The Story of Supernova “Refsdal” Told by Muse*

Grillo, C.; Karman, W.; Suyu, S. H.; Rosati, P.; Balestra, I.; Mercurio, A.; Lombardi, Marco; Treu, Tommaso; Caminha, G. B.; Halkola, A.; Rodney, Steven A.; Gavazzi, R.; Caputi, K.

doi:10.3847/0004-637x/822/2/78

Cited by 110 publications

(168 citation statements)

References 68 publications

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“…Grillo, e.g., Karman et al 2015, Grillo et al 2016, as well as the release of previously unpublished data on these fields (e.g., Ebeling et al 2014, Gruen et al 2014. Additional HST WFC3 ultraviolet imaging (Alavi et al 2016) and grism spectroscopy (Schmidt et al 2014) are also being obtained for all the Frontier Field clusters.…”

Section: Uvmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

587

574

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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.

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Section: Uvmentioning

confidence: 99%

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

587

574

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“…To complete the total mass distribution of the galaxy cluster, three additional mass components are added to describe the cluster dark matter halo on physical scales larger than those typical of the individual cluster members. These cluster halo components are parametrized as two-dimensional pseudo-isothermal elliptical mass profiles (PIEMD as defined by Kassiola & Kovner 1993; see also Grillo et al 2015a).…”

Section: Definition Of the Mass Modelmentioning

confidence: 99%

“…The SN exploded in one arm of an almost face-on spiral galaxy that is multiply imaged and highly magnified by the cluster gravitational potential (z s =1489 and z 0542; d = redshifts from Grillo et al 2015a). Furthermore, the spiral arm hosting SN Refsdal happens to be sufficiently close to a cluster member galaxy that four additional multiple images are formed with average separation of the order of arcseconds, typical of galaxy-scale strong lensing.…”

Section: Introductionmentioning

confidence: 99%

“Refsdal” Meets Popper: Comparing Predictions of the Re-Appearance of the Multiply Imaged Supernova Behind MACSJ1149.5+2223

Treu

Brammer

Diego

et al. 2016

ApJ

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113

161

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Supernova "Refsdal," multiply imaged by cluster MACS1149.5+2223, represents a rare opportunity to make a true blind test of model predictions in extragalactic astronomy, on a timescale that is short compared to a human lifetime. In order to take advantage of this event, we produced seven gravitational lens models with five independent methods, based on Hubble Space Telescope (HST) Hubble Frontier Field images, along with extensive spectroscopic follow-up observations by HST, the Very Large and the Keck Telescopes. We compare the model predictions and show that they agree reasonably well with the measured time delays and magnification ratios between the known images, even though these quantities were not used as input. This agreement is encouraging, considering that the models only provide statistical uncertainties, and do not include additional sources of uncertainties such as structure along the line of sight, cosmology, and the mass sheet degeneracy. We then present the model predictions for the other appearances of supernova "Refsdal." A future image will reach its peak in the first half of 2016, while another image appeared between 1994 and 2004. The past image would have been too faint to be detected in existing archival images. The future image should be approximately one-third as bright as the brightest known image (i.e., H 25.7 AB » mag at peak and H 26.7 AB » mag six months before peak), and thus detectable in single-orbit HST images. We will find out soon whether our predictions are correct.

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“…Those exposures, collected as part of the Grism Lens-Amplified Survey from Space (GLASS; PI Treu; GO-13459; Schmidt et al 2014;Treu et al 2015), revealed four resolved images of the background SNe arranged in an Einstein cross configuration around an elliptical cluster member. Models of the complex potential of the galaxy cluster and early-type galaxy lens suggest that three of the four images are magnified by up to a factor of ∼10-20 (Grillo et al 2015;Jauzac et al 2016;Kawamata et al 2015;Kelly et al 2015b;Oguri 2015;Sharon & Johnson 2015;Diego et al 2016;Treu et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Deja Vu All Over Again: The Reappearance of Supernova Refsdal

Kelly

Rodney

Treu

et al. 2016

ApJL

Self Cite

102

101

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In Hubble Space Telescope (HST) imaging taken on 2014 November 10, four images of supernova (SN) "Refsdal" (redshift z=1.49) appeared in an Einstein-cross-like configuration (images S1-S4) around an early-type galaxy in the cluster MACS J1149.5+2223 (z=0.54). Almost all lens models of the cluster have predicted that the SN should reappear within a year in a second host-galaxy image created by the cluster's potential. In HST observations taken on 2015 December 11, we find a new source at the predicted position of the new image of SN Refsdal approximately 8 from the previous images S1-S4. This marks the first time the appearance of a SN at a particular time and location in the sky was successfully predicted in advance! We use these data and the light curve from the first four observed images of SN Refsdal to place constraints on the relative time delay and magnification of the new image (SX) compared to images S1-S4. This enables us, for the first time, to test "blind" lens model predictions of both magnifications and time delays for a lensed SN. We find that the timing and brightness of the new image are consistent with the blind predictions of a fraction of the models. The reappearance illustrates the discriminatory power of this blind test and its utility to uncover sources of systematic uncertainty. From planned HST photometry, we expect to reach a precision of 1%-2% on the time delay between S1-S4 and SX.

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The Story of Supernova “Refsdal” Told by Muse*

Cited by 110 publications

References 68 publications

The Frontier Fields: Survey Design and Initial Results

The Frontier Fields: Survey Design and Initial Results

“Refsdal” Meets Popper: Comparing Predictions of the Re-Appearance of the Multiply Imaged Supernova Behind MACSJ1149.5+2223

Deja Vu All Over Again: The Reappearance of Supernova Refsdal

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