The magnetic field and turbulence of the cosmic web measured using a brilliant fast radio burst

Ravi, Vikram; Shannon, R. M.; Bailes, M.; Bannister, K. W.; Bhandari, Shivani; Bhat, N. D. R.; Burke-Spolaor, S.; Caleb, M.; Flynn, Chris; Jameson, A.; Johnston, S.; Keane, E. F.; Kerr, M.; Tiburzi, C.; Tuntsov, Artem V.; Vedantham, H. K.

doi:10.1126/science.aaf6807

Cited by 210 publications

(276 citation statements)

References 73 publications

(102 reference statements)

Supporting

Mentioning

255

Contrasting

Unclassified

Order By: Relevance

“…20 The factor of (1+z) −1 is a combination of the photon redshift, time dilation, and the frequency −2 dependence of cold plasma dispersion. Ravi et al (2016) also suggested that the extremely low scattering of FRB 150807 compared to its DM may be linked to its origin from a low-mass (<10 9 M e ) galaxy. However, the strong polarization and scattering properties of FRB 110523 do suggest the presence of turbulent magnetized plasma around the source (Masui et al 2015), suggesting that individual FRB environments may be quite diverse.…”

Section: Relation To Dwarf Galaxiesmentioning

confidence: 99%

“…To date, 18 FRBs have been reported-most of them detected at the Parkes telescope (Lorimer et al 2007;Keane et al 2012Keane et al , 2016Thornton et al 2013;Burke-Spolaor & Bannister 2014;Petroff et al 2015;Ravi et al 2015Ravi et al , 2016Champion et al 2016) and one each at the Arecibo (Spitler et al 2014) and Green Bank telescopes (Masui et al 2015).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Tendulkar

Bassa

Cordes

et al. 2017

ApJL

Self Cite

673

775

View full text Add to dashboard Cite

The precise localization of the repeating fast radio burst (FRB 121102) has provided the first unambiguous association (chance coincidence probability p3×10 −4 ) of an FRB with an optical and persistent radio counterpart. We report on optical imaging and spectroscopy of the counterpart and find that it is an extended (0 6-0 8) object displaying prominent Balmer and [O III] emission lines. Based on the spectrum and emission line ratios, we classify the counterpart as a low-metallicity, star-forming, m r′ = 25.1 AB mag dwarf galaxy at a redshift of z = 0.19273(8), corresponding to a luminosity distance of 972 Mpc. From the angular size, the redshift, and luminosity, we estimate the host galaxy to have a diameter 4 kpc and a stellar mass of M * ∼(4-7)×107 M e , assuming a mass-to-light ratio between 2 to 3 M e L e −1 . Based on the Hα flux, we estimate the star formation rate of the host to be 0.4 M e yr −1 and a substantial host dispersion measure (DM) depth 324 pc cm −3 . The net DM contribution of the host galaxy to FRB 121102 is likely to be lower than this value depending on geometrical factors. We show that the persistent radio source at FRB 121102's location reported by Marcote et al. is offset from the galaxy's center of light by ∼200 mas and the host galaxy does not show optical signatures for AGN activity. If FRB 121102 is typical of the wider FRB population and if future interferometric localizations preferentially find them in dwarf galaxies with low metallicities and prominent emission lines, they would share such a preference with long gamma-ray bursts and superluminous supernovae.

show abstract

Section: Relation To Dwarf Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Tendulkar

Bassa

Cordes

et al. 2017

ApJL

Self Cite

673

775

View full text Add to dashboard Cite

show abstract

“…The burst scintillation suggests weak turbulence in the ionized intergalactic medium. The localization of FRB 150807 can be used to estimate the distance at which it was emitted, if it can associated with a star or a galaxy [24]. We will discuss FRB 150807 in Section 4.…”

Section: Burst Astrophysics Short Summarymentioning

confidence: 99%

Burst Astrophysics

Netchitailo¹

2017

JHEPGC

View full text Add to dashboard Cite

This article proposes an explanation for Fast Radio Bursts (FRBs) and Gamma Ray Bursts (GRBs) through the frames of Hypersphere World-Universe Model (WUM). WUM predicts that the concentration of protons and electrons in Intergalactic Plasma decreases inversely proportional to time and in present epoch equals to The distance to FRB 150807 object is predicted to be ~800 Mpc. WUM holds that all macroobjects (galaxies, stars, and planets) contain a core composed of Dark Matter Particles. GRBs are explained as a sum of contributions of multicomponent dark matter annihilation. The spectra of such bursts depend on the composition of the Cores.

show abstract

“…Their origin is still unknown. At the time of writing, eighteen FRBs have been discovered (Lorimer et al 2007;Keane et al 2012;Thornton et al 2013;Burke-Spolaor & Bannister 2014;Masui et al 2015;Petroff et al 2015;Ravi et al 2015Ravi et al , 2016Champion et al 2016;Keane et al 2016), with only one source (Spitler et al 2014 known to repeat. A catalog of these bursts and their properties is made available by Petroff et al (2016).…”

Section: Introductionmentioning

confidence: 99%

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Chawla

Kaspi

Josephy

et al. 2017

ApJ

View full text Add to dashboard Cite

We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm −3 , while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm −3 . No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of 3.6 10 3FRBs sky −1 day −1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index α by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for α>+0.35 in the absence of scattering and free-free absorption and α>−0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz).

show abstract

The magnetic field and turbulence of the cosmic web measured using a brilliant fast radio burst

Cited by 210 publications

References 73 publications

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Burst Astrophysics

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Contact Info

Product

Resources

About