A free-form lensing grid solution for A1689 with new multiple images

Diego, J. M.; Broadhurst, Tom; Benítez, N.; Umetsu, Keiichi; Coe, Dan; Sendra, Irene; Sereno, Mauro; Izzo, L.; Covone, G.

doi:10.1093/mnras/stu2064

Cited by 50 publications

(59 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The deep HST data have resulted in an unprecedented set of strong-lensed arcs and multiple images for constraining the cluster potentials (e.g., Jauzac et al 2014Jauzac et al , 2015Lam et al 2014;Diego et al 2015Diego et al , 2016Wang et al 2015;Kawamata et al 2016), doubling or tripling the number of multiple images (Table 5, Figure 8). Subsequent observations with the GLASS HST WFC3/IR grism GO program (Schmidt et al 2014;Treu et al 2015; see 10.17909/ T9KG60) and new ground-based spectroscopic campaigns have greatly increased the number and accuracy of the redshifts for the background lensed FF galaxies (Ebeling et al 2014;Johnson et al 2014;Richard et al 2014;Balestra et al 2015;Grillo et al 2015;Hoag et al 2016).…”

Section: Lensing Models and Predictionsmentioning

confidence: 99%

“…The newly discovered arcs and new spectroscopic redshifts have been incorporated into updated HFF+ versions of the Abell 2744 and MACSJ0416.1-2403 lensing models ( Table 5); many of these have > z 3 phot (see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models; Cypriano et al 2004;Okabe & Umetsu 2008;Okabe et al 2010aOkabe et al , 2010bMerten et al 2011;Christensen et al 2012;Mann & Ebeling 2012;Jauzac et al 2014;Lam et al 2014;Richard et al 2014;Balestra et al 2015;Diego et al 2015;Grillo et al 2015;Jauzac et al 2015;Rodney et al 2015;Wang et al 2015;Kawamata et al 2016). The incorporation of these new multiple image systems often results in a reduction in the statistical uncertainty in the galaxy magnifications for a given model.…”

Section: Lensing Models and Predictionsmentioning

confidence: 99%

See 1 more Smart Citation

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

Self Cite

590

574

View full text Add to dashboard Cite

What are the faintest distant galaxies we can see with the Hubble Space Telescope (HST) now, before the launch of the James Webb Space Telescope? This is the challenge taken up by the Frontier Fields, a Director's discretionary time campaign with HST and the Spitzer Space Telescope to see deeper into the universe than ever before. The Frontier Fields combines the power of HST and Spitzer with the natural gravitational telescopes of massive highmagnification clusters of galaxies to produce the deepest observations of clusters and their lensed galaxies ever obtained. Six clusters-Abell 2744, MACSJ0416.1-2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063, and Abell 370-have been targeted by the HST ACS/WFC and WFC3/IR cameras with coordinated parallel fields for over 840 HST orbits. The parallel fields are the second-deepest observations thus far by HST with 5σ point-source depths of ∼29th ABmag. Galaxies behind the clusters experience typical magnification factors of a few, with small regions magnified by factors of 10-100. Therefore, the Frontier Field cluster HST images achieve intrinsic depths of ∼30-33 mag over very small volumes. Spitzer has obtained over 1000 hr of Director's discretionary imaging of the Frontier Field cluster and parallels in IRAC 3.6 and 4.5 μm bands to 5σ point-source depths of ∼26.5, 26.0 ABmag. We demonstrate the exceptional sensitivity of the HST Frontier Field images to faint high-redshift galaxies, and review the initial results related to the primary science goals.

show abstract

Section: Lensing Models and Predictionsmentioning

confidence: 99%

Section: Lensing Models and Predictionsmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

Self Cite

590

574

View full text Add to dashboard Cite

show abstract

“…It would be interesting to investigate systematics on clusters with more spherical mass distributions. A prime example would be Abell 1689, which has a large number of identified image systems with spectroscopic redshifts and for which existing lens models suggest it has a more circular critical curve (Broadhurst et al 2005;Limousin et al 2007;Coe et al 2010;Diego et al 2015).…”

Section: 4mentioning

confidence: 99%

The Systematics of Strong Lens Modeling Quantified: The Effects of Constraint Selection and Redshift Information on Magnification, Mass, and Multiple Image Predictability

Johnson

Sharon

2016

ApJ

View full text Add to dashboard Cite

Until now, systematic errors in strong gravitational lens modeling have been acknowledged but have never been fully quantified. Here, we launch an investigation into the systematics induced by constraint selection. We model the simulated cluster Ares 362 times using random selections of image systems with and without spectroscopic redshifts and quantify the systematics using several diagnostics: image predictability, accuracy of model-predicted redshifts, enclosed mass, and magnification. We find that for models with > 15 image systems, the image plane rms does not decrease significantly when more systems are added; however, the rms values quoted in the literature may be misleading as to the ability of a model to predict new multiple images. The mass is well constrained near the Einstein radius in all cases, and systematic error drops to < 2% for models using > 10 image systems. Magnification errors are smallest along the straight portions of the critical curve, and the value of the magnification is systematically lower near curved portions. For > 15 systems, the systematic error on magnification is ∼ 2%. We report no trend in magnification error with fraction of spectroscopic image systems when selecting constraints at random; however, when using the same selection of constraints, increasing this fraction up to ∼ 0.5 will increase model accuracy. The results suggest that the selection of constraints, rather than quantity alone, determines the accuracy of the magnification. We note that spectroscopic follow-up of at least a few image systems is crucial because as models without any spectroscopic redshifts are inaccurate across all of our diagnostics.

show abstract

“…Based on photometric studies on HST/ACS images, there are more than 100 multiple images of 40 strongly lensed background galaxy sources with redshifts ranging from z = 1 to z = 4.9 behind A 1689 (Broadhurst et al 2005;Limousin et al 2007;Diego et al 2015). Our survey was sensitive to SNe that could have exploded in these galaxies.…”

Section: Supernovae In the Resolved Strongly Lensed Multiply-imaged Gmentioning

confidence: 99%

High-redshift supernova rates measured with the gravitational telescope A 1689

Petrushevska

Amanullah

Goobar

et al. 2016

A&A

View full text Add to dashboard Cite

Aims. We present a ground-based, near-infrared search for lensed supernovae behind the massive cluster Abell 1689 at z = 0.18, which is one of the most powerful gravitational telescopes that nature provides. Methods. Our survey was based on multi-epoch J-band observations with the HAWK-I instrument on VLT, with supporting optical data from the Nordic Optical Telescope. Results. Our search resulted in the discovery of five photometrically classified, core-collapse supernovae with high redshifts of 0.671 < z < 1.703 and magnifications in the range ∆m = −0.31 to −1.58 mag, as calculated from lensing models in the literature. Owing to the power of the lensing cluster, the survey had the sensitivity to detect supernovae up to very high redshifts, z ∼ 3, albeit for a limited region of space. We present a study of the core-collapse supernova rates for 0.4 ≤ z < 2.9, and find good agreement with previous estimates and predictions from star formation history. During our survey, we also discovered two Type Ia supernovae in A 1689 cluster members, which allowed us to determine the cluster Ia rate to be 0.14,B yr −1 ), where the error bars indicate 1σ confidence intervals, statistical and systematic, respectively. The cluster rate normalized by the stellar mass is 0.10. Furthermore, we explore the optimal future survey for improving the core-collapse supernova rate measurements at z 2 using gravitational telescopes, and for detections with multiply lensed images, and we find that the planned WFIRST space mission has excellent prospects. Conclusions. Massive clusters can be used as gravitational telescopes to significantly expand the survey range of supernova searches, with important implications for the study of the high-z transient Universe.Key words. supernovae: general -gravitational lensing: strong -galaxies: star formation -galaxies: clusters

show abstract

A free-form lensing grid solution for A1689 with new multiple images

Cited by 50 publications

References 48 publications

The Frontier Fields: Survey Design and Initial Results

The Frontier Fields: Survey Design and Initial Results

The Systematics of Strong Lens Modeling Quantified: The Effects of Constraint Selection and Redshift Information on Magnification, Mass, and Multiple Image Predictability

High-redshift supernova rates measured with the gravitational telescope A 1689

Contact Info

Product

Resources

About