1,721,363 research outputs found
The Sound of Fast Radio Burst FRB 121102
No full textSound files generated from nine radio transients detected by the Very Large Array toward cosmological radio transient, FRB 121102. The sound of FRB 121102 has a "chirp" that is caused by dispersion.
Original publication is Chatterjee et al (2017), "The direct localization of a fast radio burst and its host". Original data is available at https://doi.org/10.7910/DVN/TLDKXG.</p
The Sound of Fast Radio Burst FRB 121102
No full textSound files generated from nine radio transients detected by the Very Large Array toward cosmological radio transient, FRB 121102. The sound of FRB 121102 has a "chirp" that is caused by dispersion.
Original publication is Chatterjee et al (2017), "The direct localization of a fast radio burst and its host". Original data is available at https://doi.org/10.7910/DVN/TLDKXG.</p
FRB 121102 detections from the Lovell Telescope
No full textWe provide data for FRB 121102 pulses detected with the Lovell telescope at Jodrell Bank, UK at 1.4 GHz. These detections were used in Rajwade et al. (2020). Each file is a single pulse from FRB 121102 in the standard SIGPROC filterbank format and can be read in by standard radio pulsar data processing software. The tarball contains all the filterbank files. The text file contains the name of each file in the first column and seconds into the file where the pulse is located in the second column. The start time of the pulse is with reference to the highest frequency channel i.e seconds into the file where the pulse was detected in the highest frequency channel.
Citation:
If you are planning to use these data in any publication, please do not forget to put in the following acknowledgement:
"The data used in this manuscript have been downloaded from the Zenodo open access repository 'FRB 121102 detections from the Lovell Telescope' (10.5281/zenodo.3974768).
Analysis of Very Large Array data toward FRB 121102
No full textReproducibility analysis for Very Large Array data for radio transient, FRB 121102
Binary comb models for FRB 121102
No full textThe first repeating fast radio burst source, FRB 121102, is observed to emit
bursts periodically. We show that FRB 121102 can be interpreted as an
interacting neutron star binary system with an orbital period of 159 days. We
develop a binary comb model by introducing an eccentricity in the orbit.
Besides the original funnel mode of the binary comb model, which was applied to
FRB 180916.J0158+65 by Ioka and Zhang 2020, we also identify two new modes of
the binary comb model, i.e. the tau-crossing mode and the inverse funnel mode,
and apply them to interpret FRB 121102. These new developments expand the
applicable parameter space, allowing the companion star to be a massive star, a
massive black hole, or a supermassive black hole, with the latter two having
larger parameter spaces. These models are also consistent with other
observations, such as the persistent bright radio counterpart associated with
the source. We also argue that the observed frequency dependence of the active
window does not disfavor the binary comb model, in contrast to recent claims,
and propose two possible scenarios to interpret the data.Comment: 23 pages, 12 figures, 1 tabl
Analysis of Very Large Array data toward FRB 121102
No full textReproducibility analysis for Very Large Array data for radio transient, FRB 121102
Simultaneous X-ray, gamma-ray, and radio observations of the repeating fast radio burst FRB 121102
No full textWe undertook coordinated campaigns with the Green Bank, Effelsberg, and Arecibo radio telescopes during Chandra X-ray Observatory and XMM-Newton observations of the repeating fast radio burst FRB 121102 to search for simultaneous radio and X-ray bursts. We find 12 radio bursts from FRB 121102 during 70 ks total of X-ray observations. We detect no X-ray photons at the times of radio bursts from FRB 121102 and further detect no X-ray bursts above the measured background at any time. We place a 5\u3c3 upper limit of 3
7 10 1211 erg cm 122 on the 0.5\u201310 keV fluence for X-ray bursts at the time of radio bursts for durations ms, which corresponds to a burst energy of 4
7 1045 erg at the measured distance of FRB 121102. We also place limits on the 0.5\u201310 keV fluence of 5
7 10 1210 and 1
7 10 129 erg cm 122 for bursts emitted at any time during the XMM-Newton and Chandra observations, respectively, assuming a typical X-ray burst duration of 5 ms. We analyze data from the Fermi Gamma-ray Space Telescope Gamma-ray Burst Monitor and place a 5\u3c3 upper limit on the 10\u2013100 keV fluence of 4
7 10 129 erg cm 122 (5
7 1047 erg at the distance of FRB 121102) for gamma-ray bursts at the time of radio bursts. We also present a deep search for a persistent X-ray source using all of the X-ray observations taken to date and place a 5\u3c3 upper limit on the 0.5\u201310 keV flux of 4
7 10 1215 erg s 121 cm 122 (3
7 1041 erg s 121 at the distance of FRB 121102). We discuss these non-detections in the context of the host environment of FRB 121102 and of possible sources of fast radio bursts in general.Peer reviewed: YesNRC publication: Ye
The FRB 121102 Host Is Atypical among Nearby Fast Radio Bursts
No full textWe search for host galaxy candidates of nearby fast radio bursts (FRBs), FRB 180729.J1316+55, FRB 171020, FRB 171213, FRB 180810.J1159+83, and FRB 180814.J0422+73 (the second repeating FRB). We compare the absolute magnitudes and the expected host dispersion measure DMhost of these candidates with that of the first repeating FRB, FRB 121102, as well as those of long gamma-ray bursts (LGRBs) and superluminous supernovae (SLSNe), the proposed progenitor systems of FRB 121102. We find that while the FRB 121102 host is consistent with those of LGRBs and SLSNe, the nearby FRB host candidates, at least for FRB 180729.J1316+55, FRB 171020, and FRB 180814.J0422+73, either have a smaller DMhost or are fainter than FRB 121102 host, as well as the hosts of LGRBs and SLSNe. In order to avoid the uncertainty in estimating DMhost due to the line-of-sight effect, we propose a galaxy-group-based method to estimate the electron density in the intergalactic regions, and hence, DMIGM. The result strengthens our conclusion. We conclude that the host galaxy of FRB 121102 is atypical, and LGRBs and SLSNe are likely not the progenitor systems of at least most nearby FRB sources. The recently reported two FRB hosts differ from the host of FRB 121102 and also the host candidates suggested in this paper. This is consistent with the conclusion of our paper and suggests that the FRB hosts are very diverse
Similar Scale-invariant Behaviors between Soft Gamma-Ray Repeaters and an Extreme Epoch from FRB 121102
No full textThe recent discovery of a Galactic fast radio burst (FRB) associated with a hard X-ray burst from the soft gamma-ray repeater (SGR) J1935+2154 has established the magnetar origin of at least some FRBs. In this work, we study the statistical properties of soft gamma-ray/hard X-ray bursts from SGRs 1806-20 and J1935+2154 and of radio bursts from the repeating FRB 121102. For SGRs, we show that the probability density functions for the differences of fluences, fluxes, and durations at different times have fat tails with a q-Gaussian form. The q values in the q-Gaussian distributions are approximately steady and independent of the temporal interval scale adopted, implying a scale-invariant structure of SGRs. These features indicate that SGR bursts may be governed by a self-organizing criticality (SOC) process, confirming previous findings. Very recently, 1652 independent bursts from FRB 121102 have been detected by the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Here we also investigate the scale-invariant structure of FRB 121102 based on the latest observations of FAST, and show that FRB 121102 and SGRs share similar statistical properties. Given the bimodal energy distribution of FRB 121102 bursts, we separately explore the scale-invariant behaviors of low- and high-energy bursts of FRB 121102. We find that the q values of low- and high-energy bursts are different, which further strengthens the evidence of the bimodality of the energy distribution. Scale invariance in both the high-energy component of FRB 121102 and SGRs can be well explained within the same physical framework of fractal-diffusive SOC systems.link_to_subscribed_fulltex
FRB 121102 Is Coincident with a Star-forming Region in Its Host Galaxy
No full textWe present optical, near-infrared, and mid-infrared imaging of the host galaxy of FRB 121102 with the Gemini North telescope, the Hubble Space Telescope, and the Spitzer Space Telescope. The FRB 121102 host galaxy is resolved, revealing a bright star-forming region located in the outskirts of the irregular, low-metallicity dwarf galaxy. The star-forming region has a half-light radius of 0.68 kpc(0." 20), encompassing the projected location of the compact (<0.7 pc), persistent radio source that is associated with FRB 121102. The half-light diameter of the dwarf galaxy is 5–7 kpc, and broadband spectral energy distribution fittingindicates that it has a total stellar mass of M* ∼ 108 M⊙. The properties of the host galaxy of FRB 121102 are comparable to those of extreme emission line galaxies, also known as hosts to some hydrogen-poor superluminous supernovae and long-duration γ-ray bursts. The projected location of FRB 121102 within the star-forming region supports the proposed connection of FRBs with newly born neutron stars or magnetars
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