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Title: New probe of magnetic fields in the pre-reionization epoch. II. Detectability

Authors:
; ; ; ; ;
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1352718
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 95; Journal Issue: 8; Related Information: CHORUS Timestamp: 2017-04-21 22:15:04; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English

Citation Formats

Gluscevic, Vera, Venumadhav, Tejaswi, Fang, Xiao, Hirata, Christopher, Oklopčić, Antonija, and Mishra, Abhilash. New probe of magnetic fields in the pre-reionization epoch. II. Detectability. United States: N. p., 2017. Web. doi:10.1103/PhysRevD.95.083011.
Gluscevic, Vera, Venumadhav, Tejaswi, Fang, Xiao, Hirata, Christopher, Oklopčić, Antonija, & Mishra, Abhilash. New probe of magnetic fields in the pre-reionization epoch. II. Detectability. United States. doi:10.1103/PhysRevD.95.083011.
Gluscevic, Vera, Venumadhav, Tejaswi, Fang, Xiao, Hirata, Christopher, Oklopčić, Antonija, and Mishra, Abhilash. Fri . "New probe of magnetic fields in the pre-reionization epoch. II. Detectability". United States. doi:10.1103/PhysRevD.95.083011.
@article{osti_1352718,
title = {New probe of magnetic fields in the pre-reionization epoch. II. Detectability},
author = {Gluscevic, Vera and Venumadhav, Tejaswi and Fang, Xiao and Hirata, Christopher and Oklopčić, Antonija and Mishra, Abhilash},
abstractNote = {},
doi = {10.1103/PhysRevD.95.083011},
journal = {Physical Review D},
number = 8,
volume = 95,
place = {United States},
year = {Fri Apr 21 00:00:00 EDT 2017},
month = {Fri Apr 21 00:00:00 EDT 2017}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1103/PhysRevD.95.083011

Citation Metrics:
Cited by: 2works
Citation information provided by
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  • We compute the secondary cosmic microwave background radiation (CMBR) anisotropy signal from the reionization of the Universe in the presence of tangled magnetic fields. We consider the tangled-magnetic-field-induced scalar, vector, and tensor modes for our analysis. The most interesting signal for l < or approx. 100 arises from tensor perturbations. In particular, we show that the enhancement observed by Wilkinson microwave anisotropy probe (WMAP) in the TE cross-correlation signal for l < or approx. 10 could be explained by tensor TE cross correlation from tangled magnetic fields generated during the inflationary epoch for magnetic field strength B{sub 0}{approx_equal}4.5x10{sup -9} Gmore » and magnetic field power spectrum spectral index n{approx_equal}-2.9. Alternatively, a mixture of tensor mode signal with primordial scalar modes gives weaker bounds on the value of the optical depth to the reionization surface, {tau}{sub reion}: {tau}{sub reion}=0.11{+-}0.02. This analysis can also be translated to a limit on magnetic field strength of {approx_equal}5x10{sup -9} G for wave numbers < or approx. 0.05 Mpc{sup -1}.« less
  • The implication of primordial magnetic-field-induced structure formation for the HI signal from the epoch of reionization is studied. Using semi-analytic models, we compute both the density and ionization inhomogeneities in this scenario. We show that: (a) The global HI signal can only be seen in emission, unlike in the standard ΛCDM models, (b) the density perturbations induced by primordial fields, leave distinctive signatures of the magnetic field Jeans' length on the HI two-point correlation function, (c) the length scale of ionization inhomogeneities is ∼<1 Mpc. We find that the peak expected signal (two-point correlation function) is ≅ 10{sup −4} K{supmore » 2} in the range of scales 0.5–3 Mpc for magnetic field strength in the range 5 × 10{sup −10}–3 × 10{sup −9} G. We also discuss the detectability of the HI signal. The angular resolution of the on-going and planned radio interferometers allows one to probe only the largest magnetic field strengths that we consider. They have the sensitivity to detect the magnetic field-induced features. We show that the future SKA has both the angular resolution and the sensitivity to detect the magnetic field-induced signal in the entire range of magnetic field values we consider, in an integration time of one week.« less
  • We study the impact of primordial magnetic fields on the H I absorption from the epoch of reionization. The presence of these fields results in two distinct effects: (1) the heating of the halos from the decay of the magnetic fields owing to ambipolar diffusion, and (2) an increase in the number of halos owing to additional matter fluctuations induced by magnetic fields. We analyze both of these effects and show that the latter is potentially observable because the number of halos along of line of sight can increase by many orders of magnitude. While this effect is not stronglymore » dependent on the magnetic field strength in the range 0.3-0.6 nG, it is extremely sensitive to the magnetic field power spectral index for the near scale-free models. Therefore, the detection of such absorption features could be a sensitive probe of the primordial magnetic field and its power spectrum. We discuss the detectability of these features with the ongoing and future radio interferometers. In particular, we show that LOFAR might be able to detect these absorption features at z ≅ 10 in less than 10 hr of integration if the flux of the background source is 400 mJy.« less
  • Molecular hydrogen is now understood to be the main coolant of the primordial gas clouds leading to the formation of the very first stars and galaxies. The line emissions associated with molecular hydrogen should then be a good tracer of the matter distribution at the onset of the reionization of the universe. Here, we propose intensity mapping of H{sub 2} line emission in rest-frame mid-infrared wavelengths to map out the spatial distribution of gas at redshifts z > 10. We calculate the expected mean intensity and clustering power spectrum for several H{sub 2} lines. We find that the 0-0S(3) rotationalmore » line at a rest wavelength of 9.66 {mu}m is the brightest line over the redshift range of 10-30 with an intensity of about 5-10 Jy sr{sup -1} at z {approx} 15. To reduce astrophysical and instrumental systematics, we propose the cross-correlation between multiple lines of the H{sub 2} rotational and vibrational line emission spectrum. Our estimates of the intensity can be used as guidance in planning instruments for future mid-IR spectroscopy missions such as SPICA.« less