Detection of Repeating FRB 180916.J0158+65 Down to Frequencies of 300 MHz

被引：78

作者：

Chawla, P. ^{[1
,2
]}

Andersen, B. C. ^{[1
,2
]}

Bhardwaj, M. ^{[1
,2
]}

Fonseca, E. ^{[1
,2
]}

Josephy, A. ^{[1
,2
]}

Kaspi, V. M. ^{[1
,2
]}

Michilli, D. ^{[1
,2
]}

Pleunis, Z. ^{[1
,2
]}

Bandura, K. M. ^{[3
,4
]}

Bassa, C. G. ^{[5
]}

Boyle, P. J. ^{[1
,2
]}

Brar, C. ^{[1
,2
]}

Cassanelli, T. ^{[6
,7
]}

Cubranic, D. ^{[8
]}

Dobbs, M. ^{[1
,2
]}

Dong, F. Q. ^{[8
]}

Gaensler, B. M. ^{[6
,7
]}

Good, D. C. ^{[8
]}

Hessels, J. W. T. ^{[5
,9
]}

Landecker, T. L. ^{[10
]}

Leung, C. ^{[11
,12
]}

Li, D. Z. ^{[13
,14
]}

Lin, H-H ^{[14
,15
]}

Masui, K. ^{[11
,12
]}

Mckinven, R. ^{[6
,7
]}

Mena-Parra, J. ^{[11
]}

Merryfield, M. ^{[1
,2
]}

Meyers, B. W. ^{[8
]}

Naidu, A. ^{[1
,2
]}

Ng, C. ^{[6
]}

Patel, C. ^{[1
,6
]}

Rafiei-Ravandi, M. ^{[16
]}

Rahman, M. ^{[6
]}

Sanghavi, P. ^{[3
,4
]}

Scholz, P. ^{[6
]}

Shin, K. ^{[11
,12
]}

Smith, K. M. ^{[16
]}

Stairs, I. H. ^{[8
]}

Tendulkar, S. P. ^{[1
,2
]}

Vanderlinde, K. ^{[6
,7
]}

机构：

[1] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada

[2] McGill Univ, McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 2A7, Canada

[3] West Virginia Univ, CSEE, Morgantown, WV 26505 USA

[4] West Virginia Univ, Ctr Gravitat Waves & Cosmol, Morgantown, WV 26505 USA

[5] ASTRON, Netherlands Inst Radio Astron, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands

[6] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, St George, ON M5S 3H4, Canada

[7] Univ Toronto, David A Dunlap Inst Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada

[8] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada

[9] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[10] Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, Dominion Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada

[11] MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[12] MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[13] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada

[14] Canadian Inst Theoret Astrophys, 60 St George St, St George, ON M5S 3H8, Canada

[15] Max Planck Inst Radio Astron, Huegel 69, D-53121 Bonn, Germany

[16] Perimeter Inst Theoret Phys, 31 Caroline St N, Waterloo, ON N2L 2Y5, Canada

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2020年 / 896卷 / 02期

基金：

加拿大自然科学与工程研究理事会; 加拿大创新基金会; 欧洲研究理事会; 爱尔兰科学基金会; 英国科学技术设施理事会;

关键词：

FAST RADIO-BURSTS; PULSE; CONSTRAINTS; EMISSION;

D O I：

10.3847/2041-8213/ab96bf

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the detection of seven bursts from the periodically active, repeating fast radio burst (FRB) source FRB 180916.J0158+65 in the 300-4-00 MHz frequency range with the Green Bank Telescope (GBT). Emission in multiple bursts is visible down to the bottom of the GBT band, suggesting that the cutoff frequency (if it exists) for FRB emission is lower than 300 MHz. Observations were conducted during predicted periods of activity of the source, and had simultaneous coverage with the Low Frequency Array (LOFAR) and the FRB backend on the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. We find that one of the GBT-detected bursts has potentially associated emission in the CHIME band (400-800 MHz) but we detect no bursts in the LOFAR band (110-190 MHz), placing a limit of alpha > -1.0 on the spectral index of broadband emission from the source. We also find that emission from the source is severely band-limited with burst bandwidths as low as similar to 40 MHz. In addition, we place the strictest constraint on observable scattering of the source, <1.7 ms at 350 MHz, suggesting that the circumburst environment does not have strong scattering properties. Additionally, knowing that the circumburst environment is optically thin to free-free absorption at 300 MHz, we find evidence against the association of a hyper-compact H II region or a young supernova remnant (age <50 yr) with the source.

引用

页数：13

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