Redshift Estimation and Constraints on Intergalactic and Interstellar Media from Dispersion and Scattering of Fast Radio Bursts

Cordes, James M.; Ocker, Stella Koch; Chatterjee, Shami

doi:10.48550/arxiv.2108.01172

Cited by 6 publications

(25 citation statements)

References 45 publications

(70 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…After screening them using a telescope sensitivity model, one can finally obtain a mock "observed" sample of FRBs. Based on the DM − z relation (Deng & Zhang 2014;Zhang 2018a;Pol et al 2019;Cordes et al 2021)…”

Section: The Methodsmentioning

confidence: 99%

The CHIME Fast Radio Burst Population Does Not Track the Star Formation History of the Universe

Zhang¹,

Zhang²

2021

Preprint

View full text Add to dashboard Cite

The redshift distribution of fast radio bursts (FRBs) is not well constrained. The association of the Galactic FRB 200428 with the young magnetar SGR 1935+2154 raises the working hypothesis that FRB sources track the star formation history of the universe. The discovery of FRB 20200120E in association with a globular cluster in the nearby galaxy M81, on the other hand, casts doubts on such an assumption. We apply the Monte Carlo method developed in a previous work to test different FRB redshift distribution models against the recently released first CHIME FRB catalog in terms of their distributions in specific fluence, inferred isotropic energy, and external dispersion measure (DM E ). Our results clearly show that the hypothesis that all FRBs track the star formation history of the universe is ruled out. The hypothesis that all FRBs track the accumulated stars throughout history describes the data better but still cannot pass both the energy and DM E criteria. The data seem to be better modeled with either a redshift distribution model invoking a significant delay with respect to star formation or a hybrid model invoking both a dominant delayed population and an insignificant star formation population. We discuss the implications of this finding for FRB source models.

show abstract

Section: The Methodsmentioning

confidence: 99%

The CHIME Fast Radio Burst Population Does Not Track the Star Formation History of the Universe

Zhang¹,

Zhang²

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Recently, Cordes et al (2021) published an analysis of 14 localized FRBs in which they combined the observed DM together with scattering times to assess the reported host redshifts. They found that adopting a value of f igm = 0.85 ± 0.05 lead to the most optimal redshift constraints, leading them to question the host galaxy associations of two FRBs in the sample.…”

Section: Discussionmentioning

confidence: 99%

Constraining the Cosmic Baryon Distribution with Fast Radio Burst Foreground Mapping

Lee,

Ata,

Khrykin

et al. 2021

Preprint

View full text Add to dashboard Cite

The dispersion measure (DM) of fast radio bursts (FRBs) encode the integrated electron density along the line-of-sight, which is dominated by the intergalactic medium (IGM) contribution in the case of extragalactic FRBs. In this paper, we show that incorporating wide-field spectroscopic galaxy survey data in the foreground of localized FRBs can significantly improve constraints on the partition of diffuse cosmic baryons. Using mock DMs and realistic lightcone galaxy catalogs derived from the Millennium simulation, we define spectroscopic surveys that can be carried out with 4m and 8m-class wide field spectroscopic facilities. On these simulated surveys, we carry out Bayesian density reconstructions in order to estimate the foreground matter density field. In comparison with the 'true' matter density field, we show that these can help reduce the uncertainties in the foreground structures by ∼ 2 − 3× compared to cosmic variance. We calculate the Fisher matrix to forecast that N = 30 (96) localized FRBs should be able to constrain the diffuse cosmic baryon fraction to < 10% (< 5%), and parameters governing the size and baryon fraction of galaxy circumgalactic halos to within ∼ 15−20%(∼ 7−10%). From the Fisher analysis, we show that the foreground data increases the sensitivity of localized FRBs toward our parameters of interest by ∼ 25×. We briefly introduce FLIMFLAM, an ongoing galaxy redshift survey that aims to obtain foreground data on ∼ 30 localized FRB fields.

show abstract

“…At the time there was only one FRB with published host galaxy redshift and some extra galactic pulsar data. Pulsars are known to be troublesome as they have large intrinsic redshifts and this FRB is no longer included in lists of FRBs with known host galaxies [23]. At the time of writing there are thirteen known FRB with known redshifts of their host galaxy and so it would seem a good time to revisit this relationship using this new data.…”

Section: Calculating the Redshift Of The Host Galaxymentioning

confidence: 99%

“…At the time of writing there are thirteen known FRB with known redshifts of their host galaxy and so it would seem a good time to revisit this relationship using this new data. Note reference [23] has one FRB not used here since the redshift is not know precisely.…”

Section: Calculating the Redshift Of The Host Galaxymentioning

confidence: 99%

Data from 14,577 cosmological objects and 14 FRBs confirm the predictions of new tired light (NTL) and lead to a new model of the IGM

Ashmore¹

2022

J. Phys.: Conf. Ser.

View full text Add to dashboard Cite

Predictions by New Tired Light were tested using 14,577 objects from the NED-D compilation of redshift-independent distances. These objects give an electron number density of ne = 0.499 m −3 compared to the predicted one of ne = 0.5 m −3. In NTL the Hubble constant is given by H = 2nehre /me and, using this value for ne gives 62.5 km/s per Mpc which is very close to the accepted values. NTL predicts a linear relationship between distance and ln (1 + z) with gradient (mec/2ne hre = 1.46×1026 m). Plotting all the 14,577 points gives a straight line with gradient 1.40×1026 m – just 4% off the predicted value. Using distances from the compilation the redshift is calculated by NTL and a graph of predicted versus observed redshift is drawn. This has a gradient of 0.9756 close to the value ‘1.0’ expected in a 1:1 relationship between prediction and expected. Both graphs are linear up to redshifts of ‘9’ with no hint of relativistic effects. In NTL, there is a delay between an electron in the IGM absorbing and re-emitting a photon whereby the electron recoils (leading to the redshift). Data from FRB 121102 gives the time lag between two frequencies arriving and using the extra number of photon-electron interactions made by the longer wavelength the time delay is found. This tells us the length of the delay at each interaction as ≈ 10−10 s. Using NTL and DM the redshift of the host galaxy was calculated and found to be z = 0.143 compared to the measured value of z = 0.19 – the difference lying well within the uncertainty in DMIn NTL, DM and redshift are produced by the electrons in the IGM and so there is a direct relation between them. DMIGM = (mec/2hre ){ln(1 + z)} or DMIGM = 2470{ln(1 +z){. Plotting data from 14 localised FRBs on a graph of DM versus {ln(1 + z)} does give a straight-line graph but a selection of eight from the fourteen are colinear with a gradient of 1244 ± 147 pc cm −3 much closer t that predicted. Several hosts are said to be tentative and so we will continue to plot this graph as more and more FRBs are located. Often tired light models are discounted on the basis of an old model of the IGM as having a neutral plasma at high temperature and/or they are using Compton scatter. In NTL, recoil takes place along the line of sight so there is no blurring. Several mainstream papers show that every dust particle in the IGM is positively charged with an excess of protons due to photoionisation. This means an equal number of electrons have been released into the intervening space. On this basis the IGM is a ‘dirty plasma’ with the protons trapped on dust particles and a sea of electrons in-between. When a group of electrons come together in this way, they will arrange themselves onto a BCC lattice (Wigner-Seitz crystal). Calculations show that if we use dust density restricted by considerations of an expanding Universe there is not enough to give the ne = 0.5 m −3 found by observation but would need a dust density of ρIGM ≈ 3×10−25 kgm −3. A previous paper looked at the photoionisation of Hydrogen clouds surrounding a galaxy with the protons staying behind and forming dark matter whilst the electrons went off into the IGM to form on their crystal lattice held by mutual repulsion. The mass of dark matter surrounding the Milky Way galaxy is known and so, if this is all protons, we can find the number of protons there. An equal number of electrons will have been released into the IGM and dividing this by the average volume occupied by a galaxy gives us the ne = 1 m −3 and agrees with observation.

show abstract

Redshift Estimation and Constraints on Intergalactic and Interstellar Media from Dispersion and Scattering of Fast Radio Bursts

Cited by 6 publications

References 45 publications

The CHIME Fast Radio Burst Population Does Not Track the Star Formation History of the Universe

The CHIME Fast Radio Burst Population Does Not Track the Star Formation History of the Universe

Constraining the Cosmic Baryon Distribution with Fast Radio Burst Foreground Mapping

Data from 14,577 cosmological objects and 14 FRBs confirm the predictions of new tired light (NTL) and lead to a new model of the IGM

Contact Info

Product

Resources

About