Search

This study conducts qualitative research on late adolescent digital music users aged 17–19 to explore their emotional resonance and identities in digital music consumption. The findings indicate that late adolescents are highly dependent on music, with it playing a significant role in their lives, particularly in meeting emotional needs and shaping identities. Late-adolescent digital music users seek to assert themselves through unique and unconventional music tastes. The study also uncovers the coexistence of personalization and socialization in their music-listening behaviors, dividing them into “music-experienced” and “music-socialized” groups. Regarding emotional motivation, the music-experienced group listens to music for personal empathy, while the music-socialized group seeks interpersonal emotional resonance through music-based social interaction. From a practical perspective, this study suggests that the digital music industry should focus on the emotional value generated by music and balance users’ personalization and socialization needs.

This study conducts qualitative research on late adolescent digital music users aged 17–19 to explore their emotional resonance and identities in digital music consumption. The findings indicate that late adolescents are highly dependent on music, with it playing a significant role in their lives, particularly in meeting emotional needs and shaping identities. Late-adolescent digital music users seek to assert themselves through unique and unconventional music tastes. The study also uncovers the coexistence of personalization and socialization in their music-listening behaviors, dividing them into “music-experienced” and “music-socialized” groups. Regarding emotional motivation, the music-experienced group listens to music for personal empathy, while the music-socialized group seeks interpersonal emotional resonance through music-based social interaction. From a practical perspective, this study suggests that the digital music industry should focus on the emotional value generated by music and balance users’ personalization and socialization needs.

This study conducts qualitative research on late adolescent digital music users aged 17–19 to explore their emotional resonance and identities in digital music consumption. The findings indicate that late adolescents are highly dependent on music, with it playing a significant role in their lives, particularly in meeting emotional needs and shaping identities. Late-adolescent digital music users seek to assert themselves through unique and unconventional music tastes. The study also uncovers the coexistence of personalization and socialization in their music-listening behaviors, dividing them into “music-experienced” and “music-socialized” groups. Regarding emotional motivation, the music-experienced group listens to music for personal empathy, while the music-socialized group seeks interpersonal emotional resonance through music-based social interaction. From a practical perspective, this study suggests that the digital music industry should focus on the emotional value generated by music and balance users’ personalization and socialization needs.

GW170817 is the unique gravitational-wave (GW) event that is associated to the electromagnetic (EM) counterpart GRB 170817A. NGC 4993 is identified as the host galaxy of GW170817/GRB 170817A. In this paper, we particularly focus on the spatially resolved properties of NGC 4993. We present the photometric results from the comprehensive data analysis of the high spatial-resolution images in the different optical bands. The morphological analysis reveals that NGC 4993 is a typical early-type galaxy without significant remnants of major galaxy merger. The spatially resolved stellar population properties of NGC 4993 suggest that the galaxy center has passive evolution with the outskirt formed by gas accretion. We derive the merging rate of the compact object per galaxy by a co-evolution scenario of supermassive black hole and its host galaxy. If the galaxy formation is at redshift 1.0, the merging rate per galaxy is $3.2\times 10^{-4}$ to $7.7\times 10^{-5}$ within the merging decay time from 1.0 to 5.0 Gyr. The results provide the vital information for the ongoing GW EM counterpart detections. The HST data analysis presented in this paper can be also applied for the Chinese Space Station Telescope (CSST) research in the future., Comment: RAA accepted

This study conducts qualitative research on late adolescent digital music users aged 17–19 to explore their emotional resonance and identities in digital music consumption. The findings indicate that late adolescents are highly dependent on music, with it playing a significant role in their lives, particularly in meeting emotional needs and shaping identities. Late-adolescent digital music users seek to assert themselves through unique and unconventional music tastes. The study also uncovers the coexistence of personalization and socialization in their music-listening behaviors, dividing them into “music-experienced” and “music-socialized” groups. Regarding emotional motivation, the music-experienced group listens to music for personal empathy, while the music-socialized group seeks interpersonal emotional resonance through music-based social interaction. From a practical perspective, this study suggests that the digital music industry should focus on the emotional value generated by music and balance users’ personalization and socialization needs.

Capturing TC intensity change remains a great challenge for most state-of-the-art operational forecasting systems. Recent studies found TC intensity forecasts are sensitive to three-dimensional ocean dynamics and air-sea interface processes beneath extreme winds. By performing a series of numerical simulations based on hierarchical atmosphere-wave-ocean (AWO) coupling configurations, we showed how atmosphere-ocean and atmosphere-sea wave coupling can affect the intensity of super typhoon Mangkhut (2018). The AWO coupled model can simulate TC-related strong winds, oceanic cold wake, and wind waves with high fidelity. With atmosphere-ocean (AO) coupling implemented, the simulated maximum surface wind speed is reduced by 7 m s−1 compared to the atmosphere-only run, due to TC-induced oceanic cold wakes in the former experiment. In the fully coupled AWO simulations, the wind speed deficit can be completely compensated by the wave-air coupling effect. Further analyses showed that, in the AWO experiment, two mechanisms contribute to the improvement of TC intensity. First, in the high wind scenario (>28 m s−1), the surface drag coefficient reaches an asymptotic level, assisting extreme wind speed to be maintained within the eyewall. Second, the wind speed distribution is modulated and becomes broader; higher wind within the TC area helps to offset the negative effect due to leveling off of the heat exchange coefficient as wind speed increases. Overall, the simulated TC in the AWO run can extract 8–9% more total heat energy from the ocean to maintain its strength, compared to that from the AO experiment.

Capturing TC intensity change remains a great challenge for most state-of-the-art operational forecasting systems. Recent studies found TC intensity forecasts are sensitive to three-dimensional ocean dynamics and air-sea interface processes beneath extreme winds. By performing a series of numerical simulations based on hierarchical atmosphere-wave-ocean (AWO) coupling configurations, we showed how atmosphere-ocean and atmosphere-sea wave coupling can affect the intensity of super typhoon Mangkhut (2018). The AWO coupled model can simulate TC-related strong winds, oceanic cold wake, and wind waves with high fidelity. With atmosphere-ocean (AO) coupling implemented, the simulated maximum surface wind speed is reduced by 7 m s−1 compared to the atmosphere-only run, due to TC-induced oceanic cold wakes in the former experiment. In the fully coupled AWO simulations, the wind speed deficit can be completely compensated by the wave-air coupling effect. Further analyses showed that, in the AWO experiment, two mechanisms contribute to the improvement of TC intensity. First, in the high wind scenario (>28 m s−1), the surface drag coefficient reaches an asymptotic level, assisting extreme wind speed to be maintained within the eyewall. Second, the wind speed distribution is modulated and becomes broader; higher wind within the TC area helps to offset the negative effect due to leveling off of the heat exchange coefficient as wind speed increases. Overall, the simulated TC in the AWO run can extract 8–9% more total heat energy from the ocean to maintain its strength, compared to that from the AO experiment.

We present a detection of 89 candidates of ultra-diffuse galaxies (UDGs) in a 4.9 degree$^2$ field centered on the Hickson Compact Group 95 (HCG 95) using deep $g$- and $r$-band images taken with the Chinese Near Object Survey Telescope. This field contains one rich galaxy cluster (Abell 2588 at $z$=0.199) and two poor clusters (Pegasus I at $z$=0.013 and Pegasus II at $z$=0.040). The 89 candidates are likely associated with the two poor clusters, giving about 50 $-$ 60 true UDGs with a half-light radius $r_{\rm e} > 1.5$ kpc and a central surface brightness $\mu(g,0) > 24.0$ mag arcsec$^{-2}$. Deep $z$'-band images are available for 84 of the 89 galaxies from the Dark Energy Camera Legacy Survey (DECaLS), confirming that these galaxies have an extremely low central surface brightness. Moreover, our UDG candidates are spread over a wide range in $g-r$ color, and $\sim$26% are as blue as normal star-forming galaxies, which is suggestive of young UDGs that are still in formation. Interestingly, we find that one UDG linked with HCG 95 is a gas-rich galaxy with H I mass $1.1 \times 10^{9} M_{\odot}$ detected by the Very Large Array, and has a stellar mass of $M_\star \sim 1.8 \times 10^{8}$ $M_{\odot}$. This indicates that UDGs at least partially overlap with the population of nearly dark galaxies found in deep H I surveys. Our results show that the high abundance of blue UDGs in the HCG 95 field is favored by the environment of poor galaxy clusters residing in H I-rich large-scale structures., Comment: Published in ApJ

We present a detection of 89 candidates of ultra-diffuse galaxies (UDGs) in a 4.9 degree$^2$ field centered on the Hickson Compact Group 95 (HCG 95) using deep $g$- and $r$-band images taken with the Chinese Near Object Survey Telescope. This field contains one rich galaxy cluster (Abell 2588 at $z$=0.199) and two poor clusters (Pegasus I at $z$=0.013 and Pegasus II at $z$=0.040). The 89 candidates are likely associated with the two poor clusters, giving about 50 $-$ 60 true UDGs with a half-light radius $r_{\rm e} > 1.5$ kpc and a central surface brightness $\mu(g,0) > 24.0$ mag arcsec$^{-2}$. Deep $z$'-band images are available for 84 of the 89 galaxies from the Dark Energy Camera Legacy Survey (DECaLS), confirming that these galaxies have an extremely low central surface brightness. Moreover, our UDG candidates are spread over a wide range in $g-r$ color, and $\sim$26% are as blue as normal star-forming galaxies, which is suggestive of young UDGs that are still in formation. Interestingly, we find that one UDG linked with HCG 95 is a gas-rich galaxy with H I mass $1.1 \times 10^{9} M_{\odot}$ detected by the Very Large Array, and has a stellar mass of $M_\star \sim 1.8 \times 10^{8}$ $M_{\odot}$. This indicates that UDGs at least partially overlap with the population of nearly dark galaxies found in deep H I surveys. Our results show that the high abundance of blue UDGs in the HCG 95 field is favored by the environment of poor galaxy clusters residing in H I-rich large-scale structures., Comment: Published in ApJ

It remains challenging to detect the low surface brightness structures of faint high-z galaxies, which is key to understanding the structural evolution of galaxies. The technique of image stacking allows us to measure the averaged light profile beneath the detection limit and probe the extended structure of a group of galaxies. We carry out simulations to examine the recovery of the averaged surface brightness profile through stacking model HST/ACS images of a set of galaxies as functions of Sersic index (n), effective radius (Re) and axis ratio (AR). The Sersic profile best fitting the radial profile of the stacked image is taken as the recovered profile, in comparison with the intrinsic mean profile of the model galaxies. Our results show that, in general, the structural parameters of the mean profile can be properly determined through stacking, although systematic biases need to be corrected when spreads of Re and AR are counted. We find that Sersic index is slightly overestimated and Re is underestimated at AR < 0.5 as the stacked image appears to be more compact due to the presence of inclined galaxies; the spread of Re biases the stacked profile to have a higher Sersic index. We stress that the measurements of structural parameters through stacking should take these biases into account. We estimate the biases in the recovered structural parameters from stacks of galaxies when the samples have distributions of Re, AR and n seen in local galaxies., Comment: Accepted for publication in AJ

We examine the evolution of dust attenuation curve using a sample of 9504 disk star-forming galaxies (SFGs) selected from the CANDELS and 3D-HST surveys and a new technique relying on the fact that disk SFGs of similar stellar masses at the same cosmic epoch are statistically identical in stellar populations. We attribute the discrepancy in median magnitude between face-on (b/a>0.7) and edge-on (b/a<=0.4) subsamples solely to dust attenuation, and obtain the average attenuation in the rest-frame UV and optical as functions of stellar mass and redshift out to z=2.5. Our results show that the attenuation curve becomes remarkably flatter at increasing redshift for both massive and low-mass disk SFGs, and remains likely unchanged with galaxy stellar mass at a fixed epoch within uncertainties. Compared with the Calzetti law, our dust attenuation curves appear to be slightly steeper at 0.5

We note that the coefficients in Tables 2, 3 and 4 are incorrect due to a typo in our numerical codes. The correct coefficients are presented below. In addition, L0M and L0H in Eq. 16 represent ln(z/z0) and ln(z/z0h), respectively. These errors do not affect the methodology and conclusions in the original article. We apologize for any inconvenience this may have caused.

It remains challenging to detect the low surface brightness structures of faint high-z galaxies, which is key to understanding the structural evolution of galaxies. The technique of image stacking allows us to measure the averaged light profile beneath the detection limit and probe the extended structure of a group of galaxies. We carry out simulations to examine the recovery of the averaged surface brightness profile through stacking model HST/ACS images of a set of galaxies as functions of Sersic index (n), effective radius (Re) and axis ratio (AR). The Sersic profile best fitting the radial profile of the stacked image is taken as the recovered profile, in comparison with the intrinsic mean profile of the model galaxies. Our results show that, in general, the structural parameters of the mean profile can be properly determined through stacking, although systematic biases need to be corrected when spreads of Re and AR are counted. We find that Sersic index is slightly overestimated and Re is underestimated at AR < 0.5 as the stacked image appears to be more compact due to the presence of inclined galaxies; the spread of Re biases the stacked profile to have a higher Sersic index. We stress that the measurements of structural parameters through stacking should take these biases into account. We estimate the biases in the recovered structural parameters from stacks of galaxies when the samples have distributions of Re, AR and n seen in local galaxies., Comment: Accepted for publication in AJ

We examine the evolution of dust attenuation curve using a sample of 9504 disk star-forming galaxies (SFGs) selected from the CANDELS and 3D-HST surveys and a new technique relying on the fact that disk SFGs of similar stellar masses at the same cosmic epoch are statistically identical in stellar populations. We attribute the discrepancy in median magnitude between face-on (b/a>0.7) and edge-on (b/a<=0.4) subsamples solely to dust attenuation, and obtain the average attenuation in the rest-frame UV and optical as functions of stellar mass and redshift out to z=2.5. Our results show that the attenuation curve becomes remarkably flatter at increasing redshift for both massive and low-mass disk SFGs, and remains likely unchanged with galaxy stellar mass at a fixed epoch within uncertainties. Compared with the Calzetti law, our dust attenuation curves appear to be slightly steeper at 0.5

Long Short-Term Memory (LSTM) is widely used in speech recognition. In order to achieve higher prediction accuracy, machine learning scientists have built larger and larger models. Such large model is both computation intensive and memory intensive. Deploying such bulky model results in high power consumption and leads to high total cost of ownership (TCO) of a data center. In order to speedup the prediction and make it energy efficient, we first propose a load-balance-aware pruning method that can compress the LSTM model size by 20x (10x from pruning and 2x from quantization) with negligible loss of the prediction accuracy. The pruned model is friendly for parallel processing. Next, we propose scheduler that encodes and partitions the compressed model to each PE for parallelism, and schedule the complicated LSTM data flow. Finally, we design the hardware architecture, named Efficient Speech Recognition Engine (ESE) that works directly on the compressed model. Implemented on Xilinx XCKU060 FPGA running at 200MHz, ESE has a performance of 282 GOPS working directly on the compressed LSTM network, corresponding to 2.52 TOPS on the uncompressed one, and processes a full LSTM for speech recognition with a power dissipation of 41 Watts. Evaluated on the LSTM for speech recognition benchmark, ESE is 43x and 3x faster than Core i7 5930k CPU and Pascal Titan X GPU implementations. It achieves 40x and 11.5x higher energy efficiency compared with the CPU and GPU respectively., Comment: Accepted as full paper in FPGA'17, Monterey, CA; Also appeared at 1st International Workshop on Efficient Methods for Deep Neural Networks at NIPS 2016, Barcelona, Spain

A new non-iterative approach has been developed to calculate surface fluxes. The range -5< (Formula pressented.) and (Formula pressented.) 30 is divided into eight regions, and in each of the regions, multiple linear regression is performed to obtain non-iterative solutions for surface fluxes. As compared to the other two most recent non-iterative schemes, we show that the suggested scheme has the smallest bias. The maximum relative errors of turbulent transfer coefficients for momentum CM and sensible heat CH, as compared to those obtained from the classic iterative method, are always smaller than 2 % from our new non-iterative scheme. © 2015, Springer Science+Business Media Dordrecht.

Based on classic iterative computation results, new equations to calculate the surface turbulent transfer coefficients are proposed, which allow for large ratios of the momentum and heat roughness lengths. Compared to the Launiainen scheme, our proposed scheme generates results closer to classical iterative computations. Under unstable stratification, the relative error in the Launiainen scheme increases linearly with increasing instability, even exceeding 15%, while the relative error of the present scheme is always less than 8.5%. Under stable stratification, the Launiainen scheme uses two equations, one for 0 < RiB ≤ 0.08 and another for 0.08 < RiB ≤ 0.2, and does not consider the condition that RiB > 0.2, while its relative errors in the region 0 < RiB ≤ 0.2 exceed 31 and 24% for momentum and heat transfer coefficients, respectively. In contrast, the present scheme uses only one equation for 0 < RiB ≤ 0.2 and another equation for RiB > 0.2, and the relative error of the present scheme is always less than 14%. © 2010 Springer Science+Business Media B.V.

Porphyry Cu-Au mineralisation related elements and fault-activity indicator elements from stream sediments geochemical data are integrated by log-ratio transformation-based principal component analysis, the results of which are further analysed by singularity theory and spectrum-area model. Identified geochemical anomalies spatially coincident with structural framework are not only suggestive of the presence of mineralisation but also suggest genetic relationship between mineralisation and regional fault structures. The usefulness of the singularity theory and spectrum-area model, as two mature and effective geo-information extraction methods in the fractal/multifractal context, is compared based on their theoretical foundations and practical applications. It was found that, in the study area, the spectrum-area model is more effective for characterising self-similar spatial patterns caused by specific geological processes, while the singularity theory can inform about geochemical behaviours of elements or element associations reflecting a series of geological processes. Compared to the results of the singularity technique, the results of spectrum-area modelling results, especially the geochemical background patterns, are more robust for interpreting structural framework and metallogenic background of the area. This study infers mesh-like structural control on porphyry mineralisation, and identified background geochemical patterns of multi-element association by fractal/multifractal analysis further provide indirect and/or proxy geo-information of the mesh-like structure to support mineral exploration in the Duolong mineral district., Porphyry Cu-Au mineralisation related elements and fault-activity indicator elements from stream sediments geochemical data are integrated by log-ratio transformation-based principal component analysis, the results of which are further analysed by singularity theory and spectrum-area model. Identified geochemical anomalies spatially coincident with structural framework are not only suggestive of the presence of mineralisation but also suggest genetic relationship between mineralisation and regional fault structures. The usefulness of the singularity theory and spectrum-area model, as two mature and effective geo-information extraction methods in the fractal/multifractal context, is compared based on their theoretical foundations and practical applications. It was found that, in the study area, the spectrum-area model is more effective for characterising self-similar spatial patterns caused by specific geological processes, while the singularity theory can inform about geochemical behaviours of elements or element associations reflecting a series of geological processes. Compared to the results of the singularity technique, the results of spectrum-area modelling results, especially the geochemical background patterns, are more robust for interpreting structural framework and metallogenic background of the area. This study infers mesh-like structural control on porphyry mineralisation, and identified background geochemical patterns of multi-element association by fractal/multifractal analysis further provide indirect and/or proxy geo-information of the mesh-like structure to support mineral exploration in the Duolong mineral district.