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Title: Magnification, dust and time-delay constraints from the first resolved strongly lensed Type Ia supernova iPTF16geu

Journal Article · · Monthly Notices of the Royal Astronomical Society
 [1];  [2]; ORCiD logo [1];  [1];  [1];  [3];  [4]; ORCiD logo [5];  [6];  [1]; ORCiD logo [1];  [6];  [7];  [4];  [8];  [9];  [10]
  1. Stockholm Univ. (Sweden). Oskar Klein Centre, and Albanova Univ. Center
  2. Uppsala Univ. (Sweden)
  3. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States); Univ. of Maryland, College Park, MD (United States)
  4. Univ. of California, Irvine, CA (United States). Dept. of Physics and Astronomy
  5. Space Telescope Science Inst., Baltimore, MD (United States)
  6. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  7. National Autonomous Univ. of Mexico (Mexico)
  8. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  9. Weizmann Inst. of Science, Rehovot (Israel). Benoziyo Center for Astrophysics
  10. San Diego State Univ., San Diego, CA (United States); Univ. of Tokyo, Kashiwa, Chiba (Japan)
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We report lensing magnifications, extinction, and time-delay estimates for the first resolved, multiply-imaged Type Ia supernova iPTF16geu, at z = 0.409, using Hubble Space Telescope (HST) observations in combination with supporting ground-based data. Multi-band photometry of the resolved images provides unique information about the differential dimming due to dust in the lensing galaxy. Using HST and Keck AO reference images taken after the SN faded, we obtain a total lensing magnification for iPTF16geu of $$\mu = 67.8^{+2.6}_{-2.9}$$, accounting for extinction in the host and lensing galaxy. As expected from the symmetry of the system, we measure very short time-delays for the three fainter images with respect to the brightest one: -0.23 ± 0.99, -1.43 ± 0.74 and 1.36 ± 1.07 days. Interestingly, we find large differences between the magnifications of the four supernova images, even after accounting for uncertainties in the extinction corrections: $$\Delta m_1 = -3.88^{+0.07}_{-0.06}$$, $$\Delta m_2 = -2.99^{+0.09}_{-0.08}$$, $$\Delta m_3 = -2.19^{+0.14}_{-0.15}$$ and $$\Delta m_4 = -2.40^{+0.14}_{-0.12}$$ mag, discrepant with model predictions suggesting similar image brightnesses. A possible explanation for the large differences is gravitational lensing by substructures, micro- or millilensing, in addition to the large scale lens causing the image separations. We find that the inferred magnification is insensitive to the assumptions about the dust properties in the host and lens galaxy.

Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC); Swedish Research Council (SRC); Swedish National Space Agency
Grant/Contract Number:
AC02-05CH11231
OSTI ID:
1580979
Journal Information:
Monthly Notices of the Royal Astronomical Society, Vol. 491, Issue 2; ISSN 0035-8711
Publisher:
Royal Astronomical SocietyCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 14 works
Citation information provided by
Web of Science

Figures / Tables (17)

Table 1(p. 4)table Table 1
Table 2(p. 4)table Table 2
Figure 1(p. 5)figure Figure 1
Figure 2(p. 7)figure Figure 2
Table 3(p. 7)table Table 3
Figure 3(p. 8)figure Figure 3
Figure 4(p. 9)figure Figure 4
Figure 5(p. 10)figure Figure 5
Figure 6(p. 11)figure Figure 6
Table A1(p. 13)table Table A1
Table A-3(p. 14)table Table A-3
Table A2(p. 14)table Table A2
Figure B1(p. 15)figure Figure B1
Table B1(p. 15)table Table B1
Table C1(p. 16)table Table C1
Table C2(p. 17)table Table C2
Figure D1(p. 19)figure Figure D1

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