Astrophysical Bulletin最新文献_第3页

Spectral Types of Long-Period Double-Lined Eclipsing Binary System Components from Low-Resolution Spectroscopy Data 从低分辨率光谱数据看长周期双线食双星系统成分的光谱类型

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323700177

A. Yu. Kniazev, I. Yu. Katkov, O. Yu. Malkov, L. N. Berdnikov, N. I. Shatsky, A. V. Dodin, S. G. Zheltouhov, I. A. Strahov

Abstract

We present the results of spectral observations and consequent analysis of six long-period double-lined eclipsing binaries (DLEBs) with main-sequence (MS) components from a sample formed with the aim of testing the ‘‘mass–luminosity’’ relation (MLR) for stars in the (M/M_{odot}>1.5) mass range. We analyzed all the obtained spectra using a technique that allows one to reveal the binary nature of the system and determine (T_{textrm{eff}}) and (log g) for each component, as well as the system metallicity [Fe/H] and line-of-sight extinction (E(B-V)). We computed the absolute parameters of the systems under consideration. An analysis of the obtained spectra shows that for three of the six objects (V1156 Cyg, EU Gem and V733 Per) we can clearly establish their binary nature and determine the spectral type and class for each component. Both components of the V733 Per system have already left the MS, and therefore the system must be excluded from our sample, whereas studies of V1156 Cyg and EU Gem should continue. OT And did not demonstrate a binary spectrum, however, the main component of the system is a hot A6 V star, and therefore, OT And should remain in our sample. We also revealed no binarity in the IM Del and LX Gem systems. Their brighter components turned out to be a cool giant and a supergiant, and these systems should be excluded from the sample based on the results of our analysis. We used the same technique to analyze the two spectra obtained for systems EU Gem and LX Gem using LAMOST. We have shown that the parameters determined from LAMOST spectra are in good agreement with the parameters determined for spectra obtained at the Caucasian Mountain Observatory (CMO) of SAI MSU. Our analysis allowed us to plot a first approximation of the V1156 Cyg velocity curves and show that the cool component in this system has a larger mass.

AbstractWe present the results of spectral observations and consequent analysis of six longperiod double-lined eclipsing binaries (DLEBs) with main-sequence (MS) components from a sample formed in the aim of testing the 'mass-luminosity' relation (MLR) for stars in the (M_/Modot}>1.5) mass range.我们使用一种可以揭示系统双星性质的技术分析了所有获得的光谱，并确定了每个成分的(T_{textrm{eff}})和(log g) 以及系统的金属性[Fe/H]和视线消光(E(B-V))。我们计算了所考虑系统的绝对参数。对所获光谱的分析表明，对于六个天体中的三个（V1156 Cyg、EU Gem和V733 Per），我们可以清楚地确定它们的双星性质，并确定每个成分的光谱类型和类别。V733 Per 系统的两个成分都已经离开了 MS，因此该系统必须从我们的样本中剔除，而对 V1156 Cyg 和 EU Gem 的研究则应继续进行。OT And没有显示出双星光谱，但该系统的主要成分是一颗热的A6 V恒星，因此OT And应该保留在我们的样本中。在 IM Del 和 LX Gem 系统中，我们也没有发现双星。它们的亮成分分别是一颗冷巨星和一颗超巨星，根据我们的分析结果，这些系统应该被排除在样本之外。我们使用同样的技术，利用 LAMOST 分析了 EU Gem 和 LX Gem 系统获得的两段光谱。结果表明，从 LAMOST 光谱中确定的参数与在 MSU 高加索山天文台（CMO）获得的光谱中确定的参数非常吻合。通过分析，我们绘制出了 V1156 Cyg 速度曲线的第一近似值，并表明该系统中的冷成分质量较大。

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引用次数: 0

ESPriF: the Echelle-Spectropolarimeter of the BTA Primary Focus. Correction of Low-Frequency Variations in the Star Image ESPriF：BTA 主焦点的 Echelle 光谱仪。校正星像中的低频变化

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323700220

M. V. Yushkin, E. V. Emelianov, Yu. B. Verich, V. E. Panchuk

Abstract

The development of a corrector for low-frequency variations in the star image at the input of ESPriF—the echelle spectropolarimeter of the BTA primary focus—is reported. New technical solutions have made it possible to extend the operating frequency range to 10 Hz for stars brighter than (13^{mathrm{m}}).

摘要报告了针对 BTA 主焦点的 Echelle 分光测极计 ESPriF 输入端恒星图像中的低频变化而开发的校正器。新的技术解决方案使得将亮度大于 (13^{mathrm{m}} 的恒星的工作频率范围扩展到 10 Hz 成为可能。）

引用次数: 0

RFI-Resistant Decimeter Band Radiometer for the RATAN-600 Radio Telescope 用于 RATAN-600 射电望远镜的抗射频干扰十米波段辐射计

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323600291

A. M. Ripak, V. M. Bogod, S. A. Grenkov, M. K. Lebedev

Abstract

The development of methods for the radio frequency interference mitigation becomes a fundamental challenge for any radio astronomy research. In this paper, we report on the development and creation of a new spectrometer designed for solar observations at the RATAN-600 radio telescope, capable of excising radio interference using a statistical algorithm based on the spectral kurtosis estimation. The implementation of the external analog interface and the operation of the digital signal processing system based on the FPGA are described. The maximum spectral resolution reached is 122 kHz in the frequency band of 1.0–3.0 GHz. The output spectrum has from 64 to 8192 frequency bins, depending on the requirements of the observer, the output rate is 120 spectra per second. The test results and the first observations of the Sun show that the research method can successfully detect and suppress interference from most of the local radio interference sources.

摘要无线电频率干扰缓解方法的开发成为任何射电天文学研究的基本挑战。在本文中，我们报告了为在 RATAN-600 射电望远镜上观测太阳而设计的新型光谱仪的开发和创建情况，该光谱仪能够使用基于光谱峰度估计的统计算法来消除射电干扰。文中介绍了外部模拟接口的实现和基于 FPGA 的数字信号处理系统的运行。在 1.0-3.0 GHz 频段内，达到的最大频谱分辨率为 122 kHz。根据观测者的要求，输出频谱有 64 至 8192 个频段，输出速率为每秒 120 个频谱。测试结果和对太阳的首次观测表明，该研究方法可以成功地探测和抑制来自大多数本地无线电干扰源的干扰。

引用次数: 0

The Influence of the Bar on the Dynamics of Globular Clusters in the Central Region of the Milky Way. Frequency Analysis of Orbits According to Gaia EDR3 Data 条带对银河系中央区域球状星团动力学的影响。根据盖亚 EDR3 数据进行的轨道频率分析

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s199034132360028x

A. T. Bajkova, A. A. Smirnov, V. V. Bobylev

Abstract

This work is devoted to studying the influence of the bar on the orbital dynamics of globular clusters. The orbits of 45 globular clusters in the central galactic region with a radius of 3.5 kpc were analyzed using spectral dynamics methods in order to identify objects captured by the bar. To form the 6D phase space required for orbit integration, the most accurate astrometric data to date from the Gaia satellite (EDR3), as well as new refined average distances to globular clusters, were used. Since the parameters of the Milky Way bar are known with very great uncertainty, the orbits were constructed and their frequency analysis was carried out by varying the mass, length and angular velocity of rotation of the bar in a wide range of values with a fairly small step. The integration of orbits was carried out at 2.5 billion years ago. As a result, bar-supporting globular clusters were identified for each set of bar parameters. For the first time, an analytical expression has been obtained for the dependence of the dominant frequency (f_{X}) on the angular velocity of rotation of the bar. In addition, the probabilities of globular clusters being captured by the bar were determined when the bar parameters were varied in certain ranges of values according to a random distribution law. A list of 14 globular clusters with the most significant capture probabilities is given, with five GCs—NGC 6266, NGC 6569, Terzan 5, NGC 6522, NGC 6540—showing the probability of capture by the bar (Pgeq 0.2). A conclusion is made about the regularity of the orbits of globular clusters based on the calculation of approximations of the maximum characteristic Lyapunov exponents.

摘要这项工作致力于研究条带对球状星团轨道动力学的影响。利用光谱动力学方法分析了半径为3.5 kpc的银河系中心区域45个球状星团的轨道，以确定被条带捕获的天体。为了形成轨道整合所需的 6D 相空间，使用了盖亚卫星（EDR3）迄今为止最精确的天体测量数据，以及新改进的球状星团平均距离。由于已知的银河棒参数具有很大的不确定性，因此在构建轨道时，通过以相当小的步长在很大的数值范围内改变银河棒的质量、长度和旋转角速度，对其进行了频率分析。轨道的整合是在 25 亿年前进行的。结果，在每一组棒状参数中都发现了支持棒状的球状星团。我们首次获得了主频 (f_{X})对棒状体旋转角速度的分析表达式。此外，还根据随机分布定律确定了当棒参数在一定范围内变化时，球状星团被棒捕获的概率。给出了14个俘获概率最大的球状星团的列表，其中5个球状星团--NGC 6266、NGC 6569、Terzan 5、NGC 6522和NGC 6540--被棒俘获的概率为(Pgeq 0.2)。根据对最大特征Lyapunov指数的近似计算，得出了球状星团轨道的规律性结论。

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引用次数: 0

Dependence of Solar Supergranular Lifetime on Surface Magnetic Activity and Rotation 太阳超晶粒寿命与表面磁活动和自转的关系

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323600138

G. M. Sowmya, G. Rajani, U. Paniveni, R. Srikanth

Abstract

The lifetimes and length-scales for supergranular cells in active and quiescent regions of the solar chromosphere, and the relation between the two, were studied using a time series of Ca II K filtergrams. The lifetimes, in contrast to supergranular length scale and fractal dimension, show no significant dependence on solar latitude, suggesting that cell lifetimes are independent of the differential rotation and a possible supergranular super-rotation. The functional form of the relation was obtained guided by a comparison of the distributions of the two supergranular parameters. We infer a linear dependence of cell lifetime on area, which can be understood by the assumption of the network’s evolution via a diffusion of the magnetic field. Our analysis suggests that the diffusion rate in quiet regions is about 10(%) greater than in active regions.

摘要利用 Ca II K 滤波图时间序列研究了太阳色球活动区和静止区超晶粒单元的寿命和长度尺度，以及两者之间的关系。与超晶粒长度尺度和分形维度相反，寿命与太阳纬度没有明显的关系，这表明晶胞寿命与差转和可能的超晶粒超转无关。这种关系的函数形式是通过比较两个超晶粒参数的分布得出的。我们推断细胞寿命与面积呈线性关系，这可以通过假定网络的演化是通过磁场的扩散来理解的。我们的分析表明，安静区域的扩散率要比活跃区域的扩散率大10%左右。

引用次数: 0

Optical and Radio Variability of the Blazar S4 0954+658 耀星 S4 0954+658 的光学和射电变异性

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323600229

V. V. Vlasyuk, Yu. V. Sotnikova, A. E. Volvach, O. I. Spiridonova, V. A. Stolyarov, A. G. Mikhailov, Yu. A. Kovalev, Y. Y. Kovalev, M. L. Khabibullina, M. A. Kharinov, L. Yang, M. G. Mingaliev, T. A. Semenova, P. G. Zhekanis, T. V. Mufakharov, R. Yu. Udovitskiy, A. A. Kudryashova, L. N. Volvach, A. K. Erkenov, A. S. Moskvitin, E. V. Emelianov, T. A. Fatkhullin, P. G. Tsybulev, N. A. Nizhelsky, G. V. Zhekanis, E. V. Kravchenko

Abstract

We present an optical-to-radio study of the BL Lac objectS4 0954+658 observations during 1998–2023. The measurements wereobtained with the SAO RAS Zeiss-1000 and AS-500/2 0.5-m telescopesin 2003–2023, with the RATAN-600 radio telescope at 1.25 (0.96,1.1), 2.3, 4.7 (3.7, 3.9), 8.2 (7.7), 11.2, 22.3 (21.7) GHz in1998–2023, with the IAA RAS RT-32 Zelenchukskaya and Badarytelescopes at 5.05 and 8.63 GHz in 2020–2023, and with the RT-22single-dish telescope of CrAO RAS at 36.8 GHz in 2009–2023. Inthis period the blazar was showing extremely high broadbandactivity with the variability amplitude of the flux densities upto 70–100(%) both in the optical and radio domains. During theperiod of 2014–2023 the blazar displayed extremely high activityin the radio wavelengths, and we detected multiple radio flares ofvarying amplitude and duration. The large flares last on averagefrom 0.3 to 1 year at 22–36.8 GHz and slightly longer at5–11.2 GHz. The optical flares are shorter and last 7–50 days.The characteristic time scale (tau) of variation at 5–22 GHz isabout 100 days in the most active epoch of 2014–2023 and about1000 days for the state with lower activity in 2009–2014. Wefound a general correlation between the optical, radio, and(gamma)-ray flux variations, which suggesting that we observe thesame photon population from different emission regions. Weestimated the linear size of this region as 0.5–2 pc fordifferent conditions. A broadband radio spectrum with twocomponents of the S4 0954+658 jet was modeled using bothelectrons and protons as emitting particles. The results suggestthat the synchrotron radio waves in this AGN may be produced byrelativistic protons.

摘要我们介绍了1998-2023年间对BL Lac天体S4 0954+658的光学-无线电研究观测结果。这些观测数据是在2003-2023年期间利用SAO RAS Zeiss-1000和AS-500/2 0.5米望远镜、RATAN-600射电望远镜在1.25 (0.96,1.1), 2.3, 4.7 (3.7, 3.9), 8.2 (7.7), 11.2, 22.在 1998-2023 年期间，将使用国际宇航科学院 RAS RT-32 Zelenchukskaya 和 Badaryt 望远镜，频率为 5.05 和 8.63 千兆赫；在 2009-2023 年期间，将使用克拉奥 RAS 的 RT-22 单碟望远镜，频率为 36.8 千兆赫。在此期间，该炽星在光学和射电领域都显示出极高的宽带活动性，通量密度的变异幅度高达70-100（%）。在2014-2023年期间，该星在射电波段显示出极高的活动性，我们探测到了多个不同振幅和持续时间的射电耀斑。大耀斑在22-36.8千兆赫波段平均持续0.3-1年，在5-11.2千兆赫波段持续时间稍长。在2014-2023年最活跃的纪元，5-22 GHz的特征变化时间尺度约为100天，而在2009-2014年较低活跃度的状态下约为1000天。我们发现光学、射电和（gamma）-射线通量变化之间存在普遍的相关性，这表明我们观测到了来自不同发射区的相同光子群。在不同条件下，我们估计这个区域的线性大小为0.5-2 pc。使用双电子和质子作为发射粒子，模拟了 S4 0954+658 喷射的两个组成部分的宽带射电频谱。结果表明，该AGN中的同步射电波可能是由相对论质子产生的。

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引用次数: 0

The Interstellar Ti II Distance Scale 星际 Ti II 距离标尺

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2024-03-02 DOI: 10.1134/s1990341323700219

G. A. Galazutdinov, T. A. Santander, E. Babina, J. Krełowski

Abstract

We measured the equivalent widths ((EW)s) of interstellar Ti II absorption lines at (lambda) 3383.759 for about 250 reddened objects and found a good correlation of the (EW)s with distances to the background stars, estimated using Gaia DR3 parallaxes. Hipparcos trigonometric parallaxes were used for very bright objects which were not observed by Gaia. The Ti II based distance estimation procedure is similar to the well known Ca II-method (Megier et al., 2005, 2009). However, there are at least 3 advantages of the Ti II method: in contrast to interstellar Ca II H and K lines, blending of Ti II with stellar lines is not an issue even for late B stars; Ti II is to a much less extent influenced by the saturation effect; only a single line must be measured, i.e. there is only a single measurement error to be taken into account. The relation of between Ti II (EW) and distance is given by simple equation (dapprox 30EW), where (d) is the distance in pc and (EW) is the equivalent width of the Ti II (lambda) 3383.759 line in mÅ.

摘要我们测量了大约250个变红天体在(lambda) 3383.759处的星际Ti II吸收线的等效宽度（(EW)s），发现(EW)s与利用盖亚DR3视差估算的背景恒星的距离有很好的相关性。对于盖亚没有观测到的非常明亮的天体，则使用了Hipparcos三角视差。基于 Ti II 的距离估算程序与众所周知的 Ca II 方法类似（Megier 等人，2005 年，2009 年）。不过，Ti II 方法至少有三个优点：与星际 Ca II H 和 K 线相比，Ti II 与恒星线的混合即使对于晚期 B 星也不是问题；Ti II 受饱和效应的影响要小得多；只需测量一条线，即只需考虑一个测量误差。Ti II （EW）和距离之间的关系由简单的方程 (dapprox 30EW) 给出，其中 (d) 是以 pc 为单位的距离，(EW) 是以 mÅ 为单位的 Ti II （lambda）383.759 线的等效宽度。

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引用次数: 0

Activity of M-dwarf L 98-59 and Atmospheric Escape of its Exoplanets M 型矮星 L 98-59 的活动及其系外行星的大气逃逸

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2023-12-01 DOI: 10.1134/s1990341323700165

Abstract

A study of the activity of a bright M-dwarf L 98-59, located at a distance of 10.6 pc from Earth is reported. The star has a multiplanetary system, where one of the planets, L 98-59 b, is a rocky planet with a mass not exceeding the mass of Venus. It was found that the level of chromospheric activity of L 98-59 does not exceed the average value characteristic of other cold dwarfs with similar color index values ((B-V)) . This level is below solar, the mean (log R{{}^{prime}}_{textrm{HK}}) parameter for L 98-59 is equal to (-) 5.297 dex. The data about the parent star and its activity was used to estimate the magnitude of the atmospheric escape of five planets (including the planet candidate 05). To calculate the loss of matter from the planetary atmospheres (without a detailed modeling of the processes in the ‘‘star–planet’’ system), we applied an approximation formula corresponding to the energy-limited atmospheric loss model. Estimates of the XUV photon flux—extreme ultraviolet (EUV) and X-ray photons for the medium and high activity levels, as well as the estimates of the tidal parameter (K_{textrm{tide}}(xi)) were found. Variations of the (dot{M}) parameter have been specified for five planets of the L 98-59 system, taking into account the possible activity level variations of the star. The (dot{M}) parameter variations for planets c–e range from (7.6times 10^{6}) g s ({}^{-1}) to (3.8times 10^{7}) g s ({}^{-1}) (average activity level) and (1.2) – (5.7times 10^{7}) g s ({}^{-1}) (high activity level). For the planet L 98-59 b, the an analogue of Venus, we got the following estimates: (1.3times 10^{7}) and (2.0times 10^{7}) g s ({}^{-1}) (for the intermediate and high activity levels, respectively). It can be assumed that the relatively modest outflow of matter from their atmospheres (dot{M}) , despite the proximity of the planets to their star, is due to a small flux of XUV photons from the star due to the low level of its activity.

摘要报告对距离地球 10.6 pc 的一颗明亮的 M 型矮星 L 98-59 的活动进行了研究。该恒星有一个多行星系统，其中一颗行星 L 98-59 b 是一颗岩石行星，质量不超过金星。研究发现，L 98-59 的色球活动水平并没有超过其他具有类似色指数值的冷矮星的平均值（（B-V））。这个水平低于太阳，L 98-59的平均参数（log R{}^{prime}}_{textrm{HK}}）等于（-）5.297 dex。有关母恒星及其活动的数据被用来估算五颗行星（包括候选行星05）的大气逃逸量级。为了计算行星大气中物质的损耗（不需要对 "恒星-行星 "系统中的过程进行详细建模），我们使用了与能量有限大气损耗模型相对应的近似公式。我们找到了中等和高活性水平的 XUV 光子通量--极紫外（EUV）和 X 射线光子的估计值，以及潮汐参数 (K_{textrm{tide}}(xi)) 的估计值。考虑到恒星可能的活动水平变化，为 L 98-59 系统的五颗行星确定了 (dot{M})参数的变化。c-e行星的参数变化范围从（7.6倍 10^{6}）g s （{}^{-1}）到（3.8times 10^{7}) g s({}^{-1}) （平均活动水平）和（1.2）- （5.7times 10^{7}) g s({}^{-1}) （高活动水平）。对于金星的类似行星 L 98-59 b，我们得到了以下估计值： (1.3times 10^{7}) and(2.0times 10^{7}) g s({}^{-1}) （分别为中度和高度活动水平）。可以假定，尽管行星离恒星很近，但从它们的大气中流出的物质却相对较少（(dot{M})），这是因为恒星的活动水平较低，导致来自恒星的XUV光子通量较小。

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引用次数: 0

Radio Properties of High-Redshift Galaxies at $$boldsymbol{zgeq 1}$$ 高红移星系在 $$boldsymbol{zgeq 1}$ 的射电特性

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2023-12-01 DOI: 10.1134/s1990341323700190

Abstract

Study of high-redshift radio galaxies (HzRGs) can shed light on the active galactic nuclei (AGNs) evolution in massive elliptical galaxies. The vast majority of observed high-redshift AGNs are quasars, and there are very few radio galaxies at redshifts (z>3) . We present the radio properties of 173 sources optically identified with radio galaxies at (zgeq 1) with flux densities (S_{1.4}geq 20) mJy. Literature data were collected for compilation of broadband radio spectra, estimation of radio variability, radio luminosity, and radio loudness. Almost 60 (%) of the galaxies have steep or ultra-steep radio spectra; 22 (%) have flat, inverted, upturn, and complex spectral shapes, and 18 (%) have peaked spectra (PS). The majority of the PS sources in the sample (20/31) are megahertz-peaked spectrum source candidates, i.e. possibly very young and compact radio galaxies. The median values of the variability indices at 11 and 5 GHz are (V_{S_{11}}=0.14) and (V_{S_{5}}=0.13) , which generally indicates a weak or moderate character of the long-term variability of the studied galaxies. The typical radio luminosity and radio loudness are (L_{5}=10^{43}{-}10^{44}) erg s ({}^{-1}) and (log R=3{-}4) respectively. We have found less prominent features of the bright compact radio cores in our sample compared to high-redshift quasars at (zgeq 3) . The variety of the obtained radio properties shows the different conditions for the formation of radio emission sources in galaxies.

摘要对高红移射电星系（HzRGs）的研究可以揭示大质量椭圆星系中活动星系核（AGNs）的演化过程。观测到的高红移AGN绝大多数是类星体，而红移（z>3）的射电星系非常少。我们介绍了173个在光学上被识别为射电星系的光源的射电特性，它们的通量密度为（S_{1.4}geq 20) mJy。收集的文献数据用于编制宽带射电光谱、估计射电可变性、射电光度和射电响度。近60个星系有陡峭或超陡峭的射电光谱；22个星系有平坦、倒转、上翻和复杂的光谱形状，18个星系有峰值光谱（PS）。样本中的大多数峰状光谱源（20/31）都是兆赫兹峰状光谱源候选者，即可能是非常年轻和紧凑的射电星系。11GHz和5GHz的可变性指数中值分别为(V_{S_{11}}=0.14/)和(V_{S_{5}}=0.13/)，这总体上表明所研究星系的长期可变性较弱或中等。典型的射电光度和射电响度分别是 (L_{5}=10^{43}{-}10^{44}) erg s({}^{-1}) 和 (log R=3{-}4) 。与高红移类星体相比，我们在样本中发现的明亮紧凑射电核心在(zgeq 3) 时没有那么突出。所获得的射电特性的多样性表明了星系中射电发射源形成的不同条件。

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引用次数: 0

Satellites around Edge-on Galaxies. I. Dynamical Masses 边缘星系周围的卫星。I. 动力质量

IF 1.2 4区物理与天体物理 Q3 Physics and Astronomy

Astrophysical Bulletin

Pub Date : 2023-12-01 DOI: 10.1134/s1990341323600230

Abstract

We have undertaken a search for satellites around edge-on galaxies in the EGIPS catalog, which contains 16 551 objects with declinations above (-30^{circ}) . We searched for systems with a central galaxy dominating in brightness by at least (1^{textrm{m}}) compared to its companions. As a result, we discovered 1097 candidate satellites around 764 EGIPS galaxies with projected distances less than 500 kpc and a radial velocity difference less than 300 km s ({}^{-1}) . Of these, 757 satellites around 547 central galaxies have radial velocity accuracies higher than 20 km s ({}^{-1}) and satisfy the gravitationally bound condition. The ensemble of satellites is characterized by an average projected distance of 84 kpc and an average radial velocity dispersion of 103 km s ({}^{-1}) . Treating small satellites as test particles moving on isotropic orbits around central EGIPS galaxies, we determined the projected (orbital) masses of the edge-on galaxies. Within the luminosity range of (1.3times 10^{10}) to (42times 10^{10}) (L_{odot}) , the total mass of the systems is well described by a linear dependence (log M_{p}propto 0.88logleftlangle L_{K}rightrangle_{textrm{g}}) with an average total mass-to- (K) -band luminosity equal to ((17.5pm 0.8) M_{odot}/L_{odot}) , which is typical for nearby spiral galaxies such as the Milky Way, M 31 and M 81.

摘要我们对EGIPS星表中边缘星系周围的卫星进行了搜索，该星表包含16 551个倾角超过(-30^{circ})的天体。我们寻找的系统，其中心星系的亮度与其伴星系的亮度相比，至少占了(1^{textrm{m}})。结果，我们在 764 个 EGIPS 星系周围发现了 1097 个候选卫星，它们的投影距离小于 500 kpc，径向速度差小于 300 km s （{}^{-1}）。其中，围绕547个中心星系的757颗卫星的径向速度精度高于20 km s({}^{-1}) 并且满足引力约束条件。卫星群的平均投影距离为 84 kpc，平均径向速度离散度为 103 km s({}^{-1}) 。我们把小卫星看作是围绕中心 EGIPS 星系在各向同性轨道上运动的测试粒子，从而确定了边缘星系的投影（轨道）质量。在（1.3乘以10^{10}）到（42乘以10^{10}）（L_{odot}）的光度范围内，系统的总质量可以很好地用线性依赖关系来描述（（log M_{p}propto 0.88（log/left/langle L_{K}/right/rangle_{textrm{g}}），平均总质量-带光度等于（（17.5/pm 0.8）M_{odot}/L_{odot}/)，这是银河系、M 31 和 M 81 等附近螺旋星系的典型特征。

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引用次数: 0