Cosmological Inference from within the Peculiar Local Universe
Abstract
:1. Introduction
2. Selecting Local Universe Like Environments
- (i)
- The observer halo has a Milky Way (MW)-like mass, in the range [40] for the halo mass contained within 200 kpc.
- (ii)
- The bulk velocity in a sphere of radius Mpc centred on the observer is km s−1
- (iii)
- A Virgo-cluster like halo of mass is present at a distance Mpc from the observer.
- (iv)
- The angle between the bulk flow of (ii) and the direction to the Virgo-like halo of (iii) is
- (v)
- The bulk velocity in a sphere of Mpc centered on the observer is km s−1 [19].
- (vi)
- The angle between the bulk flow of (v) and the direction to the Virgo-like halo of (iii) is .
- (vii)
- The angle between the bulk flows of (ii) and (v) is .
2.1. Peculiar Velocity Corrections in JLA
2.2. Fitting for a Bulk Flow
2.3. The Likelihood Analysis
- The same 10-parameter fit as in Ref. [37], using only the values provided by JLA.
- The 10-parameter fit using —as used in Ref. [28]—and the JLA provided and values.
- The 10-parameter fit as in 1, using only values (JLA provided) as was done in all SNe Ia analyses until 2011.
- The 10-parameter fit as in 1, using JLA provided values, after subtracting out bias corrections to .
- Exponentially falling bulk flow: 12-parameter fit (including the P and Q parameters of Equation (6), using only JLA provided values. No peculiar velocity corrections are applied.
- Linearly falling bulk flow: 12-parameter fit (including the P and Q parameters of Equation (5) using only JLA provided values. No peculiar velocity corrections are applied.
- JLA-corrected redshifts + Exponential bulk flow: 12-parameter fit: SNe Ia with peculiar velocity corrections applied by JLA, are treated as in (ii) above, while an exponentially falling bulk flow is fitted to the remaining SNe.
- JLA-corrected redshifts + Linear bulk flow: As in 7, but with the linear parametrisation of the bulk flow.
- CF-3 data and the exponential bulk flow fit: 12-parameter fit using Equation (2) with the -derived values of and (see Section 2.1) used for the low z SNe Ia to which the velocity correction can be applied. For the remaining objects, we use the JLA values, and an Exponential bulk flow is fitted using Equation (6) as described above.
- CF-3 data and the linear bulk flow fit: 12-parameter fit using Equation (5) with the -derived values of and (see Section 2.1) used for the low z SNe Ia to which the velocity correction can be applied. For the remaining objects, we use the JLA values, and a linear bulk flow is fitted using Equation (5).
Fit | −2 log | V (km s−1) @Mpc | |||||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
1. | As in Ref. [37] | −214.97 | 0.341 | 0.569 | 0.134 | 0.0385 | 0.931 | 3.059 | −0.016 | 0.071 | −19.052 | 0.108 | - |
No acceleration | −203.93 | 0.068 | 0.034 | 0.132 | 0.0327 | 0.932 | 3.045 | −0.013 | 0.071 | −19.006 | 0.110 | - | |
2. | [37] + JLA z | −221.93 | 0.340 | 0.565 | 0.133 | 0.0385 | 0.932 | 3.056 | −0.016 | 0.071 | −19.051 | 0.107 | - |
No acceleration | −210.99 | 0.070 | 0.035 | 0.131 | 0.0328 | 0.932 | 3.042 | −0.013 | 0.071 | −19.006 | 0.109 | - | |
3. | No pec. vel. corr. to z | −215.40 | 0.285 | 0.483 | 0.134 | 0.0398 | 0.932 | 3.038 | −0.016 | 0.071 | −19.051 | 0.108 | - |
No acceleration | −207.67 | 0.051 | 0.025 | 0.132 | 0.0348 | 0.932 | 3.023 | −0.014 | 0.071 | −19.012 | 0.110 | - | |
4. | No pec. vel. corr. to z or | −216.89 | 0.235 | 0.396 | 0.135 | 0.0397 | 0.932 | 3.029 | −0.016 | 0.071 | −19.040 | 0.109 | - |
No acceleration | −211.84 | 0.0413 | 0.021 | 0.133 | 0.0357 | 0.932 | 3.016 | −0.014 | 0.071 | −19.008 | 0.110 | - | |
5. | Exponential bulk flow | −217.51 | 0.289 | 0.452 | 0.134 | 0.0390 | 0.932 | 3.036 | −0.016 | 0.071 | −19.037 | 0.107 | 253 |
No acceleration | −211.3 | 0.077 | 0.039 | 0.132 | 0.0347 | 0.932 | 3.024 | −0.014 | 0.071 | −19.002 | 0.108 | 292 | |
6. | Linear bulk flow | −217.47 | 0.290 | 0.455 | 0.134 | 0.0390 | 0.932 | 3.036 | −0.016 | 0.071 | −19.038 | 0.107 | 265 |
No acceleration | −211.99 | 0.082 | 0.041 | 0.132 | 0.0347 | 0.932 | 3.025 | −0.014 | 0.071 | −19.002 | 0.108 | 282 | |
7. | JLA + Exp. bulk flow | −224.87 | 0.340 | 0.570 | 0.133 | 0.0387 | 0.932 | 3.051 | −0.016 | 0.072 | −19.052 | 0.107 | 271 |
No acceleration | −216.3 | 0.077 | 0.039 | 0.132 | 0.0347 | 0.932 | 3.024 | −0.014 | 0.071 | −19.002 | 0.108 | 295 | |
8. | JLA + Lin. bulk flow | −225.08 | 0.341 | 0.577 | 0.133 | 0.0387 | 0.932 | 3.050 | −0.016 | 0.071 | −19.054 | 0.107 | 238 |
No acceleration | −214.14 | 0.072 | 0.036 | 0.131 | 0.0328 | 0.932 | 3.041 | −0.013 | 0.071 | −19.005 | 0.109 | 251 | |
9. | + Exp. Bulk Flow | −225.61 | 0.279 | 0.427 | 0.133 | 0.0386 | 0.932 | 3.001 | −0.016 | 0.071 | −19.034 | 0.109 | 309 |
No acceleration | −220.72 | 0.086 | 0.043 | 0.132 | 0.0346 | 0.932 | 2.990 | −0.015 | 0.071 | −19.001 | 0.110 | 398 | |
Flat | −223.96 | 0.393 | 0.607 | 0.133 | 0.0357 | 0.933 | 2.998 | −0.016 | 0.071 | −19.045 | 0.110 | 338 | |
10. | + Lin. bulk flow | −225.73 | 0.277 | 0.431 | 0.133 | 0.0386 | 0.932 | 3.002 | −0.016 | 0.071 | −19.037 | 0.109 | 211 |
No acceleration | −220.16 | 0.085 | 0.042 | 0.132 | 0.0346 | 0.932 | 2.991 | −0.015 | 0.071 | −19.001 | 0.110 | 249 | |
Flat | −224.18 | 0.390 | 0.610 | 0.134 | 0.0399 | 0.932 | 3.006 | −0.016 | 0.071 | −19.047 | 0.109 | 215 |
- Of all the fits, the only ones favouring are just those that include the incorrect and incomplete peculiar velocity ‘corrections’ of JLA [25].
- While previous work has suggested that bulk flows should not bias , it in fact drops by ∼ if we undo the peculiar velocity ‘corrections’ of JLA and instead use the kinematic data from. This illustrates the huge impact of considering a realistic LU-like observer such as ourselves, rather than the randomly located observer assumed in all previous analyses [16,28,29,30]. In particular this contradicts what is stated in Table 11 of Ref. [25].
3. Extracting S8
4. Discussion
5. Conclusions
Author Contributions
Funding
Data Availability Statement
Conflicts of Interest
Appendix A. Supernova Cosmology
Appendix B. The Joint Lightcurve Analysis Catalogue
1 | There are other corrections too such as for gravitational lensing, which become more important than the effect of peculiar velocities at redshift —see Figure B.1 of Ref. [6]. |
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Mohayaee, R.; Rameez, M.; Sarkar, S. Cosmological Inference from within the Peculiar Local Universe. Universe 2024, 10, 209. https://doi.org/10.3390/universe10050209
Mohayaee R, Rameez M, Sarkar S. Cosmological Inference from within the Peculiar Local Universe. Universe. 2024; 10(5):209. https://doi.org/10.3390/universe10050209
Chicago/Turabian StyleMohayaee, Roya, Mohamed Rameez, and Subir Sarkar. 2024. "Cosmological Inference from within the Peculiar Local Universe" Universe 10, no. 5: 209. https://doi.org/10.3390/universe10050209