High Energy Astrophysics at Southampton

南安普顿高能天体物理学

• 批准号: ST/G003084/1
• 负责人: Ian McHardy
• 金额: $ 252.48万
• 依托单位: University of Southampton
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2009
• 资助国家: 英国
• 起止时间: 2009 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FG003084%2F1
• 关键词: Energy; Astrophysics; Southampton

On the stellar scale we are interested in the significance of different environments on the evolution of high mass X-ray binary (HMXB) populations, in particular between the Milky Way and the SMC, where differing star formation rates and metallicities could be crucial. What are the relative importances of local and interstellar obscuration in what we see? Here the upcoming 2Msec INTEGRAL Key Programme observation of the SMC, almost unaffected by obscuration, will be of great value. Globular clusters are outstanding laboratories for studying stellar dynamics and stellar evolution, especially for understanding the most exotic stellar populations. We are drawing together observations of large samples of globular clusters to understand which cluster properties are most important for the production of these exotic stars, and comparing with low stellar density dwarf spheroidal galaxies to isolate the stellar evolution from stellar dynamics. The Netherlands-based low frequency radio array, LOFAR, is about to open a new window on the universe providing the first radio `all sky monitor'. We will study coherent radio bursts, perhaps associated with merging neutron stars, detectable at enormous distances (to z=7), providing a unique probe of the intergalactic medium and possibly even testing theories of gravity and cosmological distance scales via identification of LIGO inspiral events We will continue our research into the coupling between accretion and outflow (jets) in X-ray binaries, and how it relates to parallel processes in AGN (where scaling laws with black hole mass are established), accreting neutron stars and white dwarfs. We have amassed the first comprehensive database of black hole spectral states and will extend this analysis to include X-ray timing and radio results. Thus we will produce the most comprehensive analysis to date of the relation between black hole accretion flows and the formation and power of relativistic jets. The results can be applied to AGN feedback in galaxies and clusters. We will greatly improve our knowledge of the scaling relationship between characteristic X-ray timescale, mass and accretion rate in Seyfert galaxies and Galactic binaries, thus testing physical models for this important universal relationship. We will determine whether the relationship applies in jet dominated ``blazars'', implying a universal origin for variability. We are building a model, based on propagating fluctuations, to provide physical understanding of all spectral-timing relationships to derive physical parameters, eg disc emissivity profile. This model, with additional X-ray reprocessing, should also explain X-ray/optical correlations in AGN so we will test it against our X-ray/optical monitoring. To provide a census of the nearby universe on which models of the more distant universe can be built, we are heavily involved in eMERLIN legacy surveys of nearby galaxy samples It is now widely accepted that some process must reheat the gas in galaxy clusters or large amounts of cool gas, which are not seen, would be found in the cores of clusters of galaxies. But what is the heating mechanism? In our most theoretical project we will investigate, via MHD simulations, whether the dissipation of turbulent energy, driven by merger events, galaxy motions and AGN outflows, may be responsible. On the largest scales, both AGN and starforming galaxies (SFGs) contribute to the faint radio source population, but what is the mix? By combining radio morphology with a variety of spectral energy diagnostics we can distinguish AGN from SFGs. Hence, using radio luminosity as a starformation rate (SFR) indicator, we can determine the evolution of the cosmic SFR in an absorption-independent manner. We will push this technique to much higher redshifts, as major contributors to eMERLIN deep field legacy surveys, and also probe the relationship between SFGs and AGN.

在恒星尺度上，我们感兴趣的是不同环境对高质量X射线双星（HMXB）群体演化的重要性，特别是在银河系和SMC之间，其中不同的恒星形成速率和金属丰度可能至关重要。在我们所看到的情况中，本地和星际遮蔽的相对重要性是什么？即将到来的 SMC 的 2Msec INTEGRAL Key Program 观察几乎不受遮蔽的影响，将具有很大的价值。球状星团是研究恒星动力学和恒星演化的杰出实验室，尤其是了解最奇异的恒星族群。我们正在收集对球状星团大样本的观测结果，以了解哪些星团特性对于这些奇异恒星的产生最重要，并与低恒星密度矮椭球星系进行比较，以将恒星演化与恒星动力学分开。总部位于荷兰的低频无线电阵列 LOFAR 即将打开宇宙新窗口，提供第一个无线电“全天监测器”。我们将研究相干射电爆发，可能与合并中子星有关，可以在很远的距离（到z=7）检测到，提供一种独特的星际介质探测器，甚至可能通过识别LIGO吸气事件来测试重力和宇宙距离尺度的理论。我们将继续研究X射线双星中吸积和流出（射流）之间的耦合，以及它与并行过程的关系 在活动星系核（建立了黑洞质量的标度定律）中，吸积中子星和白矮星。我们已经积累了第一个黑洞光谱状态综合数据库，并将将此分析扩展到包括 X 射线定时和射电结果。因此，我们将对黑洞吸积流与相对论性喷流的形成和功率之间的关系进行迄今为止最全面的分析。结果可应用于星系和星团中的活动星系核反馈。我们将极大地提高对赛弗特星系和银河双星中特征X射线时标、质量和吸积率之间的标度关系的认识，从而测试这种重要的普遍关系的物理模型。我们将确定这种关系是否适用于喷流主导的“耀变体”，这意味着变异性的普遍起源。我们正在建立一个基于传播波动的模型，以提供对所有光谱定时关系的物理理解，从而导出物理参数，例如圆盘发射率分布。该模型加上额外的 X 射线再处理，还应该解释 AGN 中的 X 射线/光学相关性，因此我们将根据 X 射线/光学监测对其进行测试。为了提供附近宇宙的普查，以便建立更遥远宇宙的模型，我们积极参与了对附近星系样本的 eMERLIN 遗留调查。现在人们普遍认为，某些过程必须重新加热星系团中的气体，或者在星系团的核心中会发现大量看不见的冷气体。但加热机制是什么？在我们最具理论性的项目中，我们将通过 MHD 模拟来研究由合并事件、星系运动和活动星系核外流驱动的湍流能量耗散是否可能是造成这一现象的原因。在最大的尺度上，活动星系核和恒星形成星系（SFG）都对微弱的射电源群产生了影响，但两者的混合是什么？通过将射电形态学与各种光谱能量诊断相结合，我们可以区分 AGN 和 SFG。因此，利用射电光度作为恒星形成率（SFR）指标，我们可以以与吸收无关的方式确定宇宙恒星形成率的演化。作为 eMERLIN 深场遗留调查的主要贡献者，我们将把这项技术推向更高的红移，并探讨 SFG 和 AGN 之间的关系。

项目成果

3C 286: a bright, compact, stable, and highly polarized calibrator for millimeter-wavelength observations

3C 286：明亮、紧凑、稳定、高偏振的校准器，用于毫米波观测

• DOI: 10.1051/0004-6361/201218801
• 发表时间: 2012
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: Agudo I

FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE

• DOI: 10.1088/0004-637x/721/2/1425
• 发表时间: 2010-10
• 期刊: The Astrophysical Journal
• 作者: A. Abdo;M. Ackermann;I. Agudo;M. Ajello;A. Allafort;H. Aller;M. Aller;E. Antolini;A. Arkharov;M. Axelsson;U. Bach;L. Baldini;J. Ballet;G. Barbiellini;D. Bastieri;K. Bechtol;R. Bellazzini;A. Berdyugin;B. Berenji;R. Blandford;D. Blinov;E. Bloom;M. Boettcher;E. Bonamente;A. Borgland;A. Bouvier;J. Bregeon;A. Brez;M. Brigida;P. Bruel;R. Buehler;C. Buemi;T. Burnett;S. Buson;G. Caliandro;R. Cameron;P. Caraveo;D. Carosati;S. Carrigan;J. Casandjian;E. Cavazzuti;C. Cecchi;O. Celik;A. Chekhtman;Wen-Ping Chen;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;J. Conrad;S. Corbel;L. Costamante;C. Dermer;A. Angelis;F. Palma;D. Donato;E. Silva;P. Drell;R. Dubois;D. Dumora;C. Farnier;C. Favuzzi;S. Fegan;E. Ferrara;W. Focke;E. Forne;P. Fortin;Y. Fukazawa;S. Funk;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;S. Germani;B. Giebels;N. Giglietto;F. Giordano;M. Giroletti;T. Glanzman;G. Godfrey;I. Grenier;J. Grove;S. Guiriec;M. Gurwell;C. Gusbar;J. Gómez;D. Hadasch;V. Hagen-Thorn;M. Hayashida;E. Hays;D. Horan;R. Hughes;G. Jóhannesson;A. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;N. Kawai;G. Kimeridze;J. Knödlseder;T. Konstantinova;E. Kopatskaya;E. Koptelova;Y. Kovalev;O. Kurtanidze;M. Kuss;A. Lähteenmäki;J. Lande;V. Larionov;E. Larionova;L. Larionova;S. Larsson;L. Latronico;S. Lee;P. Leto;M. Lister;F. Longo;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;G. Madejski;A. Makeev;E. Massaro;M. Mazziotta;W. Mcconville;J. Mcenery;I. McHardy;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;C. Monte;M. Monzani;D. Morozova;A. Morselli;I. Moskalenko;S. Murgia;M. Naumann-Godo;M. Nikolashvili;P. Nolan;J. Norris;E. Nuss;M. Ohno;T. Ohsugi;A. Okumura;N. Omodei;E. Orlando;J. Ormes;M. Ozaki;D. Paneque;J. Panetta;D. Parent;M. Pasanen;V. Pelassa;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;A. Pushkarev;S. Rainò;C. Raiteri;R. Rando;M. Razzano;A. Reimer;O. Reimer;R. Reinthal;J. Ripken;S. Ritz;M. Roca-Sogorb;A. Rodríguez;M. Roth;P. Roustazadeh;F. Ryde;H. Sadrozinski;A. Sander;J. Scargle;C. Sgro’;L. Sigua;P. Smith;K. Sokolovsky;G. Spandre;P. Spinelli;Jean-Luc Starck;M. Strickman;D. Suson;H. Takahashi;Tadayuki Takahashi;L. Takalo;Takaaki Tanaka;B. Taylor;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;M. Tornikoski;D. Torres;G. Tosti;A. Tramacere;C. Trigilio;I. Troitsky;G. Umana;T. Usher;J. Vandenbroucke;V. Vasileiou;N. Vilchez;M. Villata;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;Z. Yang;T. Ylinen;M. Ziegler

Constraints on the multi-TeV particle population in the Coma galaxy cluster with HESS observations

• DOI: 10.1051/0004-6361/200912086
• 发表时间: 2009-08-01
• 期刊: ASTRONOMY & ASTROPHYSICS
• 影响因子: 6.5
• 作者: Aharonian, F.;Akhperjanian, A. G.;Zech, A.
• 通讯作者: Zech, A.

Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy

• DOI: 10.1007/s10686-011-9247-0
• 发表时间: 2011-12-01
• 期刊: EXPERIMENTAL ASTRONOMY
• 影响因子: 3
• 作者: Actis, M.;Agnetta, G.;Zychowski, P.
• 通讯作者: Zychowski, P.

Erratum to "Observations of the Sagittarius dwarf galaxy by the HESS experiment and search for a dark matter signal" [Astropart. Phys. 29(1) (2008) 55-62]

“HESS 实验对人马座矮星系的观测并寻找暗物质信号”的勘误 [Astropart。

• DOI: 10.1016/j.astropartphys.2010.01.007
• 发表时间: 2010
• 期刊: Astroparticle Physics
• 影响因子: 3.5
• 作者: Aharonian F