The Dark Energy Survey Supernova Program results: Type Ia Supernova brightness correlates with host galaxy dust
The Dark Energy Survey Supernova Program results: Type Ia Supernova brightness correlates with host galaxy dust
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暗能量巡天超新星计划结果：Ia 型超新星亮度与宿主星系尘埃相关
DOI：
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发表时间：
2022
影响因子：
4.8
通讯作者：
T. Varga
中科院分区：
文献类型：
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作者：
C. Meldorf;A. Palmese;D. Brout;R. Chen;D. Scolnic;L. Kelsey;L. Galbany;W. Hartley;T. Davis;A. Drlica;M. Vincenzi;J. Annis;M. Dixon;O. Graur;C. Lidman;A. Möller;P. Nugent;B. Rose;M. Smith;S. Allam;D. Tucker;J. Asorey;J. Calcino;D. Carollo;K. Glazebrook;G. Lewis;G. Taylor;B. Tucker;A. Kim;H. Diehl;M. Aguena;F. Andrade;D. Bacon;E. Bertin;S. Bocquet;D. Brooks;D. Burke;J. Carretero;M. Kind;F. Castander;M. Costanzi;L. D. da Costa;S. Desai;P. Doel;S. Everett;I. Ferrero;D. Friedel;J. Frieman;J. García;M. Gatti;D. Gruen;J. Gschwend;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;D. James;K. Kuehn;M. March;J. Marshall;F. Menanteau;R. Miquel;R. Morgan;F. Paz;M. Pereira;A. P. Malagón;E. Sanchez;V. Scarpine;I. Sevilla;E. Suchyta;G. Tarlé;T. Varga
对Ia型超新星（SNe Ia）的宇宙学分析通常假设颜色和光度（β）之间存在单一的经验关系，并且不能解释主星系尘埃的变化特性。然而，从对大样本星系中的尘埃的研究中，人们知道尘埃的衰减可能会有很大的变化。在这里，我们利用国家的最先进的建模的星系属性来表征尘埃参数（尘埃衰减AV，和一个参数描述的尘埃定律斜率RV）为1100暗能量调查（DES）SN主机星系。仅利用宿主的光学和红外数据，我们发现了影响SN宇宙学的宿主尘埃的三个关键方面：1）存在一个大范围的宿主RV（≥ 1 - 6）2）高质量宿主的RV平均比低质量宿主的RV低≥ 0.7 3）对于81个光谱分类的SNe子样本，存在显著的（>3σ）红超新星Ia的哈勃图残差和宿主RV之间的相关性，当校正时，散射减少了$sim 13{{\%}}$，“质量阶跃”的重要性降低了1σ。这些代表了最近基于尘埃的预测的独立确认，这些预测试图解释超新星Ia分析中令人困惑的“质量阶跃”和内在散射（σint）。
Cosmological analyses with type Ia supernovae (SNe Ia) often assume a single empirical relation between colour and luminosity (β) and do not account for varying host-galaxy dust properties. However, from studies of dust in large samples of galaxies, it is known that dust attenuation can vary significantly. Here we take advantage of state-of-the-art modeling of galaxy properties to characterize dust parameters (dust attenuation AV, and a parameter describing the dust law slope RV) for 1100 Dark Energy Survey (DES) SN host galaxies. Utilizing optical and infrared data of the hosts alone, we find three key aspects of host dust that impact SN cosmology: 1) there exists a large range (∼1 − 6) of host RV 2) high stellar mass hosts have RV on average ∼0.7 lower than that of low-mass hosts 3) for a subsample of 81 spectroscopically classified SNe there is a significant (>3σ) correlation between the Hubble diagram residuals of red SNe Ia and the host RV that when corrected for reduces scatter by $sim 13{{\%}}$ and the significance of the ‘mass step’ to ∼1σ. These represent independent confirmations of recent predictions based on dust that attempted to explain the puzzling ‘mass step’ and intrinsic scatter (σint) in SN Ia analyses.
DOI：
10.3847/1538-4357/ac8b7a
发表时间：
2021-12
期刊：
The Astrophysical Journal
影响因子：
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作者：
D. Scolnic;D. Brout;A. Carr;A. Riess;T. Davis;Arianna M. Dwomoh;David O. Jones;Noor Ali;Pranav Charvu;R. Chen;E. Peterson;B. Popovic;B. Rose;C. Wood;P. Brown;K. Chambers;D. Coulter;K. Dettman;G. Dimitriadis;A. Filippenko;R. Foley;S. Jha;C. Kilpatrick;R. Kirshner;Yen-Chen Pan;A. Rest;C. Rojas-Bravo;M. Siebert;B. Stahl;Wei Zheng
通讯作者：
D. Scolnic;D. Brout;A. Carr;A. Riess;T. Davis;Arianna M. Dwomoh;David O. Jones;Noor Ali;Pranav Charvu;R. Chen;E. Peterson;B. Popovic;B. Rose;C. Wood;P. Brown;K. Chambers;D. Coulter;K. Dettman;G. Dimitriadis;A. Filippenko;R. Foley;S. Jha;C. Kilpatrick;R. Kirshner;Yen-Chen Pan;A. Rest;C. Rojas-Bravo;M. Siebert;B. Stahl;Wei Zheng
DOI：
10.3847/2041-8213/ab8735
发表时间：
2020-02
期刊：
The Astrophysical Journal Letters
影响因子：
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作者：
D. Scolnic;M. Smith;A. Massiah;P. Wiseman;D. Brout;R. Kessler;T. Davis;R. Foley;L. Galbany;S. Hinton;R. Hounsell;L. Kelsey;C. Lidman;E. MacAulay;R. Morgan;R. Nichol;A. Moller;B. Popovic;M. Sako;Mark Sullivan;B. Thomas;B. Tucker;T. Abbott;M. Aguena;S. Allam;J. Annis;S. Ávila;K. Bechtol;E. Bertin;E. Bertin;D. Brooks;D. Burke;A. Rosell;D. Carollo;M. Kind;J. Carretero;M. Costanzi;L. Costa;J. Vicente;S. Desai;H. Diehl;P. Doel;A. Drlica-Wagner;A. Drlica-Wagner;K. Eckert;T. Eifler;T. Eifler;S. Everett;B. Flaugher;P. Fosalba;J. Frieman;J. García-Bellido;E. Gaztañaga;D. Gerdes;K. Glazebrook;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;W. Hartley;W. Hartley;D. Hollowood;K. Honscheid;D. James;K. Kuehn;K. Kuehn;N. Kuropatkin;G. F. Lewis;T. Li;T. Li;M. Lima;M. Maia;J. Marshall;F. Menanteau;R. Miquel;A. Palmese;F. Paz-Chinchón;A. Plazas;M. Pursiainen;E. Sánchez;V. Scarpine;M. Schubnell;S. Serrano;I. Sevilla-Noarbe;N. E. Sommer;E. Suchyta;M. Swanson;G. Tarlé;T. Varga;T. Varga;A. Walker;R. Wilkinson
通讯作者：
D. Scolnic;M. Smith;A. Massiah;P. Wiseman;D. Brout;R. Kessler;T. Davis;R. Foley;L. Galbany;S. Hinton;R. Hounsell;L. Kelsey;C. Lidman;E. MacAulay;R. Morgan;R. Nichol;A. Moller;B. Popovic;M. Sako;Mark Sullivan;B. Thomas;B. Tucker;T. Abbott;M. Aguena;S. Allam;J. Annis;S. Ávila;K. Bechtol;E. Bertin;E. Bertin;D. Brooks;D. Burke;A. Rosell;D. Carollo;M. Kind;J. Carretero;M. Costanzi;L. Costa;J. Vicente;S. Desai;H. Diehl;P. Doel;A. Drlica-Wagner;A. Drlica-Wagner;K. Eckert;T. Eifler;T. Eifler;S. Everett;B. Flaugher;P. Fosalba;J. Frieman;J. García-Bellido;E. Gaztañaga;D. Gerdes;K. Glazebrook;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;W. Hartley;W. Hartley;D. Hollowood;K. Honscheid;D. James;K. Kuehn;K. Kuehn;N. Kuropatkin;G. F. Lewis;T. Li;T. Li;M. Lima;M. Maia;J. Marshall;F. Menanteau;R. Miquel;A. Palmese;F. Paz-Chinchón;A. Plazas;M. Pursiainen;E. Sánchez;V. Scarpine;M. Schubnell;S. Serrano;I. Sevilla-Noarbe;N. E. Sommer;E. Suchyta;M. Swanson;G. Tarlé;T. Varga;T. Varga;A. Walker;R. Wilkinson
DOI：
10.3847/1538-4357/abafb7
发表时间：
2020-06
期刊：
The Astrophysical Journal
影响因子：
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作者：
S. Uddin;C. Burns;M. Phillips;N. Suntzeff;C. Contreras;E. Hsiao;N. Morrell;L. Galbany;M. Stritzinger;P. Hoeflich;C. Ashall;A. Piro;W. Freedman;S. E. Persson;K. Krisciunas;P. Brown
通讯作者：
S. Uddin;C. Burns;M. Phillips;N. Suntzeff;C. Contreras;E. Hsiao;N. Morrell;L. Galbany;M. Stritzinger;P. Hoeflich;C. Ashall;A. Piro;W. Freedman;S. E. Persson;K. Krisciunas;P. Brown