Alexandra Amon

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Alexandra Amon

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    • Home
    • Research
    • Science Communication
    • Awards
    • Students
    • Trinis
    • CV
  • Home
  • Research
  • Science Communication
  • Awards
  • Students
  • Trinis
  • CV

Below is a selection of my research projects. For a full list of my (openly accessible) publications, see the arxiv or you can find my publication stats at my NASA ADS profile.

Technical talks

Royal Astronomical Society

Institute of Advanced Studies

Baryonic feedback & AdvACT

Intrinsic alignments with DESI

Intrinsic alignments with DESI

Bigwood, Amon et al (in prep.) 

Intrinsic alignments with DESI

Intrinsic alignments with DESI

Intrinsic alignments with DESI

Dwarf lensing

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

Thornton, Amon et al (in prep.)

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

The lensing collaborations teamed up for the first joint cosmological analysis and I played a a leading role in the effort. We did an extensive mock analysis to disentangle our different analysis choices and formulate a Hybrid pipeline that was suitable for the joint statistical power - a valuable stepping stone toward analyses with Rubin data. [DES & KiDS collaborations]

A non-linear solution to the S8 tension

Reanalysis of KiDS-1000, DES Y3 and HSC Y3

A non-linear solution to the S8 tension

We reviewed the evidence for a tension in the value of S8 between Planck CMB and other cosmological observations. We argue that any discrepancy may be a caused by uncertainties in the theoretical predictions arising from the modelling of the mass fluctuations on non-linear scales, either due to baryonic feedback or non-standard dark matte

We reviewed the evidence for a tension in the value of S8 between Planck CMB and other cosmological observations. We argue that any discrepancy may be a caused by uncertainties in the theoretical predictions arising from the modelling of the mass fluctuations on non-linear scales, either due to baryonic feedback or non-standard dark matter. . If our proposed explanation of the S8 tension is correct, the required suppression must extend into the mildly non-linear regime to k~0.2h/Mpc [Amon and Efstathiou 2022; Preston et al 2023].

Consistency of lensing & clustering

Vera Rubin Observatory commissioning targets

Consistency of lensing & clustering

We present new measurements of the excess surface mass density profiles using the three state-of-the-art lensing surveys (DES, HSC, KiDS) and jointly analyse with BOSS galaxy clustering to assess their consistency on small and large-scales [Amon and Robertson et al 2022].

Lensing without borders

Vera Rubin Observatory commissioning targets

Consistency of lensing & clustering

I co-pioneered the Lensing Without Borders cross-survey collaboration to test the consistency of weak lensing results [Amon+2017; Leauthaud & Amon+2021]

Vera Rubin Observatory commissioning targets

Vera Rubin Observatory commissioning targets

Vera Rubin Observatory commissioning targets

I was part of a small team preparing a note recommending target fields for commissioning, on behalf of the Dark Energy Science Collaboration [10].

DES combined-probe cosmology

DES combined-probe cosmology

DES combined-probe cosmology

Dark Energy Survey Year 3 Cosmology from Weak Lensing and Clustering 3x2pt: I played a pivotal role in the Dark Energy Survey Year 3 combined lensing and clustering cosmology analysis, leading the weak lensing results and coordinating three analysis teams to the most precise cosmological constraints of its kind [DES Collaboration 2021].

DES cosmic shear cosmology

DES combined-probe cosmology

DES combined-probe cosmology

Dark Energy Survey Year 3 Cosmology from Cosmic Shear:  I led and coordinated the Dark Energy Survey Year 3 cosmic shear lensing analysis using the most powerful data until present, of 100 million galaxies [Amon et al 2021].

DES deep fields

DES combined-probe cosmology

DES deep fields

Dark Energy Survey Deep Fields: I co-coordinated this team, responsible for the processing and validation of the deep, optical+NIR fields, crucial for the Year 3 analysis. [16]

DES redshift calibration

DES PSF and shear estimation

DES PSF and shear estimation

I used machine learning and data science techniques to develop new statistical methods for accurate weak lensing measurements, especially for estimating and calibrating photometric redshifts for the Dark Energy Survey [15, 14].

DES PSF and shear estimation

DES PSF and shear estimation

DES PSF and shear estimation

 I have worked on validating the Dark Energy Survey's Year 3 galaxy catalogue. Specifically, I tested the shape calibration, point spread function modelling and using image simulations to understand blending, and co-coordinated the shear testing team [11,12,13].

E_G: Testing gravity

DES PSF and shear estimation

E_G: Testing gravity

I performed a combined-probe test of General Relativity with weak lensing and spectroscopic data to measure the E_G statistic [Amon+2018]

KiDS i-band survey

2-degree Field Lensing Survey

2-degree Field Lensing Survey

I processed and analysed the bright-time, single i-band dataset from the KiDS survey, which already spanned >1000 sq. deg. in 2018. I tested the homogeneity of the survey, measured and validated the PSF, shears and redshift distributions and used it as a consistency test of the main KiDS data [Amon, Heymans et al 2017]

2-degree Field Lensing Survey

2-degree Field Lensing Survey

2-degree Field Lensing Survey

I was a core member of the 2dFLenS (a spectroscopic redshift survey designed as a follow-up of KiDS) taking observations and redshiting data. It uses the  2dF-AAOmega multi-fibre spectroscopic system at the Australian Astronomical Observatory [6].

Kilo-Degree Survey (KiDS)

2-degree Field Lensing Survey

Kilo-Degree Survey (KiDS)

I was a core member of the KiDS 450 sq. deg. analysis. KiDS is a large optical imaging survey, designed primarily for weak-lensing. Its exquisite quality data is taken from the VLT Survey Telescope at the ESO Paranal Observatory [ 1, 2, 3, 4, 5].


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