dust cloud and revealed the phenomenon of sideways beaming of the radiation field at the inner edge of cloud. Viewed from a distance a dust cloud surrounding a star should show a ring of bright emission in the mid infrared, coming from the inner edge of the dust cloud. A second interesting phenomenon revealed by a full solution of the radiative transfer equation is that of back radiation onto the star. The dust cloud radiates at the star and so the net spectrum of emission emerging from the star is no longer a blackbody, but has absorption bands at the wavelengths of dust emission features (Rowan-Robinson 1982). Rowan-Robinson & Harris (1982 applied this code to all the bright circumstellar dust shells in the AFGL survey. 446at https://www.cambridge.org/core/terms. https://doi

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The Detection of a Population of Submillimeter-Bright, Strongly Lensed Galaxies

Cited by 395 publications

References 42 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Disentangling a group of lensed submm galaxies at z∼ 2.9

Panchromatic radiation from galaxies as a probe of galaxy formation and evolution

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