ILLUMINATING A DARK LENS: A TYPE Ia SUPERNOVA MAGNIFIED BY THE FRONTIER FIELDS GALAXY CLUSTER ABELL 2744

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Rodney, Steven A. ^{[1, 2]} ; Patel, Brandon ^[3] ; Scolnic, Daniel ^[4] ; Foley, Ryan J. ^{[5, 6]} ; Molino, Alberto ^{[7, 8]} ; Brammer, Gabriel ^[9] ; Jauzac, Mathilde ^{[10, 11]} ; Bradac, Marusa ^[12] ; Broadhurst, Tom ^{[13, 14]} ; Coe, Dan ^[9] ; Diego, Jose M. ^[15] ; Graur, Or ^{[16, 17]} ; Hjorth, Jens ^[18] ; Hoag, Austin ^[12] ; Jha, Saurabh W. ; Johnson, Traci L. ^[19] ; Kelly, Patrick ^[20] ; Lam, Daniel ^[21] ; McCully, Curtis ^{[22, 23]} ; Medezinski, Elinor ^{[2, 24]} ; Meneghetti, Massimo ^{[25, 26]} ; Merten, Julian ^[27] ; Richard, Johan ^[28] ; Riess, Adam ^{[9, 2]} ; Sharon, Keren ^[19] ; Strolger, Louis-Gregory ^{[9, 29]} ; Treu, Tommaso ^[30] ; Wang, Xin ^[22] ; Williams, Liliya L. R. ^[31] ; Zitrin, Adi ^[32]

Afiliação do(s) autor(es):Mostrar menos -

^[1] Univ S Carolina, Dept Phys & Astron, Columbia, SC 29208 - USA

^[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 - USA

^[3] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 - USA

^[4] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 - USA

^[5] Univ Illinois, Dept Phys, Urbana, IL 61801 - USA

^[6] Univ Illinois, Dept Astron, Urbana, IL 61801 - USA

^[7] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo - Brazil

^[8] CSIC, Inst Astrofis Andalucia, E-18080 Granada - Spain

^[9] Space Telescope Sci Inst, Baltimore, MD 21218 - USA

^[10] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE - England

^[11] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban - South Africa

^[12] Univ Calif Davis, Davis, CA 95616 - USA

^[13] Euskal Herriko Unibertsitatea UPV EHU, Fis Teorikoa Zientzia & Teknol Fak, Leioa, Bizkaia - Spain

^[14] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao - Spain

^[15] CSIC, IFCA, Inst Fis Cantabria, UC, E-39005 Santander - Spain

^[16] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 - USA

^[17] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 - USA

^[18] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen - Denmark

^[19] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 - USA

^[20] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 - USA

^[21] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong - Peoples R China

^[22] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 - USA

^[23] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 - USA

^[24] Hebrew Univ Jerusalem, IL-9190401 Jerusalem - Israel

^[25] Osservatorio Astron Bologna, INAF, I-40127 Bologna - Italy

^[26] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna - Italy

^[27] Univ Oxford, Dept Phys, Oxford OX1 3RH - England

^[28] Univ Lyon 1, CRAL, Observ Lyon, F-69561 St Genis Laval - France

^[29] Western Kentucky Univ, Dept Phys, Bowling Green, KY 42101 - USA

^[30] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 - USA

^[31] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 - USA

^[32] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 - USA

• Tipo de documento: Artigo Científico
• Fonte: ASTROPHYSICAL JOURNAL; v. 811, n. 1 SEP 20 2015.
• Citações Web of Science: 33

Resumo

SN HFF14Tom is a Type Ia SN discovered at z = 1.3457 +/- 0.0001 behind the galaxy cluster Abell 2744 (z = 0.308). In a cosmology-independent analysis, we find that HFF14Tom is 0.77 +/- 0.15 mag brighter than unlensed Type Ia SNe at similar redshift, implying a lensing magnification of mu(obs) = 2.03 +/- 0.29. This observed magnification provides a rare opportunity for a direct empirical test of galaxy cluster lens models. Here we test 17 lens models, 13 of which were generated before the SN magnification was known, qualifying as pure ``blind tests.{''} The models are collectively fairly accurate: 8 of the models deliver median magnifications that are consistent with the measured mu to within 1 sigma. However, there is a subtle systematic bias: the significant disagreements all involve models overpredicting the magnification. We evaluate possible causes for this mild bias, and find no single physical or methodological explanation to account for it. We do find that model accuracy can be improved to some extent with stringent quality cuts on multiply imaged systems, such as requiring that a large fraction have spectroscopic redshifts. In addition to testing model accuracies as we have done here, Type Ia SN magnifications could also be used as inputs for future lens models of Abell 2744 and other clusters, providing valuable constraints in regions where traditional strong-and weak-lensing information is unavailable. (AU)

• Processo FAPESP: 14/11806-9 - Desafios para a nova geração de mapeamentos fotométricos de grande campo como o J-PAS
• Beneficiário: Alberto Molino Benito
• Linha de fomento: Bolsas no Brasil - Pós-Doutorado