LENS MODELS OF<i>HERSCHEL</i>-SELECTED GALAXIES FROM HIGH-RESOLUTION NEAR-IR OBSERVATIONS

Calanog, Jae; Fu, Hai; Cooray, Asantha; Wardlow, J. L.; Ma, Bo; Amber, S.; Baker, A. J.; Baes, M.; Bock, J. J.; Bourne, N.; Bussmann, R. S.; Casey, Caitlin M.; Chapman, Stephen; Clements, D. L.; Conley, A.; Dannerbauer, H.; Zotti, G. de; Dunne, L.; Dye, S.; Eales, Stephen Anthony; Farrah, D.; Furlanetto, C.; Harris, A. I.; Ivison, R. J.; Kim, S.; Maddox, S.; Magdis, G.; Messias, H.; Michalowski, Michal; Negrello, M.; Nightingale, J. W.; O'Bryan, Jon; Oliver, Seb; Riechers, Dominik A.; Scott, D.; Serjeant, S.; Simpson, J. M.; Smith, M.; Timmons, Nicholas; Thacker, Cameron; Valiante, Elisabetta; Vieira, J. D.

doi:10.1088/0004-637x/797/2/138

Cited by 50 publications

(93 citation statements)

References 129 publications

(246 reference statements)

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“…Near-IR follow-up observations with the Hubble Space Telescope (HST) and the Keck telescope in adaptive optics (AO) are available for tens of candidate lensed galaxies in the H-ATLAS fields (Fu et al 2012;Bussmann et al 2013;Calanog et al 2014;Negrello et al 2014). Some of these sources have also been observed with the Sub-millimeter Array (SMA) at ∼0.5 arcsec resolution at 880 µm (Negrello et al 2010;Bussmann et al 2012Bussmann et al , 2013, while six of them have been recently imaged in band 7 with the ALMA with better resolution and sensitivity (PI: Eales).…”

Section: Data S E T Smentioning

confidence: 99%

“…Wide-area extragalactic surveys performed at sub-millimeter (submm) to millimeter (mm) wavelengths with the Herschel Space Observatory (Pilbratt et al 2010) and the South Pole Telescope (SPT; Carlstrom et al 2011) have led to the discovery of several dusty star-forming galaxies (DSFGs) at z 1 whose luminosity is magnified by a foreground galaxy or a group/cluster of galaxies (Negrello et al 2010(Negrello et al , 2014Conley et al 2011;Cox et al 2011; Bussmann E-mail: NegrelloM@cardiff.ac.uk Vieira et al 2013;Wardlow et al 2013;Calanog et al 2014;Messias et al 2014;Dye et al 2015;Nayyeri et al 2016;Spilker et al 2016). The selection of strongly lensed galaxies at these wavelengths is made possible by the (predicted) steep number counts of high-redshift sub-mm galaxies (Blain 1996;Negrello et al 2007); in fact, almost exclusively, those galaxies whose flux density has been boosted by an event of lensing can be observed above a certain threshold, namely ∼100 mJy at 500 µm (Negrello et al 2010;Wardlow et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…Preliminary source catalogues derived from the full H-ATLAS were then used to identify the sub-mm brightest candidate lensed galaxies for follow-up observations with both ground based and space telescopes to measure their redshifts (Frayer et al 2011;Omont et al 2011Omont et al , 2013Valtchanov et al 2011;Harris et al 2012;Lupu et al 2012;George et al 2013;Messias et al 2014) and confirm their nature (Negrello et al 2010(Negrello et al , 2014Bussmann et al 2012Bussmann et al , 2013Fu et al 2012;Calanog et al 2014). Using the same methodology, i.e.…”

Section: Introductionmentioning

confidence: 99%

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TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²

Negrello

Amber

Amvrosiadis

et al. 2016

Mon. Not. R. Astron. Soc.

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136

243

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Section: Data S E T Smentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²

Negrello

Amber

Amvrosiadis

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

136

243

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“…4  for SDSS and 2MASS, respectively. The astrometrically calibrated Gemini-S images served as the basis for aligning higher resolution imaging with a smaller field of view from the Hubble Space Telescope (HST) or Keck (when available), which were originally presented in Calanog et al (2014).…”

Section: Gemini-south Imagingmentioning

confidence: 99%

HerMES: ALMA IMAGING OFHERSCHEL-SELECTED DUSTY STAR-FORMING GALAXIES

Bussmann

Riechers

Fialkov

et al. 2015

ApJ

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108

159

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The Herschel Multi-tiered Extragalactic Survey (HerMES) has identified large numbers of dusty star-forming galaxies (DSFGs) over a wide range in redshift. A detailed understanding of these DSFGs is hampered by the limited spatial resolution of Herschel. We present 870 μm 0 45 resolution imaging obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) of a sample of 29 HerMES DSFGs that have far-infrared (FIR) flux densities that lie between the brightest of sources found by Herschel and fainter DSFGs found via groundbased surveys in the submillimeter region. The ALMA imaging reveals that these DSFGs comprise a total of 62 sources (down to the 5s point-source sensitivity limit in our ALMA sample; 0.2 mJy s » ). Optical or nearinfrared imaging indicates that 36 of the ALMA sources experience a significant flux boost from gravitational lensing ( 1.1 m > ), but only six are strongly lensed and show multiple images. We introduce and make use of UVMCMCFIT, a general-purpose and publicly available Markov chain Monte Carlo visibility-plane analysis tool to analyze the source properties. Combined with our previous work on brighter Herschel sources, the lens models presented here tentatively favor intrinsic number counts for DSFGs with a break near 8 mJy at 880 m m and a steep fall-off at higher flux densities. Nearly 70% of the Herschel sources break down into multiple ALMA counterparts, consistent with previous research indicating that the multiplicity rate is high in bright sources discovered in singledish submillimeter or FIR surveys. The ALMA counterparts to our Herschel targets are located significantly closer to each other than ALMA counterparts to sources found in the LABOCA ECDFS Submillimeter Survey. Theoretical models underpredict the excess number of sources with small separations seen in our ALMA sample. The high multiplicity rate and small projected separations between sources seen in our sample argue in favor of interactions and mergers plausibly driving both the prodigious emission from the brightest DSFGs as well as the sharp downturn above S 8 mJy 880 = .

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“…This model serves as a control for our experiments, allowing us to quantify the overall importance of the ENV/LOS for constraining cosmology. This approach almost surely produces biased constraints on the Hubble constant, and so it is rarely used in studies that derive constraints on precision cosmology, but it still appears in some studies that focus on lens and source properties (e.g., Calanog et al 2014;Hezaveh et al 2013). …”

Section: Introductionmentioning

confidence: 99%

Quantifying Environmental and Line-of-sight Effects in Models of Strong Gravitational Lens Systems

McCully

Keeton

Wong

et al. 2017

ApJ

120

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Matter near a gravitational lens galaxy or projected along the line of sight (LOS) can affect strong lensing observables by more than contemporary measurement errors. We simulate lens fields with realistic threedimensional mass configurations (self-consistently including voids), and then fit mock lensing observables with increasingly complex lens models to quantify biases and uncertainties associated with different ways of treating the lens environment (ENV) and LOS. We identify the combination of mass, projected offset, and redshift that determines the importance of a perturbing galaxy for lensing. Foreground structures have a stronger effect on the lens potential than background structures, due to nonlinear effects in the foreground and downweighting in the background. There is dramatic variation in the net strength of ENV/LOS effects across different lens fields; modeling fields individually yields stronger priors for H 0 than ray tracing through N-body simulations. Models that ignore mass outside the lens yield poor fits and biased results. Adding external shear can account for tidal stretching from galaxies at redshifts  z z lens , but it requires corrections for external convergence and cannot reproduce nonlinear effects from foreground galaxies. Using the tidal approximation is reasonable for most perturbers as long as nonlinear redshift effects are included. Even then, the scatter in H 0 is limited by the lens profile degeneracy. Asymmetric image configurations produced by highly elliptical lens galaxies are less sensitive to the lens profile degeneracy, so they offer appealing targets for precision lensing analyses in future surveys like LSST and Euclid.

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LENS MODELS OFHERSCHEL-SELECTED GALAXIES FROM HIGH-RESOLUTION NEAR-IR OBSERVATIONS

Cited by 50 publications

References 129 publications

TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²

TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²

HerMES: ALMA IMAGING OFHERSCHEL-SELECTED DUSTY STAR-FORMING GALAXIES

Quantifying Environmental and Line-of-sight Effects in Models of Strong Gravitational Lens Systems

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LENS MODELS OFHERSCHEL-SELECTED GALAXIES FROM HIGH-RESOLUTION NEAR-IR OBSERVATIONS

Cited by 50 publications

References 129 publications

TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg2

TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg2

HerMES: ALMA IMAGING OFHERSCHEL-SELECTED DUSTY STAR-FORMING GALAXIES

Quantifying Environmental and Line-of-sight Effects in Models of Strong Gravitational Lens Systems

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TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²

TheHerschel-ATLAS: a sample of 500 μm-selected lensed galaxies over 600 deg²