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1. Extragalactic fast X-ray transient from a weak relativistic jet associated with a Type Ic-BL supernova

Author

Sun, H., Li, W. -X., Liu, L. -D., Gao, H., Wang, X. -F., Yuan, W., Zhang, B., Filippenko, A. V., Xu, D., An, T., Ai, S., Brink, T. G., Liu, Y., Liu, Y. -Q., Wang, C. -Y., Wu, Q. -Y., Wu, X. -F., Yang, Y., Zhang, B. -B., Zheng, W. -K., Ahumada, T., Dai, Z. -G., Delaunay, J., Elias-Rosa, N., Benetti, S., Fu, S. -Y., Howell, D. A., Huang, Y. -F., Kasliwal, M. M., Karambelkar, V., Stein, R., Lei, W. -H., Lian, T. -Y., Peng, Z. -K., Ridnaia, A. V., Svinkin, D. S., Wang, X. -Y., Wang, A. -L., Wei, D. -M., An, J., Andrews, M., Bai, J. -M, Dai, C. -Y., Ehgamberdiev, S. A., Fan, Z., Farah, J., Feng, H. -C., Fynbo, J. P. U., Guo, W. -J., Guo, Z., Hu, M. -K., Hu, J. -W., Jiang, S. -Q., Jin, J. -J., Li, A., Li, J. -D., Li, R. -Z., Liang, Y. -F., Ling, Z. -X., Liu, X., Mao, J. -R., McCully, C., Mirzaqulov, D., Newsome, M., Gonzalez, E. Padilla, Pan, X., Terreran, G., Tinyanont, S., Wang, B. -T., Wang, L. -Z., Wen, X. -D., Xiang, D. -F., Xue, S. -J., Yang, J., Zhu, Z. -P., Cai, Z. -M., Castro-Tirado, A. J., Chen, F. -S., Chen, H. -L., Chen, T. -X., Chen, W., Chen, Y. -H., Chen, Y. -F., Chen, Y., Cheng, H. -Q., Cordier, B., Cui, C. -Z., Cui, W. -W., Dai, Y. -F., Fan, D. -W., Feng, H., Guan, J., Han, D. -W., Hou, D. -J., Hu, H. -B., Huang, M. -H., Huo, J., Jia, S. -M., Jia, Z. -Q., Jiang, B. -W., Jin, C. -C., Jin, G., Kuulkers, E., Li, C. -K., Li, D. -Y., Li, J. -F., Li, L. -H., Li, M. -S., Li, W., Li, Z. -D., Liu, C. -Z, Liu, H. -Y., Liu, H. -Q., Liu, M. -J., Lu, F. -J., Luo, L. -D., Ma, J., Mao, X., Nandra, K., O'Brien, P., Pan, H. -W., Rau, A., Rea, N., Sanders, J., Song, L. -M., Sun, S. -L., Sun, X. -J., Tan, Y. -Y., Tang, Q. -J., Tao, Y. -H., Wang, H., Wang, J., Wang, L., Wang, W. -X., Wang, Y. -L., Wang, Y. -S., Xiong, D. -R., Xu, H. -T., Xu, J. -J., Xu, X. -P., Xu, Y. -F., Xu, Z., Xue, C. -B., Xue, Y. -L., Yan, A. -L., Yang, H. -N., Yang, X. -T., Yang, Y. -J., Zhang, C., Zhang, J., Zhang, M., Zhang, S. -N., Zhang, W. -D., Zhang, W. -J., Zhang, Y. -H., Zhang, Z., Zhang, Z. -L., Zhao, D. -H., Zhao, H. -S., Zhao, X. -F., Zhao, Z. -J., Zhou, Y. -L., Zhu, Y. -X., and Zhu, Z. -C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Massive stars end their life as core-collapse supernovae, amongst which some extremes are Type Ic broad-lined supernovae associated with long-duration gamma-ray bursts (LGRBs) having powerful relativistic jets. Their less-extreme brethren make unsuccessful jets that are choked inside the stars, appearing as X-ray flashes or low-luminosity GRBs. On the other hand, there exists a population of extragalactic fast X-ray transients (EFXTs) with timescales ranging from seconds to thousands of seconds, whose origins remain obscure. Known sources that contribute to the observed EFXT population include the softer analogs of LGRBs, shock breakouts of supernovae, or unsuccessful jets. Here, we report the discovery of the bright X-ray transient EP240414a detected by the Einstein Probe (EP), which is associated with the Type Ic supernova SN 2024gsa at a redshift of 0.401. The X-ray emission evolution is characterised by a very soft energy spectrum peaking at < 1.3 keV, which makes it distinct from known LGRBs, X-ray flashes, or low-luminosity GRBs. Follow-up observations at optical and radio bands revealed the existence of a weak relativistic jet that interacts with an extended shell surrounding the progenitor star. Located on the outskirts of a massive galaxy, this event reveals a new population of explosions of Wolf-Rayet stars characterised by a less powerful engine that drives a successful but weak jet, possibly owing to a progenitor star with a smaller core angular momentum than in traditional LGRB progenitors., Comment: 43 pages, 9 figures, 4 tables, submitted. Comments are welcome

Published
2024

2. Soft X-ray prompt emission from a high-redshift gamma-ray burst EP240315a

Author

Liu, Y., Sun, H., Xu, D., Svinkin, D. S., Delaunay, J., Tanvir, N. R., Gao, H., Zhang, C., Chen, Y., Wu, X. -F., Zhang, B., Yuan, W., An, J., Bruni, G., Frederiks, D. D., Ghirlanda, G., Hu, J. -W., Li, A., Li, C. -K., Li, J. -D., Malesani, D. B., Piro, L., Raman, G., Ricci, R., Troja, E., Vergani, S. D., Wu, Q. -Y., Yang, J., Zhang, B. -B., Zhu, Z. -P., Postigo, A. de Ugarte, Demin, A. G., Dobie, D., Fan, Z., Fu, S. -Y., Fynbo, J. P. U., Geng, J. -J., Gianfagna, G., Hu, Y. -D., Huang, Y. -F., Jiang, S. -Q., Jonker, P. G., Julakanti, Y., Kennea, J. A., Kokomov, A. A., Kuulkers, E., Lei, W. -H., Leung, J. K., Levan, A. J., Li, D. -Y., Li, Y., Littlefair, S. P., Liu, X., Lysenko, A. L., Ma, Y. -N., Martin-Carrillo, A., O'Brien, P., Parsotan, T., Quirola-Vasquez, J., Ridnaia, A. V., Ronchini, S., Rossi, A., Mata-Sanchez, D., Schneider, B., Shen, R. -F., Thakur, A. L., Tohuvavohu, A., Torres, M. A. P., Tsvetkova, A. E., Ulanov, M. V., Wei, J. -J., Xiao, D., Yin, Y. -H. I., Bai, M., Burwitz, V., Cai, Z. -M., Chen, F. -S., Chen, H. -L., Chen, T. -X., Chen, W., Chen, Y. -F., Chen, Y. -H., Cheng, H. -Q., Cui, C. -Z., Cui, W. -W., Dai, Y. -F., Dai, Z. -G., Eder, J., Fan, D. -W., Feldman, C., Feng, H., Feng, Z., Friedrich, P., Gao, X., Guan, J., Han, D. -W, Han, J., Hou, D. -J., Hu, H. -B., Hu, T., Huang, M. -H., Huo, J., Hutchinson, I., Ji, Z., Jia, S. -M., Jia, Z. -Q., Jiang, B. -W., Jin, C. -C., Jin, G., Jin, J. -J., Keereman, A., Lerman, H., Li, J. -F., Li, L. -H., Li, M. -S., Li, W., Li, Z. -D., Lian, T. -Y., Liang, E. -W., Ling, Z. -X., Liu, C. -Z., Liu, H. -Y., Liu, H. -Q., Liu, M. -J., Liu, Y. -R., Lu, F. -J., LU, H. -J., Luo, L. -D., Ma, F. L., Ma, J., Mao, J. -R., Mao, X., McHugh, M., Meidinger, N., Nandra, K., Osborne, J. P., Pan, H. -W., Pan, X., Ravasio, M. E., Rau, A., Rea, N., Rehman, U., Sanders, J., Santovincenzo, A., Song, L. -M., Su, J., Sun, L. -J., Sun, S. -L., Sun, X. -J., Tan, Y. -Y., Tang, Q. -J., Tao, Y. -H., Tong, J. -Z., Wang, H., Wang, J., Wang, L., Wang, W. -X., Wang, X. -F., Wang, X. -Y., Wang, Y. -L., Wang, Y. -S., Wei, D. -M., Willingale, R., Xiong, S. -L., Xu, H. -T., Xu, J. -J., Xu, X. -P., Xu, Y. -F., Xu, Z., Xue, C. -B., Xue, Y. -L., Yan, A. -L., Yang, F., Yang, H. -N., Yang, X. -T., Yang, Y. -J, Yu, Y. -W., Zhang, J., Zhang, M., Zhang, S. -N., Zhang, W. -D., Zhang, W. -J., Zhang, Y. -H., Zhang, Z., Zhang, Z. -L., Zhao, D. -H., Zhao, H. -S., Zhao, X. -F., Zhao, Z. -J., Zhou, L. -X., Zhou, Y. -L., Zhu, Y. -X., Zhu, Z. -C., and Zuo, X. -X.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Long gamma-ray bursts (GRBs) are believed to originate from core collapse of massive stars. High-redshift GRBs can probe the star formation and reionization history of the early universe, but their detection remains rare. Here we report the detection of a GRB triggered in the 0.5--4 keV band by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated as EP240315a, whose bright peak was also detected by the Swift Burst Alert Telescope and Konus-Wind through off-line analyses. At a redshift of $z=4.859$, EP240315a showed a much longer and more complicated light curve in the soft X-ray band than in gamma-rays. Benefiting from a large field-of-view ($\sim$3600 deg$^2$) and a high sensitivity, EP-WXT captured the earlier engine activation and extended late engine activity through a continuous detection. With a peak X-ray flux at the faint end of previously known high-$z$ GRBs, the detection of EP240315a demonstrates the great potential for EP to study the early universe via GRBs., Comment: 41 pages, 8 figures, 7 tables

Published
2024

3. Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of H$\beta$ Emission in Mrk 142

Author

Khatu, V. C., Gallagher, S. C., Horne, K., Cackett, E. M., Hu, C., Pasquini, S., Hall, P., Wang, J. -M., Bian, W. -H., Li, Y. -R., Bai, J. -M., Chen, Y. -J., Du, P., Goad, M., Jiang, B. -W., Li, S. -S., Songsheng, Y. -Y., Wang, C., Xiao, M., and Yu, Z.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We performed a rigorous reverberation-mapping analysis of the broad-line region (BLR) in a highly accreting ($L/L_{\mathrm{Edd}}=0.74-3.4$) active galactic nucleus, Markarian 142 (Mrk 142), for the first time using concurrent observations of the inner accretion disk and the BLR to determine a time lag for the $H\beta$ $\mathrm{\lambda}$4861 emission relative to the ultraviolet (UV) continuum variations. We used continuum data taken with the Niel Gehrels Swift Observatory in the UVW2 band, and the Las Cumbres Observatory, Dan Zowada Memorial Observatory, and Liverpool Telescope in the g band, as part of the broader Mrk 142 multi-wavelength monitoring campaign in 2019. We obtained new spectroscopic observations covering the $H\beta$ broad emission line in the optical from the Gemini North Telescope and the Lijiang 2.4-meter Telescope for a total of 102 epochs (over a period of eight months) contemporaneous to the continuum data. Our primary result states a UV-to-$H\beta$ time lag of $8.68_{-0.72}^{+0.75}$ days in Mrk 142 obtained from light-curve analysis with a Python-based Running Optimal Average algorithm. We placed our new measurements for Mrk 142 on the optical and UV radius-luminosity relations for NGC 5548 to understand the nature of the continuum driver. The positions of Mrk 142 on the scaling relations suggest that UV is closer to the "true" driving continuum than the optical. Furthermore, we obtain $\log(M_{\bullet}/M_{\odot}) = 6.32\pm0.29$ assuming UV as the primary driving continuum., Comment: 35 pages, 12 figures, 11 tables, accepted for publication in ApJ

Published
2023

5. The Lobster Eye Imager for Astronomy Onboard the SATech-01 Satellite

Author

Ling, Z. X., Sun, X. J., Zhang, C., Sun, S. L., Jin, G., Zhang, S. N., Zhang, X. F., Chang, J. B., Chen, F. S., Chen, Y. F., Cheng, Z. W., Fu, W., Han, Y. X., Li, H., Li, J. F., Li, Y., Li, Z. D., Liu, P. R., Lv, Y. H., Ma, X. H., Tang, Y. J., Wang, C. B., Xie, R. J., Xue, Y. L., Yan, A. L., Zhang, Q., Bao, C. Y., Cai, H. B., Cheng, H. Q., Cui, C. Z., Dai, Y. F., Fan, D. W., Hu, H. B., Hu, J. W., Huang, M. H., Jia, Z. Q., Jin, C. C., Li, D. Y., Li, J. Q., Liu, H. Y., Liu, M. J., Liu, Y., Pan, H. W., Qiu, Y. L., Sugizaki, M., Sun, H., Wang, W. X., Wang, Y. L., Wu, Q. Y., Xu, X. P., Xu, Y. F., Yang, H. N., Yang, X., Zhang, B., Zhang, M., Zhang, W. D., Zhang, Z., Zhao, D. H., Cong, X. Q., Jiang, B. W., Li, L. H., Qiu, X. B., Sun, J. N., Su, D. T., Wang, J., Wu, C., Xu, Z., Yang, X. M., Zhang, S. K., Zhang, N., Zhu, Y. F., Ban, H. Y., Bi, X. Z., Cai, Z. M., Chen, W., Chen, X., Chen, Y. H., Cui, Y., Duan, X. L., Feng, Z. G, Gao, Y., He, J. W., He, T., Huang, J. J., Li, F., Li, J. S., Li, T. J., Li, T. T., Liu, H. Q., Liu, L., Liu, R., Liu, S., Meng, N., Shi, Q., Sun, A. T., Wang, Y. M., Wang, Y. B., Wu, H. C., Xu, D. X, Yang, Y. Q, Yang, Y., Yu, X. S., Zhang, K. X., Zhang, Y. L., Zhang, Y. H., Zhang, Y. T., Zhou, H., Zhu, X. C., Cheng, J. S., Qin, L., Wang, L., Wang, Q. L., Bai, M., Gao, R. L., Ji, Z., Liu, Y. R., Ma, F. L., Shi, Y. J., Su, J., Tan, Y. Y., Tong, J. Z., Xu, H. T., Xue, C. B., Xue, G. F., and Yuan, W.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

The Lobster Eye Imager for Astronomy (LEIA), a pathfinder of the Wide-field X-ray Telescope of the Einstein Probe (EP) mission, was successfully launched onboard the SATech-01 satellite of the Chinese Academy of Sciences on 27 July 2022. In this paper, we introduce the design and on-ground test results of the LEIA instrument. Using state-of-the-art Micro-Pore Optics (MPO), a wide field-of-view (FoV) of 346 square degrees (18.6 degrees * 18.6 degrees) of the X-ray imager is realized. An optical assembly composed of 36 MPO chips is used to focus incident X-ray photons, and four large-format complementary metal-oxide semiconductor (CMOS) sensors, each of 6 cm * 6 cm, are used as the focal plane detectors. The instrument has an angular resolution of 4 - 8 arcmin (in FWHM) for the central focal spot of the point spread function, and an effective area of 2 - 3 cm2 at 1 keV in essentially all the directions within the field of view. The detection passband is 0.5 - 4 keV in the soft X-rays and the sensitivity is 2 - 3 * 10-11 erg s-1 cm-2 (about 1 mini-Crab) at 1,000 second observation. The total weight of LEIA is 56 kg and the power is 85 W. The satellite, with a design lifetime of 2 years, operates in a Sun-synchronous orbit of 500 km with an orbital period of 95 minutes. LEIA is paving the way for future missions by verifying in flight the technologies of both novel focusing imaging optics and CMOS sensors for X-ray observation, and by optimizing the working setups of the instrumental parameters. In addition, LEIA is able to carry out scientific observations to find new transients and to monitor known sources in the soft X-ray band, albeit limited useful observing time available., Comment: Accepted by RAA

Published
2023
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8. A Simple Prognostic Scoring System for Hepatocellular Carcinoma Treated with DEB-TACE

Author

Jiang B, Lu D, Dai J, Li K, Du Q, Xie B, Xie J, Zhu X, and Xie X

Subjects
hepatocellular carcinoma, transcatheter arterial chemoembolization, prognosis prediction model, Neoplasms. Tumors. Oncology. Including cancer and carcinogens, RC254-282
Abstract

Bo Jiang,1 Dong Lu,2 Jiaying Dai,3 Kunfeng Li,4 Qianqian Du,1 Bo Xie,5 Jun Xie,6 Xianhai Zhu,2 Xiang Xie1 1Department of Interventional Ultrasound, The Second Affiliated Hospital, Anhui Medical University, Hefei, Anhui, 230022, People’s Republic of China; 2Department of Interventional Radiology, The First Affiliated Hospital of USTC, Division of Life Sciences & Medicine, University of Science & Technology of China, Hefei, 230001, People’s Republic of China; 3Department of Interventional Radiology, Anqing Municipal Hospital, Anqing, Anhui, 246000, People’s Republic of China; 4Department of Radiology, Tongling People’s Hospital, Tongling, Anhui, 244300, People’s Republic of China; 5Department of Interventional Radiology, The First Affiliated Hospital of Bengbu Medical University, Bengbu, 233000, People’s Republic of China; 6Department of Radiology, Fuyang People’s Hospital, Fuyang, Anhui, 236600, People’s Republic of ChinaCorrespondence: Xiang Xie, Department of Interventional Ultrasound, The Second Affiliated Hospital, Anhui Medical University, Hefei, Anhui, 230022, People’s Republic of China, Email 15956922618@163.comObjective: To develop a simple and effective prognostic scoring system to predict the efficacy of drug-eluting bead-transcatheter arterial chemoembolization (DEB-TACE) in the treatment of hepatocellular carcinoma (HCC).Methods: Data were retrospectively collected from 230 patients with HCC who received DEB-TACE treatment at six medical centers between January 2019 and December 2022. We developed a predictive score based on independent risk factors for overall survival (OS), validated the model using a validation cohort, and compared its prognostic accuracy with commonly used HCC staging systems.Results: The number of tumors, albumin-bilirubin levels, alpha-fetoprotein levels, and portal vein thrombus grade were identified as independent factors influencing OS. Based on these factors, we established the DEB-TACE treatment of HCC (DTH) scoring system. The DTH score correlated well with OS, which decreased as the DTH score increased. According to the DTH score, patients were categorized into three risk groups: low-risk (DTH-A, 0– 4 points), medium-risk (DTH-B, 5– 6 points), and high-risk (DTH-A, 7 points). The OS of each risk group was 18.73± 0.62 months, 12.73± 0.10 months, and 6.93± 0.19 months, respectively (p< 0.001). The external cohort validation confirmed the accuracy of the DTH score, demonstrating superior predictive performance compared to other commonly used HCC scoring systems.Conclusion: The DTH-HCC scoring system effectively predicts the outcomes of HCC patients undergoing DEB-TACE as initial treatment. This model can aid in the initial planning and decision-making process for DEB-TACE treatment in HCC patients.Keywords: hepatocellular carcinoma, transcatheter arterial chemoembolization, prognosis prediction model

Published
2024

9. First wide field-of-view X-ray observations by a lobster eye focusing telescope in orbit

Author

Zhang, C., Ling, Z. X., Sun, X. J., Sun, S. L., Liu, Y., Li, Z. D., Xue, Y. L., Chen, Y. F., Dai, Y. F., Jia, Z. Q., Liu, H. Y., Zhang, X. F., Zhang, Y. H., Zhang, S. N., Chen, F. S., Cheng, Z. W., Fu, W., Han, Y. X., Li, H., Li, J. F., Li, Y., Liu, P. R., Ma, X. H., Tang, Y. J., Wang, C. B., Xie, R. J., Yan, A. L., Zhang, Q., Jiang, B. W., Jin, G., Li, L. H., Qiu, X. B., Su, D. T., Sun, J. N., Xu, Z., Zhang, S. K., Zhang, Z., Zhang, N., Bi, X. Z., Cai, Z. M., He, J. W., Liu, H. Q., Zhu, X. C., Cheng, H. Q., Cui, C. Z., Fan, D. W., Hu, H. B., Huang, M. H., Jin, C. C., Li, D. Y., Pan, H. W., Wang, W. X., Xu, Y. F., Yang, X., Zhang, B., Zhang, M., Zhang, W. D., Zhao, D. H., Bai, M., Ji, Z., Liu, Y. R., Ma, F. L., Su, J., Tong, J. Z., Wang, Y. S., Zhao, Z. J., Feldman, C., O'Brien, P., Osborne, J. P., Willingale, R., Burwitz, V., Hartner, G., Langmeier, A., Müller, T., Rukdee, S., Schmidt, T., Kuulkers, E., and Yuan, W.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

As a novel X-ray focusing technology, lobster eye micro-pore optics (MPO) feature both a wide observing field of view and true imaging capability, promising sky monitoring with significantly improved sensitivity and spatial resolution in soft X-rays. Since first proposed by Angel (1979), the optics have been extensively studied, developed and trialed over the past decades. In this Letter, we report on the first-light results from a flight experiment of the Lobster Eye Imager for Astronomy ($LEIA$), a pathfinder of the wide-field X-ray telescope of the Einstein Probe mission. The piggyback imager, launched in July 2022, has a mostly un-vignetted field of view of $18.6^\circ \times 18.6^\circ $. Its spatial resolution is in the range of 4$-$7 arcmin in FWHM and the focal spot effective area is 2$-$3 cm$^2$, both showing only mild fluctuations across the field of view. We present images of the Galactic center region, Sco X-1 and the diffuse Cygnus Loop nebular taken in snapshot observations over 0.5$-$4 keV. These are truly wide-field X-ray images of celestial bodies observed, for the first time, by a focusing imaging telescope. Initial analyses of the in-flight data show excellent agreement between the observed images and the on-ground calibration and simulations. The instrument and its characterization are briefly described, as well as the flight experiment. The results provide a solid basis for the development of the present and proposed wide-field X-ray missions using lobster eye MPO., Comment: 11 pages, 4 figures. Accepted for publication in Astrophysical Journal Letter

Published
2022
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10. Unravelling the nature of the dual AGN in the galaxy pair system IRAS 05589+2828 and 2MASX J06021107+2828382

Author

Benítez, E., Jiménez-Bailón, E., Negrete, C. A., Ruschel-Dutra, D., Rodríguez-Espinosa, J. M., Cruz-González, I., Rodríguez, L. F., Chavushyan, V. H., Marziani, P., Gutiérrez, L., González-Martin, O., Jiang, B. W., and D'Onofrio, M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have studied the nuclear region of the previously detected dual AGN system in the galaxy pair IRAS 05589+2828 and 2MASX J06021107+2828382 through new optical spectroscopy observations, along with radio and X-ray archival data. Our multiwavelength data strongly suggest that the Sy1 \iras\, (z=0.0330$\pm$0.0002) conforms to a dual AGN system with the Sy2 \twomas\, (z=0.0334$\pm$0.0001) with a projected separation obtained from the radio data of 20.08\arcsec\, ($\sim$13.3\,kpc). Analysis of the optical spectra reveals a faint narrow extended emission from H$\alpha$ and [OIII] amidst the two AGN, supporting evidence for an ongoing merger. \iras\, is a double component narrow emission line AGN, with complex broad Balmer emission line profiles that clearly show a strong red-peaklet with a velocity shift of $\sim$3500\,km\,s$^{-1}$. The black hole mass estimates of \iras\, and \twomas\, are log\,M$\rm_{BH}$\,=\,8.59\,$\pm$\,0.14 (M$_\odot$) and log\,M$\rm_{BH}$\,=\,8.21$\pm$0.2 (M$_\odot$), respectively. In the X-ray bands, \iras\, is compatible with a Type 1 object, showing both spectral and flux variability. \chandra\, data of 2MASX\,J06021107+2828382 allowed us to measure a high hardness ratio in this source, providing evidence for a Type 2 AGN. The 22 GHz image obtained with the {\it Karl G. Jansky Very Large Array} has revealed that both AGN are compact radio objects with spectral indices -0.26$\pm$0.03 and -0.70$\pm$0.11, confirming for the first time its dual AGN nature in the radio bands., Comment: Accepted for publication in MNRAS. 20 pages, 15 figures

Published
2022
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13. Exploring the Molecular Mechanisms and Shared Gene Signatures Between Systemic Lupus Erythematosus and Bladder Urothelial Carcinoma

Author

Wang K, Wang S, Ding Y, Kou Z, Jiang B, and Hou S

Subjects
systemic lupus erythematosus, bladder urothelial carcinoma, gene signatures, immune response, mmp9, Medicine (General), R5-920
Abstract

Kongjia Wang,1 Shufei Wang,2 Yixin Ding,3 Zengshun Kou,1 Bo Jiang,1 Sichuan Hou1 1Department of Urology, Qingdao Municipal Hospital, Qingdao University, Qingdao, People’s Republic of China; 2College of Clinical and Basic Medical Sciences, Shandong First Medical University & Shandong Academy of Medical Sciences, Jinan, People’s Republic of China; 3Department of Oncology, The Affiliated Hospital of Qingdao University, Qingdao, People’s Republic of ChinaCorrespondence: Bo Jiang; Sichuan Hou, Email jiangboqdy@126.com; housichuandoctor@126.comBackground: Systemic lupus erythematosus (SLE) is a chronic autoimmune disease associated with increased susceptibility to cancer, including bladder urothelial carcinoma (BLCA). This study investigates the shared molecular mechanisms and gene signatures between SLE and BLCA, shedding light on potential biomarkers and therapeutic targets.Methods: We compiled gene datasets related to SLE and BLCA from various databases and identified common genes. Differential gene expression analysis, protein-protein interaction networks, and hub gene identification were performed. We studied functional enrichment, immune infiltration, and transcription factor/miRNA regulation networks. We also explored gene-disease interactions and protein-chemical/drug networks. Hub gene expression levels and diagnostic values were validated in TCGA and GEO databases. Prognostic analysis was performed on the core gene MMP9 in the TCGA-BLCA database to study its prognostic value. Finally, the mRNA expression of MMP9 was verified in bladder cancer cell lines and BLCA patient blood. The diagnostic value of MMP9 for BLCA was verified by receiver operating characteristic(ROC) curve analysis of the expression of MMP9 in patients’ blood.Results: We identified 524 common genes between SLE and BLCA, enriched in pathways related to apoptosis and cytokine regulation. Immune infiltration analysis for two diseases. Transcription factors and microRNAs were implicated in regulating these common genes. The gene-disease network linked hub genes with various diseases, emphasizing their roles in autoimmune disease and cancer. Protein-chemical/drug networks highlighted potential treatment options. Finally, our study found that MMP9 is a potential therapeutic target with diagnostic and prognostic value and Immune-related biomarkers in patients with BLCA and SLE.Conclusion: Our study reveals shared molecular mechanisms, genetic signatures, and immune infiltrates between SLE and BLCA. MMP9 emerges as a potential diagnostic and prognostic biomarker in BLCA, warranting further investigation. These findings provide insights into the pathogenesis of SLE-associated BLCA and may guide future research and therapeutic strategies.Keywords: systemic lupus erythematosus, bladder urothelial carcinoma, gene signatures, immune response, MMP9

Published
2024

14. Neutron capture measurement and resonance parameter analysis of natSm

Author

Li, X. X., Liu, L. X., Jiang, W., Ren, J., Wang, H. W., Fan, G. T., He, J. J., Wang, D. X., Zhang, S. Y, An, Z. D., Cao, X. G., Song, L. L., Zhang, Y., Hu, X. R., Hao, Z. R., Kuang, P., Jiang, B., Wang, X. H., Hu, J. F., Liu, Y. D., Ma, X., Ma, C. W., Wang, Y. T., Su, J., Zhang, L. Y., Yang, Y. X., Liu, W. B., Su, W. Q., Jin, S., and Chen, K. J.

Subjects
Nuclear Experiment
Abstract

Multiple isotopes of samarium element are the isotopes produced by the s process, and 154Sm is produced by the r process. In addition, 144Sm is p nuclei in nuclear astrophysics. The measurement of these can help us to better understand the results of relevant photonuclear reaction experiments. On the other hand, 149Sm is a 235U fission product with a 1% yield, its cross sections are important to reactor neutronics. In this work, the neutron capture yield of the natural samarium target was measured at the back-streaming white neutron beamline (Back-n) of the China Spallation Neutron Source (CSNS), and the resonance parameters were analyzed by SAMMY code. The resonance peaks and the neutron separation energies contributed by the different isotopes are considered individually. The results of the capture yield found signs of the possibility of two resonance peaks at 8 eV, which awaits further experimental examination. Cross-section was calculated according to resonance parameters and was compared with other experimental results and evaluation databases of ENDF/B-VIII.0 and CENDL-3.2. A clear difference between ENDF/B VIII.0 and CENDL-3.2 database appears at 23.2 eV, the experimental result at this energy is smaller than data of ENDF/B VIII.0 database but CENDL-3.2 database. Most of the controversial experimental results invariably come from the samarium 149 isotope., Comment: 10 pages,7 figures

Published
2022

18. Dust distributions in the Magellanic Clouds

Author

Chen, B. -Q., Guo, H. -L., Gao, J., Yang, M., Liu, Y. -L., and Jiang, B. -W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present high-resolution maps of the dust reddening in the Magellanic Clouds (MCs). The maps cover the Large and Small Magellanic Cloud (LMC and SMC) area and have a spatial angular resolution between $\sim$ 26 arcsec and 55 arcmin. Based on the data from the optical and near-infrared (IR) photometric surveys, including the Gaia Survey, the SkyMapper Southern Survey (SMSS), the Survey of the Magellanic Stellar History (SMASH), the Two Micron All Sky Survey (2MASS) and the near-infrared $YJK_{\rm{S}}$ VISTA survey of the Magellanic Clouds system (VMC), we have obtained multi-band photometric stellar samples containing over 6 million stars in the LMC and SMC area. Based on the measurements of the proper motions and parallaxes of the individual stars from Gaia Early Data Release 3 (Gaia EDR3), we have built clean samples that contain stars from the LMC, SMC and Milky Way (MW), respectively. We apply the spectral energy distribution (SED) fitting to the individual sample stars to estimate their reddening values. As a result, we have derived the best-fitting reddening values of ~ 1.9 million stars in the LMC, 1.5 million stars in the SMC and 0.6 million stars in the MW, which are used to construct dust reddening maps in the MCs. Our maps are consistent with those from the literature. The resultant high-resolution dust maps in the MCs are not only important tools for reddening correction of sources in the MCs, but also fundamental for the studies of the distribution and properties of dust in the two galaxies., Comment: 13 pages, 14 figures, accepted for publication in MNRAS

Published
2022
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22. On Granulation and Irregular Variation of Red Supergiants

Author

Ren, Yi and Jiang, B. W.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The mechanism and characteristics of the irregular variations of red supergiants (RSGs) are studied based on the RSG samples in Small Magellanic Cloud (SMC), Large Magellanic Cloud (LMC) and M31. With the time-series data from All-Sky Automated Survey for SuperNovae (ASAS-SN) and Intermediate Palomar Transient Factory survey, we use the continuous time autoregressive moving average model to estimate the variability features of the light curves and their power spectral density. The characteristic evolution timescale and amplitude of granulations are further derived from fitting the posterior power spectral density with the COR function, which is a Harvey-like granulation model. The consistency of theoretical predictions and results is checked to verify the correctness of the assumption that granulations on RSGs contribute to irregular variation. The relations between granulation and stellar parameters are obtained and compared with the results of red giant branch stars and Betelgeuse. It is found that the relations are in agreement with predictions from basic physical process of granulation and fall close to the extrapolated relations of RGB stars. The granulations in most of the RSGs evolve at a timescale of several days to a year with the characteristic amplitude of 10-1000 mmag. The results imply that the irregular variations of RSGs can be attributed to the evolution of granulations. When comparing the results from SMC, LMC and M31, the timescale and amplitude of granulation seem to increase with metallicity. The analytical relations of the granulation parameters with stellar parameters are derived for the RSG sample of each galaxy., Comment: 27 pages, 12 figures, 5 tables, accepted for publication in ApJ

Published
2020
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23. The post-maximum behaviour of the changing-look Seyfert galaxy NGC 1566

Author

Oknyansky, V. L., Winkler, H., Tsygankov, S. S., Lipunov, V. M., Gorbovskoy, E. S., van Wyk, F., Buckley, D. A. H., Jiang, B. W., and Tyurina, N. V.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present results of the long-term multi-wavelength study of optical, UV and X-ray variability of the nearby changing-look (CL) Seyfert NGC 1566 observed with the Swift Observatory and the MASTER Global Robotic Network from 2007 to 2019. We started spectral observations with South African Astronomical Observatory 1.9-m telescope soon after the brightening was discovered in July 2018 and present here the data for the interval between Aug. 2018 to Sep. 2019. This paper concentrates on the remarkable post-maximum behaviour after July 2018 when all bands decreased with some fluctuations. We observed three significant re-brightenings in the post-maximum period during 17 Nov. 2018 - 10 Jan. 2019, 29 Apr. - 19 Jun. 2019 and 27 Jul.- 6 Aug. 2019. An X-ray flux minimum occurred in Mar. 2019. The UV minimum occurred about 3 months later. It was accompanied by a decrease of the Luv/Lx ratio. New post-maximum spectra covering (31 Nov. 2018 - 23 Sep. 2019) show dramatic changes compared to 2 Aug. 2018, with fading of the broad lines and [Fe X]6374 until Mar. 2019. These lines became somewhat brighter in Aug.-Sep. 2019. Effectively, two CL states were observed for this object: changing to type 1.2 and then returning to the low state as a type 1.8 Sy. We suggest that the changes are due mostly to fluctuations in the energy generation. The estimated Eddington ratios are about 0.055% for minimum in 2014 and 2.8% for maximum in 2018., Comment: 11 pages, 9 figured, accepted for publication in MNRAS

Published
2020
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24. On Carbon Nanotubes in the Interstellar Medium

Author

Li, Qi, Li, Aigen, Jiang, B. W., and Chen, Tao

Subjects
Astrophysics - Astrophysics of Galaxies, Condensed Matter - Materials Science
Abstract

Since their discovery in 1991, carbon nanotubes (CNTs) -- a novel one-dimensional carbon allotrope -- have attracted considerable interest worldwide because of their potential technological applications such as electric and optical devices. In the astrophysical context, CNTs may be present in the interstellar space since many of the other allotropes of carbon (e.g., amorphous carbon, fullerenes, nanodiamonds, graphite, polycyclic aromatic hydrocarbons, and possibly graphene as well) are known to be widespread in the Universe, as revealed by presolar grains in carbonaceous primitive meteorites and/or by their fingerprint spectral features in astronomical spectra. In addition, there are also experimental and theoretical pathways to the formation of CNTs in the interstellar medium (ISM). In this work, we examine their possible presence in the ISM by comparing the observed interstellar extinction curve with the ultraviolet/optical absorption spectra experimentally obtained for single-walled CNTs of a wide range of diameters and chiralities. Based on the absence in the interstellar extinction curve of the ~4.5 and 5.25 eV $\pi$-plasmon absorption bands which are pronounced in the experimental spectra of CNTs, we place an upper limit of ~10 ppm of C/H (i.e., ~4% of the total interstellar C) on the interstellar CNT abundance., Comment: 7 pages, 2 figures; accepted for publication in MNRAS

Published
2020
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26. How Much Graphene in Space?

Author

Li, Qi, Li, Aigen, and Jiang, B. W.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The possible presence of graphene in the interstellar medium (ISM) is examined by comparing the interstellar extinction curve with the ultraviolet absorption of graphene calculated from its dielectric functions experimentally obtained with the electron energy loss spectroscopy (EELS) method. Based on the absence in the interstellar extinction curve of the ~2755 Angstrom $\pi$--$\pi^{\ast}$ electronic interband transition of graphene, we place an upper limit of ~20ppm of C/H on the interstellar graphene abundance, exceeding the previous estimate by a factor of ~3 which made use of the dielectric functions measured with the spectroscopic ellipsometry (SE) method. Compared with the SE method which measures graphene in air (and hence its surface is contaminated) in a limited energy range of ~0.7--5 eV, the EELS probes a much wider energy range of ~0--50 eV and is free of contamination. The fact that the EELS dielectric functions are substantially smaller than that of SE naturally explains why a higher upper limit on the graphene abundance is derived with EELS. Inspired by the possible detection of C$_{24}$, a planar graphene sheet, in several Galactic and extragalactic planetary nebulae, we also examine the possible presence of C$_{24}$ in the diffuse ISM by comparing the model IR emission of C$_{24}$ with the observed IR emission of the Galactic cirrus and the diffuse ISM toward $l = 44^{o}20^\prime$ and $b=-0^{o}20^\prime$. An upper limit of ~20 ppm on C$_{24}$ is also derived from the absence of the characteristic vibrational bands of C$_{24}$ at ~6.6, 9.8 and 20 $\mu$m in the observed IR emission., Comment: 9 pages, 5 figures; accepted for publication in MNRAS

Published
2019
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27. Three dimensional dust mapping of 12 supernovae remnants in the Galactic anticentre

Author

Yu, Bin, Chen, B. Q., Jiang, B. W., and Zijlstra, A.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present three dimensional (3D) dust mapping of 12 supernova remnants (SNRs) in the Galactic anti-center (Galactic longitude $l$ between 150\degr\ and 210\degr) based on a recent 3D interstellar extinction map. The dust distribution of the regions which cover the full extents in the radio continuum for the individual SNRs are discussed. Four SNRs show significant spatial coincidences between molecular clouds (MCs) revealed from the 3D extinction mapping and the corresponding radio features. The results confirm the interactions between these SNRs and their surrounding MCs. Based on these correlations, we provide new distance estimates of the four SNRs, G189.1+3.0 (IC443, $d=1729^{+116}_{-94} \rm \,pc$), G190.9-2.2 ($d=1036^{+17}_{-81} \rm \,pc$), G205.5+0.5 ($d=941^{+96}_{-94}$ or $1257^{+92}_{-101} \rm \,pc$) and G213.0-0.6 ($d=1146^{+79}_{-80} \rm \,pc$). In addition, we find indirect evidences of potential interactions between SNRs and MCs for three other SNRs. New distance constraints are also given for these three SNRs., Comment: 14 pages, 13 figures, accepted for publication in MNRAS

Published
2019
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29. Topological background discrimination in the PandaX-III neutrinoless double beta decay experiment

Author

Galan, J, Chen, X, Du, H, Fu, C, Giboni, K, Giuliani, F, Han, K, Jiang, B, Ji, X, Lin, H, Lin, Y, Liu, J, Ni, K, Ren, X, Wang, S, Wu, S, Xie, C, Yang, Y, Zhang, D, Zhang, T, Zhao, L, Aune, S, Bedfer, Y, Berthoumieux, E, Calvet, D, d'Hose, N, Ferrer-Ribas, E, Kunne, F, Manier, B, Neyret, D, Papaevangelou, T, Chen, L, Hu, S, Jian, S, Li, P, Li, X, Zhang, H, Zhao, M, Zhou, J, Mao, Y, Qiao, H, Yuan, Y, Wang, M, Chen, Y, Khan, A N, Raper, N, Tang, J, Wang, W, Feng, C, Li, C, Liu, S, Wang, X, Zhu, D, Castel, J F, Cebrián, S, Dafni, T, Irastorza, I G, Luzón, G, Mirallas, H, Sun, X, Tan, A, Haxton, W, Mei, Y, Kobdaj, C, and Yan, Y

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

The PandaX-III experiment plans to search for neutrinoless double beta decay (0$\nu\beta\beta$) of $^{136}$Xe in the China JinPing underground Laboratory (CJPL). The experiment will use a high pressure gaseous Time Projection Chamber (TPC) to register both the energy and the electron track topology of an event. This article is devoted to the software side of the experiment. As software tool we use REST, a framework developed for the reconstruction and simulation of TPC-based detector systems. We study the potential for background reduction by introducing appropiate parameters based on the properties of 0$\nu\beta\beta$ events. We exploit for the first time not only the energy density of the electron track-ends, but also the electron scattering angles produced by an electron near the end of its trajectory. To implement this, we have added new algorithms for detector signal and track processing inside REST. Their assessment shows that background can be reduced by about 7 orders of magnitude while keeping 0$\nu\beta\beta$ efficiency above 20% for the PandaX-III baseline readout scheme, a 2-dimensional 3mm-pitch stripped readout. More generally, we use the potential of REST to handle 2D/3D data to assess the impact on signal-to-background significance at different detector granularities, and to validate the PandaX-III baseline choice. Finally, we demonstrate the potential to discriminate surface background events generated at the readout plane in the absence of $t_o$, by making use of event parameters related with the diffusion of electrons., Comment: 40 pages, 15 figures. Prepared for submission to Journal of Physics G

Published
2019
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30. The Period-Luminosity Relations of Red Supergiants in M33 and M31

Author

Ren, Yi, Jiang, B. W., Yang, Ming, and Gao, Jian

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Based on previously selected preliminary samples of Red Supergiants (RSGs) in M33 and M31, the foreground stars and luminous Asymptotic Giant Branch stars (AGBs) are further excluded, which leads to the samples of 717 RSGs in M33 and 420 RSGs in M31. With the time-series data from the iPTF survey spanning nearly 2000 days, the period and amplitude of RSGs are analyzed. According to the lightcurves characteristics, they are classified into four categories in which 84 and 56 objects in M33 and M31 respectively are semi-regular variables. For these semi-regular variables, the pulsation mode is identified by comparing with the theoretical model, which yielded 19 (7) sources in the first overtone mode in M33 (M31), and the other 65 (49) RSGs in M33 (M31) in the fundamental mode. The period-luminosity (P-L) relation is analyzed for the RSGs in the fundamental mode. It is found the P-L relation is tight in the infrared, i.e. the 2MASS $JHK_{\rm S}$ bands and the short-wavelength bands of Spitzer. Meanwhile, the inhomogeneous extinction causes the P-L relation scattering in the $V$ band, and the dust emission causes the less tight P-L relation in the Spitzer/[8.0] and [24] bands. The derived P-L relations in the 2MASS/$K_{\rm S}$ band are in agreement with those of RSGs in SMC, LMC and the Milky Way within the uncertainty range. It is found that the number ratio of RSGs pulsating in the fundamental mode to the first overtone mode increases with metallicity., Comment: 110 pages, 22 figures, 7 tables, accepted for publication in ApJS

Published
2019
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31. Photonic crystals for nano-light in moir\'e graphene superlattices

Author

Sunku, S. S., Ni, G. X., Jiang, B. -Y., Yoo, H., Sternbach, A., McLeod, A. S., Stauber, T., Xiong, L., Taniguchi, T., Watanabe, K., Kim, P., Fogler, M. M., and Basov, D. N.

Subjects
Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

Graphene is an atomically thin plasmonic medium that supports highly confined plasmon polaritons, or nano-light, with very low loss. Electronic properties of graphene can be drastically altered when it is laid upon another graphene layer, resulting in a moir\'e superlattice. The relative twist angle between the two layers is a key tuning parameter of the interlayer coupling in thus obtained twisted bilayer graphene (TBG). We studied propagation of plasmon polaritons in TBG by infrared nano-imaging. We discovered that the atomic reconstruction occurring at small twist angles transforms the TBG into a natural plasmon photonic crystal for propagating nano-light. This discovery points to a pathway towards controlling nano-light by exploiting quantum properties of graphene and other atomically layered van der Waals materials eliminating need for arduous top-down nanofabrication.

Published
2019
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33. Multiple topological phases in tetradymite compounds M2Te2P(M=Ti,Zr, or Hf)

Author

Pan, M. J., primary, Li, B.-X., additional, Wang, H., additional, Liu, J. D., additional, Chen, F. M., additional, Huang, J. R., additional, Qu, G. X., additional, Gao, S. Y., additional, Jiang, B., additional, Huang, Y.-B., additional, Shi, X., additional, Xia, T.-L., additional, Weng, H. M., additional, and Qian, T., additional

Published
2024
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34. POS0939 SERUM URATE CHANGE AMONG GOUT PATIENTS TREATED WITH SODIUM-GLUCOSE COTRANSPORTER TYPE 2 INHIBITORS VS. SULFONYLUREA: A COMPARATIVE EFFECTIVENESS ANALYSIS

Author

Yokose, C., primary, Challener, G., additional, Jiang, B., additional, Zhou, B., additional, Mccormick, N., additional, Tanikella, S., additional, Panchot, K., additional, Kohler, M. J., additional, Yinh, J., additional, Zhang, Y., additional, Bates, D., additional, Januzzi, J., additional, Sise, M., additional, Wexler, D., additional, and Choi, H., additional

Published
2024
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37. The Ultraviolet Extinction in the $GALEX$ Bands

Author

Sun, Mingxu, Jiang, B. W., Zhao, He, Gao, Jian, Gao, Shuang, Jian, Mingjie, and Yuan, Haibo

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Interstellar extinction in ultraviolet is the most severe in comparison with optical and infrared wavebands and a precise determination plays an important role in correctly recovering the ultraviolet brightness and colors of objects. By finding the observed bluest colors at given effective temperature and metallicity range of dwarf stars, stellar intrinsic colors, $C^0_{\rm B,V}$, $C^0_{\rm NUV,B}$, $C^0_{\rm FUV,B}$ and $C^0_{\rm FUV,NUV}$, are derived according to the stellar parameters from the LAMOST spectroscopic survey and photometric results from the $GALEX$ and APASS surveys. With the derived intrinsic colors, the ultraviolet color excesses are calculated for about 25,000 A- and F-type dwarf stars. Analysis of the color excess ratios yields the extinction law related to the $GALEX$ UV bands: $E_{{\rm NUV,B}}$/$E_{{\rm B,V}} = 3.77$, $E_{{\rm FUV,B}}$/$E_{{\rm B,V}} = 3.39$, $E_{{\rm FUV,NUV}}$/$E_{{\rm B,V}} = -0.38$. The results agree very well with previous works in the $NUV$ band and in general with the extinction curve derived by Fitzpatrick (1999) for $R_{\rm V}=3.35$., Comment: 31 pages, 16 figures, 3 tables, APJ in press

Published
2018
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38. Probing the 9.7\mu m Interstellar Silicate Extinction Profile through the Spitzer/IRS Spectroscopy of OB Stars

Author

Shao, Z. Z., Jiang, B. W., Li, Aigen, Gao, Jian, Lv, Z. P., and Yao, J. W.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The 9.7$\mu$m interstellar spectral feature, arising from the Si--O stretch of amorphous silicate dust, is the strongest extinction feature in the infrared (IR). In principle, the spectral profile of this feature could allow one to diagnose the mineralogical composition of interstellar silicate material. However, observationally, the 9.7$\mu$m interstellar silicate extinction profile is not well determined. Here we utilize the Spitzer/IRS spectra of five early-type (one O- and four B-type) stars and compare them with that of unreddened stars of the same spectral type to probe the interstellar extinction of silicate dust around 9.7$\mu$m. We find that, while the silicate extinction profiles all peak at ~9.7$\mu$m, two stars exhibit a narrow feature of FWHM ~2.0$\mu$m and three stars display a broad feature of FWHM ~3.0$\mu$m. We also find that the width of the 9.7$\mu$m extinction feature does not show any environmental dependence. With a FWHM of ~2.2$\mu$m, the mean 9.7\mu m extinction profile, obtained by averaging over our five stars, closely resembles that of the prototypical diffuse interstellar medium along the lines of sight toward Cyg OB2 No.12 and WR 98a. Finally, an analytical formula is presented to parameterize the interstellar extinction in the IR at $0.9\mu {\rm m} < \lambda < 15\mu {\rm m}$., Comment: 17 pages, 13 figures, 5 tables; accepted for publication in MNRAS

Published
2018
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39. The Distance and the near-IR extinction of the Monoceros Supernova Remnant

Author

Zhao, H., Jiang, B. W., Gao, S., Li, J., and Sun, M. X.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Supernova remnants (SNRs) embody the information of the influence on dust properties by the supernova explosion. Based on the color indexes from the 2MASS photometric survey and the stellar parameters from the SDSS$-$DR12$/$APOGEE and LAMOST$-$DR2$/$LEGUE spectroscopic surveys, the near-infrared extinction law and the distance of the Monoceros SNR are derived together with its nearby two nebulas -- the Rosette Nebula and NGC 2264. The distance is found at the position of the sharp increase of interstellar extinction with distance and the nebular extinction is calculated by subtracting the foreground interstellar extinction. The distance of the Monoceros SNR is determined to be $1.98\,$kpc, larger than previous values. Meanwhile, the distance of the Rosette Nebula is $1.55\,$kpc, generally consistent with previous work. The distance between these two nebulas suggests no interaction between them. The distance of NGC 2264, $1.20\,$kpc, exceeds previous values. The color excess ratio, $E_{\rm JH}/E_{\rm JK_S}$, is 0.657 for the Monoceros SNR, consistent with the average value 0.652 for the Milky Way (Xue et al. 2016). The consistency is resulted from that the SNR material is dominated by interstellar dust rather than the supernova ejecta. $E_{\rm JH}/E_{\rm JK_S}$ equals to 0.658 for the Rosette Nebula, further proving the universality of the near-infrared extinction law., Comment: 28 pages, 15 figures, accepted by ApJ on February 1, 2018

Published
2018
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40. Soliton superlattices in twisted hexagonal boron nitride.

Author

Ni, GX, Wang, H, Jiang, B-Y, Chen, LX, Du, Y, Sun, ZY, Goldflam, MD, Frenzel, AJ, Xie, XM, Fogler, MM, and Basov, DN

Subjects
MD Multidisciplinary
Abstract

Properties of atomic van der Waals heterostructures are profoundly influenced by interlayer coupling, which critically depends on stacking of the proximal layers. Rotational misalignment or lattice mismatch of the layers gives rise to a periodic modulation of the stacking, the moiré superlattice. Provided the superlattice period extends over many unit cells, the coupled layers undergo lattice relaxation, leading to the concentration of strain at line defects - solitons - separating large area commensurate domains. We visualize such long-range periodic superstructures in thin crystals of hexagonal boron nitride using atomic-force microscopy and nano-infrared spectroscopy. The solitons form sub-surface hexagonal networks with periods of a few hundred nanometers. We analyze the topography and infrared contrast of these networks to obtain spatial distribution of local strain and its effect on the infrared-active phonons of hBN.

Published
2019

41. Data-driven prediction of battery cycle life before capacity degradation

Author

Severson, KA, Attia, PM, Jin, N, Perkins, N, Jiang, B, Yang, Z, Chen, MH, Aykol, M, Herring, PK, Fraggedakis, D, Bazant, MZ, Harris, SJ, Chueh, WC, and Braatz, RD

Subjects
Electrical and Electronic Engineering, Environmental Engineering
Abstract

Accurately predicting the lifetime of complex, nonlinear systems such as lithium-ion batteries is critical for accelerating technology development. However, diverse aging mechanisms, significant device variability and dynamic operating conditions have remained major challenges. We generate a comprehensive dataset consisting of 124 commercial lithium iron phosphate/graphite cells cycled under fast-charging conditions, with widely varying cycle lives ranging from 150 to 2,300 cycles. Using discharge voltage curves from early cycles yet to exhibit capacity degradation, we apply machine-learning tools to both predict and classify cells by cycle life. Our best models achieve 9.1% test error for quantitatively predicting cycle life using the first 100 cycles (exhibiting a median increase of 0.2% from initial capacity) and 4.9% test error using the first 5 cycles for classifying cycle life into two groups. This work highlights the promise of combining deliberate data generation with data-driven modelling to predict the behaviour of complex dynamical systems.

Published
2019

45. On the Optical-to-Silicate Extinction Ratio as a Probe of the Dust Size in Active Galactic Nuclei

Author

Shao, Z. Z., Jiang, B. W., and Li, Aigen

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Dust plays a central role in the unification theory of active galactic nuclei (AGNs). Whether the dust that forms the torus around an AGN is tenth-$\mu$m-sized like interstellar grains or much larger has a profound impact on correcting for the obscuration of the dust torus to recover the intrinsic spectrum and luminosity of the AGN. Here we show that the ratio of the optical extinction in the visual band ($A_V$) to the optical depth of the 9.7 $\mu$m silicate absorption feature ($\Delta\tau_{9.7}$) could potentially be an effective probe of the dust size. The anomalously lower ratio of $A_V/\Delta\tau_{9.7} \approx 5.5$ of AGNs compared to that of the Galactic diffuse interstellar medium of $A_V/\Delta\tau_{9.7} \approx 18$ reveals that the dust in AGN torus could be substantially larger than the interstellar grains of the Milky Way and of the Small Magellanic Cloud, and therefore, one might expect a flat extinction curve for AGNs., Comment: 20 pages, 9 figures; accepted for publication in The Astrophysical Journal

Published
2017
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46. STUDY ON EPOXY RESIN/MULTI-WALLED CARBON NANOTUBES CONDUCTIVE COATING ON AZ31 MAGNESIUM ALLOY AFTER MICRO-ARC OXIDATION.

Author

ZHANG, C., WANG, C., JIANG, B., and SONG, R. G.

Subjects
MAGNESIUM alloy corrosion, MULTIWALLED carbon nanotubes, WEAR resistance, EPOXY resins, CORROSION resistance
Abstract

After micro-arc oxidation, the surface properties of AZ31 magnesium alloy have been improved. However, micro-arc oxidation treatment leads to high insulation, which limits its application in electronic devices. To increase conductivity, a conductive coating was developed by adding multi-walled carbon nanotubes (MWCNTs) to the epoxy resin. The microstructure and performance of the coating were tested by SEM, thermogravimetric analyzer, four-probe conductivity meter, high-temperature friction and wear tester, and electrochemical workstation. The results indicate that the optimal conductivity with a resistivity of 303 Ω ⋅ m is obtained when the MWCNT content is at 4 wt%. In addition, MWCNTs are filled with a network structure of epoxy resin, which increases the density of the coating and enhances their wear and corrosion resistance. [ABSTRACT FROM AUTHOR]

Published
2024
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47. The NuSTAR Serendipitous Survey: The 40 month Catalog and the Properties of the Distant High Energy X-ray Source Population

Author

Lansbury, G. B., Stern, D., Aird, J., Alexander, D. M., Fuentes, C., Harrison, F. A., Treister, E., Bauer, F. E., Tomsick, J. A., Balokovic, M., Del Moro, A., Gandhi, P., Ajello, M., Annuar, A., Ballantyne, D. R., Boggs, S. E., Brandt, N., Brightman, M., Chen, C. J., Christensen, F. E., Civano, F., Comastri, A., Craig, W. W., Forster, K., Grefenstette, B. W., Hailey, C. J., Hickox, R., Jiang, B., Jun, H., Koss, M., Marchesi, S., Melo, A. D., Mullaney, J. R., Noirot, G., Schulze, S., Walton, D. J., Zappacosta, L., and Zhang, W.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the first full catalog and science results for the NuSTAR serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide ~20Ms of effective exposure time over 331 fields, with an areal coverage of 13 sq deg, and 497 sources detected in total over the 3-24 keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic followup. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily comprised of active galactic nuclei (AGNs), detected over a large range in redshift from z = 0.002 - 3.4 (median of = 0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log( f_3-24keV / erg s^-1 cm^-2 ) ~ -14 to -11, and in rest-frame 10-40 keV luminosity, from log( L_10-40keV / erg s^-1 ) ~ 39 to 46, with a median of 44.1. Approximately 79% of the NuSTAR sources have lower energy (<10 keV) X-ray counterparts from XMM-Newton, Chandra, and Swift/XRT. The mid-infrared (MIR) analysis, using WISE all-sky survey data, shows that MIR AGN color selections miss a large fraction of the NuSTAR-selected AGN population, from ~15% at the highest luminosities (Lx > 10^44 erg s^-1) to ~80% at the lowest luminosities (Lx < 10^43 erg s^-1). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the Type 2 fraction) is F_Type2 = 53(+14-15)%, for a well-defined subset of the 8-24 keV selected sample. This is higher, albeit at a low significance level, than the Type 2 fraction measured for redshift- and luminosity-matched AGNs selected by <10 keV X-ray missions., Comment: 49 pages, 23 figures, 8 tables. Accepted for publication in ApJ

Published
2016
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48. Fundamental limits to graphene plasmonics.

Author

Ni, GX, McLeod, AS, Sun, Z, Wang, L, Xiong, L, Post, KW, Sunku, SS, Jiang, B-Y, Hone, J, Dean, CR, Fogler, MM, and Basov, DN

Subjects
MD Multidisciplinary, General Science & Technology
Abstract

Plasmon polaritons are hybrid excitations of light and mobile electrons that can confine the energy of long-wavelength radiation at the nanoscale. Plasmon polaritons may enable many enigmatic quantum effects, including lasing 1 , topological protection2,3 and dipole-forbidden absorption 4 . A necessary condition for realizing such phenomena is a long plasmonic lifetime, which is notoriously difficult to achieve for highly confined modes 5 . Plasmon polaritons in graphene-hybrids of Dirac quasiparticles and infrared photons-provide a platform for exploring light-matter interaction at the nanoscale6,7. However, plasmonic dissipation in graphene is substantial 8 and its fundamental limits remain undetermined. Here we use nanometre-scale infrared imaging to investigate propagating plasmon polaritons in high-mobility encapsulated graphene at cryogenic temperatures. In this regime, the propagation of plasmon polaritons is primarily restricted by the dielectric losses of the encapsulated layers, with a minor contribution from electron-phonon interactions. At liquid-nitrogen temperatures, the intrinsic plasmonic propagation length can exceed 10 micrometres, or 50 plasmonic wavelengths, thus setting a record for highly confined and tunable polariton modes. Our nanoscale imaging results reveal the physics of plasmonic dissipation and will be instrumental in mitigating such losses in heterostructure engineering applications.

Published
2018

49. RPS4Y1 Promotes High Glucose-Induced Endothelial Cell Apoptosis and Inflammation by Activation of the p38 MAPK Signaling

Author

Chen Y, Tang C, Zhao Q, Xu T, Kang Q, Jiang B, and Zhang L

Subjects
rps4y1, huvec, diabetes mellitus, high glucose, p38 mapk signaling, Specialties of internal medicine, RC581-951
Abstract

Yuan Chen,1,&ast; Yiheng Chen,2,&ast; Chonghui Tang,3 Qian Zhao,1 Tailin Xu,1 Qi Kang,1 Bin Jiang,2 Li Zhang4 1Department of Endocrinology, The First People’s Hospital of Zunyi, Zunyi, Guizhou, 563000, People’s Republic of China; 2Department of Hand and Plastic Surgery, The Second Affiliated Hospital of Wenzhou Medical University, Wenzhou, Zhejiang, 325000, People’s Republic of China; 3Department of Neurosurgery, Affiliated Cixi Hospital, Wenzhou Medical University, Wenzhou, Zhejiang, 315300, People’s Republic of China; 4Department of Neurosurgery, China-Japan Friendship Hospital, Beijing, 100029, People’s Republic of China&ast;These authors contributed equally to this workCorrespondence: Li ZhangDepartment of Neurosurgery, China-Japan Friendship Hospital, No. 2 Yinghua East Road, District of Chaoyang, Beijing, 100029, People’s Republic of ChinaEmail ftzy73129@sina.comAim: Endothelial dysfunction is a key pathological basis for diabetes mellitus complications, including diabetic nephropathy, diabetic retinopathy, and diabetic cardiomyopathy. This study aimed to reveal the functional role of ribosomal protein S4 Y-linked 1 (RPS4Y1) in endothelial dysfunction.Methods: Human umbilical vein endothelial cells (HUVECs) were subjected to high glucose. The expression of RPS4Y1 in cells was overexpressed or silenced by plasmid or siRNA transfection. MTT assay, flow cytometry, JC-1 probe, scratch test, tube formation, and ELISA were conducted to assess the effects of RPS4Y1 on cell. Western blot was performed to assay the downstream signaling of RPS4Y1. The inhibitors of p38, ERK, and Jnk were used to treat cells to validate the involvement of them in RPS4Y1-mediated endothelial dysfunction.Results: RPS4Y1 was upregulated in HUVECs in response to high glucose in both dose- and time-dependent manners. Overexpression of RPS4Y1 induced viability loss, apoptosis, and inflammation, but inhibited cell migration and tube formation. Silence of RPS4Y1 impacted these aspects in a contrary trend. The phosphorylation of p38 rather than ERK and Jnk was activated by RPS4Y1. In addition, the dysfunction of HUVECs mediated by RPS4Y1 was attenuated by SB203580 (a specific inhibitor of p38 signaling).Conclusion: The highly expressed RPS4Y1 in endothelial cells may contribute to high glucose-induced dysfunction through regulating p38 MAPK signaling. RPS4Y1 might be a potential therapeutic target for treating diabetes mellitus complications.Keywords: RPS4Y1, HUVEC, diabetes mellitus, high glucose, p38 MAPK signaling

Published
2021

50. Sleep-Related Hypermotor Epilepsy: Etiology, Electro-Clinical Features, and Therapeutic Strategies

Author

Wan H, Wang X, Chen Y, Jiang B, Hu W, Zhang K, and Shao X

Subjects
semiology, seizure onset zone (soz), epileptogenic zone, hypermotor, electroencephalogram, Psychiatry, RC435-571, Neurophysiology and neuropsychology, QP351-495
Abstract

Huijuan Wan,1– 3,&ast; Xing Wang,4,&ast; Yiyi Chen,1,2 Bin Jiang,3 Yangmei Chen,5 Wenhan Hu,6 Kai Zhang,7 Xiaoqiu Shao1,2 1Department of Neurology, Beijing Tiantan Hospital, Capital Medical University, Beijing, People’s Republic of China; 2China National Clinical Research Center for Neurological Diseases (NCRC-ND), Beijing, People’s Republic of China; 3Department of Neurology, First Affiliated Hospital, Xiamen University, Xiamen, People’s Republic of China; 4Department of Neurology, Chongqing University Central Hospital, Chongqing Emergency Medical Centre, Chongqing, People’s Republic of China; 5Department of Neurology, The Second Affiliated Hospital of Chongqing Medical University, Chongqing, People’s Republic of China; 6Beijing Neurosurgical Institute, Capital Medical University, Beijing, People’s Republic of China; 7Department of Neurosurgery, Beijing Tiantan Hospital, Capital Medical University, Beijing, People’s Republic of China&ast;These authors contributed equally to this workCorrespondence: Xiaoqiu ShaoDepartment of Neurology, Beijing Tiantan Hospital, Capital Medical University, No. 119 South 4th Ring West Road, Fengtai District, Beijing, 100070, People’s Republic of ChinaTel +86-135-5203-4066Email shaoxiaoqiu2000@aliyun.comAbstract: Sleep-related hypermotor epilepsy (SHE) is a group of clinical syndromes with heterogeneous etiologies. SHE is difficult to diagnose and treat in the early stages due to its diverse clinical manifestations and difficulties in differentiating from non-epileptic events, which seriously affect patients’ quality of life and social behavior. The overall prognosis for SHE is unsatisfactory, but different etiologies affect patients’ prognoses. Surgical treatment is an effective method for carefully selected patients with refractory SHE; nevertheless, preoperative assessment remains challenging because of the low sensitivity of noninvasive scalp electroencephalogram and imaging to detect abnormalities. However, through a careful analysis of semiology, the clinician can deduce the potential epileptogenic zone. This paper summarizes the research status of the background, etiology, electro-clinical features, diagnostic criteria, prognosis, and treatment of SHE to provide a more in-depth understanding of its pathophysiological mechanism, improve the accuracy in the diagnosis of this group of syndromes, and further explore more targeted therapy plans.Keywords: semiology, seizure onset zone, SOZ, epileptogenic zone, hypermotor, electroencephalogram

Published
2021

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