Flat Spectrum(平谱)研究综述
Flat Spectrum 平谱 - We also find that the thermal noise of the mechanical oscillator is enhanced at low frequencies relative to the vacuum noise, while having a flat spectrum at high frequencies. [1] Birds trained on harmonic spectrum generalized their discrimination to vocoded sounds, and birds trained on pitch generalized their discrimination to harmonic sounds with a flat spectrum. [2] At low frequencies, this direct contribution also has a flat spectrum but with a much smaller amplitude than the memory part. [3] In fact, noise presents a flat spectrum with large time-frequency supports, while signal components are narrow energy ridges. [4] By grinding these R/Y/G/B MOF⊃dye powders and adjusting the mass proportions of each primary-colour component, a white light emission with a quasi-flat spectrum is obtained. [5] Due to its properties of flat spectrum and fast generation the Orthogonal-Frequency Division Multiplexing (OFDM) technique for EIS represents an efficient and a low foot-print alternative compared to the classical sweep frequency technique. [6] The modeled peak flux of radio emission and the flat spectrum are generally consistent with the observations. [7] These observations reveal a flat spectrum over this frequency range with spectral index $\alpha \approx -0. [8] The results demonstrate that with the joint effects of phase modulation-induced spectrum expansion and nonlinear filtering of delayed interference, wideband chaos with flat spectrum and excellent TDS suppression characteristics can be generated over a wide dynamic operation range. [9] The source exhibits a flat spectrum from 600 nm to 1880 nm at -10 dB level except for the residual pump peak. [10] Coherent broadband sources with flat spectrum are usually generated the supercontinuum from a highly nonlinear fibre [2]. [11] 1 Jy, under the assumption of a flat spectrum and wide bandwidth. [12] Conventional techniques deal with phase-based RF cancellation which inherently results in non-flat spectrum (especially for wideband signals). [13] 8 W with a flat spectrum from 480 nm to 2100 nm at the $-$ 10 dB level, except for the residual pump peak. [14] Spectral index maps of the eight frEGGs were constructed, showing a flat spectrum in radio frequencies in general. [15] Our numerical results indicate that, as a direct result of the spectral expansion effect of the sinusoidal phase modulation and the phase-to-intensity conversion effect of the dispersive component, the original chaotic carrier can be encrypted as an uncorrelated chaotic signal with a flat spectrum and an efficiently-suppressed time delay signature, this greatly enhances the privacy of the modulated chaotic carrier. [16] This is based on our intranight optical monitoring of a well-defined sample of 10 candidates selected on the criteria of a flat spectrum and an abnormally high linear polarization at radio wavelengths. [17]我们还发现，相对于真空噪声，机械振荡器的热噪声在低频处增强，而在高频处具有平坦的频谱。 [1] 受过谐波频谱训练的鸟类将它们的辨别力推广到声码声音，而受过音高训练的鸟类将它们的辨别力推广到具有平坦频谱的谐波声音。 [2] 在低频下，这种直接贡献也具有平坦的频谱，但幅度比存储部分小得多。 [3] 事实上，噪声呈现出具有大时频支持的平坦频谱，而信号分量是狭窄的能量脊。 [4] 通过研磨这些R/Y/G/B MOF⊃染料粉末并调整各原色组分的质量比例，得到具有准平坦光谱的白光发射。 [5] 由于其平坦的频谱和快速生成的特性，用于 EIS 的正交频分复用 (OFDM) 技术与经典的扫频技术相比是一种高效且占用空间小的替代方案。 [6] 模拟的无线电发射峰值通量和平坦频谱与观测结果基本一致。 [7] 这些观察结果揭示了该频率范围内的平坦频谱，频谱指数 $\alpha \ 约 -0。 [8] 结果表明，在相位调制引起的频谱扩展和延迟干扰的非线性滤波的共同作用下，可以在较宽的动态工作范围内产生具有平坦频谱和优异 TDS 抑制特性的宽带混沌。 [9] 该光源在 -10 dB 水平下呈现出从 600 nm 到 1880 nm 的平坦光谱，但残余泵峰除外。 [10] 具有平坦光谱的相干宽带源通常由高度非线性光纤产生超连续谱 [2]。 [11] 1 Jy，在平坦频谱和宽带宽的假设下。 [12] 传统技术处理基于相位的 RF 消除，这固有地导致非平坦频谱（特别是对于宽带信号）。 [13] 8 W，从 480 nm 到 2100 nm 的平坦光谱在 $-$ 10 dB 电平，残余泵峰除外。 [14] 构建了 8 个 frEGG 的频谱索引图，总体上显示了无线电频率的平坦频谱。 [15] 我们的数值结果表明，由于正弦相位调制的频谱扩展效应和色散分量的相位到强度转换效应的直接结果，原始混沌载波可以被加密为具有平坦频谱的不相关混沌信号和有效抑制的时间延迟签名，这极大地增强了调制混沌载波的隐私。 [16] 这是基于我们对根据平坦光谱和无线电波长异常高线性极化标准选择的 10 个候选者的定义明确的样本的夜间光学监测。 [17]
synchrotron peak frequency 同步加速器峰值频率
the synchrotron radiation and inverse Compton radiation, which can be simply separated by these fitting curves; (2) the higher the synchrotron peak frequency of the source, the greater the synchrotron radiation component, and the less the inverse Compton radiation component; (3) at 1 keV of the X-ray waveband, the synchrotron radiation component accounts for 17%, 27%, and 73% of the total X-ray emission, for FSRQs (Flat Spectrum Radio Quasars), LBLs (Low synchrotron peak frequency BL Lac objects), and HBLs (High synchrotron peak frequency BL Lac objects), respectively; (4) there is a strong positive correlation between the synchrotron peak frequency and the synchrotron radiation flux density at 1 keV, while no correlation exists between the synchrotron peak frequency and the inverse Compton radiation flux density; (5) the radiation mechanism of LBLs may be similar to that of FSRQs in the X-ray waveband. [1] Radio-loud jets are largely divided into classes based on the angle of observation (blazars versus radio galaxies), spectral line widths (Flat Spectrum Radio Quasars/FSRQs versus BL Lac objects/BL Lacs), and location of the synchrotron peak frequency in their spectral energy distribution (high-spectral peaked/HSP, intermediate-spectral peaked/ISP, or low-spectral peaked/LSP). [2]同步辐射和逆康普顿辐射，可以通过这些拟合曲线简单地分开； (2)源的同步辐射峰值频率越高，同步辐射分量越大，逆康普顿辐射分量越小； (3) 在 X 射线波段 1 keV 处，同步辐射分量占 X 射线总发射量的 17%、27% 和 73%，对于 FSRQs（平谱射电类星体）、LBLs（低同步辐射峰频率 BL Lac 物体）和 HBLs（高同步加速器峰值频率 BL Lac 物体）； (4) 1 keV时同步加速器峰值频率与同步加速器辐射通量密度呈强正相关，而同步加速器峰值频率与逆康普顿辐射通量密度之间不存在相关性； (5) LBLs在X射线波段的辐射机制可能与FSRQs相似。 [1] 射电大喷流主要根据观察角度（耀变体与射电星系）、谱线宽度（平面光谱射电类星体/FSRQ 与 BL Lac 天体/BL Lac）以及同步加速器峰值频率在它们中的位置分为几类。光谱能量分布（高光谱峰化/HSP，中光谱峰化/ISP，或低光谱峰化/LSP）。 [2]
Relatively Flat Spectrum 相对平坦的频谱
The dissipative soliton is generated by a passively mode-locked erbium-doped fiber laser with a net positive group-velocity dispersion in the cavity, which has a large energy spectral density and a relatively flat spectrum with steep edges. [1] This cluster hosts a relatively flat spectrum ($\alpha^{610}_{235}\sim -1. [2]耗散孤子由被动锁模掺铒光纤激光器产生，腔内具有净正群速度色散，具有较大的能谱密度和较平坦的光谱，具有陡峭的边缘。 [1] 这个集群拥有一个相对平坦的频谱 ($\alpha^{610}_{235}\sim -1. [2]
flat spectrum radio 平面频谱无线电
The derived photon spectra display characteristic features observed in both BL Lac sources and flat spectrum radio quasars, with the distinction made by varying the strength of the external photon fields, the jet magnetization, and the number of pairs per proton contained within. [1] We have monitored the flat spectrum radio quasar, 3C 279, in the optical $B$, $V$, $R$ and $I$ passbands from 2018 February to 2018 July for 24 nights, with a total of 716 frames, to study flux, colour and spectral variability on diverse timescales. [2] the synchrotron radiation and inverse Compton radiation, which can be simply separated by these fitting curves; (2) the higher the synchrotron peak frequency of the source, the greater the synchrotron radiation component, and the less the inverse Compton radiation component; (3) at 1 keV of the X-ray waveband, the synchrotron radiation component accounts for 17%, 27%, and 73% of the total X-ray emission, for FSRQs (Flat Spectrum Radio Quasars), LBLs (Low synchrotron peak frequency BL Lac objects), and HBLs (High synchrotron peak frequency BL Lac objects), respectively; (4) there is a strong positive correlation between the synchrotron peak frequency and the synchrotron radiation flux density at 1 keV, while no correlation exists between the synchrotron peak frequency and the inverse Compton radiation flux density; (5) the radiation mechanism of LBLs may be similar to that of FSRQs in the X-ray waveband. [3] The flat spectrum radio quasar 3C 279 is known to exhibit pronounced variability in the high-energy (100 MeV 100 GeV) γ-ray domain. [4] We report on results of a multi-band monitoring campaign from radio to gamma rays of the high-redshift flat spectrum radio quasar S5 0836+710 during a high activity period detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. [5] We present the jet kinematics of the flat spectrum radio quasar (FSRQ) 4C +21. [6] Almost 10 yr of $\gamma$-ray observations with the Fermi Large Area Telescope (LAT) have revealed extreme $\gamma$-ray outbursts from flat spectrum radio quasars (FSRQs), temporarily making these objects the brightest $\gamma$-ray emitters in the sky. [7] For the blazar sub-class of flat spectrum radio quasars, these data provide measurements of the main emission lines and of the underlying continuum. [8] No preference for either $m$ is found in flat spectrum radio quasars. [9] We performed a long-term optical (B, V, R bands), infra-red (J and K bands) and radio band (15, 22, 37 GHz band) study on the flat spectrum radio quasar, 3C 454. [10] A comparison of the broadband parameters derived from the SED modeling reveals the similarity of $\gamma$-NLSy1 objects with blazars, in particular more with flat spectrum radio quasars. [11] PKS J1222$+$0413 has a much greater black hole mass than most other NLS1s, $M_\mathrm{BH}\approx2\times10^{8}$ M$_\odot$, similar to those found in flat spectrum radio quasars (FSRQs). [12] These blazars are classified following a two-fold approach i) according to the strength of their optical lines as Flat Spectrum Radio Quasars, FSRQs, BL Lac-type objects, BL Lacs, or blazar candidates of unknown types, BCUs and ii) according to the position of their synchrotron peak, using archival data as low-, intermediateor high-synchrotron peaked objects, LSPs, ISPS and HSPs respectively. [13] We study the properties of the innermost jet of the flat spectrum radio quasar 1633+382 (4C~38. [14] We present a long term light curve (LC) of the flat spectrum radio quasar (FSRQ) 4C +21. [15] We discuss the EBL level obtained from the spectra of both BL Lacs and flat spectrum radio quasars (FSRQ) in order to investigate the impact of internal absorption in different classes of objects. [16] However, the broad band spectral energy distribution of the gamma-ray emitting NLS1s are found to be similar to flat spectrum radio quasars. [17] This is a gamma ray loud FSRQ (flat spectrum radio quasar) with a redshift of z = 0. [18] Twenty-six of these radio-loud quasars are identified as Flat Spectrum Radio Quasars (FSRQs) and fifty-four are identified as Steep Spectrum Radio Quasars (SSRQs) based on their radio spectral index. [19] We present a phenomenological method for predicting the number of Flat Spectrum Radio Quasars (FSRQs) that should be detected by upcoming Square Kilometer Array (SKA) SKA1-MID Wide Band 1 and Medium-Deep band 2 surveys. [20] This construction is applied to multiwavelength flares of the flat spectrum radio quasar 3C 279, fitting snap-shot SEDs and generating light curves that are consistent with observed variability timescales. [21] We present an in-depth and systematic analysis of a sample of 20 powerful blazars, including 12 BL Lacs and 8 flat spectrum radio quasars, utilizing Fermi/LAT observations from the period 2008--2018 using various analysis tools such as flux distribution, symmetry analysis, and time series analysis. [22] Additionally, under the assumption that the majority of these sources are blazars, three machine-learning algorithms are employed to classify the sample into flat spectrum radio quasars or BL Lacertae objects. [23] Radio-loud jets are largely divided into classes based on the angle of observation (blazars versus radio galaxies), spectral line widths (Flat Spectrum Radio Quasars/FSRQs versus BL Lac objects/BL Lacs), and location of the synchrotron peak frequency in their spectral energy distribution (high-spectral peaked/HSP, intermediate-spectral peaked/ISP, or low-spectral peaked/LSP). [24] The flat spectrum radio quasar PKS 1510-089 is a monitored target in many wavelength bands due to its high variability. [25] We present an optical variability study of 44 newly identified blazar candidates behind the Magellanic Clouds, including 27 flat spectrum radio quasars (FSRQs) and 17 BL Lacertae objects (BL Lacs). [26] In this two-jet model (the origin of the spine-sheath jet structure), protected by the SAD jet, the fast and narrow SE jet inside the slow and broad SAD jet generates the VHE (very high energy ≥ 100 GeV) Synchrotron Self Compton (SSC) gamma-ray emission without the attenuation by the photons in the BLR (broad line region) of flat spectrum radio quasar (FSRQ). [27] We confirm the BL Lac nature of 23 sources, and the flat spectrum radio quasar nature of other 7 ones. [28] Using the gamma-ray luminosity functions for blazars including flat spectrum radio quasars (FSRQs) and BL Lac objects, as well as the $Fermi$-LAT detection efficiency, we estimate contributions from {blazars resolved by $Fermi$-LAT as well as the unresolved counterpart. [29] The flat spectrum radio quasar CTA 102 ( z = 1. [30]衍生的光子光谱显示了在 BL Lac 源和平面光谱射电类星体中观察到的特征，其区别是通过改变外部光子场的强度、射流磁化强度和其中包含的每个质子对数来区分的。 [1] 我们从 2018 年 2 月到 2018 年 7 月在光学 $B$、$V$、$R$ 和 $I$ 通带中监测了平面频谱无线电类星体 3C 279 24 晚，共 716 帧，以研究不同时间尺度上的通量、颜色和光谱变化。 [2] 同步辐射和逆康普顿辐射，可以通过这些拟合曲线简单地分开； (2)源的同步辐射峰值频率越高，同步辐射分量越大，逆康普顿辐射分量越小； (3) 在 X 射线波段 1 keV 处，同步辐射分量占 X 射线总发射量的 17%、27% 和 73%，对于 FSRQs（平谱射电类星体）、LBLs（低同步辐射峰频率 BL Lac 物体）和 HBLs（高同步加速器峰值频率 BL Lac 物体）； (4) 1 keV时同步加速器峰值频率与同步加速器辐射通量密度呈强正相关，而同步加速器峰值频率与逆康普顿辐射通量密度之间不存在相关性； (5) LBLs在X射线波段的辐射机制可能与FSRQs相似。 [3] 众所周知，平谱射电类星体 3C 279 在高能 (100 MeV 100 GeV) γ 射线域中表现出明显的可变性。 [4] nan [5] 我们介绍了平面频谱射电类星体 (FSRQ) 4C +21 的射流运动学。 [6] 费米大面积望远镜 (LAT) 近 10 年的 $\gamma$ 射线观测揭示了平谱射电类星体 (FSRQ) 的极端 $\gamma$ 射线爆发，暂时使这些天体成为最亮的 $\gamma$-天空中的射线发射器。 [7] 对于平坦频谱射电类星体的耀变体子类，这些数据提供了对主要发射线和潜在连续体的测量。 [8] 在平坦频谱无线电类星体中没有发现对任何一个 $m$ 的偏好。 [9] 我们对平坦频谱无线电类星体 3C 454 进行了长期光学（B、V、R 波段）、红外线（J 和 K 波段）和无线电波段（15、22、37 GHz 波段）研究。 [10] 对从 SED 建模导出的宽带参数的比较揭示了 $\gamma$-NLSy1 物体与耀变体的相似性，尤其是与平谱射电类星体的相似性。 [11] PKS J1222$+$0413 的黑洞质量比大多数其他 NLS1 大得多，$M_\mathrm{BH}\approx2\times10^{8}$M$_\odot$，类似于在平谱射电类星体中发现的那些（ FSRQ）。 [12] 这些耀变体按照两种方法分类 i) 根据其光线的强度为平面光谱射电类星体、FSRQ、BL Lac 型天体、BL Lac 或未知类型的耀变体候选者、BCU 和 ii) 根据它们的同步加速器峰值的位置，使用档案数据分别作为低、中或高同步加速器峰值对象、LSP、ISPS 和 HSP。 [13] 我们研究了平谱射电类星体 1633+382 (4C~38. [14] 我们提出了平面光谱射电类星体 (FSRQ) 4C +21 的长期光变曲线 (LC)。 [15] 我们讨论了从 BL Lacs 和平谱射电类星体 (FSRQ) 的光谱中获得的 EBL 水平，以研究不同类别物体的内部吸收的影响。 [16] 然而，发现发射伽马射线的 NLS1 的宽带光谱能量分布与平谱射电类星体相似。 [17] 这是一个伽马射线响亮的 FSRQ（平谱射电类星体），红移 z = 0。 [18] 这些无线电响亮的类星体中有 26 个被确定为平谱射电类星体 (FSRQ)，54 个根据其射电频谱指数被确定为陡谱射电类星体 (SSRQ)。 [19] 我们提出了一种现象学方法，用于预测即将到来的平方公里阵列 (SKA) SKA1-MID 宽带 1 和中深带 2 调查应检测到的平面频谱无线电类星体 (FSRQ) 的数量。 [20] 这种结构适用于平面光谱射电类星体 3C 279 的多波长耀斑，拟合快照 SED 并生成与观测到的可变时间尺度一致的光曲线。 [21] nan [22] 此外，在这些来源中的大多数是耀变体的假设下，使用三种机器学习算法将样本分类为平坦频谱无线电类星体或 BL Lacertae 物体。 [23] 射电大喷流主要根据观察角度（耀变体与射电星系）、谱线宽度（平面光谱射电类星体/FSRQ 与 BL Lac 天体/BL Lac）以及同步加速器峰值频率在它们中的位置分为几类。光谱能量分布（高光谱峰化/HSP，中光谱峰化/ISP，或低光谱峰化/LSP）。 [24] 平谱射电类星体 PKS 1510-089 由于其高度可变性而成为许多波段的监测目标。 [25] nan [26] 在这个由 SAD 射流保护的双射流模型（脊鞘射流结构的起源）中，慢而宽的 SAD 射流内部的快速狭窄 SE 射流产生 VHE（非常高能量 ≥ 100 GeV）同步加速器自康普顿 (SSC) 伽马射线发射没有被平谱射电类星体 (FSRQ) 的 BLR（宽线区域）中的光子衰减。 [27] 我们确认了 23 个源的 BL Lac 性质，以及其他 7 个源的平谱无线电类星体性质。 [28] 使用包括平谱射电类星体 (FSRQ) 和 BL Lac 天体在内的耀变体的伽马射线光度函数，以及 $Fermi$-LAT 探测效率，我们估计了由 $Fermi$-LAT 解析的耀变体的贡献以及未解决的对应物。 [29] 平谱射电类星体 CTA 102 ( z = 1. [30]