Multi-frequency study on markarian 421 during the first two years of operation of the MAGIC stereo telescopes

Markarian 421 (Mrk~421) is one of the classical blazars at X-ray and very high energies (VHE; $>$100 GeV). Its spectral energy distribution (SED) can be accurately characterized by current instruments because of its close proximity, which makes Mrk~421 one of the best sources to study the nature of blazars. The goal of this PhD thesis is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk~421. The results might be applied to other blazars which cannot be studied with this level of detail because their emissions are weaker, or they are located further away. This thesis reports results from $\sim$70 hours of observations with MAGIC in 2010 and 2011 (the first two years of the operation of the MAGIC stereo telescopes), as well as the results from the multi-wavelength (MW) observation campaigns in 2010 and 2011, where more than 20 instruments participated, covering energies from radio to VHE. The MW data from the 2010 and 2011 campaigns show that, for both years, the fractional variability $F_{\rm var}$ increases with the energy for both the low-energy and the high-energy bumps in the SED of Mrk~421. Furthermore, $F_{\rm var}(\text{optical})$ was similar to F_{\rm var}(\text{HE-\gamma$-ray;$>100 MeV}), and $F_{\rm var}(\text{X-ray})$ was similar to F_{\rm var}(\text{VHE-\gamma-ray}). This observed characteristic is expected from the strong correlation between the synchrotron photons and the up-scattered photons by inverse-Compton effect within the synchrotron self-Compton (SSC) emission model, thus allowing for the first time of the consistency test on this widely used theoretical model. During the MW campaign in 2010, we measured the decay of a flaring activity during 13 days in March. We could perform MW observations every day, which enables an unprecedented characterization of the time-evolution of the radio to $\gamma$-ray emission of Mrk~421. The broadband SEDs during this flaring episode, resolved on timescales of one day, were characterized with two leptonic scenarios: a one-zone SSC model, and a two-zone SSC model where one zone is responsible for the quiescent emission while the other (smaller) zone, which is spatially separated from the former one, contributes to the daily-variable emission occurring mostly at X-rays and VHE $\gamma$ rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs. However, the two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity. The proposed two-zone scenario would naturally lead to the correlated variability in the X-ray and VHE bands without variability in the optical/UV band, as well as to shorter timescales for the variability in the X-ray and VHE bands with respect to the variability in the other bands. This concept of a second small emission region containing a narrow electron spectrum in order to explain the short timescale flaring activity in the X-ray and VHE bands could be generalized to other blazars. The results from the 2010 March flaring activity of Mrk~421 are reported in Sections~\ref{LightCurves} -- \ref{Discussion}, and they are the main scientific achievement of this PhD thesis. Preliminary results were reported (as an oral contribution) in the 33rd International Cosmic Ray Conference (Rio de Janeiro, July 2013), one of the most prestigious conferences in the field of the VHE astronomy and astro-particle physics in general. The final results (reviewed and approved within the \Fermic, MAGIC, and VERITAS Collaborations) have been submitted for publication in the Astronomy and Astrophysics journal in 2014 June. During the MW campaign in 2011, Mrk~421 had an atypically high activity in the optical band, together with a very low state in the X-ray/VHE band. Typically, blazar emission models for Mrk~421 focus on the explanation of the variability in the X-ray and $\gamma$-ray bands. This data set is suitable for examining emission models and estimate if they can describe the evolution of the whole broadband SEDs including the variabilities in optical, X-ray, and $\gamma$-ray bands. We found that the one-zone SSC model can describe the relatively slow variation of the 2011 broadband SEDs. The modeling of these SEDs shows that the main factor dominating the spectral evolution could be the electron energy distribution (EED), instead of the environmental parameters like the blob size and the Doppler factor. To explain the featured high optical state together with the low X-ray/VHE state, several changes were needed in comparison to the typical state from 2009: a harder power-law index in the first segment in the EED, a lower first break in the EED, and a softer power-law index in the second segment in the EED. Besides, these optical high states had synchrotron peak frequencies 10 times lower than the typical state, while their synchrotron peak energy-fluxes were similar to those of the typical state. On the contrary, the 2010~March flaring activity showed that a high peak energy-flux was accompanied by a high peak frequency in comparison to the typical state, which has also been observed on several other blazars. This contrast showed that the broadband variability in the emission of Mrk~421 during 2011 had a different \emph{flavor} with respect to the typical blazar broadband flaring activity. This PhD thesis shows that most variations in the SED of Mrk~421 can be produced through changes in the EED, which could shed light into how particles get accelerated in the vicinity of super-massive black holes, or within the relativistic jets of the active galactic nuclei. However, the results also show a large complexity in the evolution of the broadband (radio to VHE $\gamma$-rays) SED. Thus longer and deeper observations are needed to understand what characteristics get repeated over time and hence typical, what characteristics are atypical, and ultimately, whether the lessons learned with Mrk~421 can be extended to high-synchrotron-peaked blazars in general

Multi-frequency study on markarian 421 during the first two years of operation of the MAGIC stereo telescopes

Markarian 421 (Mrk~421) is one of the classical blazars at X-ray and very high energies (VHE; $>$100 GeV). Its spectral energy distribution (SED) can be accurately characterized by current instruments because of its close proximity, which makes Mrk~421 one of the best sources to study the nature of blazars. The goal of this PhD thesis is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk~421. The results might be applied to other blazars which cannot be studied with this level of detail because their emissions are weaker, or they are located further away. This thesis reports results from $\sim$70 hours of observations with MAGIC in 2010 and 2011 (the first two years of the operation of the MAGIC stereo telescopes), as well as the results from the multi-wavelength (MW) observation campaigns in 2010 and 2011, where more than 20 instruments participated, covering energies from radio to VHE. The MW data from the 2010 and 2011 campaigns show that, for both years, the fractional variability $F_{\rm var}$ increases with the energy for both the low-energy and the high-energy bumps in the SED of Mrk~421. Furthermore, $F_{\rm var}(\text{optical})$ was similar to F_{\rm var}(\text{HE-\gamma$-ray;$>100 MeV}), and $F_{\rm var}(\text{X-ray})$ was similar to F_{\rm var}(\text{VHE-\gamma-ray}). This observed characteristic is expected from the strong correlation between the synchrotron photons and the up-scattered photons by inverse-Compton effect within the synchrotron self-Compton (SSC) emission model, thus allowing for the first time of the consistency test on this widely used theoretical model. During the MW campaign in 2010, we measured the decay of a flaring activity during 13 days in March. We could perform MW observations every day, which enables an unprecedented characterization of the time-evolution of the radio to $\gamma$-ray emission of Mrk~421. The broadband SEDs during this flaring episode, resolved on timescales of one day, were characterized with two leptonic scenarios: a one-zone SSC model, and a two-zone SSC model where one zone is responsible for the quiescent emission while the other (smaller) zone, which is spatially separated from the former one, contributes to the daily-variable emission occurring mostly at X-rays and VHE $\gamma$ rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs. However, the two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity. The proposed two-zone scenario would naturally lead to the correlated variability in the X-ray and VHE bands without variability in the optical/UV band, as well as to shorter timescales for the variability in the X-ray and VHE bands with respect to the variability in the other bands. This concept of a second small emission region containing a narrow electron spectrum in order to explain the short timescale flaring activity in the X-ray and VHE bands could be generalized to other blazars. The results from the 2010 March flaring activity of Mrk~421 are reported in Sections~\ref{LightCurves} -- \ref{Discussion}, and they are the main scientific achievement of this PhD thesis. Preliminary results were reported (as an oral contribution) in the 33rd International Cosmic Ray Conference (Rio de Janeiro, July 2013), one of the most prestigious conferences in the field of the VHE astronomy and astro-particle physics in general. The final results (reviewed and approved within the \Fermic, MAGIC, and VERITAS Collaborations) have been submitted for publication in the Astronomy and Astrophysics journal in 2014 June. During the MW campaign in 2011, Mrk~421 had an atypically high activity in the optical band, together with a very low state in the X-ray/VHE band. Typically, blazar emission models for Mrk~421 focus on the explanation of the variability in the X-ray and $\gamma$-ray bands. This data set is suitable for examining emission models and estimate if they can describe the evolution of the whole broadband SEDs including the variabilities in optical, X-ray, and $\gamma$-ray bands. We found that the one-zone SSC model can describe the relatively slow variation of the 2011 broadband SEDs. The modeling of these SEDs shows that the main factor dominating the spectral evolution could be the electron energy distribution (EED), instead of the environmental parameters like the blob size and the Doppler factor. To explain the featured high optical state together with the low X-ray/VHE state, several changes were needed in comparison to the typical state from 2009: a harder power-law index in the first segment in the EED, a lower first break in the EED, and a softer power-law index in the second segment in the EED. Besides, these optical high states had synchrotron peak frequencies 10 times lower than the typical state, while their synchrotron peak energy-fluxes were similar to those of the typical state. On the contrary, the 2010~March flaring activity showed that a high peak energy-flux was accompanied by a high peak frequency in comparison to the typical state, which has also been observed on several other blazars. This contrast showed that the broadband variability in the emission of Mrk~421 during 2011 had a different \emph{flavor} with respect to the typical blazar broadband flaring activity. This PhD thesis shows that most variations in the SED of Mrk~421 can be produced through changes in the EED, which could shed light into how particles get accelerated in the vicinity of super-massive black holes, or within the relativistic jets of the active galactic nuclei. However, the results also show a large complexity in the evolution of the broadband (radio to VHE $\gamma$-rays) SED. Thus longer and deeper observations are needed to understand what characteristics get repeated over time and hence typical, what characteristics are atypical, and ultimately, whether the lessons learned with Mrk~421 can be extended to high-synchrotron-peaked blazars in general

X-PuDu at SemEval-2022 Task 7: A Replaced Token Detection Task Pre-trained Model with Pattern-aware Ensembling for Identifying Plausible Clarifications

This paper describes our winning system on SemEval 2022 Task 7: Identifying Plausible Clarifications of Implicit and Underspecified Phrases in Instructional Texts. A replaced token detection pre-trained model is utilized with minorly different task-specific heads for SubTask-A: Multi-class Classification and SubTask-B: Ranking. Incorporating a pattern-aware ensemble method, our system achieves a 68.90% accuracy score and 0.8070 spearman's rank correlation score surpassing the 2nd place with a large margin by 2.7 and 2.2 percent points for SubTask-A and SubTask-B, respectively. Our approach is simple and easy to implement, and we conducted ablation studies and qualitative and quantitative analyses for the working strategies used in our system.Comment: Accepted at the 16th International Workshop on Semantic Evaluation (SemEval-2022), NAAC

Efficient parameter inference for gravitational wave signals in the presence of transient noises using temporal and time-spectral fusion normalizing flow

Glitches represent a category of non-Gaussian and transient noise that frequently intersects with gravitational wave (GW) signals, exerting a notable impact on the processing of GW data. The inference of GW parameters, crucial for GW astronomy research, is particularly susceptible to such interference. In this study, we pioneer the utilization of temporal and time-spectral fusion normalizing flow for likelihood-free inference of GW parameters, seamlessly integrating the high temporal resolution of the time domain with the frequency separation characteristics of both time and frequency domains. Remarkably, our findings indicate that the accuracy of this inference method is comparable to traditional non-glitch sampling techniques. Furthermore, our approach exhibits greater efficiency, boasting processing times on the order of milliseconds. In conclusion, the application of normalizing flow emerges as pivotal in handling GW signals affected by transient noises, offering a promising avenue for enhancing the field of GW astronomy research.Comment: 13 pages, 10 figure

Rapid identification of time-frequency domain gravitational wave signals from binary black holes using deep learning

Recent developments in deep learning techniques have offered an alternative and complementary approach to traditional matched filtering methods for the identification of gravitational wave (GW) signals. The rapid and accurate identification of GW signals is crucial for the progress of GW physics and multi-messenger astronomy, particularly in light of the upcoming fourth and fifth observing runs of LIGO-Virgo-KAGRA. In this work, we use the 2D U-Net algorithm to identify the time-frequency domain GW signals from stellar-mass binary black hole (BBH) mergers. We simulate BBH mergers with component masses from 5 to 80 $M_{\odot}$ and account for the LIGO detector noise. We find that the GW events in the first and second observation runs could all be clearly and rapidly identified. For the third observation run, about $80\%$ GW events could be identified and GW190814 is inferred to be a BBH merger event. Moreover, since the U-Net algorithm has advantages in image processing, the time-frequency domain signals obtained through U-Net can preliminarily determine the masses of GW sources, which could help provide the mass priors for future parameter inferences. We conclude that the U-Net algorithm could rapidly identify the time-frequency domain GW signals from BBH mergers and provide great help for future parameter inferences.Comment: 11 pages, 9 figure

Neuron-Specific HuR-Deficient Mice Spontaneously Develop Motor Neuron Disease

Human Ag R (HuR) is an RNA binding protein in the ELAVL protein family. To study the neuron-specific function of HuR, we generated inducible, neuron-specific HuR-deficient mice of both sexes. After tamoxifen-induced deletion of HuR, these mice developed a phenotype consisting of poor balance, decreased movement, and decreased strength. They performed significantly worse on the rotarod test compared with littermate control mice, indicating coordination deficiency. Using the grip-strength test, it was also determined that the forelimbs of neuron-specific HuR-deficient mice were much weaker than littermate control mice. Immunostaining of the brain and cervical spinal cord showed that HuR-deficient neurons had increased levels of cleaved caspase-3, a hallmark of cell apoptosis. Caspase-3 cleavage was especially strong in pyramidal neurons and α motor neurons of HuR-deficient mice. Genome-wide microarray and real-time PCR analysis further indicated that HuR deficiency in neurons resulted in altered expression of genes in the brain involved in cell growth, including trichoplein keratin filament-binding protein, Cdkn2c, G-protein signaling modulator 2, immediate early response 2, superoxide dismutase 1, and Bcl2. The additional enriched Gene Ontology terms in the brain tissues of neuron-specific HuR-deficient mice were largely related to inflammation, including IFN-induced genes and complement components. Importantly, some of these HuR-regulated genes were also significantly altered in the brain and spinal cord of patients with amyotrophic lateral sclerosis. Additionally, neuronal HuR deficiency resulted in the redistribution of TDP43 to cytosolic granules, which has been linked to motor neuron disease. Taken together, we propose that this neuron-specific HuR-deficient mouse strain can potentially be used as a motor neuron disease model