RUI: Spatially-Resolved Kinematics of Reverberation-Mapped Active Galactic Nuclei Host Galaxies

RUI：混响映射的活动星系核宿主星系的空间分辨运动学

• 批准号: 1909297
• 负责人: Vardha Bennert
• 金额: $ 29.12万
• 依托单位: California Polytechnic State University Foundation
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2019
• 资助国家: 美国
• 起止时间: 2019-09-01 至 2024-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1909297&HistoricalAwards=false
• 关键词: RUI; Spatially; Resolved; Kinematics; Reverberation

Part 1Most galaxies harbor in their center a very massive black hole with a mass that can range from millions to billions of times the mass of the Sun. They are also known as supermassive black holes. The origin of supermassive black holes is an important open question in astronomy. For supermassive black holes growing through accretion of dust and gas in the centers of so-called "active galaxies", their mass can be measured through an observing technique known as "echo mapping". In this work, the PI will study the properties of the host galaxies for a sample of 33 active galaxies for which the mass of the supermassive black hole has been previously determined through echo mapping. They have obtained data with some of the largest telescopes world-wide, the Keck telescope (Hawaii) and the Very Large Telescope (Chile). Their state-of-the art instruments allow the PI to measure spectra (the distribution of light over different wavelengths, similar to a rainbow) over the entire galaxy within one single observation. They will study the relationship between the mass of the supermassive black hole and the kinematics of the stars in the galaxy, a measure of the galaxy mass. The tightness of such a relationship indicates that supermassive black holes and galaxies grow together. Their sample extends existing relationships into the high mass regime and can be used to study trends with mass and galaxy morphology. This will enhance understanding of the growth and evolution of supermassive black holes and galaxies. While echo mapping is time consuming, its results have enabled black-hole mass estimates for active galaxies across the universe. The PI's sample will serve as a calibrator for these black-hole mass measurements. Part 2Supermassive Black Holes are very massive black holes in the center of galaxies with millions to billions of times the mass of the Sun. The origin of supermassive black holes is an important open question in astronomy. For supermassive black holes growing through accretion of dust and gas in the centers of so-called "active galaxies", their mass can be measured through an observing technique known as "echo mapping". In this work, the PI will study the properties of the host galaxies for a sample of 33 active galaxies for which the mass of the supermassive black hole has been previously determined through echo mapping. They have obtained data with some of the largest telescopes world-wide, the Keck telescope (Hawaii) and the Very Large Telescope (Chile). Their state-of-the art instruments allow the PI to measure spectra over the entire galaxy within one single observation. They will study the relationship between the mass of the supermassive black hole and the kinematics of the stars in the galaxy, a measure of the galaxy mass. The tightness of such a relationship indicates that supermassive black holes and galaxies grow together. In addition, they will fit images (either created from the spectra or taken by the Hubble Space Telescope) for a detailed host-galaxy decomposition. The sample extends existing relationships into the high mass regime and can be used to study trends with mass and galaxy morphology. This will enhance understanding of the growth and evolution of supermassive black holes and galaxies. While echo mapping is time consuming, its results have enabled black-hole mass estimates for active galaxies across the universe. The PI's sample will serve as a calibrator for these black-hole mass measurements.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

大多数星系的中心都有一个巨大质量的黑洞，其质量可以是太阳质量的几百万到几十亿倍。它们也被称为超大质量黑洞。超大质量黑洞的起源是天文学中一个重要的悬而未决的问题。对于通过尘埃和气体在所谓的“活动星系”中心吸积而成长起来的超大质量黑洞，其质量可以通过一种被称为“回声映射法”的观测技术来测量。在这项工作中，PI将研究一个由33个活动星系组成的样本的宿主星系的性质，这些星系的超大质量黑洞的质量之前已经通过回波映射确定。他们用一些世界上最大的望远镜--凯克望远镜(夏威夷)和甚大望远镜(智利)--获得了数据。他们最先进的仪器允许PI在一次观测中测量整个银河系的光谱(不同波长的光的分布，类似于彩虹)。他们将研究超大质量黑洞的质量与星系中恒星的运动学之间的关系，运动学是衡量星系质量的一种指标。这种关系的紧密程度表明，超大质量黑洞和星系是共同成长的。他们的样本将现有的关系扩展到高质量区域，并可用于研究质量和星系形态的趋势。这将加强对超大质量黑洞和星系生长和演化的理解。虽然回波映射很耗时，但它的结果已经使整个宇宙中活动星系的黑洞质量估计成为可能。圆周率探测器的样品将作为这些黑洞质量测量的校准器。超大质量黑洞是位于星系中心的非常大质量的黑洞，质量是太阳的数百万到数十亿倍。超大质量黑洞的起源是天文学中一个重要的悬而未决的问题。对于通过尘埃和气体在所谓的“活动星系”中心吸积而成长起来的超大质量黑洞，其质量可以通过一种被称为“回声映射法”的观测技术来测量。在这项工作中，PI将研究一个由33个活动星系组成的样本的宿主星系的性质，这些星系的超大质量黑洞的质量之前已经通过回波映射确定。他们用一些世界上最大的望远镜--凯克望远镜(夏威夷)和甚大望远镜(智利)--获得了数据。他们最先进的仪器使PI可以在一次观测中测量整个银河系的光谱。他们将研究超大质量黑洞的质量与星系中恒星的运动学之间的关系，运动学是衡量星系质量的一种指标。这种关系的紧密程度表明，超大质量黑洞和星系是共同成长的。此外，它们将匹配图像(从光谱创建或由哈勃太空望远镜拍摄)，以进行详细的宿主星系分解。该样本将现有的关系扩展到高质量区域，并可用于研究质量和星系形态的趋势。这将加强对超大质量黑洞和星系生长和演化的理解。虽然回波映射很耗时，但它的结果已经使整个宇宙中活动星系的黑洞质量估计成为可能。PI的样本将作为这些黑洞质量测量的校准器。这一奖项反映了NSF的法定使命，并通过使用基金会的智力优势和更广泛的影响审查标准进行评估，被认为值得支持。

项目成果

Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548

• DOI: 10.3847/1538-4357/abbad7
• 发表时间: 2020-10
• 期刊: The Astrophysical Journal
• 作者: P. Williams;A. Pancoast;T. Treu;B. Brewer;B. Peterson;A. Barth;M. Malkan;G. D. Rosa;K. Horne;G. Kriss;N. Arav;M. Bentz;E. Cackett;E. Bontà;M. Dehghanian;C. Done;G. Ferland;C. Grier;J. Kaastra;E. Kara;C. Kochanek;S. Mathur;M. Mehdipour;R. Pogge;D. Proga;M. Vestergaard;T. Waters;S. Adams;M. Anderson;P. Ar'evalo;T. Beatty;V. Bennert;A. Bigley;S. Bisogni;G. Borman;T. Boroson;M. Bottorff;W. Brandt;A. Breeveld;M. Brotherton;J. E. Brown;J. Brown;G. Canalizo;M. Carini;K. Clubb;J. Comerford;E. Corsini;D. Crenshaw;S. Croft;K. Croxall;A. Deason;A. D. Lorenzo-C'aceres;K. Denney;M. Dietrich;R. Edelson;N. Efimova;J. Ely;P. Evans;M. Fausnaugh;A. Filippenko;K. Flatland;O. Fox;E. Gardner;E. Gates;N. Gehrels;S. Geier;J. Gelbord;L. Gonzalez;V. Gorjian;J. Greene;D. Grupe;A. Gupta;P. Hall;C. Henderson;S. Hicks;E. Holmbeck;T. Holoien;T. Hutchison;M. Im;J. Jensen;C. Johnson;M. Joner;J. Jones;S. Kaspi;P. Kelly;J. Kennea;M. Kim;S. Kim;S. Kim;A. King;S. Klimanov;C. Knigge;Y. Krongold;M. W. Lau;J. Lee;D. Leonard;Miao Li;P. Lira;C. Lochhaas;Zhiyuan Ma;E. Manne-Nicholas;F. Macinnis;J. Mauerhan;R. McGurk;I. M. Hardy;C. Montuori;L. Morelli;A. Mosquera;D. Mudd;F. Muller-S'anchez;S. Nazarov;R. Norris;J. Nousek;M. L. Nguyen;P. Ochner;D. N. Okhmat;I. Papadakis;J. Parks;L. Pei;M. Penny;A. Pizzella;R. Poleski;J. Pott;S. Rafter;H. Rix;J. Runnoe;D. Saylor;J. Schimoia;B. Scott;S. Sergeev;B. Shappee;I. Shivvers;M. Siegel;G. Simonian;A. Siviero;A. Skielboe;G. Somers;M. Spencer;D. Starkey;D. Stevens;H. Sung;J. Tayar;N. Tejos;C. S. Turner;P. Uttley;J. Saders;S. Vaughan;L. Vican;S. Villanueva;C. Villforth;Y. Weiss;J. Woo;H. Yan;S. Young;H. Yuk;W. Zheng;W. Zhu;Y. Zu

The Close AGN Reference Survey (CARS): Tracing the circumnuclear star formation in the super-Eddington NLS1 Mrk 1044

近距离 AGN 参考巡天 (CARS)：追踪超级爱丁顿 NLS1 Mrk 1044 中的环核恒星形成

• DOI: 10.1051/0004-6361/202243697
• 发表时间: 2022
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: Winkel, N.;Husemann, B.;Davis, T. A.;Smirnova-Pinchukova, I.;Bennert, V. N.;Combes, F.;Gaspari, M.;Jahnke, K.;Neumann, J.;O’Dea, C. P.
• 通讯作者: O’Dea, C. P.

Space Telescope and Optical Reverberation Mapping Project. IX. Velocity–Delay Maps for Broad Emission Lines in NGC 5548

• DOI: 10.3847/1538-4357/abce60
• 发表时间: 2021-02
• 期刊: The Astrophysical Journal
• 作者: K. Horne;G. D. Rosa;B. Peterson;A. Barth;J. Ely;M. Fausnaugh;G. Kriss;L. Pei;M. Bentz;E. Cackett;R. Edelson;M. Eracleous;M. Goad;C. Grier;J. Kaastra;C. Kochanek;Y. Krongold;S. Mathur;H. Netzer;D. Proga;N. Tejos;M. Vestergaard;C. Villforth;S. Adams;M. D. Anderson;P. Arévalo;T. Beatty;V. Bennert;A. Bigley;S. Bisogni;G. Borman;T. Boroson;M. Bottorff;W. Brandt;A. Breeveld;M. Brotherton;J. E. Brown;J. Brown;G. Canalizo;M. Carini;K. Clubb;J. Comerford;E. Corsini;D. Crenshaw;S. Croft;K. Croxall;E. Bontà;A. Deason;M. Dehghanian;A. D. Lorenzo-Cáceres;K. Denney;M. Dietrich;C. Done;N. Efimova;P. A. Evans;G. J. Ferland;A. Filippenko;K. Flatland;O. Fox;E. Gardner;E. Gates;N. Gehrels;S. Geier;J. Gelbord;L. Gonzalez;V. Gorjian;J. Greene;D. Grupe;A. Gupta;P. Hall;C. Henderson;S. Hicks;E. Holmbeck;T. Holoien;T. Hutchison;M. Im;J. Jensen;C. A. Johnson;M. D. Joner;J. Jones;S. Kaspi;P. L. Kelly;J. Kennea;M. Kim;S. Kim;S. Kim;A. King;S. Klimanov;K. Korista;M. W. Lau;J. C. Lee;D. Leonard;Miao Li;P. Lira;C. Lochhaas;Zhiyuan Ma;F. Macinnis;M. Malkan;E. Manne-Nicholas;J. Mauerhan;R. McGurk;I. McHardy;C. Montuori;L. Morelli;A. Mosquera;D. Mudd;F. Müller-Sánchez;S. Nazarov;R. P. Norris;J. Nousek;M. L. Nguyen;P. Ochner;D. N. Okhmat;A. Pancoast;I. Papadakis;J. Parks;M. Penny;A. Pizzella;R. Pogge;R. Poleski;J. Pott;S. Rafter;H. Rix;J. Runnoe;D. Saylor;J. Schimoia;K. Schnülle;B. Scott;S. Sergeev;B. Shappee;I. Shivvers;M. Siegel;G. Simonian;A. Siviero;A. Skielboe;G. Somers;M. Spencer;D. Starkey;D. Stevens;H.-I. Sung;J. Tayar;T. Treu;C. S. Turner;P. Uttley;J. V. van Saders;L. Vican;S. Villanueva;Y. Weiss;Jong-hak Woo;H. Yan;S. Young;H. Yuk;W. Zheng;W. Zhu;Y. Zu

What Does the Geometry of the Hβ BLR Depend On?

Hβ BLR 的几何形状取决于什么？

• DOI: 10.3847/1538-4357/accc84
• 发表时间: 2023
• 期刊: The Astrophysical Journal
• 作者: Villafaña, Lizvette;Williams, Peter R.;Treu, Tommaso;Brewer, Brendon J.;Barth, Aaron J.;U, Vivian;Bennert, Vardha N.;Guo, Hengxiao;Bentz, Misty C.;Canalizo, Gabriela
• 通讯作者: Canalizo, Gabriela

An [O iii] search for extended emission around AGN with H i mapping: a distant cloud ionized by Mkn 1

[O-iii] 使用 H-i 映射搜索 AGN 周围的扩展发射：由 Mkn 1 电离的遥远云

• DOI: 10.1093/mnras/staa1510
• 发表时间: 2020
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Knese, Erin Darnell;Keel, William C;Knese, Greg;Bennert, Vardha N;Moiseev, Alexei;Grokhovskaya, Aleksandra;Dodonov, Sergei N
• 通讯作者: Dodonov, Sergei N