It is well known that the rich culture of old Maya contained, among other, also a very complicated and complex calendar, in which they recorded not only historical events, but also significant astronomical phenomena. Main source of information is the Dresden Codex, roughly covering the interval between 280 and 1325 AD. The problem of the so-called correlation between Mayan and our calendars (expressing the difference between Long Count of Mayan calendar and Julian date) is very old, there exist about fifty different solutions that mutually differ by up to hundreds of years. Out of these, historians mostly accept the so-called Goodman-Mart?nez-Thompson (GMT) value of 584 283 days, which is based almost entirely on historical events. On the contrary, we stressed very precisely dated astronomical data, demonstrated the contradictions of GMT with them, and derived the so-called B?hm correlation (BB) of 622 261 days, which is in excellent agreement with astronomical phenomena recorded in Dresden Codex. Maya researchers are mostly convinced that Maya did not pay much attention to Mercury. Here we conclude that the truth is opposite; we analyze the data in Dresden Codex and find many records corresponding to visibility of Mercury near its maximum elongations from the Sun, and also to their conjunctions.
{"title":"Did old Maya observe Mercury?","authors":"J. Vondrák, V. Böhm, B. Böhm","doi":"10.2298/saj211222002v","DOIUrl":"https://doi.org/10.2298/saj211222002v","url":null,"abstract":"It is well known that the rich culture of old Maya contained, among other, also a very complicated and complex calendar, in which they recorded not only historical events, but also significant astronomical phenomena. Main source of information is the Dresden Codex, roughly covering the interval between 280 and 1325 AD. The problem of the so-called correlation between Mayan and our calendars (expressing the difference between Long Count of Mayan calendar and Julian date) is very old, there exist about fifty different solutions that mutually differ by up to hundreds of years. Out of these, historians mostly accept the so-called Goodman-Mart?nez-Thompson (GMT) value of 584 283 days, which is based almost entirely on historical events. On the contrary, we stressed very precisely dated astronomical data, demonstrated the contradictions of GMT with them, and derived the so-called B?hm correlation (BB) of 622 261 days, which is in excellent agreement with astronomical phenomena recorded in Dresden Codex. Maya researchers are mostly convinced that Maya did not pay much attention to Mercury. Here we conclude that the truth is opposite; we analyze the data in Dresden Codex and find many records corresponding to visibility of Mercury near its maximum elongations from the Sun, and also to their conjunctions.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2022-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674792","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In light of recent debates on the existence of a gigaparsec-scale structure traced by gamma-ray bursts, namely the Hercules-Corona Borealis Great Wall (HCBGW), we revisit large-scale homogeneity in the spatial distribution of quasars. Our volume-limited sample of quasars in the redshift range 1:6 < z ?2:1, which is constructed from the data release 7 of the Sloan Digital Sky Survey quasar catalogue, covers about half of the suspected HCBGW region. We analyze the sample in two complementary ways: fractal analysis of determining the average scale of homogeneity and friends- of-friends analysis of identifying specific large-scale structures. The quasar distribution on average reaches homogeneity at rh = 136?38h-1 Mpc and the richness and comoving size frequencies of large (>?150h-1 Mpc) quasar groups are consistent with the prediction of homogeneous distribution. These results put constraints on the spatial extent of the HCBGW but do not contradict its existence since our quasar sample does not cover the entire HCBGW region.
鉴于最近关于存在一个由伽马射线暴追踪的千兆秒差距尺度结构，即大力神-北冕长城(HCBGW)的争论，我们重新审视了类星体空间分布的大规模均匀性。我们在红移范围1:6 < z ?2:1的类星体样本体积有限，它是根据斯隆数字巡天类星体目录的数据发布7构建的，覆盖了大约一半的疑似HCBGW区域。我们用两种互补的方法对样品进行分析:分形分析用于确定均匀性的平均尺度，友元分析用于识别特定的大尺度结构。类星体的平均分布在rh = 136?38h- 1mpc和大(b> ?150h- 1mpc)类星体群与预测的均匀分布一致。这些结果限制了HCBGW的空间范围，但并不矛盾它的存在，因为我们的类星体样本并没有覆盖整个HCBGW区域。
{"title":"Large-scale homogeneity in the distribution of quasars in the Hercules-Corona Borealis Great Wall region","authors":"H. Fujii","doi":"10.2298/saj2204029f","DOIUrl":"https://doi.org/10.2298/saj2204029f","url":null,"abstract":"In light of recent debates on the existence of a gigaparsec-scale structure traced by gamma-ray bursts, namely the Hercules-Corona Borealis Great Wall (HCBGW), we revisit large-scale homogeneity in the spatial distribution of quasars. Our volume-limited sample of quasars in the redshift range 1:6 < z ?2:1, which is constructed from the data release 7 of the Sloan Digital Sky Survey quasar catalogue, covers about half of the suspected HCBGW region. We analyze the sample in two complementary ways: fractal analysis of determining the average scale of homogeneity and friends- of-friends analysis of identifying specific large-scale structures. The quasar distribution on average reaches homogeneity at rh = 136?38h-1 Mpc and the richness and comoving size frequencies of large (>?150h-1 Mpc) quasar groups are consistent with the prediction of homogeneous distribution. These results put constraints on the spatial extent of the HCBGW but do not contradict its existence since our quasar sample does not cover the entire HCBGW region.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2022-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674875","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This paper presents a comparative study of physical properties of a sample of 89 blue early-type galaxies (ETGs) from the local universe by fitting SEDs to their multi-wavelength photometric and spectroscopic data. The detailed template-based SED fitting analysis using the MAGPHY S and SED3FIT codes on the interstellar dust extinction corrected UV-to-far-IR spectro-photometric data enabled us to trace the evolutionary sequence of the blue ETGs on the color-magnitude diagram. This study evidenced a decreasing trend of the SFR, sSFR, dust mass, and dust mass fraction over the sequence from the SF - to - the Seyferts - to - the LINERs. The UV-optical colors also enabled us to estimate the look-back time of the last starburst phase in SF, Seyfert, and LINER galaxies, probably pointing towards the evolutionary sequence of the blue ETGs. Despite the blue colors and strong emission lines in the optical regime of the electromagnetic spectrum, the blue ETGs in the present sample occupy a position off the main sequence, commonly known as the green valley, on the CMD plot and hence indicate the transitional state of their non-secular evolution. A marginal positive correlation was noticed between SFR per unit dust mass and the temperature of the cool ISM. The declining trend of the cold dust temperature Tc over the sequence from the SF-to-Seyfert-to-LINER implies that the AGNs in the systems are not enough powerful to affect the cold component of the ISM.
{"title":"Stellar and dust properties in a sample of blue early type galaxies","authors":"S. P. Deshmukh, N. Vagshette, M. Patil","doi":"10.2298/saj2205023d","DOIUrl":"https://doi.org/10.2298/saj2205023d","url":null,"abstract":"This paper presents a comparative study of physical properties of a sample of 89 blue early-type galaxies (ETGs) from the local universe by fitting SEDs to their multi-wavelength photometric and spectroscopic data. The detailed template-based SED fitting analysis using the MAGPHY S and SED3FIT codes on the interstellar dust extinction corrected UV-to-far-IR spectro-photometric data enabled us to trace the evolutionary sequence of the blue ETGs on the color-magnitude diagram. This study evidenced a decreasing trend of the SFR, sSFR, dust mass, and dust mass fraction over the sequence from the SF - to - the Seyferts - to - the LINERs. The UV-optical colors also enabled us to estimate the look-back time of the last starburst phase in SF, Seyfert, and LINER galaxies, probably pointing towards the evolutionary sequence of the blue ETGs. Despite the blue colors and strong emission lines in the optical regime of the electromagnetic spectrum, the blue ETGs in the present sample occupy a position off the main sequence, commonly known as the green valley, on the CMD plot and hence indicate the transitional state of their non-secular evolution. A marginal positive correlation was noticed between SFR per unit dust mass and the temperature of the cool ISM. The declining trend of the cold dust temperature Tc over the sequence from the SF-to-Seyfert-to-LINER implies that the AGNs in the systems are not enough powerful to affect the cold component of the ISM.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2022-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674929","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In the present paper we consider the Type-2.x and Type-3.x extraterrestrial von- Neumann probes and study the problem of their detectability by the world's largest single-dish radio telescope: the Five-hundred-meter Aperture Spherical Radio Telescope (FAST). For this purpose we estimate the radio spectral parameters and analyse the obtained results in the context of technical characteristics of FAST. As a result, it is shown that FAST can detect both the galactic and extragalactic self-replicating probes with high precision.
{"title":"Can the China's fast telescope detect extraterrestrial von-Neumann probes?","authors":"Z. Osmanov","doi":"10.2298/saj2103047o","DOIUrl":"https://doi.org/10.2298/saj2103047o","url":null,"abstract":"In the present paper we consider the Type-2.x and Type-3.x extraterrestrial\u0000 von- Neumann probes and study the problem of their detectability by the\u0000 world's largest single-dish radio telescope: the Five-hundred-meter Aperture\u0000 Spherical Radio Telescope (FAST). For this purpose we estimate the radio\u0000 spectral parameters and analyse the obtained results in the context of\u0000 technical characteristics of FAST. As a result, it is shown that FAST can\u0000 detect both the galactic and extragalactic self-replicating probes with high\u0000 precision.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45473715","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In the present manuscript we consider the possibility of conducting SETI with small-size (with diameters less than 1 m) optical telescopes. Calculations are performed for typical parameters of the mentioned type of telescopes. In particular, we show that the techno-signatures of Type-2.x and Type-3.x civilizations might be detected. It is demonstrated that it is possible to detect hot megastructures (up to 4000 K) built around Main Sequence stars and pulsars, as well as von Neumann extraterrestrial probes.
{"title":"Prospects of SETI by small size optical telescopes","authors":"Z. Osmanov, V. Berezhiani","doi":"10.2298/SAJ210922003O","DOIUrl":"https://doi.org/10.2298/SAJ210922003O","url":null,"abstract":"In the present manuscript we consider the possibility of conducting SETI with\u0000 small-size (with diameters less than 1 m) optical telescopes. Calculations\u0000 are performed for typical parameters of the mentioned type of telescopes. In\u0000 particular, we show that the techno-signatures of Type-2.x and Type-3.x\u0000 civilizations might be detected. It is demonstrated that it is possible to\u0000 detect hot megastructures (up to 4000 K) built around Main Sequence stars\u0000 and pulsars, as well as von Neumann extraterrestrial probes.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47777247","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We have done photometric calibration of the 60 cm Nedeljkovic telescope equipped with the FLI PL 230 CCD camera, mounted at the Astronomical Station Vidojevica (Serbia), using standard stars from the Landolt catalog. We have imaged 31 fields of standard stars using Johnson's BVRI filters during three nights in August 2019. We have measured both extinction and color correction. Relating our calibrated magnitudes to the magnitudes of standard stars from the Landolt catalog, we have achieved accuracy of 2%-5% for the BVRI magnitudes.
{"title":"BVRI photometric calibration of the Nedeljkovic telescope","authors":"A. Vudragovic, M. Jurkovic","doi":"10.2298/SAJ210404003V","DOIUrl":"https://doi.org/10.2298/SAJ210404003V","url":null,"abstract":"We have done photometric calibration of the 60 cm Nedeljkovic telescope\u0000 equipped with the FLI PL 230 CCD camera, mounted at the Astronomical Station\u0000 Vidojevica (Serbia), using standard stars from the Landolt catalog. We have\u0000 imaged 31 fields of standard stars using Johnson's BVRI filters during three\u0000 nights in August 2019. We have measured both extinction and color\u0000 correction. Relating our calibrated magnitudes to the magnitudes of standard\u0000 stars from the Landolt catalog, we have achieved accuracy of 2%-5% for the\u0000 BVRI magnitudes.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46835345","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We present results from photometric monitoring of V900 Mon, one of the newly discovered and still under-studied object from the FU Orionis type. The FUor phenomenon is very rarely observed, but it is essential for stellar evolution. Since we only know about twenty stars of this type, the study of each new object is very important for our knowledge. Our data were obtained in optical spectral region with the BVRI Johnson-Cousins set of filters during the period from September 2011 to April 2021. In order to follow the photometric history of the object, we measured its stellar magnitudes on available plates from the Mikulski Archive for Space Telescopes. The collected archival data suggest that the rise in brightness of V900 Mon began after January 1989 and the outburst goes on so far. In November 2009, when the outburst was registered, the star had already reached the level of brightness close to the current one. Our observations indicate that during the period 2011-2017 the stellar magnitude increased gradually in each pass band. The observed amplitude of the outburst is about 4 magnitudes (R). During the last three years, the increase in brightness has stopped and there has even been a slight decline. The comparison of light curves of the known FUor objects shows that they are very diverse and are rarely repeated. However, the photometric data we have so far show that V900 Mon's light curve is somewhat similar to those of V1515 Cyg and V733 Cep.
{"title":"Long-term optical photometric monitoring of the FUor star V900 Mon","authors":"E. Semkov, S. Peneva, S. Ibryamov","doi":"10.2298/saj2102031s","DOIUrl":"https://doi.org/10.2298/saj2102031s","url":null,"abstract":"We present results from photometric monitoring of V900 Mon, one of the newly\u0000 discovered and still under-studied object from the FU Orionis type. The\u0000 FUor phenomenon is very rarely observed, but it is essential for stellar\u0000 evolution. Since we only know about twenty stars of this type, the study of\u0000 each new object is very important for our knowledge. Our data were obtained\u0000 in optical spectral region with the BVRI Johnson-Cousins set of filters\u0000 during the period from September 2011 to April 2021. In order to follow the\u0000 photometric history of the object, we measured its stellar magnitudes on\u0000 available plates from the Mikulski Archive for Space Telescopes. The\u0000 collected archival data suggest that the rise in brightness of V900 Mon\u0000 began after January 1989 and the outburst goes on so far. In November 2009,\u0000 when the outburst was registered, the star had already reached the level of\u0000 brightness close to the current one. Our observations indicate that during\u0000 the period 2011-2017 the stellar magnitude increased gradually in each pass\u0000 band. The observed amplitude of the outburst is about 4 magnitudes (R).\u0000 During the last three years, the increase in brightness has stopped and\u0000 there has even been a slight decline. The comparison of light curves of the\u0000 known FUor objects shows that they are very diverse and are rarely repeated.\u0000 However, the photometric data we have so far show that V900 Mon's light\u0000 curve is somewhat similar to those of V1515 Cyg and V733 Cep.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45046692","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Using a recently introduced synthetic method to compute the asteroid secular frequencies (Knezevic and Milani 2019), in this paper we survey the locations of secular resonances in the 9 dynamically distinct zones of the asteroid belt. Positions of all resonances up to order four, of a significant fraction of the order six resonances, and of a several order eight ones were determined, plotted in the space of proper elements, and discussed in relation to the local dynamics and to the structure and shape of the nearby asteroid collisional families. Only the resonant combinations with fundamental frequencies of Jupiter and Saturn were considered, with a few special cases involving other planets and largest asteroids. Accuracy of the polynomial fit to determine the frequencies was found to be satisfactory for the purpose of determination of secular resonance positions. This enabled a precise identification of dynamical mechanisms affecting the computation of frequencies (close vicinity of the mean motion resonances and libration in secular resonances), and of the cycle slips" as a primary technical drawback causing deterioration of the results. For each zone we also presented and discussed a fairly complete sample of recent works dealing with interaction of the secular resonances with asteroid families present in that zone. Finally, a few words were devoted to possibilities for future work.
{"title":"Survey of secular resonances in the asteroid belt","authors":"Z. Knežević","doi":"10.2298/saj210903004k","DOIUrl":"https://doi.org/10.2298/saj210903004k","url":null,"abstract":"Using a recently introduced synthetic method to compute the asteroid secular frequencies (Knezevic and Milani 2019), in this paper we survey the locations of secular resonances in the 9 dynamically distinct zones of the asteroid belt. Positions of all resonances up to order four, of a significant fraction of the order six resonances, and of a several order eight ones were determined, plotted in the space of proper elements, and discussed in relation to the local dynamics and to the structure and shape of the nearby asteroid collisional families. Only the resonant combinations with fundamental frequencies of Jupiter and Saturn were considered, with a few special cases involving other planets and largest asteroids. Accuracy of the polynomial fit to determine the frequencies was found to be satisfactory for the purpose of determination of secular resonance positions. This enabled a precise identification of dynamical mechanisms affecting the computation of frequencies (close vicinity of the mean motion resonances and libration in secular resonances), and of the cycle slips\" as a primary technical drawback causing deterioration of the results. For each zone we also presented and discussed a fairly complete sample of recent works dealing with interaction of the secular resonances with asteroid families present in that zone. Finally, a few words were devoted to possibilities for future work.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68675140","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Gravitational waves (GW) in the nano-Hz domain are expected to be radiated by close-binaries of supermassive black holes (CB-SMBHs; components bound in a Keplerian binary at mutual distance less than ~ 0.1 pc), which are relicts of galaxy mergers and anticipated to be measured via the Pulsar Timing Array (PTA) technique. The challenge of present CB-SMBH investigations is that their signatures are elusive and not easily disentangled from a single SMBH. PTAs will typically have a glimpse of an early portion of the binary inspiral to catch the frequency evolution of the binary only with sufficiently high mass and initially high eccentricity. Thus, we have to make use of electromagnetic observations to determine orbital parameters of CB-SMBHs and test nano-Hz GW properties. The 2D reverberation mapping (RM) is a powerful tool for probing kinematics and geometry of ionized gas in the SMBHs (single or binary) vicinity, yet it can lose information due to projection on the line of sight of the observer. Nevertheless, spectroastrometry with AMBER, GRAVITY, and successors can provide an independent measurement of the emitting region's size, geometry, and kinematics. These two techniques combined can resolve CB-SMBHs. In this review, we focus on RM and spectroastrometry observational signatures of CB-SMBHs with non-zero eccentricity from recent simulations with particular attention to recent developments and open issues.
{"title":"Investigating close binary supermassive black holes at high angular resolution","authors":"A. Kovačević","doi":"10.2298/saj2102001k","DOIUrl":"https://doi.org/10.2298/saj2102001k","url":null,"abstract":"Gravitational waves (GW) in the nano-Hz domain are expected to be radiated by close-binaries of supermassive black holes (CB-SMBHs; components bound in a Keplerian binary at mutual distance less than ~ 0.1 pc), which are relicts of galaxy mergers and anticipated to be measured via the Pulsar Timing Array (PTA) technique. The challenge of present CB-SMBH investigations is that their signatures are elusive and not easily disentangled from a single SMBH. PTAs will typically have a glimpse of an early portion of the binary inspiral to catch the frequency evolution of the binary only with sufficiently high mass and initially high eccentricity. Thus, we have to make use of electromagnetic observations to determine orbital parameters of CB-SMBHs and test nano-Hz GW properties. The 2D reverberation mapping (RM) is a powerful tool for probing kinematics and geometry of ionized gas in the SMBHs (single or binary) vicinity, yet it can lose information due to projection on the line of sight of the observer. Nevertheless, spectroastrometry with AMBER, GRAVITY, and successors can provide an independent measurement of the emitting region's size, geometry, and kinematics. These two techniques combined can resolve CB-SMBHs. In this review, we focus on RM and spectroastrometry observational signatures of CB-SMBHs with non-zero eccentricity from recent simulations with particular attention to recent developments and open issues.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674706","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Gravitational Waves (GWs) have become a major source of insight in Multi Messenger Astronomy since their first direct detection in 2015 (Abbott et al. 2016) where the Nobel prize in Physics was awarded in 2017 to LIGO founders Barry C. Barish, Kip S. Thorne, and Rainer Weiss. They complement electromagnetic and particle measurements by providing cosmic scale evidence which cannot be detected in any other way. Their rise to prominence has not been straightforward since the founder of general relativity, Albert Einstein, who predicted GWs, was nevertheless skeptical of their existence and detectability. This skepticism put a damper on Gravitational Wave (GW) research that was not overcome until the 1950's, the decade of Einstein's death. Since then, ever more sensitive GW detectors have been designed for construction on earth and in space. Each of these detector approaches was designed to expand the types of cosmic events that could be detected.
自2015年首次直接探测到引力波(GWs)以来，引力波(GWs)已成为多信使天文学的主要洞察来源(Abbott et al. 2016)， 2017年诺贝尔物理学奖授予了LIGO创始人Barry C. Barish, Kip S. Thorne和Rainer Weiss。它们通过提供宇宙尺度的证据来补充电磁和粒子测量，这是其他任何方式都无法探测到的。自从广义相对论的创始人阿尔伯特·爱因斯坦预言了重力波的存在和可探测性之后，重力波的崛起并不是一帆风顺的。这种怀疑态度阻碍了引力波(GW)的研究，直到20世纪50年代，也就是爱因斯坦去世的那十年，引力波的研究才被克服。从那时起，更灵敏的GW探测器被设计用于在地球和太空中建造。这些探测器的每一种方法都是为了扩展可以探测到的宇宙事件的类型。
{"title":"The past, present and future of gravitational wave astronomy","authors":"H. Leverenz, M. Filipović","doi":"10.2298/saj210518001l","DOIUrl":"https://doi.org/10.2298/saj210518001l","url":null,"abstract":"Gravitational Waves (GWs) have become a major source of insight in Multi Messenger Astronomy since their first direct detection in 2015 (Abbott et al. 2016) where the Nobel prize in Physics was awarded in 2017 to LIGO founders Barry C. Barish, Kip S. Thorne, and Rainer Weiss. They complement electromagnetic and particle measurements by providing cosmic scale evidence which cannot be detected in any other way. Their rise to prominence has not been straightforward since the founder of general relativity, Albert Einstein, who predicted GWs, was nevertheless skeptical of their existence and detectability. This skepticism put a damper on Gravitational Wave (GW) research that was not overcome until the 1950's, the decade of Einstein's death. Since then, ever more sensitive GW detectors have been designed for construction on earth and in space. Each of these detector approaches was designed to expand the types of cosmic events that could be detected.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68675055","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：