Drew Jamieson’s scientific contributions

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Publications (4)


Can Baryon Acoustic Oscillations Illuminate the Parity-Violating Galaxy 4PCF?
  • Preprint

October 2024

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2 Reads

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Drew Jamieson

Measurements of the galaxy 4-Point Correlation Function (4PCF) from theSloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey (SDSS BOSS) have recently found strong statistical evidence for parity violation. If this signal is of genuine physical origin, it must stem from beyond-Standard Model physics, most likely during the very early Universe, prior to decoupling (z\sim1,020). Since the Baryon Acoustic Oscillation (BAO) features imprint at decoupling, they are expected in the parity-odd galaxy 4PCF, and so detecting them would be an additional piece of evidence that the signal is genuine. We demonstrate in a toy parity-violating model how the BAO imprint on the parity-odd 4PCF. We then outline how to perform a model-independent search for BAO in the odd 4PCF, desirable since, if the signal is real, we may not know for some time what model of e.g. inflation is producing it. If BAO are detected in the parity-odd sector, they can be used as a standard ruler as is already done in the 2PCF and 3PCF. We derive a simple formula relating the expected precision on the BAO scale to the overall parity-odd detection significance. Pursuing BAO in the odd 4PCF of future redshift surveys such as DESI, Euclid, Spherex, and Roman will be a valuable additional avenue to determine if parity violation in the distribution of galaxies is of genuine cosmological origin.


Parity-Odd power spectra: Concise statistics for cosmological parity violation

August 2024

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5 Reads

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8 Citations

Monthly Notices of the Royal Astronomical Society

Drew Jamieson

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We introduce the Parity-Odd Power (POP) spectra, a novel set of observables for probing parity violation in cosmological N-point statistics. POP spectra are derived from composite fields obtained by applying nonlinear transformations, involving also gradients, curls, and filtering functions, to a scalar field. This compresses the parity-odd trispectrum into a power spectrum. These new statistics offer several advantages: they are computationally fast to construct, estimating their covariance is less demanding compared to estimating that of the full parity-odd trispectrum, and they are simple to model theoretically. We measure the POP spectra on simulations of a scalar field with a specific parity-odd trispectrum shape. We compare these measurements to semi-analytic theoretical calculations and find agreement. We also explore extensions and generalizations of these parity-odd observables.


Figure 2. Here we show the trispectrum in the thin bin limit (top panel) and the binning scheme (lower six panels). The shape of the trispectrum template from Eq. (42) appears in the top panel. The bottom six panels indicate the binning scheme with n i = k i /k F , N =
Figure 5. On the left panel, we display the correlation matrix, Eq. (47), for the vector-pseudovector (upper triangle) and scalarpseudoscalar (lower triangle) estimators. The correlation matrix is dominated by the diagonal, with off-diagonal contributions less than 10%. On the right panels, we display histograms of the χ 2 values from 64 random non-Gaussian fields compared with the distribution from Gaussian realizations in gray. The peak of the dashed, analytical χ 2 curve coincides with the number of bins analyzed.
Parity-Odd Power Spectra: Concise Statistics for Cosmological Parity Violation
  • Preprint
  • File available

June 2024

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12 Reads

We introduce the Parity-Odd Power (POP) spectra, a novel set of observables for probing parity violation in cosmological N-point statistics. POP spectra are derived from composite fields obtained by applying nonlinear transformations, involving also gradients, curls, and filtering functions, to a scalar field. This compresses the parity-odd trispectrum into a power spectrum. These new statistics offer several advantages: they are computationally fast to construct, estimating their covariance is less demanding compared to estimating that of the full parity-odd trispectrum, and they are simple to model theoretically. We measure the POP spectra on simulations of a scalar field with a specific parity-odd trispectrum shape. We compare these measurements to semi-analytic theoretical calculations and find agreement. We also explore extensions and generalizations of these parity-odd observables.

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FIG. 2. Comparison of hb h P e i from cross-correlation measurements in observations and simulations. The solid red and blue lines are the MTNG and Magneticum simulations, respectively. For the Magneticum simulations we choose "Box2b," which has the highest mass resolution. However, "Box2b" lacks data at z ¼ 0. The data point at z ¼ 0 is from "Box0" and is marked with a star symbol. The points with error bars are previous cross-correlation measurements from observational data [7,12-16].
FIG. 3. Comparison of the box length and the dark matter particle mass used in this paper. The x axis gives the box size in units of comoving Mpc=h. The y axis indicates the dark matter particle mass. Due to differences in cosmology parameters between TNG and Magneticum simulations, we normalize the mass of dark matter particles using Ω m . The green triangles represent the Magneticum simulations whose names are given next to them. The red star represents the MTNG simulation. The blue circles show TNG300-1, TNG300-2, TNG300-3, from top to bottom.
FIG. 5. Cosmological parameter dependence of hb h P e i. The blue line is the ratio of hb h P e i predicted by the halo model with Planck 2015 and WMAP7 parameters. The orange line is the ratio of hb h P e i predicted by MTNG and Magneticum simulations ("Box2b").
Statistics of thermal gas pressure as a probe of cosmology and galaxy formation

March 2024

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28 Reads

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4 Citations

Physical Review D

The statistics of thermal gas pressure are a new and promising probe of cosmology and astrophysics. The large-scale cross-correlation between galaxies and the thermal Sunyaev-Zeldovich effect gives the bias-weighted mean electron pressure, ⟨ b h P e ⟩ . In this paper, we show that ⟨ b h P e ⟩ is sensitive to the amplitude of fluctuations in matter density, for example ⟨ b h P e ⟩ ∝ ( σ 8 Ω m 0.81 h 0.67 ) 3.14 at redshift z = 0 . We find that at z < 0.5 the observed ⟨ b h P e ⟩ is smaller than that predicted by the state-of-the-art hydrodynamical simulations of galaxy formation, MillenniumTNG, by a factor of 0.93. This can be explained by a lower value of σ 8 and Ω m , similar to the so-called “ S 8 tension” seen in the gravitational lensing effect, although the influence of astrophysics cannot be completely excluded. The difference between and MillenniumTNG at z < 2 is small, indicating that the difference in the galaxy formation models used by these simulations has little impact on ⟨ b h P e ⟩ at this redshift range. At higher z , we find that both simulations are in a modest tension with the existing upper bounds on ⟨ b h P e ⟩ . We also find a significant difference between these simulations there, which we attribute to a larger sensitivity to the galaxy formation models in the high redshift regime. Therefore, more precise measurements of ⟨ b h P e ⟩ at all redshifts will provide a new test of our understanding of cosmology and galaxy formation. Published by the American Physical Society 2024

Citations (1)


... Despite these intriguing measurements, questions remain regarding the robustness of the results. Improvements can be made through various approaches, including the development of new statistical methods [25], the identification of distinctive features in parity-odd signals [26], and the explicit fitting of theoretical models, which serves as the primary motivation for this paper. ...

Reference:

Full Parity-Violating Trispectrum in Axion Inflation: Reduction to Low-D Integrals
Parity-Odd power spectra: Concise statistics for cosmological parity violation
  • Citing Article
  • August 2024

Monthly Notices of the Royal Astronomical Society