YNAO OpenIR研究单元&专题: 高能天体物理研究组
http://ir.ynao.ac.cn:80/handle/114a53/56
2024-03-29T01:29:01Z
2024-03-29T01:29:01Z
基于慧眼观测研究 4U 1543−47 在 2021 年的爆发
靳沛
http://ir.ynao.ac.cn:80/handle/114a53/26394
2024-03-26T06:35:05Z
2024-03-26T06:24:23Z
题名: 基于慧眼观测研究 4U 1543−47 在 2021 年的爆发
作者: 靳沛
摘要: We present a detailed analysis of the observations with the Hard X-ray Modulation
Telescope of the black hole X-ray transient 4U 1543−47 during its outburst in 2021.
We find a clear state transition during the outburst decay both in the hardness-intensity
diagram and light curve of the source. Using previous measurements of the black-hole
mass and distance to the source, we find that the source luminosity during this transition
is around Eddington. The light curves before and after the state transition can be well
fitted by two exponential functions with short (∼ 16 days) and long (∼ 130 days) decay
time scales, respectively. During the super-Eddington period the hard component in the
X-ray spectra has a large photon index Γ ∼ 4.5, similar to the "hypersoft" state of the
2005 outburst of the black-hole transient GRO J1655−40. We detect strong reflection
features in all observations that can be well fitted with the model RELXILLNS with a
temperature kTbb ∼ 1 keV of the black-body incident spectrum. This indicates that the
emission of the accretion disk plays an important role in shaping the reflection spectra.
The fluxes of the RELXILLNS and the GAUSSIAN components show different correlations
before and after the transition. The best-fitting emissivity index of the disk changes
significantly during the state transition, from ∼ 3 − 4.5 in the super-Eddington period
to ∼ 8.0 in the sub-Eddington period. These results suggest that the accretion disk may
have changed significantly near the Eddington limit.
摘要: 慧眼卫星对黑洞 X 射线双星 4U 1543-47 在 2021 年的高亮度爆发进行了密集的观测(135 次曝光)。利用高密度观测优势,我们获得了源从约 2.3 个爱丁
顿光度至约 0.5 个爱丁顿光度的完整的爆发衰减过程。通过光变曲线和硬度强度图的分析,我们发现在爆发衰减的过程中存在一个明显的状态转换过程。利用之前对黑洞质量和距离的测量结果,我们发现转换态恰处在一个爱丁顿光度附近。我们使用指数衰减函数去拟合光变曲线,发现在态转换之前的超爱丁顿时期光变曲线的衰减特征时标约为 16 天,而之后的亚爱丁顿时期衰减特征时标约为
130 天。源的能谱在软态表现出非常强的反射特征。我们使用入射谱为温度约为
1keV 的黑体成分的反射模型 RELXILLNS 较好的拟合了反射成分。这表明软光子在塑造反射特征中起关键作用。我们发现一些能谱参数也在转换态时发生了变化:1、在超爱丁顿时期,能谱的硬光子成分具有非常陡的光子指数(∼4.5)。这
一特征跟黑洞 X-ray 源 GRO J1655−40 在 2005 年爆发中的超爱丁顿光度下的超软态的特征相似。2、反射成分 RELXILLNS 的流量和窄线成分 GAUSSIAN 的流量之间的相关性也在转换态时发生变化。3、发射指数在转换态时发生了清楚的变化:
超爱丁顿时期发射指数大约为 3–4.5,而亚爱丁顿时期约为 8。这些结果都暗示着,在爱丁顿光度附近吸积盘的几何结构发生了变化。
2024-03-26T06:24:23Z
Investigation into the reflection properties of the neutron star low-mass X-ray binary 4U 1636-53
Lyu, M.
Zhang GB(张国宝)
Wang, H. G.
García, F.
http://ir.ynao.ac.cn:80/handle/114a53/26326
2023-10-23T03:05:38Z
2023-10-23T02:46:23Z
题名: Investigation into the reflection properties of the neutron star low-mass X-ray binary 4U 1636-53
作者: Lyu, M.; Zhang GB(张国宝); Wang, H. G.; García, F.
摘要: <p>We present the spectroscopy of the neutron star low-mass X-ray binary 4U 1636-53 using six simultaneous XMM-Newton and Rossi X-ray Timing Explorer observations. We applied different self-consistent reflection models to explore the features when the disk is illuminated by either the corona or the neutron star surface. We found that the spectra could be well fitted by these two types of models, with the derived emissivity index below a typical value of 3. The relative low emissivity can be explained if the neutron star and the corona, working together as an extended illuminator, simultaneously illuminate and ionize the disk. Additionally, the derived ionization parameter in the lamppost geometry is larger than the theoretical prediction. This inconsistency likely suggests that the corona does not emit isotropically in a realistic context. Furthermore, we also found that there is a possible trend between the height of the corona and the normalization of the disk emission. This could be understood either as a variation in the reflected radiation pressure or in the context of a jet base. Finally, we found that the disk is less ionized if it is illuminated by the neutron star, indicating that the illuminating source has significant influence on the physical properties of the disk. © The Authors 2023.</p>
2023-10-23T02:46:23Z
Constraints on extragalactic background light using TeV observations of BL Lacertae objects
Qin, Longhua
Wang JC(王建成)
Gao, Quangui
Na, Weiwei
Li, Huaizhen
Wang, Ao
Yang CY(杨初源)
Yang, Jianping
http://ir.ynao.ac.cn:80/handle/114a53/26049
2023-06-19T01:19:44Z
2023-06-12T06:47:43Z
题名: Constraints on extragalactic background light using TeV observations of BL Lacertae objects
作者: Qin, Longhua; Wang JC(王建成); Gao, Quangui; Na, Weiwei; Li, Huaizhen; Wang, Ao; Yang CY(杨初源); Yang, Jianping
摘要: <p>The extragalactic background light (EBL) in the infrared to ultraviolet bands partly absorbs very high energy (VHE; E ≥ 100 GeV) γ -ray photons travelling over cosmological distances via pair production. In this paper, to get stronger constraints on EBL, we use the deliberate selection of the EBL model and data of five BL Lacs with better statistics and the harder spectra to limit the EBL density and the radiation mechanism of BL Lacs. We constrain the upper limit of the EBL density by fitting the spectral energy distributions of TeV BL Lacs and find that our results are compatible with the published measurement, reaching 50 nW m−2 sr−1. We also obtain that the EBL is not necessarily transparent to VHE photons. We fix the intrinsic spectral index Γi of TeV BL Lacs as 1.0 and 1.5 under observation evidence and model assumption. Comparing the EBL density given by galaxy count and Spitzer observations, we then obtain that 1ES 1101−232 has Γi ≤ 1.0 and 1ES 0229+200 should have Γi not harder than 1.0. We demonstrate that the common radiation assumption of BL Lacs, in which the Γi is softer than 1.5, should be revisited. Furthermore, we propose that the upper EBL density could be given by fitting the hardest energy spectra of TeV BL Lacs. © 2023 The Author(s)</p>
2023-06-12T06:47:43Z
Jitter Mechanism as a Kind of Coherent Radiation: Constrained by the GRB 221009A Emission at 18 TeV
Mao JR(毛基荣)
Wang JC(王建成)
http://ir.ynao.ac.cn:80/handle/114a53/25899
2023-06-05T05:19:43Z
2023-05-05T02:45:35Z
题名: Jitter Mechanism as a Kind of Coherent Radiation: Constrained by the GRB 221009A Emission at 18 TeV
作者: Mao JR(毛基荣); Wang JC(王建成)
摘要: <p>The emission of gamma-ray burst (GRB) 221009A at 18 TeV has been detected by the large high-altitude air shower observatory. We suggest jitter radiation as a possible explanation for the TeV emission for this energetic GRB. In our scenario, the radiation field is linked to the perturbation field, and the perturbation field is dominated by kinetic turbulence. Kinetic turbulence takes a vital role in both magnetic field generation and particle acceleration. The jitter radiation can reach the TeV energy band when we consider either electron cooling or Landau damping. We further suggest that the jitter radiation in the very high-energy band is coherent emission. Our modeling results can be constrained by the observational results of GRB 221009A in the TeV energy band. This radiation mechanism is expected to have wide applications in the high-energy astrophysical research field.</p>
2023-05-05T02:45:35Z
用随机过程方法研究耀变体的光变
张偲恒
http://ir.ynao.ac.cn:80/handle/114a53/25776
2023-02-13T02:54:55Z
2023-02-06T05:32:14Z
题名: 用随机过程方法研究耀变体的光变
作者: 张偲恒
摘要: An active galactic nucleus (AGN) is a compact region at the center of a galaxy, galaxies with AGNs are called "active galaxies". Compared with normal galaxies active galaxies have very strong radiation in radio, infrared and X-ray band. If the direction of the line of sight is very close to the direction of the jet, the nuclear region is easy to be observed, and the active galactic nuclei show the characteristics of quasars, which have strong radiation in optical, UV and X-ray bands, this radiation basically comes from the accretion process of the accretion disk. Blazar is a special kind of active galactic nucleus, its relativistic jet almost points to the observer, and its radiation basically comes from synchrotron radiation and inverse Compton scattering in the jet.The radiation of blazar has significant variability.The origin of blazar variability is unclear, which is the hot issue of current research.Here, we use the stochastic process method celerite, which is different from the traditional Fourier-like methods, to analyze the gamma ray and radio long-term variabilities of 4C 01.02. This method can obtain more reliable power spectrum and reduce the influence of noiseThe results show that the simplest kernel in celerite, damped random walk (DRW),can successfully fit both radio and gamma-ray long-term light curves, and the more complex second-order stochastic process (stochastically-driven damped harmonic oscillator,SHO) does not significantly improve the goodness of fit.The intrinsic characteristic timescale of gamma ray variability is about 3 years, and such a long timescale cannot be generated in the leptonic emission model, but it is allowed in the hadronic model. We therefore speculate that the long-term gamma-ray emission of 4C 01.02 may originate from hadronic process.The intrinsic characteristic timescale of radio variability is about 10 years. It may correspond to the escape timescale of the radio emission region, indicating that radio emission is produced in the large-scale jet.The characteristic time scale obtained from jet radiation may also be associated with the standard accretion disk. The characteristic time scale obtained from gamma-ray data is close to the typical thermal time scale of accretion disk.The periodic light variability of AGN is also analyzed by the method used above and discussed, and its possible physical origin is listed.
摘要: 活动星系核(AGN)是位于星系中心的一个致密区域,拥有活动星系核的星系被称为“活动星系”, 活动星系与正常星系相比有很强的射电,红外和X射线辐射,其中X射线辐射基本来自吸积盘,红外辐射来自于尘埃环,射电辐射一般来自喷流的同步辐射。如果视线方向与喷流的方向很接近,核区就容易被观测到,活动星系核就呈现出类星体的特征,在光学,紫外和X射线波段有很强的辐射,这些辐射基本来自于吸积盘的吸积过程。耀变体是特殊的活动星系核,它的相对论喷流几乎指向观测者,其辐射基本来自于喷流中的同步辐射和逆康普顿散射。耀变体辐射有明显的光变,耀变体光变的起源目前尚不明确,是当前研究的热点。一些活动星系核的光变存在周期性,对其周期性的分析可以进一步了解活动星系核中心黑洞,吸积盘和喷流的物理性质。该工作使用不同于传统的类傅里叶方法的随机过程方法celerite分析耀变体4C 01.02的gamma射线和射电波段的长期光变特征,这种方法可以得到更加可靠的功率谱以及减少噪声的影响。结果表明celerite中最简单的阻尼随机游走模型(damped random walk,DRW)可以成功地拟合射电和gamma射线的长期光变曲线,而较为复杂的二阶随机过程(stochastically-driven, damped harmonic oscillator,SHO)并没有显著提升拟合优度。得到的内禀的gamma射线光变特征时标约为3年,如此长的时标不能在轻子辐射模型中产生,但是在强子模型中是允许产生的,我们由此推测4C 01.02长期的gamma射线辐射可能起源于强子过程。射电光变的内禀特征时标约为10年,它可能对应于射电辐射区的逃逸时标,表明射电辐射产生于大尺度喷流。从喷流辐射中得到的特征时标也可能与标准吸积盘联系在一起,其特征时标和典型的吸积盘热时标接近。工作中也用上述方法对活动星系核的周期性光变进行了分析和讨论,列举了其可能的物理起源。
2023-02-06T05:32:14Z
耀变体的伽马射线能谱特征
曾雨航
http://ir.ynao.ac.cn:80/handle/114a53/25772
2023-02-13T02:52:19Z
2023-02-06T05:32:11Z
题名: 耀变体的伽马射线能谱特征
作者: 曾雨航
摘要: After the Large Area Telescope (LAT) onboard Fermi gamma-ray space telescope operating in orbit, a large amount of data has shown that the GeV spectrum displays a power-law or log-parabola form. However, the GeV spectrum of individual sources may be more complex, with suspected hardening. But the reliability of the spectral hardening remains to be tested. To solve this problem, we searched 36 blazars with suspected hardening in the 𝛾-ray spectrum from literature. And we investigated their 𝛾-ray GeV spectrum by using the latest pass 8 data of Fermi-LAT. Then we studied the GeV spectrum evolution in different flare states of 6 blazars in combination with their light curves. We found that the 𝛾-ray spectral hardening in most of the sources are not reliable. For example, the GeV 𝛾-ray spectral hardening of Mrk 501 and 3C 279 do not exist.A significant (∼ 4𝜎) hardening at ∼ 1 GeV is found in the 𝛾-ray spectrum of 1ES 0502+675 during a moderately flaring state (August 7, 2009 to June 3, 2010). The photon index below and above the break energy is 2.36 ± 0.31 and 1.33 ± 0.11, respectively, which is the first case of blazars with obvious 𝛾-ray spectral hardening.In the frame of a one-zone synchrotron self-Compton (SSC) model, the spectral hardening is interpreted as the transition between the synchrotron component and the SSC component. This could be the result of a slight increase of the break/maximum Lorentz factor of the electrons.We will continue to pay attention to the 𝛾-ray spectral hardening of blazars in the follow-up research, and combine with data from other telescopes for further study.
摘要: 费米大面积望远镜 (LAT)在轨以来,大量数据表明耀变体的GeV伽马射线能谱通常呈现出幂律或是对数抛物线的谱型。然而,个别源的能谱结构或许更复杂,有疑似硬化的结构,但可靠性还有待检验。针对这一问题,我们在文献中搜寻了36个伽马射线能谱有疑似硬化结构的耀变体,利用最新的Fermi-LAT的Pass 8数据研究它们的伽马射线能谱结构,并结合光变曲线研究了6个耀变体不同耀发态的能谱演化。我们发现大部分源的伽马射线能谱硬化并不显著,比如Mrk 501和3C 279的GeV伽马射线能谱硬化并不真实存在。我们在1ES 0502+675的费米数据中发现了明显的能谱硬化现象。它只出现在一个中度耀发态的时期(2009年8月7日 – 2010年6月3日),在大于1 GeV处光子谱指数从2.36 ± 0.31变为1.33 ± 0.11。这是目前在耀变体中发现的唯一一个有明显伽马射线能谱硬化的源。在单区同步自康普顿模型的模型中,我们把能谱硬化解释为同步辐射成分和同步自康普顿成分过渡,即1 GeV 以后的辐射由同步辐射贡献,而1 GeV 以上的辐射由同步自康普顿过程贡献。这可能与电子分布的截断能量和最大洛伦兹因子有关。我们将在后续的研究中继续关注耀变体伽马射线能谱硬化的现象,并结合其他望远镜的数据进行深入研究。
2023-02-06T05:32:11Z
Data analysis and key science results of LHAASO-WCDA
Zha, Min
Gao, Chuandong
Hu, Shicong
Lin, Shujie
Wang, Zhen
Xiang, Guangman
Yao, Zhiguo
Zhou, Hao
Aharonian, F.
An, Q.
Axikegu
Bai, L. X.
Bai, Y. X.
Bao, Y. W.
Bastieri, D.
Bi, X. J.
Bi, Y. J.
Cai, H.
Cai, J. T.
Cao, Z.
Zhou, J. N.
Chang, J.
Chang, J. F.
Chang, X. C.
Chen, B. M.
Chen, J.
Chen, L.
Zhou, X. X.
Zhu, C. G.
Chen, M. J.
Chen, M. L.
Chen, Q. H.
Chen, S. H.
Chen, S. Z.
Chen, T. L.
Chen, X. L.
Chen, Y.
Cheng, N.
Cheng, Y. D.
Cui, S. W.
Cui, X. H.
Cui, Y. D.
Dai, B. Z.
Dai, H. L.
Dai, Z. G.
Danzengluobu
della Volpe, D.
D’Ettorre Piazzoli, B.
Dong, X. J.
Fan, J. H.
Fan, Y. Z.
Fan, Z. X.
Fang, J.
Fang, K.
Feng, C. F.
Feng, L.
Feng, S. H.
Feng, Y. L.
Gao, B.
Goa, C. D.
Gao, Q.
Gao, W.
Ge, M. M.
Geng, L. S.
Gong, G. H.
Gou, Q. B.
Gu, M. H.
Guo, J. G.
Guo, X. L.
Guo, Y. Q.
Guo, Y. Y.
Han, Y. A.
He, H. H.
He, H. N.
He, J. C.
He, S. L.
He, X. B.
He, Y.
Heller, M.
Hor, Y. K.
Hou, C.
Hou X(侯贤)
Hu, H. B.
Hu, S.
Zheng, Y.
Hu, X. J.
Huang, D. H.
Huang, Q. L.
Huang, W. H.
Huang, X. T.
Huang, Z. C.
Ji, F.
Ji, X. L.
Jia, H. Y.
Jiang, K.
Jiang, Z. J.
Jin, C.
Kuleshov, D.
Levochkin, K.
Li, B. B.
Li, C.
Zhou, P.
Li, F.
Li, H. B.
Li, H. C.
Li, H. Y.
Li, J.
Li, K.
Li, W. L.
Li, X.
Zhu, H.
Li, X. R.
Li, Y.
Li, Y. Z.
Li, Z.
Zhou, R.
Liang, E. W.
Liang, Y. F.
Lin, S. J.
Liu, B.
Liu, C.
Liu, D.
Liu, H.
Liu, H. D.
Liu, J.
Liu, J. L.
Liu, J. S.
Liu, J. Y.
Liu, M. Y.
Liu, R. Y.
Liu, S. M.
Liu, W.
Liu, Y. N.
Liu, Z. X.
Long, W. J.
Lu, R.
Lv, H. K.
Ma, B. Q.
Ma, L. L.
Ma, X. H.
Mao JR(毛基荣)
Masood, A.
Mitthumsiri, W.
Montaruli, T.
Nan, Y. C.
Pang, B. Y.
Pattarakijwanich, P.
Pei, Z. Y.
Qi, M. Y.
Qiao, B. Q.
Ruffolo, D.
Rulev, V.
Sáiz, A.
Shao, L.
Shchegolev, O.
Sheng, X. D.
Shi, J. R.
Song, H. C.
Stenkin, Yu. V.
Stepanov, V.
Sun, Q. N.
Sun, X. N.
Sun, Z. B.
Tam, P. H.
Tang, Z. B.
Tian, W. W.
Wang, B. D.
Wang, C.
Wang, H.
Wang, H. G.
Wang JC(王建成)
http://ir.ynao.ac.cn:80/handle/114a53/25736
2023-01-23T07:33:16Z
2023-01-23T07:15:34Z
题名: Data analysis and key science results of LHAASO-WCDA
作者: Zha, Min; Gao, Chuandong; Hu, Shicong; Lin, Shujie; Wang, Zhen; Xiang, Guangman; Yao, Zhiguo; Zhou, Hao; Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao, Z.; Zhou, J. N.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.; Chen, J.; Chen, L.; Zhou, X. X.; Zhu, C. G.; Chen, M. J.; Chen, M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; della Volpe, D.; D’Ettorre Piazzoli, B.; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, Y. L.; Gao, B.; Goa, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou X(侯贤); Hu, H. B.; Hu, S.; Zheng, Y.; Hu, X. J.; Huang, D. H.; Huang, Q. L.; Huang, W. H.; Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, C.; Zhou, P.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.; Li, W. L.; Li, X.; Zhu, H.; Li, X. R.; Li, Y.; Li, Y. Z.; Li, Z.; Zhou, R.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao JR(毛基荣); Masood, A.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qiao, B. Q.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang JC(王建成)
摘要: <p>The Water Cherenkov Detector Array (WCDA) is an important component of Large High Altitude Air Shower Observatory (LHAASO). The main scientific target of WCDA is continuously surveying the northern sky at the level of few percent of Crab unit. In this proceeding, based on its first year data of WCDA-1 data, the result about the Crab Nebular observation and its energy spectrum measurment have been presented. And with WCDA full array data taking since Mar. 2021, some preliminary results have been reported. © Copyright owned by the author(s).</p>
2023-01-23T07:15:34Z
Gamma-ray performance study of the HERD payload
Adriani, O.
Alemanno, F.
Aloisio, R.
Altomare, C.
Ambrosi, G.
An, Q.
Antonelli, M.
Azzarello, P.
Bai, L.
Bai, Y. L.
Bao, T. W.
Barbanera, M.
Barbato, F. C.
Bernardini, P.
Berti, E.
Bertucci, B.
Bi, X. J.
Bigongiari, G.
Bongi, M.
Bonvicini, V.
Bordas, P.
Bosch-Ramon, V.
Bottai, S.
Brogi, P.
Cadoux, F.
Campana, D.
Cao, W. W.
Cao, Z.
Casaus, J.
Catanzani, E.
Cattaneo, P. W.
Chang, J.
Chang, Y. H.
Chen, G. M.
Chen, Y.
Cianetti, F.
Comerma, A.
Cortis, D.
Cui, X. H.
Cui, X. Z.
Dai, C.
Dai, Z. G.
D'Alessandro, R.
De Gaetano, S.
De Mitri, I.
de Palma, F.
Di Felice, V.
Di Giovanni, A.
Di Santo, M.
Di Venere, L.
Dong, J. N.
Dong, Y. W.
Donvito, G.
Duranti, M.
D'Urso, D.
Evoli, C.
Fang, K.
Fariña, L.
Favre, Y.
Feng, C. Q.
Feng, H.
Feng, H. B.
Feng, Z. K.
Finetti, N.
Formato, V.
Frieden, J. M.
Fusco, P.
Gao, J. R.
Gargano, F.
Gascon-Fora, D.
Gasparrini, D.
Giglietto, N.
Giovacchini, F.
Gomez, S.
Gong, K.
Gou, Q. B.
Guida, R.
Guo, D. Y.
Guo, J. H.
Guo, Y. Q.
He, H. H.
Hu, H. B.
Hu, J. Y.
Hu, P.
Hu, Y. M.
Huang, G. S.
Huang, J.
Huang, W. H.
Huang, X. T.
Huang, Y. B.
Huang, Y. F.
Ionica, M.
Jouvin, L.
Kotenko, A.
Kyratzis, D.
La Marra, D.
Li, M. J.
Li, Q. Y.
Li, R.
Li, S. L.
Li, T.
Li, X.
Li, Z.
Li, Z. H.
Liang, E. W.
Liang, M. J.
Liao, C. L.
Licciulli, F.
Lin, S. J.
Liu, D.
Liu, H. B.
Liu, H.
Liu, J. B.
Liu, S. B.
Liu, X.
Liu, X. W.
Liu, Y. Q.
Loparco, F.
Loporchio, S.
Lu, X.
Lyu, J. G.
Lyu, L. W.
Maestro, P.
Mancini, E.
Manera, R.
Marin, J.
Marrocchesi, P. S.
Marsella, G.
Martinez, G.
Martinez, M.
Marzullo, D.
Mauricio, J.
Mocchiutti, E.
Morettini, G.
Mori, N.
Mussolin, L.
Nicola Mazziotta, M.
Oliva, A.
Orlandi, D.
Osteria, G.
Pacini, L.
Panico, B.
Pantaleo, F. R.
Papa, S.
Papini, P.
Paredes, J. M.
Parenti, A.
Pauluzzi, M.
Pearce, M.
Peng, W. X.
Perfetto, F.
Perrina, C.
Perrotta, G.
Pillera, R.
Pizzolotto, C.
Qiao, R.
Qin, J. J.
Quadrani, L.
Quan, Z.
Rappoldi, A.
Raselli, G.
Ren, X. X.
Renno, F.
Ribo, M.
http://ir.ynao.ac.cn:80/handle/114a53/25721
2023-01-23T07:57:16Z
2023-01-16T10:32:26Z
题名: Gamma-ray performance study of the HERD payload
作者: Adriani, O.; Alemanno, F.; Aloisio, R.; Altomare, C.; Ambrosi, G.; An, Q.; Antonelli, M.; Azzarello, P.; Bai, L.; Bai, Y. L.; Bao, T. W.; Barbanera, M.; Barbato, F. C.; Bernardini, P.; Berti, E.; Bertucci, B.; Bi, X. J.; Bigongiari, G.; Bongi, M.; Bonvicini, V.; Bordas, P.; Bosch-Ramon, V.; Bottai, S.; Brogi, P.; Cadoux, F.; Campana, D.; Cao, W. W.; Cao, Z.; Casaus, J.; Catanzani, E.; Cattaneo, P. W.; Chang, J.; Chang, Y. H.; Chen, G. M.; Chen, Y.; Cianetti, F.; Comerma, A.; Cortis, D.; Cui, X. H.; Cui, X. Z.; Dai, C.; Dai, Z. G.; D'Alessandro, R.; De Gaetano, S.; De Mitri, I.; de Palma, F.; Di Felice, V.; Di Giovanni, A.; Di Santo, M.; Di Venere, L.; Dong, J. N.; Dong, Y. W.; Donvito, G.; Duranti, M.; D'Urso, D.; Evoli, C.; Fang, K.; Fariña, L.; Favre, Y.; Feng, C. Q.; Feng, H.; Feng, H. B.; Feng, Z. K.; Finetti, N.; Formato, V.; Frieden, J. M.; Fusco, P.; Gao, J. R.; Gargano, F.; Gascon-Fora, D.; Gasparrini, D.; Giglietto, N.; Giovacchini, F.; Gomez, S.; Gong, K.; Gou, Q. B.; Guida, R.; Guo, D. Y.; Guo, J. H.; Guo, Y. Q.; He, H. H.; Hu, H. B.; Hu, J. Y.; Hu, P.; Hu, Y. M.; Huang, G. S.; Huang, J.; Huang, W. H.; Huang, X. T.; Huang, Y. B.; Huang, Y. F.; Ionica, M.; Jouvin, L.; Kotenko, A.; Kyratzis, D.; La Marra, D.; Li, M. J.; Li, Q. Y.; Li, R.; Li, S. L.; Li, T.; Li, X.; Li, Z.; Li, Z. H.; Liang, E. W.; Liang, M. J.; Liao, C. L.; Licciulli, F.; Lin, S. J.; Liu, D.; Liu, H. B.; Liu, H.; Liu, J. B.; Liu, S. B.; Liu, X.; Liu, X. W.; Liu, Y. Q.; Loparco, F.; Loporchio, S.; Lu, X.; Lyu, J. G.; Lyu, L. W.; Maestro, P.; Mancini, E.; Manera, R.; Marin, J.; Marrocchesi, P. S.; Marsella, G.; Martinez, G.; Martinez, M.; Marzullo, D.; Mauricio, J.; Mocchiutti, E.; Morettini, G.; Mori, N.; Mussolin, L.; Nicola Mazziotta, M.; Oliva, A.; Orlandi, D.; Osteria, G.; Pacini, L.; Panico, B.; Pantaleo, F. R.; Papa, S.; Papini, P.; Paredes, J. M.; Parenti, A.; Pauluzzi, M.; Pearce, M.; Peng, W. X.; Perfetto, F.; Perrina, C.; Perrotta, G.; Pillera, R.; Pizzolotto, C.; Qiao, R.; Qin, J. J.; Quadrani, L.; Quan, Z.; Rappoldi, A.; Raselli, G.; Ren, X. X.; Renno, F.; Ribo, M.
摘要: <p>The High Energy cosmic-Radiation Detection (HERD) facility has been proposed as a space astronomy payload onboard the future China's Space Station. HERD is planned for operation starting around 2027 for about 10 years In addition to the unprecedented sensitivity for dark matter searches and cosmic-ray measurements up to the knee energy, it should perform gamma-ray monitoring and full sky survey from few hundred MeV up to tens of TeV. We present the first study of the HERD gamma-ray performance obtained with full simulations of the whole detector geometry. HERD will be a cubic detector composed with 5 active faces. We present a study conducted inside the HERD analysis software package, which includes a detailed description of the detector materials. In this work we present the HERD effective area, the point spread function and the resulting gamma-ray sensitivity. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)</p>
2023-01-16T10:32:26Z
Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Hou X(侯贤)
You, Y.
Ji, L.
Soria, R.
Zhang, S. N.
Ge, M. Y.
Tao, L.
Zhang, S.
Feng, H.
Zhou M(周明)
Tuo, Y. L.
Song, L. M.
Wang JC(王建成)
http://ir.ynao.ac.cn:80/handle/114a53/25711
2023-06-05T05:16:05Z
2023-01-16T08:34:27Z
题名: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
作者: Hou X(侯贤); You, Y.; Ji, L.; Soria, R.; Zhang, S. N.; Ge, M. Y.; Tao, L.; Zhang, S.; Feng, H.; Zhou M(周明); Tuo, Y. L.; Song, L. M.; Wang JC(王建成)
摘要: <p>Pulsating ultraluminous X-ray sources (PULXs) are accreting pulsars with apparent X-ray luminosity exceeding 10(39) erg s(-1). We perform Monte Carlo simulations to investigate whether a high collimation effect (or strong beaming effect) is dominant in the presence of accretion outflows, for the fan beam emission of the accretion column of the neutron stars in PULXs. We show that the three nearby PULXs (RX J0209.6-7427, Swift J0243.6+6124, and SMC X-3), namely, the Three Musketeers here, have their main pulsed emission not strongly collimated even if strong outflows exist. This conclusion can be extended to the current sample of extragalactic PULXs, if accretion outflows are commonly produced from them. This means that the observed high luminosity of PULXs is indeed intrinsic, which can be used to infer the existence of very strong surface magnetic fields of similar to 10(13-14) G, possibly multipole fields. However, if strong outflows are launched from the accretion disks in PULXs as a consequence of disk spherization by radiation pressure, regular dipole magnetic fields of similar to 10(12) G may be required, comparable to that of the Three Musketeers, which have experienced large luminosity changes from well below their Eddington limit (2 x 10(38) erg s(-1) for an NS) to super-Eddington and whose maximum luminosity fills the luminosity gap between Galactic pulsars and extragalactic PULXs.</p>
2023-01-16T08:34:27Z
A 3D Likelihood Analysis Tool for LHAASO-KM2A data
Cao, Zhen
Aharonian, F.
An, Q.
Axikegu
Bai, L. X.
Bai, Y. X.
Bao, Y. W.
Bastieri, D.
Bi, X. J.
Bi, Y. J.
Cai, H.
Cai, J. T.
Cao, Zhe
Chang, J.
Chang, J. F.
Chen, B. M.
Chen, E. S.
Chen, J.
Chen, Liang
Chen, Long
Chen, M. J.
Chen, M. L.
Chen, Q. H.
Chen, S. H.
Chen, S. Z.
Chen, T. L.
Chen, X. L.
Chen, Y.
Cheng, N.
Cheng, Y. D.
Cui, S. W.
Cui, X. H.
Cui, Y. D.
D'Ettorre Piazzoli, B.
Dai, B. Z.
Dai, H. L.
Dai, Z. G.
Danzengluobu
della Volpe, D.
Dong, X. J.
Duan, Kaikai
Fan, J. H.
Fan, Y. Z.
Fan, Z. X.
Fang, J.
Fang, K.
Feng, C. F.
Feng, L.
Feng, S. H.
Feng, Y. L.
Gao, B.
Gao, C. D.
Gao, L. Q.
Gao, Q.
Gao, W.
Ge, M. M.
Geng, L. S.
Gong, G. H.
Gou, Q. B.
Gu, M. H.
Guo, F. L.
Guo, J. G.
Guo, X. L.
Guo, Y. Q.
Guo, Y. Y.
Han, Y. A.
He, H. H.
He, H. N.
He, J. C.
He, S. L.
He, X. B.
He, Y.
Heller, M.
Hor, Y. K.
Hou, C.
Hou X(侯贤)
Hu, H. B.
Hu, S.
Hu, S. C.
Hu, X. J.
Huang, D. H.
Huang, Q. L.
Huang, W. H.
Huang, X. T.
Huang, Xiaoyuan
Huang, Z. C.
Ji, F.
Ji, X. L.
Jia, H. Y.
Jiang, K.
Jiang, Z. J.
Jin, C.
Ke, T.
Kuleshov, D.
Levochkin, K.
Li, B. B.
Li, Cheng
Li, Cong
Li, F.
Li, H. B.
Li, H. C.
Li, H. Y.
Li, Jian
Li, Jie
Li, K.
Li, W. L.
Li, X. R.
Li, Xin
Li, Y.
Li, Y. Z.
Li, Zhe
Li, Zhuo
Liang, E. W.
Liang, Y. F.
Lin, S. J.
Liu, B.
Liu, C.
Liu, D.
Liu, H.
Liu, H. D.
Liu, J.
Liu, J. L.
Liu, J. S.
Liu, J. Y.
Liu, M. Y.
Liu, R. Y.
Liu, S. M.
Liu, W.
Liu, Y.
Liu, Y. N.
Liu, Z. X.
Long, W. J.
Lu, R.
Lv, H. K.
Ma, B. Q.
Ma, L. L.
Ma, X. H.
Mao JR(毛基荣)
Masood, A.
Min, Z.
Mitthumsiri, W.
Montaruli, T.
Nan, Y. C.
Pang, B. Y.
Pattarakijwanich, P.
Pei, Z. Y.
Qi, M. Y.
Qi, Y. Q.
Qiao, B. Q.
Qin, J. J.
Ruffolo, D.
Rulev, V.
Sáiz, A.
Shao, L.
Shchegolev, O.
Sheng, X. D.
Shi, J. R.
Song, H. C.
Stenkin, Yu. V.
Stepanov, V.
Su, Y.
Sun, Q. N.
Sun, X. N.
Sun, Z. B.
Tam, P. H.
Tang, Z. B.
Tian, W. W.
Wang, B. D.
Wang, C.
Wang, H.
Wang, H. G.
Wang JC(王建成)
http://ir.ynao.ac.cn:80/handle/114a53/25701
2023-01-16T06:04:12Z
2023-01-13T08:14:47Z
题名: A 3D Likelihood Analysis Tool for LHAASO-KM2A data
作者: Cao, Zhen; Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, B. M.; Chen, E. S.; Chen, J.; Chen, Liang; Chen, Long; Chen, M. J.; Chen, M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; D'Ettorre Piazzoli, B.; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; della Volpe, D.; Dong, X. J.; Duan, Kaikai; Fan, J. H.; Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, F. L.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou X(侯贤); Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.; Huang, W. H.; Huang, X. T.; Huang, Xiaoyuan; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Ke, T.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, Cheng; Li, Cong; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, Jian; Li, Jie; Li, K.; Li, W. L.; Li, X. R.; Li, Xin; Li, Y.; Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao JR(毛基荣); Masood, A.; Min, Z.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang JC(王建成)
摘要: <p>The square kilometer array (KM2A) is the main array of the Large High Altitude Air Shower Observatory (LHAASO), which is the most sensitive gamma-ray detector for energies above a few tens of TeV. We are developing a software pipeline based on the experimental data, Monte-Carlo simulations and the pointing track of the arrays. The pipeline is able to perform 3D (sky images at different energies) fits of KM2A data, similar to those used for Fermi-LAT and DAMPE gamma-ray analysis. This 3D likelihood analysis could fit source models of arbitrary morphology to the sky images, and get energy spectra information and detection significances simultaneously. The analysis with this software could give consistent results with those using traditional method. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)</p>
2023-01-13T08:14:47Z