A thorough detector response calibration using radioactive sources is necessary for the Jiangmen Underground Neutrino Observatory. Herein, we discuss the design of a source positioning system based on ultrasonic techn...A thorough detector response calibration using radioactive sources is necessary for the Jiangmen Underground Neutrino Observatory. Herein, we discuss the design of a source positioning system based on ultrasonic technology, aiming for a 3-cm precision over the entire35-m diameter detector sphere. A prototype system is constructed and demonstrated for the experiment.展开更多
We study the hybrid mesons with the exotic quantum number I^(G)J^(PG)=0+1-+and investigate their decays into theηη’,a1(1260)π,f1(1285)η,f1(1420)η,K*(892)■,K1(1270)■,and K1(1400)■channels.It is found that the ...We study the hybrid mesons with the exotic quantum number I^(G)J^(PG)=0+1-+and investigate their decays into theηη’,a1(1260)π,f1(1285)η,f1(1420)η,K*(892)■,K1(1270)■,and K1(1400)■channels.It is found that the QCD axial anomaly enhances the decay width of theηη’channel although this mode is strongly suppressed by the small p-wave phase space.Our results support the interpretation of theη1(1855)recently observed by BESⅢas the ssg hybrid meson of I^(G)J^(PC)=0^(+)1^(-+).The QCD axial anomaly ensures theηη’decay mode to be a characteristic signal of the hybrid nature of theη1(1855).展开更多
The Tianlai cylinder array is a pathfinder for developing and testing 21 cm intensity mapping techniques.In this paper,we use numerical simulation to assess how its measurement is affected by thermal noise and the err...The Tianlai cylinder array is a pathfinder for developing and testing 21 cm intensity mapping techniques.In this paper,we use numerical simulation to assess how its measurement is affected by thermal noise and the errors in calibration and map-making process,and the error in the sky map reconstructed from a drift scan survey.Here we consider only the single frequency,unpolarized case.The beam is modeled by fitting to the electromagnetic simulation of the antenna,and the variations of the complex gains of the array elements are modeled by Gaussian processes.Mock visibility data are generated and run through our data processing pipeline.We find that the accuracy of the current calibration is limited primarily by the absolute calibration,where the error comes mainly from the approximation of a single dominating point source.We then studied the m-mode map-making with the help of Moore-Penrose inverse.We find that discarding modes with singular values smaller than a threshold could generate visible artifacts in the map.The impacts of the residue variation of the complex gain and thermal noise are also investigated.The thermal noise in the map varies with latitude,being minimum at the latitude passing through the zenith of the telescope.The angular power spectrum of the reconstructed map show that the current Tianlai cylinder pathfinder,which has a shorter maximum baseline length in the North-South direction,can measure modes up to l■2πb_(NS)/λ~200 very well,but would lose a significant fraction of higher angular modes when noise is present.These results help us to identify the main limiting factors in our current array configuration and data analysis procedure,and suggest that the performance can be improved by reconfiguration of the array feed positions.展开更多
The Tianlai cylinder pathfinder is a radio interferometer array to test 21 cm intensity mapping techniques in the post-reionization era.It works in passive drift scan mode to survey the sky visible in the northern hem...The Tianlai cylinder pathfinder is a radio interferometer array to test 21 cm intensity mapping techniques in the post-reionization era.It works in passive drift scan mode to survey the sky visible in the northern hemisphere.To deal with the large instantaneous field of view and the spherical sky,we decompose the drift scan data into m-modes,which are linearly related to the sky intensity.The sky map is reconstructed by solving the linear interferometer equations.Due to incomplete uv coverage of the interferometer baselines,this inverse problem is usually ill-posed,and regularization method is needed for its solution.In this paper,we use simulation to investigate two frequently used regularization methods,the Truncated Singular Value Decomposition(TSVD),and the Tikhonov regularization techniques.Choosing the regularization parameter is very important for its application.We employ the generalized cross validation method and the L-curve method to determine the optimal value.We compare the resulting maps obtained with the different regularization methods,and for the different parameters derived using the different criteria.While both methods can yield good maps for a range of regularization parameters,in the Tikhonov method the suppression of noisy modes are more gradually applied,produce more smooth maps which avoids some visual artefacts in the maps generated with the TSVD method.展开更多
The burst of radio emission by an extensive air shower provides a promising alternative for detecting ultra-high energy cosmic rays. We have developed an inde- pendent numerical program to simulate these radio signals...The burst of radio emission by an extensive air shower provides a promising alternative for detecting ultra-high energy cosmic rays. We have developed an inde- pendent numerical program to simulate these radio signals. Our code is based on a microscopic treatment, with both the geosynchrotron radiation and charge included. Here we give the first presentation of our basic program and its results. When the time-domain signals for different polarizations are computed, we find that the pulses take on a bipolar pattern and the spectrum is suppressed towards the lower frequencies. We investigate how showers at different heights in the atmosphere contribute to the total signal, and examine the signal strength and distribution at sites with different elevations. We also study the signal from showers with different inclination angles and azimuth directions. In all these cases we find the charge excess effect is important.展开更多
We combine the kinematics of 159 globular clusters(GCs)provided by the Gaia Early Data Release 3(EDR3)with other observational data to classify the GCs,and to estimate the mass of the Milky Way(MW).We use the agemetal...We combine the kinematics of 159 globular clusters(GCs)provided by the Gaia Early Data Release 3(EDR3)with other observational data to classify the GCs,and to estimate the mass of the Milky Way(MW).We use the agemetallicity relation,integrals of motion,action space and the GC orbits to identify the GCs as either formed in situ(Bulge and Disk)or ex situ(via accretion).We find that 45.3%have formed in situ,while 38.4%may be related to known merger events:Gaia-Sausage-Enceladus,the Sagittarius dwarf galaxy,the Helmi streams,the Sequoia galaxy and the Kraken galaxy.We also further identify three new sub-structures associated with the Gaia-Sausage-Enceladus.The remaining 16.3%of GCs are unrelated to the known mergers and thought to be from small accretion events.We select 46 GCs which have radii 8.0<r<37.3 kpc and obtain the anisotropy parameterβ=0.315_(-0.049)^(+0.055),which is lower than the recent result using the sample of GCs in Gaia Data Release 2,but still in agreement with it by considering the error bar.By using the same sample,we obtain the MW mass inside the outermost GC as M(<37.3 kpc)=0.423_(-0.02)^(+0.02)×10^(12)M_(⊙),and the corresponding M_(200)=1.11_(-0.18)^(+0.25)×10^(12)M_(⊙).The estimated mass is consistent with the results in many recent studies.We also find that the estimatedβand mass depend on the selected sample of GCs.However,it is difficult to determine whether a GC fully traces the potential of the MW.展开更多
A great challenge for 21 cm intensity mapping experiments is the strong foreground radiation which is orders of magnitude brighter than the 21 cm signal.Removal of the foreground takes advantage of the fact that its f...A great challenge for 21 cm intensity mapping experiments is the strong foreground radiation which is orders of magnitude brighter than the 21 cm signal.Removal of the foreground takes advantage of the fact that its frequency spectrum is smooth while the redshifted 21 cm signal spectrum is stochastic.However,a complication is the nonsmoothness of the instrument response.This paper describes the electromagnetic simulation of the Tianlai cylinder array,a pathfinder for 21 cm intensity mapping experiments.Due to the vast scales involved,a direct simulation requires a large amount of computing resources.We have made the simulation practical by using a combination of methods:first simulate a single feed,then an array of feed units,finally with the feed array and a cylindrical reflector together,obtain the response for a single cylinder.We studied its radiation pattern,bandpass response and the effects of mutual coupling between feed units,and compared the results with observation.Many features seen in the measurement result are reproduced well in the simulation,especially the oscillatory features which are associated with the standing waves on the reflector.The mutual coupling between feed units is quantified with Sparameters,which decrease as the distance between the two feeds increases.Based on the simulated S-parameters,we estimate the correlated noise which has been seen in the visibility data,and the results show very good agreement with the data in both magnitude and frequency structures.These results provide useful insights on the problem of 21 cm signal extraction for real instruments.展开更多
This paper presents the design,calibration,and survey strategy of the Fast Radio Burst(FRB)digital backend and its real-time data processing pipeline employed in the Tianlai Cylinder Pathfinder Array.The array,consist...This paper presents the design,calibration,and survey strategy of the Fast Radio Burst(FRB)digital backend and its real-time data processing pipeline employed in the Tianlai Cylinder Pathfinder Array.The array,consisting of three parallel cylindrical reflectors and equipped with 96 dual-polarization feeds,is a radio interferometer array designed for conducting drift scans of the northern celestial semi-sphere.The FRB digital backend enables the formation of 96 digital beams,effectively covering an area of approximately 40 square degrees with the 3 dB beam.Our pipeline demonstrates the capability to conduct an automatic search of FRBs,detecting at quasi-realtime and classifying FRB candidates automatically.The current FRB searching pipeline has an overall recall rate of88%.During the commissioning phase,we successfully detected signals emitted by four well-known pulsars:PSR B0329+54,B2021+51,B0823+26,and B2020+28.We report the first discovery of an FRB by our array,designated as FRB 20220414A.We also investigate the optimal arrangement for the digitally formed beams to achieve maximum detection rate by numerical simulation.展开更多
In a semi-numerical model of reionization, the evolution of ionization fraction is approximately simulated by the criterion of ionizing photon to baryon ratio. We incorporate a semi-analytical model of galaxy formatio...In a semi-numerical model of reionization, the evolution of ionization fraction is approximately simulated by the criterion of ionizing photon to baryon ratio. We incorporate a semi-analytical model of galaxy formation based on the Millennium II N-body simulation into the semi-numerical modeling of reionization. The semianalytical model is used to predict the production of ionizing photons, then we use the semi-numerical method to model the reionization process. Such an approach allows more detailed modeling of the reionization, and also connects observations of galaxies at low and high redshifts to the reionization history. The galaxy formation model we use was designed to match the low-z observations, and it also fits the high redshift luminosity function reasonably well, but its prediction about star formation falls below the observed value, and we find that it also underpredicts the stellar ionizing photon production rate, hence the reionization cannot be completed at z ~ 6. We also consider simple modifications of the model with more top heavy initial mass functions, which can allow the reionization to occur at earlier epochs. The incorporation of the semi-analytical model may also affect the topology of the HI regions during the epoch of reionization, and the neutral regions produced by our simulations with the semi-analytical model, which appeared less poriferous than the simple halo-based models.展开更多
Detecting primordial fluctuations from the cosmic dark ages requires extremely large low-frequency radio telescope arrays deployed on the far side of the Moon.The antenna of such an array must be lightweight,easily st...Detecting primordial fluctuations from the cosmic dark ages requires extremely large low-frequency radio telescope arrays deployed on the far side of the Moon.The antenna of such an array must be lightweight,easily storable and transportable,deployable on a large scale,durable,and capable of good electrical performance.A membrane antenna is an excellent candidate to meet these criteria.We study the design of a low-frequency membrane antenna for a lunar-based low-frequency(<30 MHz)radio telescope constructed from polyimide film widely used in aerospace applications,owing to its excellent dielectric properties and high stability as a substrate material.We first design and optimize an antenna in free space through dipole deformation and coupling principles,then simulate an antenna on the lunar surface with a simple lunar soil model,yielding an efficiency greater than 90%in the range of 12-19 MHz and greater than 10%in the range of 5-35 MHz.The antenna inherits the omni-directional radiation pattern of a simple dipole antenna in the 5-30 MHz frequency band,giving a large field of view and allowing detection of the 21 cm global signal when used alone.A demonstration prototype is constructed,and its measured electrical property is found to be consistent with simulated results using|S11|measurements.This membrane antenna can potentially fulfill the requirements of a lunar low-frequency array,establishing a solid technical foundation for future large-scale arrays for exploring the cosmic dark ages.展开更多
The growth characteristics of Aspergillus parasitic us incubated on two culture media were ex-amined using shortwave infrared(SWIR,1000-2500 nm)hyperspectral imaging(HSI)in this work.HSI images of the A.parasiticus co...The growth characteristics of Aspergillus parasitic us incubated on two culture media were ex-amined using shortwave infrared(SWIR,1000-2500 nm)hyperspectral imaging(HSI)in this work.HSI images of the A.parasiticus colonies growing on rose bengal medium(RBM)and maize agar medium(MAM)were recorded daily for 6 days.The growth phases of A.parasiticus were indicated through the pixel number and average spectra of colonies.On score plot of the first principal component(PC1)and PC2,four growth zones with varying mycelium densities were identified.Eight characteristic wavelengths(1095,1145,1195,1279,1442,1655,1834 and 1929 nm)were selected from PC1 loading,average spectra of each colony as well as each growth zone.F urthermore,support vector machine(S VM)classifier based on the eight wavelengths was built,and the classification accuracies for the four zones(from outer to inner zones)on the colonies on RBM were 99.77%,9935%,99.75%and 99.60%and 99.77%,9939%,99.31%and 98.22%for colonies on MAM.In addition,a new score plot of PC2 and PC3 was used to differ-entiate the colonies incubated on RBM and MAM for 6 days.Then characteristic wavelengths of 1067,1195,1279,1369,1459,1694,1834 and 1929 nm were selected from the loading of PC2 and PCg.Based on them,a new SVM model was developed to diferentiate colonies on RBM and MAM with accuracy of 100.00%and 9999%,respectively.In conclusion,SWIR hyperspectral image is a powerful tool for evaluation of growth characteristics of A.parasiticus incubated in diferent culture media.展开更多
In section‘Track decoding’of this article,one of the paragraphs was inadvertently missed out after the text'…shows the flow diagram of the Tr2-1121 track mode.'The missed paragraph is provided below.
We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The...We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The framework integrates advanced algorithms for precise calibration,accurate particle identification,and efficient event reconstruction,aiming to account for critical experimental factors such as charge-sharing effects,multi-hit event resolution,and detector response nonuniformity.Its robust performance was demonstrated through the successful analysis of light-charged particles in the 25 MeV/u^(86)Kr+^(124)Sn experiment conducted at the first Radioactive Ion Beam Line in Lanzhou,allowing for precise extraction of physical observables,including energy,momentum,and particle type.Furthermore,utilizing the reconstructed physical information,such as the number of effective physical events and energy spectra to optimize the track recognition algorithm,the final track recognition efficiencies of approximately 90%were achieved.This framework establishes a valuable reference methodology for SSDT-based detector systems in heavy-ion reaction experiments,thereby significantly enhancing the accuracy and efficiency of data analysis in nuclear physics research.展开更多
By combining femtoscopic interferometry with an optical deblurring algorithm,we present a novel method to image the source in heavy-ion collisions(HICs),while simultaneously determining the interaction strength betwee...By combining femtoscopic interferometry with an optical deblurring algorithm,we present a novel method to image the source in heavy-ion collisions(HICs),while simultaneously determining the interaction strength between particle pairs.The spatial distribution of the emission source has been reconstructed for protons(p)and antiprotons(^(-)p)from the respective pp and^(-)p^(-)p correlation functions in Au+Au collisions at√S_(NN)=200 GeV.Within experimental uncertainties,protons and antiprotons share the same freeze-out distribution showing higher density in the center compared to the widely assumed Gaussian shape.The results evidence the matter–antimatter symmetry in coordinate space at the freeze-out moment before the nucleons are fully randomized in the collisions.展开更多
The redshifted 21 cm line,arising from neutral hydrogen,offers a unique probe into the intergalactic medium and the first stars and galaxies formed in the early universe.However,detecting this signal is a challenging ...The redshifted 21 cm line,arising from neutral hydrogen,offers a unique probe into the intergalactic medium and the first stars and galaxies formed in the early universe.However,detecting this signal is a challenging task because of artificial radio-frequency interference(RFI)and systematic errors such as ground effects.The interior of the Antarctic continent provides an excellent location to make such observations,with minimal RFI and relatively stable foreground signals.Moreover,a flat plateau in central Antarctica,with an ice cap over 2000 m deep,will show less ground reflection of radio waves,reducing the signal complexity in the area around the probing antenna.It may be advantageous to perform cosmological 21 cm experiments in Antarctica,and a 21 cm Antarctic global spectrum experiment can potentially be deployed on the Antarctic ice cap.We have performed preliminary instrumental design,system calibration,and implementation of such an instrument optimized for extreme cold and capable of long-term autonomous operation.This system shows the ability to effectively detect the 21 cm signal,confirming Antarctica as an excellent observational site for radio cosmology.展开更多
In 2012,we investigated the possible molecular states composed of two charmed mesons[Phys.Rev.D 88(2013)114008;2012 arXiv:1211.5007[hep-ph]].The D^(*)D𝐷system with the quantum numbers of I(J^(P))=0(1^(+))was f...In 2012,we investigated the possible molecular states composed of two charmed mesons[Phys.Rev.D 88(2013)114008;2012 arXiv:1211.5007[hep-ph]].The D^(*)D𝐷system with the quantum numbers of I(J^(P))=0(1^(+))was found to be a good candidate of the loosely bound molecular state.This state is very close to theD*D threshold with a binding energy around 0.47 MeV.This prediction was confirmed by the new LHCb observation of𝑇T^(+)_(cc)[see Franz Muheim’s talk at the European Physical Society conference on high energy physics 2021].展开更多
In 21 cm intensity mapping,the spectral smoothness of the foreground is exploited to separate it from the much weaker 21 cm signal.However,the non-smooth frequency response of the instrument complicates this process.R...In 21 cm intensity mapping,the spectral smoothness of the foreground is exploited to separate it from the much weaker 21 cm signal.However,the non-smooth frequency response of the instrument complicates this process.Reflections and standing waves generate modulations on the frequency response.Here we report the analysis of the standing waves in the bandpass of the signal channels of the Tianlai Cylinder Array.By Fourier transforming the bandpass into the delay time domain,we find various standing waves generated on the telescope.A standing wave with time delay at~142 ns is most clearly identified which is produced in the 15-meter feed cable.We also identify a strong peak at a shorter delay ofτ<50 ns,which may be a mix of the standing wave between the reflector and feed,and the standing wave on the 4 m intermediate frequency(IF)cable.We also show that a smoother frequency response could be partially recovered by removing the reflection-inducted modulations.However,the standing wave on the antenna is direction-dependent,which poses a more difficult challenge for high precision calibration.展开更多
Observations are beginning to constrain the history of the epoch of reionization(EoR).Modeling the reionization process is indispensable to interpret the observations,to infer the properties of ionizing sources,and to...Observations are beginning to constrain the history of the epoch of reionization(EoR).Modeling the reionization process is indispensable to interpret the observations,to infer the properties of ionizing sources,and to probe the various astrophysical processes from the observational data.Here we present an improved version of the seminumerical simulation islandFAST,by incorporating inhomogeneous recombinations and a corresponding inhomogeneous ionizing background,and simulate the reionization process of neutral islands during the late EoR.We find that the islands are more fragmented in models with inhomogeneous recombinations than the case with a homogeneous recombination number.In order to investigate the effects of basic assumptions in the reionization modeling,we compare the results from islandFAST with those from 21cmFAST for the same assumptions on the ionizing photon sources and sinks,to find how the morphology of the ionization field and the reionization history depend on the different treatments of these two models.Such systematic bias should be noted when interpreting the upcoming observations.展开更多
Recent observations show that the spectra of cosmic ray nuclei start to harden above ～ 102 GeV, which contradicts the conventional steady-state cosmic ray model. We had suggested that this anomaly is due to the propa...Recent observations show that the spectra of cosmic ray nuclei start to harden above ～ 102 GeV, which contradicts the conventional steady-state cosmic ray model. We had suggested that this anomaly is due to the propagation effect of cosmic rays released from local young cosmic ray sources; the total flux of cosmic rays should be computed with the Myriad Model, where a contribution from sources in the local catalog is added to the background. However, although the hardening could be elegantly explained in this model, the model parameters obtained from the fit are skewed toward a region with fast diffusion and a low supernova rate in the Galaxy, in disagreement with other observations. We further explore this model in order to set up a concordant picture. Two possible improvements related to cosmic ray sources are considered. First, instead of the usual axisymmetric disk model, we examine a spiral model for the source distribution. Second, for nearby and young sources which are necessary to explain the hardening, we allow for an energy-dependent escape. We find that a major improvement comes from incorporating an energy-dependent escape time for local sources, and with both modifications not only are the cosmic ray proton and helium anomalies resolved, but also the parameters attain values in a reasonable range compatible with other analyses.展开更多
The Tianlai Dish Pathfinder Array is a radio interferometer array consisting of 16 six-meter dish antennas.The original digital backend integration time is at the seconds level,designed for H I intensity mapping exper...The Tianlai Dish Pathfinder Array is a radio interferometer array consisting of 16 six-meter dish antennas.The original digital backend integration time is at the seconds level,designed for H I intensity mapping experiment.A new digital backend with millisecond response is added to enable it to search for fast radio burst during its observations.The design and calibration of this backend,and the real time search pipeline for it are described in this paper.It is capable of forming 16 digital beams for each linear polarization,covering an area of 19.6 square degrees.The search pipeline is capable of searching for,recording and classifying FRBs automatically in real time.In commissioning,we succeeded in capturing the signal pulses from the pulsars PSR B0329+54 and B2021+51.展开更多
基金supported by the ‘‘Strategic Priority Research Program’’ of the Chinese Academy of Sciences(No.XDA10010800)the ‘‘Fundamental Research Funds for the Central Universities’’(No.3102017zy010)
文摘A thorough detector response calibration using radioactive sources is necessary for the Jiangmen Underground Neutrino Observatory. Herein, we discuss the design of a source positioning system based on ultrasonic technology, aiming for a 3-cm precision over the entire35-m diameter detector sphere. A prototype system is constructed and demonstrated for the experiment.
基金supported by the National Natural Science Foundation of China(Grant Nos.12075019,11975033,and 12070131001)the Jiangsu Provincial Double-Innovation Program(Grant No.JSSCRC2021488)the Fundamental Research Funds for the Central Universities。
文摘We study the hybrid mesons with the exotic quantum number I^(G)J^(PG)=0+1-+and investigate their decays into theηη’,a1(1260)π,f1(1285)η,f1(1420)η,K*(892)■,K1(1270)■,and K1(1400)■channels.It is found that the QCD axial anomaly enhances the decay width of theηη’channel although this mode is strongly suppressed by the small p-wave phase space.Our results support the interpretation of theη1(1855)recently observed by BESⅢas the ssg hybrid meson of I^(G)J^(PC)=0^(+)1^(-+).The QCD axial anomaly ensures theηη’decay mode to be a characteristic signal of the hybrid nature of theη1(1855).
基金supported by the National SKA Program of China,No.2022SKA0110100supported by the National Natural Science Foundation of China under grant No.1220030249。
文摘The Tianlai cylinder array is a pathfinder for developing and testing 21 cm intensity mapping techniques.In this paper,we use numerical simulation to assess how its measurement is affected by thermal noise and the errors in calibration and map-making process,and the error in the sky map reconstructed from a drift scan survey.Here we consider only the single frequency,unpolarized case.The beam is modeled by fitting to the electromagnetic simulation of the antenna,and the variations of the complex gains of the array elements are modeled by Gaussian processes.Mock visibility data are generated and run through our data processing pipeline.We find that the accuracy of the current calibration is limited primarily by the absolute calibration,where the error comes mainly from the approximation of a single dominating point source.We then studied the m-mode map-making with the help of Moore-Penrose inverse.We find that discarding modes with singular values smaller than a threshold could generate visible artifacts in the map.The impacts of the residue variation of the complex gain and thermal noise are also investigated.The thermal noise in the map varies with latitude,being minimum at the latitude passing through the zenith of the telescope.The angular power spectrum of the reconstructed map show that the current Tianlai cylinder pathfinder,which has a shorter maximum baseline length in the North-South direction,can measure modes up to l■2πb_(NS)/λ~200 very well,but would lose a significant fraction of higher angular modes when noise is present.These results help us to identify the main limiting factors in our current array configuration and data analysis procedure,and suggest that the performance can be improved by reconfiguration of the array feed positions.
基金the support of the National SKA Program of China (Nos. 2022SKA0110100 and 2022SKA0110101)the National Natural Science Foundation of China (Nos. 12203061, 12273070, and 12303004)。
文摘The Tianlai cylinder pathfinder is a radio interferometer array to test 21 cm intensity mapping techniques in the post-reionization era.It works in passive drift scan mode to survey the sky visible in the northern hemisphere.To deal with the large instantaneous field of view and the spherical sky,we decompose the drift scan data into m-modes,which are linearly related to the sky intensity.The sky map is reconstructed by solving the linear interferometer equations.Due to incomplete uv coverage of the interferometer baselines,this inverse problem is usually ill-posed,and regularization method is needed for its solution.In this paper,we use simulation to investigate two frequently used regularization methods,the Truncated Singular Value Decomposition(TSVD),and the Tikhonov regularization techniques.Choosing the regularization parameter is very important for its application.We employ the generalized cross validation method and the L-curve method to determine the optimal value.We compare the resulting maps obtained with the different regularization methods,and for the different parameters derived using the different criteria.While both methods can yield good maps for a range of regularization parameters,in the Tikhonov method the suppression of noisy modes are more gradually applied,produce more smooth maps which avoids some visual artefacts in the maps generated with the TSVD method.
基金Supported by the National Natural Science Foundation of China
文摘The burst of radio emission by an extensive air shower provides a promising alternative for detecting ultra-high energy cosmic rays. We have developed an inde- pendent numerical program to simulate these radio signals. Our code is based on a microscopic treatment, with both the geosynchrotron radiation and charge included. Here we give the first presentation of our basic program and its results. When the time-domain signals for different polarizations are computed, we find that the pulses take on a bipolar pattern and the spectrum is suppressed towards the lower frequencies. We investigate how showers at different heights in the atmosphere contribute to the total signal, and examine the signal strength and distribution at sites with different elevations. We also study the signal from showers with different inclination angles and azimuth directions. In all these cases we find the charge excess effect is important.
基金support by the National Key R&D Program(No.2017YFA0402603)the Inter-government cooperation Flagship program(Grant No.2018YFE0120800)+2 种基金the National Natural Science Foundation of China(NSFC,Grant Nos.11773034 and 11633004)the Chinese Academy of Sciences(CAS)Strategic Priority Research Program XDA15020200the CAS Interdisciplinary Innovation Team(JCTD-2019-05)。
文摘We combine the kinematics of 159 globular clusters(GCs)provided by the Gaia Early Data Release 3(EDR3)with other observational data to classify the GCs,and to estimate the mass of the Milky Way(MW).We use the agemetallicity relation,integrals of motion,action space and the GC orbits to identify the GCs as either formed in situ(Bulge and Disk)or ex situ(via accretion).We find that 45.3%have formed in situ,while 38.4%may be related to known merger events:Gaia-Sausage-Enceladus,the Sagittarius dwarf galaxy,the Helmi streams,the Sequoia galaxy and the Kraken galaxy.We also further identify three new sub-structures associated with the Gaia-Sausage-Enceladus.The remaining 16.3%of GCs are unrelated to the known mergers and thought to be from small accretion events.We select 46 GCs which have radii 8.0<r<37.3 kpc and obtain the anisotropy parameterβ=0.315_(-0.049)^(+0.055),which is lower than the recent result using the sample of GCs in Gaia Data Release 2,but still in agreement with it by considering the error bar.By using the same sample,we obtain the MW mass inside the outermost GC as M(<37.3 kpc)=0.423_(-0.02)^(+0.02)×10^(12)M_(⊙),and the corresponding M_(200)=1.11_(-0.18)^(+0.25)×10^(12)M_(⊙).The estimated mass is consistent with the results in many recent studies.We also find that the estimatedβand mass depend on the selected sample of GCs.However,it is difficult to determine whether a GC fully traces the potential of the MW.
基金supported by the Ministry of Science and Technology(MOST)-BRICS Flagship Project 2018YFE0120800National SKA Program of China No.2020SKA0110401+6 种基金the National Key R&D Program 2017YFA0402603the National Natural Science Foundation of China(NSFC,Grant Nos.11973047,11633004 and U1631118)the Chinese Academy of Sciences(CAS)Strategic Priority Research Program XDA15020200the CAS Frontier Science Key Project QYZDJ–SSW–SLH017the CAS Inter-disciplinary Innovation Team(JCTD-2019-05)the CAS Key Instruments project ZDKYYQ20200008the Hebei Key Laboratory of Radio Astronomy Technology(HKLRAT)。
文摘A great challenge for 21 cm intensity mapping experiments is the strong foreground radiation which is orders of magnitude brighter than the 21 cm signal.Removal of the foreground takes advantage of the fact that its frequency spectrum is smooth while the redshifted 21 cm signal spectrum is stochastic.However,a complication is the nonsmoothness of the instrument response.This paper describes the electromagnetic simulation of the Tianlai cylinder array,a pathfinder for 21 cm intensity mapping experiments.Due to the vast scales involved,a direct simulation requires a large amount of computing resources.We have made the simulation practical by using a combination of methods:first simulate a single feed,then an array of feed units,finally with the feed array and a cylindrical reflector together,obtain the response for a single cylinder.We studied its radiation pattern,bandpass response and the effects of mutual coupling between feed units,and compared the results with observation.Many features seen in the measurement result are reproduced well in the simulation,especially the oscillatory features which are associated with the standing waves on the reflector.The mutual coupling between feed units is quantified with Sparameters,which decrease as the distance between the two feeds increases.Based on the simulated S-parameters,we estimate the correlated noise which has been seen in the visibility data,and the results show very good agreement with the data in both magnitude and frequency structures.These results provide useful insights on the problem of 21 cm signal extraction for real instruments.
基金support of the National SKA program of China(Nos.2022SKA0110100 and 2022SKA0110101)the National Natural Science Foundation of China(NSFC,Grant Nos.1236114814,12203061,12273070,and 12303004)。
文摘This paper presents the design,calibration,and survey strategy of the Fast Radio Burst(FRB)digital backend and its real-time data processing pipeline employed in the Tianlai Cylinder Pathfinder Array.The array,consisting of three parallel cylindrical reflectors and equipped with 96 dual-polarization feeds,is a radio interferometer array designed for conducting drift scans of the northern celestial semi-sphere.The FRB digital backend enables the formation of 96 digital beams,effectively covering an area of approximately 40 square degrees with the 3 dB beam.Our pipeline demonstrates the capability to conduct an automatic search of FRBs,detecting at quasi-realtime and classifying FRB candidates automatically.The current FRB searching pipeline has an overall recall rate of88%.During the commissioning phase,we successfully detected signals emitted by four well-known pulsars:PSR B0329+54,B2021+51,B0823+26,and B2020+28.We report the first discovery of an FRB by our array,designated as FRB 20220414A.We also investigate the optimal arrangement for the digitally formed beams to achieve maximum detection rate by numerical simulation.
基金supported by the MOST 863 Project (No. 2012AA121701)the National Natural Science Foundation of China (Grant No. 11073024)+1 种基金CAS grant KJCX2-EW-W01the John Templeton Foundation
文摘In a semi-numerical model of reionization, the evolution of ionization fraction is approximately simulated by the criterion of ionizing photon to baryon ratio. We incorporate a semi-analytical model of galaxy formation based on the Millennium II N-body simulation into the semi-numerical modeling of reionization. The semianalytical model is used to predict the production of ionizing photons, then we use the semi-numerical method to model the reionization process. Such an approach allows more detailed modeling of the reionization, and also connects observations of galaxies at low and high redshifts to the reionization history. The galaxy formation model we use was designed to match the low-z observations, and it also fits the high redshift luminosity function reasonably well, but its prediction about star formation falls below the observed value, and we find that it also underpredicts the stellar ionizing photon production rate, hence the reionization cannot be completed at z ~ 6. We also consider simple modifications of the model with more top heavy initial mass functions, which can allow the reionization to occur at earlier epochs. The incorporation of the semi-analytical model may also affect the topology of the HI regions during the epoch of reionization, and the neutral regions produced by our simulations with the semi-analytical model, which appeared less poriferous than the simple halo-based models.
基金We acknowledge the support of the National SKA program of China(2022SKA0110100,2022SKA0110101)the Natural Science Foundation of China(12273070,12203061,1236114814,12303004).
文摘Detecting primordial fluctuations from the cosmic dark ages requires extremely large low-frequency radio telescope arrays deployed on the far side of the Moon.The antenna of such an array must be lightweight,easily storable and transportable,deployable on a large scale,durable,and capable of good electrical performance.A membrane antenna is an excellent candidate to meet these criteria.We study the design of a low-frequency membrane antenna for a lunar-based low-frequency(<30 MHz)radio telescope constructed from polyimide film widely used in aerospace applications,owing to its excellent dielectric properties and high stability as a substrate material.We first design and optimize an antenna in free space through dipole deformation and coupling principles,then simulate an antenna on the lunar surface with a simple lunar soil model,yielding an efficiency greater than 90%in the range of 12-19 MHz and greater than 10%in the range of 5-35 MHz.The antenna inherits the omni-directional radiation pattern of a simple dipole antenna in the 5-30 MHz frequency band,giving a large field of view and allowing detection of the 21 cm global signal when used alone.A demonstration prototype is constructed,and its measured electrical property is found to be consistent with simulated results using|S11|measurements.This membrane antenna can potentially fulfill the requirements of a lunar low-frequency array,establishing a solid technical foundation for future large-scale arrays for exploring the cosmic dark ages.
基金the National Natural Science Foundation of China(No.31772062)Gannan Camellia Industry Development and Innovative Center Open Fund(Grant No.YK201610).
文摘The growth characteristics of Aspergillus parasitic us incubated on two culture media were ex-amined using shortwave infrared(SWIR,1000-2500 nm)hyperspectral imaging(HSI)in this work.HSI images of the A.parasiticus colonies growing on rose bengal medium(RBM)and maize agar medium(MAM)were recorded daily for 6 days.The growth phases of A.parasiticus were indicated through the pixel number and average spectra of colonies.On score plot of the first principal component(PC1)and PC2,four growth zones with varying mycelium densities were identified.Eight characteristic wavelengths(1095,1145,1195,1279,1442,1655,1834 and 1929 nm)were selected from PC1 loading,average spectra of each colony as well as each growth zone.F urthermore,support vector machine(S VM)classifier based on the eight wavelengths was built,and the classification accuracies for the four zones(from outer to inner zones)on the colonies on RBM were 99.77%,9935%,99.75%and 99.60%and 99.77%,9939%,99.31%and 98.22%for colonies on MAM.In addition,a new score plot of PC2 and PC3 was used to differ-entiate the colonies incubated on RBM and MAM for 6 days.Then characteristic wavelengths of 1067,1195,1279,1369,1459,1694,1834 and 1929 nm were selected from the loading of PC2 and PCg.Based on them,a new SVM model was developed to diferentiate colonies on RBM and MAM with accuracy of 100.00%and 9999%,respectively.In conclusion,SWIR hyperspectral image is a powerful tool for evaluation of growth characteristics of A.parasiticus incubated in diferent culture media.
文摘In section‘Track decoding’of this article,one of the paragraphs was inadvertently missed out after the text'…shows the flow diagram of the Tr2-1121 track mode.'The missed paragraph is provided below.
基金supported by the National Natural Science Foundation of China(NNSFC)(Nos.12375123,12205160,and 12335008)the Natural Science Foundation of Henan Province,China(No.242300421048)the postgraduate research and practice innovation project of Henan Normal University(No.YB202402).
文摘We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The framework integrates advanced algorithms for precise calibration,accurate particle identification,and efficient event reconstruction,aiming to account for critical experimental factors such as charge-sharing effects,multi-hit event resolution,and detector response nonuniformity.Its robust performance was demonstrated through the successful analysis of light-charged particles in the 25 MeV/u^(86)Kr+^(124)Sn experiment conducted at the first Radioactive Ion Beam Line in Lanzhou,allowing for precise extraction of physical observables,including energy,momentum,and particle type.Furthermore,utilizing the reconstructed physical information,such as the number of effective physical events and energy spectra to optimize the track recognition algorithm,the final track recognition efficiencies of approximately 90%were achieved.This framework establishes a valuable reference methodology for SSDT-based detector systems in heavy-ion reaction experiments,thereby significantly enhancing the accuracy and efficiency of data analysis in nuclear physics research.
基金supported by the National Natural Science Foundation of China(Grant Nos.12335008 and 12205160)the support of the Center for High Performance Computing and Initiative Scientific Research Program in Tsinghua University。
文摘By combining femtoscopic interferometry with an optical deblurring algorithm,we present a novel method to image the source in heavy-ion collisions(HICs),while simultaneously determining the interaction strength between particle pairs.The spatial distribution of the emission source has been reconstructed for protons(p)and antiprotons(^(-)p)from the respective pp and^(-)p^(-)p correlation functions in Au+Au collisions at√S_(NN)=200 GeV.Within experimental uncertainties,protons and antiprotons share the same freeze-out distribution showing higher density in the center compared to the widely assumed Gaussian shape.The results evidence the matter–antimatter symmetry in coordinate space at the freeze-out moment before the nucleons are fully randomized in the collisions.
基金supported by the Polar Research Institute of China and the Chinese Arctic and Antarctic Administrationsupported by the Chinese Academy of Science Key Instrument(ZDKYYQ20200008)the National Natural Science Foundation of China(12473094 and 12273070).
文摘The redshifted 21 cm line,arising from neutral hydrogen,offers a unique probe into the intergalactic medium and the first stars and galaxies formed in the early universe.However,detecting this signal is a challenging task because of artificial radio-frequency interference(RFI)and systematic errors such as ground effects.The interior of the Antarctic continent provides an excellent location to make such observations,with minimal RFI and relatively stable foreground signals.Moreover,a flat plateau in central Antarctica,with an ice cap over 2000 m deep,will show less ground reflection of radio waves,reducing the signal complexity in the area around the probing antenna.It may be advantageous to perform cosmological 21 cm experiments in Antarctica,and a 21 cm Antarctic global spectrum experiment can potentially be deployed on the Antarctic ice cap.We have performed preliminary instrumental design,system calibration,and implementation of such an instrument optimized for extreme cold and capable of long-term autonomous operation.This system shows the ability to effectively detect the 21 cm signal,confirming Antarctica as an excellent observational site for radio cosmology.
基金Supported by the China National Funds for Distinguished Young Scientists(Grant No.11825503)the National Key Research and Development Program of China(Grant No.2020YFA0406400)+1 种基金the 111 Project(Grant No.B20063)the National Natural Science Foundation of China(Grant No.11975033,12070131001,and 12047501).
文摘In 2012,we investigated the possible molecular states composed of two charmed mesons[Phys.Rev.D 88(2013)114008;2012 arXiv:1211.5007[hep-ph]].The D^(*)D𝐷system with the quantum numbers of I(J^(P))=0(1^(+))was found to be a good candidate of the loosely bound molecular state.This state is very close to theD*D threshold with a binding energy around 0.47 MeV.This prediction was confirmed by the new LHCb observation of𝑇T^(+)_(cc)[see Franz Muheim’s talk at the European Physical Society conference on high energy physics 2021].
基金the support of NAOC Astronomical Technology Centersupport of the Ministry of Science and Technology(MOST)grant(2012AA121701)+10 种基金supported by MOST grant(2016YFE0100300)the National Natural Science Foundation of China(NSFC,Grant Nos.11633004 and 11473044)the Chinese Academy of Sciences(CAS)grant(QYZDJ-SSW-SLH017)partially supported by the MOST grant(2018YFE0120800)National Key R&D Program 2017YFA0402603the CAS Interdisciplinary Innovation Team(JCTD-2019-05)Part of the computations are performed on the Tianhe-2 supercomputer(with the support of the NSFC grant U1501501)partially supported by NSF Award(AST-1616554)partial support from CNRS(IN2P3&INSU)Observatoire de ParisIrfu/CEA。
文摘In 21 cm intensity mapping,the spectral smoothness of the foreground is exploited to separate it from the much weaker 21 cm signal.However,the non-smooth frequency response of the instrument complicates this process.Reflections and standing waves generate modulations on the frequency response.Here we report the analysis of the standing waves in the bandpass of the signal channels of the Tianlai Cylinder Array.By Fourier transforming the bandpass into the delay time domain,we find various standing waves generated on the telescope.A standing wave with time delay at~142 ns is most clearly identified which is produced in the 15-meter feed cable.We also identify a strong peak at a shorter delay ofτ<50 ns,which may be a mix of the standing wave between the reflector and feed,and the standing wave on the 4 m intermediate frequency(IF)cable.We also show that a smoother frequency response could be partially recovered by removing the reflection-inducted modulations.However,the standing wave on the antenna is direction-dependent,which poses a more difficult challenge for high precision calibration.
基金supported by the National Key R&D Program of China No.2018YFE0120800the National Natural Science Foundation of China grant No.11973047+1 种基金the National Key R&D Program of China No.2022YFF0504300the National SKA Program of China Nos.2020SKA0110401,and 2020SKA0110402。
文摘Observations are beginning to constrain the history of the epoch of reionization(EoR).Modeling the reionization process is indispensable to interpret the observations,to infer the properties of ionizing sources,and to probe the various astrophysical processes from the observational data.Here we present an improved version of the seminumerical simulation islandFAST,by incorporating inhomogeneous recombinations and a corresponding inhomogeneous ionizing background,and simulate the reionization process of neutral islands during the late EoR.We find that the islands are more fragmented in models with inhomogeneous recombinations than the case with a homogeneous recombination number.In order to investigate the effects of basic assumptions in the reionization modeling,we compare the results from islandFAST with those from 21cmFAST for the same assumptions on the ionizing photon sources and sinks,to find how the morphology of the ionization field and the reionization history depend on the different treatments of these two models.Such systematic bias should be noted when interpreting the upcoming observations.
基金Supported by the National Natural Science Foundation of China
文摘Recent observations show that the spectra of cosmic ray nuclei start to harden above ～ 102 GeV, which contradicts the conventional steady-state cosmic ray model. We had suggested that this anomaly is due to the propagation effect of cosmic rays released from local young cosmic ray sources; the total flux of cosmic rays should be computed with the Myriad Model, where a contribution from sources in the local catalog is added to the background. However, although the hardening could be elegantly explained in this model, the model parameters obtained from the fit are skewed toward a region with fast diffusion and a low supernova rate in the Galaxy, in disagreement with other observations. We further explore this model in order to set up a concordant picture. Two possible improvements related to cosmic ray sources are considered. First, instead of the usual axisymmetric disk model, we examine a spiral model for the source distribution. Second, for nearby and young sources which are necessary to explain the hardening, we allow for an energy-dependent escape. We find that a major improvement comes from incorporating an energy-dependent escape time for local sources, and with both modifications not only are the cosmic ray proton and helium anomalies resolved, but also the parameters attain values in a reasonable range compatible with other analyses.
基金supported by the Ministry of Science and Technology(MOST)2018YFE0120800the National Key R&D Program 2017YFA0402603+2 种基金the National Natural Science Foundation of China(NSFC)grants 11633004 and 11473044the Chinese Academy of Sciences(CAS)grant QYZDJ-SSW-SLH017the Hebei Key Laboratory of Radio Astronomy Technology(HKLRAT)。
文摘The Tianlai Dish Pathfinder Array is a radio interferometer array consisting of 16 six-meter dish antennas.The original digital backend integration time is at the seconds level,designed for H I intensity mapping experiment.A new digital backend with millisecond response is added to enable it to search for fast radio burst during its observations.The design and calibration of this backend,and the real time search pipeline for it are described in this paper.It is capable of forming 16 digital beams for each linear polarization,covering an area of 19.6 square degrees.The search pipeline is capable of searching for,recording and classifying FRBs automatically in real time.In commissioning,we succeeded in capturing the signal pulses from the pulsars PSR B0329+54 and B2021+51.
