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270 results on '"Tian, W. -W"'

51. Construction and on-site performance of the LHAASO WFCTA camera

Author

Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, H., Cai, J. T., Cao, Z., Cao, Z., Chang, J., Chang, J. F., Chang, X. C., Chen, B. M., Chen, J., Chen, L., Chen, L., Chen, L., Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, X. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Volpe, D. della, Piazzoli, B. D’Ettorre, Dong, X. J., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, Y. L., Gao, B., Gao, C. D., Gao, Q., Gao, W., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. C., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, Q. L., Huang, W. H., Huang, X. T., Huang, Z. C., Ji, F., Ji, X. L., Jia, H. Y., Jiang, K., Jiang, Z. J., Jin, C., Kuleshov, D., Levochkin, K., Li, B. B., Li, C., Li, C., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, K., Li, W. L., Li, X., Li, X., Li, X. R., Li, Y., Li, Y. Z., Li, Z., Li, Z., Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y. N., Liu, Z. X., Long, W. J., Lu, R., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Mitthumsiri, W., Montaruli, T., Nan, Y. C., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Ruffolo, D., Rulev, V., Sáiz, A., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. R., Song, H. C., Stenkin, Yu. V., Stepanov, V., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R. N., Wang, W., Wang, W., Wang, X. G., Wang, X. J., Wang, X. Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z., Wang, Z., Wang, Z. H., Wang, Z. X., Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, W. X., Wu, X. F., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, G., Xiao, H. B., Xin, G. G., Xin, Y. L., Xing, Y., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yang, C. W., Yang, F. F., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, J. W., Zhang, L., Zhang, L., Zhang, L. X., Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. R., Zhang, S S., Zhang, X., Zhang, X. P., Zhang, Y., Zhang, Y., Zhang, Y. F., Zhang, Y. L., Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.

Published
2021
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52. Kinematic Study of the Blazar S5 0716+714

Author

Bach, U., Krichbaum, T. P., Ros, E., Britzen, S., Tian, W. W., Kraus, A., Witzel, A., and Zensus, J. A.

Subjects
Astrophysics
Abstract

We present the results of a multi-frequency study of the structural evolution of the VLBI jet in the BL Lac object 0716+714 over the last 10 years. We show VLBI images obtained at 5 GHz, 8.4 GHz, 15 GHz and 22 GHz. The milliarcsecond source structure is best described by a one-sided core-dominated jet of ~10 mas length. Embedded jet components move superluminally with speeds ranging from 5 c to 16 c (assuming z=0.3). Such fast superluminal motion is not typical for BL Lac objects, however it is still in the range of jet speeds typically observed in quasars (10 c to 20 c). In 0716+714, younger components, that were ejected more recently, seem to move systematically slower than the older components. This and a systematic position angle variation of the inner (1 mas) portion of the VLBI jet, suggests an at least partly geometric origin of the observed velocity variations. The observed rapid motion and the derived Lorentz factors are discussed with regard to the rapid Intra-Day Variability (IDV) and the gamma-ray observations, from which very high Doppler factors are inferred., Comment: 12 pages, 9 figures, accepted for publication in A&A, minor language editing and a reference added in section 1 to match the accepted version; Figs. 3 & 4 are in colors now

Published
2004
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53. VLBI, MERLIN and HST observations of the giant radio galaxy 3C236

Author

Schilizzi, R. T., Tian, W. W., Conway, J. E., Nan, R., Miley, G. K., Barthel, P. D., Normandeau, M., Dallacasa, D., and Gurvits, L. I.

Subjects
Astrophysics
Abstract

We present VLBI and MERLIN data at 1.66 and 4.99 GHz on the central component coincident with the nucleus of the giant radio galaxy, 3C236. The nuclear radio structure is composed of two complexes of emission which are resolved on scales from 1 milli-arcsec (mas) to 1 arcsec. Oscillations with an amplitude of about 5 degrees can be seen in the compact radio structure. Spectral index distributions are plotted at angular resolutions of 10 and 25 mas and allow us to identify the core component in the south-east emission complex. Re-examination of the HST WFPC-2 image of 3C236 by de Koff et al. (2000), shows that the normal to the dust disk in the nucleus is ~30 degrees from the plane of the sky and within 12 degrees of parallel to the overall orientation of the radio source. We suggest that the radio axis is also at an angle of ~30 degrees to the plane of the sky and that the north-west jet is on the approaching side. This orientation implies an overall size of 4.5 Mpc (H_o = 75 km/s/Mpc, q_o = 0.5) for 3C236. The coincidence of a dust feature and the south-east compact jet, within the astrometric errors, leads us to suggest that the dust may be in the form of a cloud encountered by the jet in the first ~400 pc of its journey out from the nucleus. One-sided emission at 5 GHz on 1 mas scales would suggest that the jets are ejected initially at <= 35 degrees to the line of sight, but this is difficult to reconcile with the obvious orientation stability of the jet system as a whole. Free-free absorption of the counter-jet may be an alternative explanation for the one-sideness., Comment: 11 pages, 9 figures, accepted for Astronomy and Astrophysics

Published
2000
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54. Pulsars identified from the NRAO VLA Sky Survey

Author

Han, J. L. and Tian, W. W.

Subjects
Astrophysics
Abstract

We identified 97 strong pulsars from the NRAO VLA Sky Survey (NVSS) at 1.4 GHz north of Dec(J2000) $>-40\degr$. The total flux density, linear polarization intensity and polarization angle (PA) of all pulsars are extracted from the NVSS catalog. The well-calibrated PA measurement of 5 pulsars can be used for absolute PA calibrations in other observations. Comparing the source positions with those in the pulsar catalog, we got the first measurement of the proper motion upper limit of PSR B0031-07, which is $\mu_{\alpha}\cos\delta = -102 \pm 74 mas/yr$ and $\mu_{\delta} = -105 \pm 78 mas/yr$., Comment: 7 pages; 3 figures; one big table; To appear in A&A Supplements

Published
1999
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55. P978: IXAZOMIB VERSUS LENALIDOMIDE OR IXAZOMIB AND LENALIDOMIDE COMBINATION AS MAINTENANCE REGIMEN FOR PATIENTS WITH MULTIPLE MYELOMA: INTERIM ANALYSIS OF A MULTI-CENTER PROSPECTIVE STUDY IN CHINA

Author

Zhuang, Z., primary, Tian, Y., additional, Yu, H., additional, Shi, L., additional, Tian, W.-W., additional, Liu, Q., additional, Zou, D., additional, Dong, F., additional, Ma, Y., additional, Feng, R., additional, Liu, S., additional, Liu, H., additional, Jing, H., additional, Sun, W., additional, Ma, L.-M., additional, Bao, L., additional, Fu, R., additional, Wu, Y., additional, Chen, W., additional, and Zhuang, J., additional

Published
2022
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56. PB2038: LENALIDOMIDE OR BORTEZOMIB AS MAINTENANCE TREATMENT OVERCOMES INFERIOR IMPACT OF HIGH-RISK CYTOGENETIC ABNORMALITIES IN TRANSPLANT-INELIGIBLE PATIENTS WITH NEWLY DIAGNOSED MULTIPLE MYELOMA IN CHINA

Author

Zhuang, Z., primary, Tian, Y., additional, Shi, L., additional, Zou, D., additional, Feng, R., additional, Tian, W.-W., additional, Yu, H., additional, Dong, F., additional, Liao, A., additional, Ma, Y., additional, Liu, Q., additional, Liu, S., additional, Jing, H., additional, Fu, R., additional, Ma, L.-M., additional, Liu, H., additional, Sun, W., additional, Bao, L., additional, Wu, Y., additional, Chen, W., additional, and Zhuang, J., additional

Published
2022
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58. Observation of the Crab Nebula with LHAASO-KM2A − a performance study *

Author

Aharonian, F., primary, An, Q., additional, Axikegu, 克古, additional, Bai, L. X., additional, Bai, Y. X., additional, Bao, Y. W., additional, Bastieri, D., additional, Bi, X. J., additional, Bi, Y. J., additional, Cai, H., additional, Cai, J. T., additional, Cao, Z., additional, Chang, J., additional, Chang, J. F., additional, Chang, X. C., additional, Chen, B. M., additional, Chen, J., additional, Chen, L., additional, Chen, M. J., additional, Chen, M. L., additional, Chen, Q. H., additional, Chen, S. H., additional, Chen, S. Z., additional, Chen, T. L., additional, Chen, X. L., additional, Chen, Y., additional, Cheng, N., additional, Cheng, Y. D., additional, Cui, S. W., additional, Cui, X. H., additional, Cui, Y. D., additional, Dai, B. Z., additional, Dai, H. L., additional, Dai, Z. G., additional, Danzengluobu, 罗布, additional, Volpe, D. della, additional, Piazzoli, B. D'Ettorre, additional, Dong, X. J., additional, Fan, J. H., additional, Fan, Y. Z., additional, Fan, Z. X., additional, Fang, J., additional, Fang, K., additional, Feng, C. F., additional, Feng, L., additional, Feng, S. H., additional, Feng, Y. L., additional, Gao, B., additional, Gao, C. D., additional, Gao, Q., additional, Gao, W., additional, Ge, M. M., additional, Geng, L. S., additional, Gong, G. H., additional, Gou, Q. B., additional, Gu, M. H., additional, Guo, J. G., additional, Guo, X. L., additional, Guo, Y. Q., additional, Guo, Y. Y., additional, Han, Y. A., additional, He, H. H., additional, He, H. N., additional, He, J. C., additional, He, S. L., additional, He, X. B., additional, He, Y., additional, Heller, M., additional, Hor, Y. K., additional, Hou, C., additional, Hou, X., additional, Hu, H. B., additional, Hu, S., additional, Hu, S. C., additional, Hu, X. J., additional, Huang, D. H., additional, Huang, Q. L., additional, Huang, W. H., additional, Huang, X. T., additional, Huang, Z. C., additional, Ji, F., additional, Ji, X. L., additional, Jia, H. Y., additional, Jiang, K., additional, Jiang, Z. J., additional, Jin, C., additional, Kuleshov, D., additional, Levochkin, K., additional, Li, B. B., additional, Li, C., additional, Li, F., additional, Li, H. B., additional, Li, H. C., additional, Li, H. Y., additional, Li, J., additional, Li, K., additional, Li, W. L., additional, Li, X., additional, Li, X. R., additional, Li, Y., additional, Li, Y. Z., additional, Li, Z., additional, Liang, E. W., additional, Liang, Y. F., additional, Lin, S. J., additional, Liu, B., additional, Liu, C., additional, Liu, D., additional, Liu, H., additional, Liu, H. D., additional, Liu, J., additional, Liu, J. L., additional, Liu, J. S., additional, Liu, J. Y., additional, Liu, M. Y., additional, Liu, R. Y., additional, Liu, S. M., additional, Liu, W., additional, Liu, Y. N., additional, Liu, Z. X., additional, Long, W. J., additional, Lu, R., additional, Lv, H. K., additional, Ma, B. Q., additional, Ma, L. L., additional, Ma, X. H., additional, Mao, J. R., additional, Masood, A., additional, Mitthumsiri, W., additional, Montaruli, T., additional, Nan, Y. C., additional, Pang, B. Y., additional, Pattarakijwanich, P., additional, Pei, Z. Y., additional, Qi, M. Y., additional, Ruffolo, D., additional, Rulev, V., additional, Sáiz, A., additional, Shao, L., additional, Shchegolev, O., additional, Sheng, X. D., additional, Shi, J. R., additional, Song, H. C., additional, Stenkin, Yu. V., additional, Stepanov, V., additional, Sun, Q. N., additional, Sun, X. N., additional, Sun, Z. B., additional, Tam, P. H. T., additional, Tang, Z. B., additional, Tian, W. W., additional, Wang, B. D., additional, Wang, C., additional, Wang, H., additional, Wang, H. G., additional, Wang, J. C., additional, Wang, J. S., additional, Wang, L. P., additional, Wang, L. Y., additional, Wang, R. N., additional, Wang, W., additional, Wang, X. G., additional, Wang, X. J., additional, Wang, X. Y., additional, Wang, Y. D., additional, Wang, Y. J., additional, Wang, Y. P., additional, Wang, Z., additional, Wang, Z. H., additional, Wang, Z. X., additional, Wei, D. M., additional, Wei, J. J., additional, Wei, Y. J., additional, Wen, T., additional, Wu, C. Y., additional, Wu, H. R., additional, Wu, S., additional, Wu, W. X., additional, Wu, X. F., additional, Xi, S. Q., additional, Xia, J., additional, Xia, J. J., additional, Xiang, G. M., additional, Xiao, G., additional, Xiao, H. B., additional, Xin, G. G., additional, Xin, Y. L., additional, Xing, Y., additional, Xu, D. L., additional, Xu, R. X., additional, Xue, L., additional, Yan, D. H., additional, Yang, C. W., additional, Yang, F. F., additional, Yang, J. Y., additional, Yang, L. L., additional, Yang, M. J., additional, Yang, R. Z., additional, Yang, S. B., additional, Yao, Y. H., additional, Yao, Z. G., additional, Ye, Y. M., additional, Yin, L. Q., additional, Yin, N., additional, You, X. H., additional, You, Z. Y., additional, Yu, Y. H., additional, Yuan, Q., additional, Zeng, H. D., additional, Zeng, T. X., additional, Zeng, W., additional, Zeng, Z. K., additional, Zha, M., additional, Zhai, X. X., additional, Zhang, B. B., additional, Zhang, H. M., additional, Zhang, H. Y., additional, Zhang, J. L., additional, Zhang, J. W., additional, Zhang, L., additional, Zhang, L. X., additional, Zhang, P. F., additional, Zhang, P. P., additional, Zhang, R., additional, Zhang, S. R., additional, Zhang, S. S., additional, Zhang, X., additional, Zhang, X. P., additional, Zhang, Y., additional, Zhang, Y. F., additional, Zhang, Y. L., additional, Zhao, B., additional, Zhao, J., additional, Zhao, L., additional, Zhao, L. Z., additional, Zhao, S. P., additional, Zheng, F., additional, Zheng, Y., additional, Zhou, B., additional, Zhou, H., additional, Zhou, J. N., additional, Zhou, P., additional, Zhou, R., additional, Zhou, X. X., additional, Zhu, C. G., additional, Zhu, F. R., additional, Zhu, H., additional, Zhu, K. J., additional, and Zuo, X., additional

Published
2021
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60. Science with the Murchison Widefield Array: Phase I results and Phase II opportunities – Corrigendum

Author

Beardsley, A. P., primary, Johnston-Hollitt, M., additional, Trott, C. M., additional, Pober, J. C., additional, Morgan, J., additional, Oberoi, D., additional, Kaplan, D. L., additional, Lynch, C. R., additional, Anderson, G. E., additional, McCauley, P. I., additional, Croft, S., additional, James, C. W., additional, Wong, O. I., additional, Tremblay, C. D., additional, Norris, R. P., additional, Cairns, I. H., additional, Lonsdale, C. J., additional, Hancock, P. J., additional, Gaensler, B. M., additional, Bhat, N. D. R., additional, Li, W., additional, Hurley-Walker, N., additional, Callingham, J. R., additional, Seymour, N., additional, Yoshiura, S., additional, Joseph, R. C., additional, Takahashi, K., additional, Sokolowski, M., additional, Miller-Jones, J. C. A., additional, Chauhan, J. V., additional, Bojičić, I., additional, Filipović, M. D., additional, Leahy, D., additional, Su, H., additional, Tian, W. W., additional, McSweeney, S. J., additional, Meyers, B. W., additional, Kitaeff, S., additional, Vernstrom, T., additional, Gürkan, G., additional, Heald, G., additional, Xue, M., additional, Riseley, C. J., additional, Duchesne, S. W., additional, Bowman, J. D., additional, Jacobs, D. C., additional, Crosse, B., additional, Emrich, D., additional, Franzen, T. M. O., additional, Horsley, L., additional, Kenney, D., additional, Morales, M. F., additional, Pallot, D., additional, Steele, K., additional, Tingay, S. J., additional, Walker, M., additional, Wayth, R. B., additional, Williams, A., additional, and Wu, C., additional

Published
2020
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64. Science with the Murchison Widefield Array: Phase I results and Phase II opportunities

Author

Beardsley, A. P., primary, Johnston-Hollitt, M., additional, Trott, C. M., additional, Pober, J. C., additional, Morgan, J., additional, Oberoi, D., additional, Kaplan, D. L., additional, Lynch, C. R., additional, Anderson, G. E., additional, McCauley, P. I., additional, Croft, S., additional, James, C. W., additional, Wong, O. I., additional, Tremblay, C. D., additional, Norris, R. P., additional, Cairns, I. H., additional, Lonsdale, C. J., additional, Hancock, P. J., additional, Gaensler, B. M., additional, Bhat, N. D. R., additional, Li, W., additional, Hurley-Walker, N., additional, Callingham, J. R., additional, Seymour, N., additional, Yoshiura, S., additional, Joseph, R. C., additional, Takahashi, K., additional, Sokolowski, M., additional, Miller-Jones, J. C. A., additional, Chauhan, J. V., additional, Bojičić, I., additional, Filipović, M. D., additional, Leahy, D., additional, Su, H., additional, Tian, W. W., additional, McSweeney, S. J., additional, Meyers, B. W., additional, Kitaeff, S., additional, Vernstrom, T., additional, Gürkan, G., additional, Heald, G., additional, Xue, M., additional, Riseley, C. J., additional, Duchesne, S. W., additional, Bowman, J. D., additional, Jacobs, D. C., additional, Crosse, B., additional, Emrich, D., additional, Franzen, T. M. O., additional, Horsley, L., additional, Kenney, D., additional, Morales, M. F., additional, Pallot, D., additional, Steele, K., additional, Tingay, S. J., additional, Walker, M., additional, Wayth, R. B., additional, Williams, A., additional, and Wu, C., additional

Published
2019
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68. Galactic synchrotron distribution derived from 152 H ii region absorption features in the full GLEAM survey

Author

Su, H, primary, Macquart, J P, additional, Hurley-Walker, N, additional, McClure-Griffiths, N M, additional, Jackson, C A, additional, Tingay, S J, additional, Tian, W W, additional, Gaensler, B M, additional, McKinley, B, additional, Kapińska, A D, additional, Hindson, L, additional, Hancock, P, additional, Wayth, R B, additional, Staveley-Smith, L, additional, Morgan, J, additional, Johnston-Hollitt, M, additional, Lenc, E, additional, Bell, M E, additional, Callingham, J R, additional, Dwarkanath, K S, additional, For, B-Q, additional, Offringa, A R, additional, Procopio, P, additional, Wu, C, additional, and Zheng, Q, additional

Published
2018
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77. Chandra observation of PWN G16.73+0.08 in SNR G16.7+0.1.

Author

Chang, H. K., Chung, S. F., Yang, C. Y., and Tian, W. W.

Subjects
NEBULAE, GALAXIES, SUPERNOVA remnants, SUPERNOVAE, MAGNETIC fields, PULSARS
Abstract

We present X-ray observations of pulsar wind nebula (PWN) G16.73+0.08/supernova remnant (SNR) G16.7+0.1 using archival data of Chandra ACIS. The X-ray emission peak location of this PWN is found to be offset by 24 arcsec from the centre of the 1.4-GHz emission of this nebula. The X-ray nebula is elongated in the direction from the X-ray peak to the 1.4-GHz emission centre. This offset suggests that G16.73+0.08 is an evolved PWNinteractingwith the SNR reverse shock.We identify a point source, CXO J182058.16 - 142001.5, near the location of the X-ray peak. The spectrum of the X-ray nebula can be described by an absorbed power law of photon index 0.98+0.79-0.71 and hydrogen column density NH = 4.99+2.75-2.28 x 1022 cm-2. CXO J182058.16 - 142001.5 is likely a pulsar. We estimate its spin-down power to be about 2.6 x 1036 erg s-1. Assuming its age at 3000 and 10 000 yr, its dipole magnetic field strength at the polar surface is estimated to be about 4.2 x 1013 and 1.3 x 1013 G, respectively. [ABSTRACT FROM AUTHOR]

Published
2018
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88. PSRs J0248+6021 and J2240+5832: young pulsars in the northern Galactic plane

Author

Theureau, G., primary, Parent, D., additional, Cognard, I., additional, Desvignes, G., additional, Smith, D. A., additional, Casandjian, J. M., additional, Cheung, C. C., additional, Craig, H. A., additional, Donato, D., additional, Foster, R., additional, Guillemot, L., additional, Harding, A. K., additional, Lestrade, J.-F., additional, Ray, P. S., additional, Romani, R. W., additional, Thompson, D. J., additional, Tian, W. W., additional, and Watters, K., additional

Published
2010
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100. Suzaku observation of supernova remnant G332.5-5.6.

Author

Zhu, H., Tian, W. W., and Wu, D.

Subjects
*ASTRONOMICAL observations, *X-ray imaging, *PLASMA gases, *SUPERNOVA remnants, *HYDROGEN, *ELECTRON temperature, *COSMIC abundances, *SPECTROMETERS
Abstract

We analyse the Suzaku X-ray Imaging Spectrometer data of the central region of supernova remnant G332.5-5.6. The X-ray data are well described by a single non-equilibrium ionization thermal model, vnei, with an absorbing hydrogen column density of 1.4+0.4-0.1 × 1021 cm-2. The plasma is characterized by an electron temperature of 0.49+0.08-0.06 keV with subsolar abundances for O (0.58+0.06-0.05 solar value) and Fe (0.72+0.06-0.05 solar value) and slightly overabundance for Mg (1.23+0.14-0.14 solar value). It seems that the central X-ray emission originates from a projection effect or evaporation of residual clouds inside G332.5-5.6. We estimate a distance of 3.0 ± 0.8 kpc for G332.5-5.6 based on the extinction-distance relation. G332.5-5.6 has an age of 7-9 kyr. [ABSTRACT FROM AUTHOR]

Published
2015
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