The cosmic microwave background radiation fluctuations from H i perturbations prior to reionization

By Somnath Bharadwaj, Sheikh Saiyad Ali. 2004

179 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Charting the parameter space of the global 21-cm signal (2016, background): “(1) we neglect the peculiar velocity term since in the global signal it averages out to linear order and adds only a tiny correction (Bharadwaj & Ali 2004; Barkana & Loeb 2005a).”
The global 21-centimeter background from high redshifts (2006, background): “Here we have assumed that the patch expands uniformly with the Hubble flow; radial peculiar velocities also affect δTb by changing the mapping from distance to frequency (Bharadwaj & Ali 2004; Barkana & Loeb 2005a).”
Cosmological Parameter Estimation Using 21 cm Radiation from the Epoch of Reionization (2005, background): “To calculate @r/@ , we first relate the conformal distance to the observed frequency (Bharadwaj & Ali 2004): r ¼ Z 1 = 0 1 vr=cð Þ½ c da a2H að Þ ; ð3Þ where vr is the LOS peculiar velocity and H(a) is the Hubble constant.”
21cmfast: a fast, seminumerical simulation of the high‐redshift 21‐cm signal (2010, background): “…the well-studied Kaiser effect (e.g. Kaiser 1987), and the power spectrum of fluctuations is enhanced on all scales by a geometric factor of 1.87 (Bharadwaj & Ali 2004; Barkana & 7 Note that this expression is exact, as long as the dvr/dr field is constant over the width of the 21-cm line and…”
21 cm cosmology in the 21st century (2011, background): “Returning now to the calculation of temperature fluctuations, to obtain solutions for equations (48) and (49), we let δT = gT (k, z)δ, δe = ge(k, z)δ, δα = Wα(k, z)δ, and δΛX = WX(k, z)δ [98].”
Detecting the Earliest Galaxies through Two New Sources of 21 Centimeter Fluctuations (2004, methodology): “The fractional perturbation indvr/dr has a simple Fourier transform, δ̃drvr = −µ2δ̃ (Kaiser 1987; Bharadwaj & Ali 2004), which is used to separate the angular structure of the power-spectrum [see § 3 and Barkana & Loeb (2005)].”