Models of the strongly lensed quasar DES J0408-5354

A. Agnello; H. Lin; L. Buckley-Geer; T. Treu; V. Bonvin; F. Courbin; C. Lemon; T. Morishita; A. Amara; M. W. Auger; S. Birrer; J. Chan; T. Collett; A. More; C. D. Fassnacht; J. Frieman; P. J. Marshall; R. G. McMahon; G. Meylan; S. H. Suyu; F. Castander; D. Finley; A. Howell; C. Kochanek; M. Makler; P. Martini; N. Morgan; B. Nord; F. Ostrovski; P. Schechter; D. Tucker; R. Wechsler; T. M.C. Abbott; F. B. Abdalla; S. Allam; A. Benoit-Lévy; E. Bertin; D. Brooks; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; M. Crocce; C. E. Cunha; C. B. D'Andrea; L. N. da Costa; S. Desai; J. P. Dietrich; T. F. Eifler; B. Flaugher; P. Fosalba; J. García-Bellido; E. Gaztanaga; M. S. Gill; D. A. Goldstein; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; K. Honscheid; D. J. James; K. Kuehn; N. Kuropatkin; T. S. Li; M. Lima; M. A.G. Maia; M. March; J. L. Marshall; P. Melchior; F. Menanteau; R. Miquel; R. L.C. Ogando; A. A. Plazas; A. K. Romer; E. Sanchez; R. Schindler; M. Schubnell; I. Sevilla-Noarbe; M. Smith; R. C. Smith; F. Sobreira; E. Suchyta; M. E.C. Swanson; G. Tarle; D. Thomas; A. R. Walker

doi:10.1093/mnras/stx2242

Models of the strongly lensed quasar DES J0408-5354

A. Agnello, H. Lin, L. Buckley-Geer, T. Treu, V. Bonvin, F. Courbin, C. Lemon, T. Morishita, A. Amara, M. W. Auger, S. Birrer, J. Chan, T. Collett, A. More, C. D. Fassnacht, J. Frieman, P. J. Marshall, R. G. McMahon, G. Meylan, S. H. SuyuF. Castander, D. Finley, A. Howell, C. Kochanek, M. Makler, P. Martini, N. Morgan, B. Nord, F. Ostrovski, P. Schechter, D. Tucker, R. Wechsler, T. M.C. Abbott, F. B. Abdalla, S. Allam, A. Benoit-Lévy, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Crocce, C. E. Cunha, C. B. D'Andrea, L. N. da Costa, S. Desai, J. P. Dietrich, T. F. Eifler, B. Flaugher, P. Fosalba, J. García-Bellido, E. Gaztanaga, M. S. Gill, D. A. Goldstein, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, T. S. Li, M. Lima, M. A.G. Maia, M. March, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. L.C. Ogando, A. A. Plazas, A. K. Romer, E. Sanchez, R. Schindler, M. Schubnell, I. Sevilla-Noarbe, M. Smith, R. C. Smith, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, D. Thomas, A. R. Walker

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Abstract

We present detailed modelling of the recently discovered, quadruply lensed quasar J0408-5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ R_{E, G2} ≲ 0.2 arcsec and enclosed mass M_p(R_{E, G2}) ≲ 1.0 × 10¹⁰ M_O˙. The main deflector has stellar mass log₁₀(M_*/MO˙) = 11.49_-0.32^+0.46, a projected mass M_p(R_{E, G1}) ≈ 6 × 10¹¹ M_O˙ within its Einstein radius R_{E, G1} = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267-280 km s^-1. Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (Δt_AB = (135.0 ± 12.6) d, Δt_BD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408-5354 on lensed quasar finding strategies, due to its chromaticity and morphology.

Original language	English
Article number	stx2242
Pages (from-to)	4038-4050
Number of pages	13
Journal	Monthly Notices of the Royal Astronomical Society
Volume	472
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stx2242
State	Published - Dec 1 2017

Funding

AA and TT acknowledge support by the Packard Foundations through a Packard Research Fellowship and by the National Science Foundation through grant AST-1450141. This paper was written as part of the STRong lensing Insights into the Dark Energy Survey (STRIDES) collaboration, a broad external collaboration of the Dark Energy Survey, http://strides.astro.ucla.edu We are grateful to the anonymous referee for a 'fresh' and thorough reading of the paper, which helped clarify several points. Funding for the DES Projects has been provided by the DOE and NSF(USA), MISE(Spain), STFC(UK), HEFCE(UK). NCSA(UIUC), KICP(U. Chicago), CCAPP(Ohio State), MIFPA(Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), MINECO(Spain), DFG(Germany) and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, and Texas A&M University. The DES Data Management System is supported by the NSF under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986 and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC under the EU's 7th Framework Programme including grants ERC 240672, 291329 and 306478.

Funders	Funder number
Centro de Excelencia Severo Ochoa	SEV-2012-0234
Collaborating Institutions are Argonne Lab
Collaborating Institutions in the Dark Energy Survey
Dark Energy Survey
IFAE Barcelona
MIFPA
NOAO
STRIDES
National Science Foundation	AST-1450141
David and Lucile Packard Foundation
U.S. Department of Energy
Merck Institute for Science Education
University of Illinois at Urbana-Champaign
Stanford University
Lawrence Berkeley National Laboratory
University of Pennsylvania
Ohio State University
University of Chicago
University of Michigan
Texas A and M University	FPA2013-47986, AYA2012-39559, AST-1138766, ESP2013-48274
University of Portsmouth
Seventh Framework Programme	1138766, 240672, 306478, 291329, 1450141
SLAC National Accelerator Laboratory
Center for Cosmology and Astroparticle Physics, Ohio State University
Kavli Institute for Cosmological Physics, University of Chicago
Science and Technology Facilities Council
University College London
European Research Council
University of Nottingham
University of Sussex
Deutsche Forschungsgemeinschaft
Ministerio de Economía y Competitividad
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos

Keywords

Catalogues
Gravitational lensing: strong
Methods: statistical
Techniques: image processing

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10.1093/mnras/stx2242

Cite this

Agnello, A., Lin, H., Buckley-Geer, L., Treu, T., Bonvin, V., Courbin, F., Lemon, C., Morishita, T., Amara, A., Auger, M. W., Birrer, S., Chan, J., Collett, T., More, A., Fassnacht, C. D., Frieman, J., Marshall, P. J., McMahon, R. G., Meylan, G., ... Walker, A. R. (2017). Models of the strongly lensed quasar DES J0408-5354. Monthly Notices of the Royal Astronomical Society, 472(4), 4038-4050. Article stx2242. https://doi.org/10.1093/mnras/stx2242

@article{71e8009313c247b79111e9bce82377f6,

title = "Models of the strongly lensed quasar DES J0408-5354",

abstract = "We present detailed modelling of the recently discovered, quadruply lensed quasar J0408-5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ RE, G2 ≲ 0.2 arcsec and enclosed mass Mp(RE, G2) ≲ 1.0 × 1010 MO˙. The main deflector has stellar mass log10(M*/MO˙) = 11.49-0.32+0.46, a projected mass Mp(RE, G1) ≈ 6 × 1011 MO˙ within its Einstein radius RE, G1 = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267-280 km s-1. Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (ΔtAB = (135.0 ± 12.6) d, ΔtBD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408-5354 on lensed quasar finding strategies, due to its chromaticity and morphology.",

keywords = "Catalogues, Gravitational lensing: strong, Methods: statistical, Techniques: image processing",

author = "A. Agnello and H. Lin and L. Buckley-Geer and T. Treu and V. Bonvin and F. Courbin and C. Lemon and T. Morishita and A. Amara and Auger, {M. W.} and S. Birrer and J. Chan and T. Collett and A. More and Fassnacht, {C. D.} and J. Frieman and Marshall, {P. J.} and McMahon, {R. G.} and G. Meylan and Suyu, {S. H.} and F. Castander and D. Finley and A. Howell and C. Kochanek and M. Makler and P. Martini and N. Morgan and B. Nord and F. Ostrovski and P. Schechter and D. Tucker and R. Wechsler and Abbott, {T. M.C.} and Abdalla, {F. B.} and S. Allam and A. Benoit-L{\'e}vy and E. Bertin and D. Brooks and Burke, {D. L.} and Rosell, {A. Carnero} and Kind, {M. Carrasco} and J. Carretero and M. Crocce and Cunha, {C. E.} and D'Andrea, {C. B.} and {da Costa}, {L. N.} and S. Desai and Dietrich, {J. P.} and Eifler, {T. F.} and B. Flaugher and P. Fosalba and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gill, {M. S.} and Goldstein, {D. A.} and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and K. Honscheid and James, {D. J.} and K. Kuehn and N. Kuropatkin and Li, {T. S.} and M. Lima and Maia, {M. A.G.} and M. March and Marshall, {J. L.} and P. Melchior and F. Menanteau and R. Miquel and Ogando, {R. L.C.} and Plazas, {A. A.} and Romer, {A. K.} and E. Sanchez and R. Schindler and M. Schubnell and I. Sevilla-Noarbe and M. Smith and Smith, {R. C.} and F. Sobreira and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and D. Thomas and Walker, {A. R.}",

note = "Publisher Copyright: {\textcopyright} 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.",

year = "2017",

month = dec,

day = "1",

doi = "10.1093/mnras/stx2242",

language = "English",

volume = "472",

pages = "4038--4050",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Agnello, A, Lin, H, Buckley-Geer, L, Treu, T, Bonvin, V, Courbin, F, Lemon, C, Morishita, T, Amara, A, Auger, MW, Birrer, S, Chan, J, Collett, T, More, A, Fassnacht, CD, Frieman, J, Marshall, PJ, McMahon, RG, Meylan, G, Suyu, SH, Castander, F, Finley, D, Howell, A, Kochanek, C, Makler, M, Martini, P, Morgan, N, Nord, B, Ostrovski, F, Schechter, P, Tucker, D, Wechsler, R, Abbott, TMC, Abdalla, FB, Allam, S, Benoit-Lévy, A, Bertin, E, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Eifler, TF, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Gill, MS, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, Maia, MAG, March, M, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Romer, AK, Sanchez, E, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Smith, RC, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D & Walker, AR 2017, 'Models of the strongly lensed quasar DES J0408-5354', Monthly Notices of the Royal Astronomical Society, vol. 472, no. 4, stx2242, pp. 4038-4050. https://doi.org/10.1093/mnras/stx2242

TY - JOUR

T1 - Models of the strongly lensed quasar DES J0408-5354

AU - Agnello, A.

AU - Lin, H.

AU - Buckley-Geer, L.

AU - Treu, T.

AU - Bonvin, V.

AU - Courbin, F.

AU - Lemon, C.

AU - Morishita, T.

AU - Amara, A.

AU - Auger, M. W.

AU - Birrer, S.

AU - Chan, J.

AU - Collett, T.

AU - More, A.

AU - Fassnacht, C. D.

AU - Frieman, J.

AU - Marshall, P. J.

AU - McMahon, R. G.

AU - Meylan, G.

AU - Suyu, S. H.

AU - Castander, F.

AU - Finley, D.

AU - Howell, A.

AU - Kochanek, C.

AU - Makler, M.

AU - Martini, P.

AU - Morgan, N.

AU - Nord, B.

AU - Ostrovski, F.

AU - Schechter, P.

AU - Tucker, D.

AU - Wechsler, R.

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Benoit-Lévy, A.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Carretero, J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - da Costa, L. N.

AU - Desai, S.

AU - Dietrich, J. P.

AU - Eifler, T. F.

AU - Flaugher, B.

AU - Fosalba, P.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gill, M. S.

AU - Goldstein, D. A.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Honscheid, K.

AU - James, D. J.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Li, T. S.

AU - Lima, M.

AU - Maia, M. A.G.

AU - March, M.

AU - Marshall, J. L.

AU - Melchior, P.

AU - Menanteau, F.

AU - Miquel, R.

AU - Ogando, R. L.C.

AU - Plazas, A. A.

AU - Romer, A. K.

AU - Sanchez, E.

AU - Schindler, R.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Smith, R. C.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thomas, D.

AU - Walker, A. R.

PY - 2017/12/1

Y1 - 2017/12/1

N2 - We present detailed modelling of the recently discovered, quadruply lensed quasar J0408-5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ RE, G2 ≲ 0.2 arcsec and enclosed mass Mp(RE, G2) ≲ 1.0 × 1010 MO˙. The main deflector has stellar mass log10(M*/MO˙) = 11.49-0.32+0.46, a projected mass Mp(RE, G1) ≈ 6 × 1011 MO˙ within its Einstein radius RE, G1 = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267-280 km s-1. Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (ΔtAB = (135.0 ± 12.6) d, ΔtBD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408-5354 on lensed quasar finding strategies, due to its chromaticity and morphology.

AB - We present detailed modelling of the recently discovered, quadruply lensed quasar J0408-5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ RE, G2 ≲ 0.2 arcsec and enclosed mass Mp(RE, G2) ≲ 1.0 × 1010 MO˙. The main deflector has stellar mass log10(M*/MO˙) = 11.49-0.32+0.46, a projected mass Mp(RE, G1) ≈ 6 × 1011 MO˙ within its Einstein radius RE, G1 = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267-280 km s-1. Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (ΔtAB = (135.0 ± 12.6) d, ΔtBD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408-5354 on lensed quasar finding strategies, due to its chromaticity and morphology.

KW - Catalogues

KW - Gravitational lensing: strong

KW - Methods: statistical

KW - Techniques: image processing

UR - http://www.scopus.com/inward/record.url?scp=85030705547&partnerID=8YFLogxK

U2 - 10.1093/mnras/stx2242

DO - 10.1093/mnras/stx2242

M3 - Article

AN - SCOPUS:85030705547

SN - 0035-8711

VL - 472

SP - 4038

EP - 4050

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

M1 - stx2242

ER -

Models of the strongly lensed quasar DES J0408-5354

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