The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models
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DOI：
10.3847/2041-8213/aa8fc7
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发表时间：
2017-10
期刊：
影响因子：
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通讯作者：
P. Cowperthwaite;E. Berger;V. Villar;B. Metzger;M. Nicholl;R. Chornock;P. Blanchard;W. Fong;R. Margutti;M. Soares-Santos;K. Alexander;S. Allam;J. Annis;D. Brout;D. Brown;R. Butler;H.-Y. Chen;H. Diehl;Zoheyr Doctor;M. Drout;T. Eftekhari;B. Farr;D. Finley;R. Foley;J. Frieman;C. Fryer;J. Garc'ia-Bellido;M. Gill;J. Guillochon;K. Herner;D. Holz;D. Kasen;R. Kessler;J. Marriner;T. Matheson;E. Neilsen;Jr.;E. Quataert;A. Palmese;A. Rest;M. Sako;D. Scolnic;N. Smith;D. Tucker;P. G. Williams;E. Balbinot;J. Carlin;E. Cook;F. Durret;T. Li;P. Lopes;A. C. Lourencco;J. Marshall;G. Medina;J. Muir;R. Muñoz;M. Sauseda;D. Schlegel;L. Secco;A. K. Vivas;W. Wester;A. Zenteno;Y. Zhang;T. Abbott;M. Banerji;K. Bechtol;A. Benoit-Lévy;E. Bertin;E. Buckley-Geer;D. Burke;D. Capozzi;A. Rosell;M. Kind;F. Castander;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;C. Davis;D. Depoy;S. Desai;J. Dietrich;A. Drlica-Wagner;T. Eifler;A. Evrard;E. Fernández;B. Flaugher;P. Fosalba;E. Gaztañaga;D. Gerdes;T. Giannantonio;D. Goldstein;D. Gruen;R. Gruendl;G. Gutiérrez;K. Honscheid;B. Jain;D. James;T. Jeltema;M. Johnson;M. Johnson;S. Kent;E. Krause;R. Kron;K. Kuehn;N. Kuropatkin;O. Lahav;M. Lima;H. Lin;M. Maia;M. March;P. Martini;R. McMahon;F. Menanteau;C. Miller;R. Miquel;J. Mohr;E. Neilsen;R. Nichol;R. Ogando;A. Plazas;N. Roe;A. Romer;A. Roodman;E. Rykoff;E. Sánchez;V. Scarpine;R. Schindler;M. Schubnell;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;R. Thomas;M. Troxel;V. Vikram;A. Walker;R. Wechsler;J. Weller;B. Yanny;J. Zuntz
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文献类型：
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作者：
P. Cowperthwaite;E. Berger;V. Villar;B. Metzger;M. Nicholl;R. Chornock;P. Blanchard;W. Fong;R. Margutti;M. Soares-Santos;K. Alexander;S. Allam;J. Annis;D. Brout;D. Brown;R. Butler;H.-Y. Chen;H. Diehl;Zoheyr Doctor;M. Drout;T. Eftekhari;B. Farr;D. Finley;R. Foley;J. Frieman;C. Fryer;J. Garc'ia-Bellido;M. Gill;J. Guillochon;K. Herner;D. Holz;D. Kasen;R. Kessler;J. Marriner;T. Matheson;E. Neilsen;Jr.;E. Quataert;A. Palmese;A. Rest;M. Sako;D. Scolnic;N. Smith;D. Tucker;P. G. Williams;E. Balbinot;J. Carlin;E. Cook;F. Durret;T. Li;P. Lopes;A. C. Lourencco;J. Marshall;G. Medina;J. Muir;R. Muñoz;M. Sauseda;D. Schlegel;L. Secco;A. K. Vivas;W. Wester;A. Zenteno;Y. Zhang;T. Abbott;M. Banerji;K. Bechtol;A. Benoit-Lévy;E. Bertin;E. Buckley-Geer;D. Burke;D. Capozzi;A. Rosell;M. Kind;F. Castander;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;C. Davis;D. Depoy;S. Desai;J. Dietrich;A. Drlica-Wagner;T. Eifler;A. Evrard;E. Fernández;B. Flaugher;P. Fosalba;E. Gaztañaga;D. Gerdes;T. Giannantonio;D. Goldstein;D. Gruen;R. Gruendl;G. Gutiérrez;K. Honscheid;B. Jain;D. James;T. Jeltema;M. Johnson;M. Johnson;S. Kent;E. Krause;R. Kron;K. Kuehn;N. Kuropatkin;O. Lahav;M. Lima;H. Lin;M. Maia;M. March;P. Martini;R. McMahon;F. Menanteau;C. Miller;R. Miquel;J. Mohr;E. Neilsen;R. Nichol;R. Ogando;A. Plazas;N. Roe;A. Romer;A. Roodman;E. Rykoff;E. Sánchez;V. Scarpine;R. Schindler;M. Schubnell;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;R. Thomas;M. Troxel;V. Vikram;A. Walker;R. Wechsler;J. Weller;B. Yanny;J. Zuntz
我们提出了紫外，光学和近红外（NIR）测光的第一个电磁对应的引力波源从先进的激光干涉仪引力波天文台（LIGO）/室女座，二中子星星合并GW 170817。我们的数据集从合并后0.47-18.5天的光学对应物的发现延伸，包括暗能量相机（DECam），Gemini-South/FLAMINGOS-2（GS/F2）和哈勃太空望远镜（HST）的观测。由该测光结果推断出的0.6天的光谱能量分布（SED）可以用黑体模型很好地描述，该黑体模型的温度为8300 K，半径为R = 4.5 × 10 14 cm（对应于膨胀速度v = 0.3 c），测热光度为L bol = 5 × 10 41 erg s−1。在1.5天，我们发现了一个多组分的SED跨越光学和近红外，随后我们观察到快速褪色的紫外和蓝色光学波段和显着变红的光学/近红外颜色。通过对整个数据集进行建模，我们发现，从56 Ni的放射性衰变中加热的模型，或仅从r-过程元素中具有单一不透明度成分的模型，未能捕获快速的光学衰减和红色光学/近红外颜色。相反，具有与贫镧系元素和富镧系元素喷出物一致的两个组分的模型提供了与数据的良好拟合;所得到的“蓝色”组分具有M ej蓝色= 0.01 M和v ej蓝色= 0.3 c，而“红色”组分具有M ej红色= 0.04 M和v ej红色= 0.1 c。这些喷出物的质量是大致一致的估计r-过程的生产率所需的解释银河系r-过程的丰度，提供了第一个证据表明，二进制中子星星（BNS）合并可以是一个主要网站的r-过程的富集。
We present UV, optical, and near-infrared (NIR) photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at 0.47–18.5 days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the Hubble Space Telescope (HST). The spectral energy distribution (SED) inferred from this photometry at 0.6 days is well described by a blackbody model with T ≈ 8300 K, a radius of R ≈ 4.5 × 10 14 cm (corresponding to an expansion velocity of v ≈ 0.3 c ), and a bolometric luminosity of L bol ≈ 5 × 10 41 erg s−1. At 1.5 days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set, we find that models with heating from radioactive decay of 56Ni, or those with only a single component of opacity from r-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data; the resulting “blue” component has M ej blue ≈ 0.01 M ⊙ and v ej blue ≈ 0.3 c , and the “red” component has M ej red ≈ 0.04 M ⊙ and v ej red ≈ 0.1 c . These ejecta masses are broadly consistent with the estimated r-process production rate required to explain the Milky Way r-process abundances, providing the first evidence that binary neutron star (BNS) mergers can be a dominant site of r-process enrichment.