Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗
Using the combined resolving power of the Hubble Space Telescope and gravitational lensing, we resolve star-forming structures in a z ~ 2.5 galaxy on scales much smaller than the usual kiloparsec diffraction limit of HST. SGAS J111020.0+645950.8 is a clumpy, star-forming galaxy lensed by the galaxy...
| Main Authors: | , , , , , , , , |
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| Format: | Article |
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IOP Publishing
2017
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| Online Access: | http://hdl.handle.net/1721.1/112253 |
| _version_ | 1826200430441398272 |
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| author | Johnson, Traci L. Sharon, Keren Gladders, Michael D. Rigby, Jane R. Wuyts, Eva Whitaker, Katherine E. Florian, Michael Murray, Katherine T. Bayliss, Matthew B |
| author2 | MIT Kavli Institute for Astrophysics and Space Research |
| author_facet | MIT Kavli Institute for Astrophysics and Space Research Johnson, Traci L. Sharon, Keren Gladders, Michael D. Rigby, Jane R. Wuyts, Eva Whitaker, Katherine E. Florian, Michael Murray, Katherine T. Bayliss, Matthew B |
| author_sort | Johnson, Traci L. |
| collection | MIT |
| description | Using the combined resolving power of the Hubble Space Telescope and gravitational lensing, we resolve star-forming structures in a z ~ 2.5 galaxy on scales much smaller than the usual kiloparsec diffraction limit of HST. SGAS J111020.0+645950.8 is a clumpy, star-forming galaxy lensed by the galaxy cluster SDSS J1110+6459 at z = 0.659, with a total magnification across the entire arc. We use a hybrid parametric/non-parametric strong lensing mass model to compute the deflection and magnification of this giant arc, reconstruct the light distribution of the lensed galaxy in the source plane, and resolve the star formation into two dozen clumps. We develop a forward-modeling technique to model each clump in the source plane. We ray-trace the model to the image plane, convolve with the instrumental point-spread function (PSF), and compare with the GALFIT model of the clumps in the image plane, which decomposes clump structure from more extended emission. This technique has the advantage, over ray-tracing, of accounting for the asymmetric lensing shear of the galaxy in the image plane and the instrument PSF. At this resolution, we can begin to study star formation on a clump-by-clump basis, toward the goal of understanding feedback mechanisms and the buildup of exponential disks at high redshift. Key words: galaxies: clusters: individual (SDSS J1110+6459) – gravitational lensing: strong |
| first_indexed | 2024-09-23T11:36:21Z |
| format | Article |
| id | mit-1721.1/112253 |
| institution | Massachusetts Institute of Technology |
| last_indexed | 2024-09-23T11:36:21Z |
| publishDate | 2017 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1122532024-06-27T14:33:47Z Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ Johnson, Traci L. Sharon, Keren Gladders, Michael D. Rigby, Jane R. Wuyts, Eva Whitaker, Katherine E. Florian, Michael Murray, Katherine T. Bayliss, Matthew B MIT Kavli Institute for Astrophysics and Space Research Bayliss, Matthew B Using the combined resolving power of the Hubble Space Telescope and gravitational lensing, we resolve star-forming structures in a z ~ 2.5 galaxy on scales much smaller than the usual kiloparsec diffraction limit of HST. SGAS J111020.0+645950.8 is a clumpy, star-forming galaxy lensed by the galaxy cluster SDSS J1110+6459 at z = 0.659, with a total magnification across the entire arc. We use a hybrid parametric/non-parametric strong lensing mass model to compute the deflection and magnification of this giant arc, reconstruct the light distribution of the lensed galaxy in the source plane, and resolve the star formation into two dozen clumps. We develop a forward-modeling technique to model each clump in the source plane. We ray-trace the model to the image plane, convolve with the instrumental point-spread function (PSF), and compare with the GALFIT model of the clumps in the image plane, which decomposes clump structure from more extended emission. This technique has the advantage, over ray-tracing, of accounting for the asymmetric lensing shear of the galaxy in the image plane and the instrument PSF. At this resolution, we can begin to study star formation on a clump-by-clump basis, toward the goal of understanding feedback mechanisms and the buildup of exponential disks at high redshift. Key words: galaxies: clusters: individual (SDSS J1110+6459) – gravitational lensing: strong 2017-11-20T19:55:33Z 2017-11-20T19:55:33Z 2017-07 2017-05 2017-11-08T14:26:25Z Article http://purl.org/eprint/type/JournalArticle 1538-4357 0004-637X http://hdl.handle.net/1721.1/112253 Johnson, Traci L., et al. “Star Formation at Z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction.” The Astrophysical Journal, vol. 843, no. 2, July 2017, p. 78. © 2017 The American Astronomical Society http://dx.doi.org/10.3847/1538-4357/aa7756 The Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing IOP Publishing |
| spellingShingle | Johnson, Traci L. Sharon, Keren Gladders, Michael D. Rigby, Jane R. Wuyts, Eva Whitaker, Katherine E. Florian, Michael Murray, Katherine T. Bayliss, Matthew B Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title | Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title_full | Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title_fullStr | Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title_full_unstemmed | Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title_short | Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110 = 6459. I. Lens Modeling and Source Reconstruction∗ |
| title_sort | star formation at z 2 481 in the lensed galaxy sdss j1110 6459 i lens modeling and source reconstruction∗ |
| url | http://hdl.handle.net/1721.1/112253 |
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