Speaker
Description
There is no consensus on how baryonic feedback shapes the underlying matter distribution. This uncertainty is a limiting systematic for cosmic shear inference, particularly in the era of LSST, and a fundamental question in the study of galaxy evolution. Modern simulations are tuned to reproduce a variety of galaxy observations, however, previous studies demonstrated that the implied amplitude of baryon feedback is dependent on the chosen observable: e.g., X-ray gas fractions, which are sensitive to material within the virial radius of massive clusters, or kinematic Sunyaev Zeldovich (kSZ) profiles, which extend to a few virial radii [Bigwood+2024, McCarthy+2024]. In this talk, we address the uncertain observational landscape, by adopting a multi-observation view of feedback. We will present measurements for the gas and mass distribution as seen by eROSITA X-rays, DESI+ACT kSZ, and galaxy-galaxy lensing across a wide range of redshifts (0<z<0.8) and halo masses (13-15). Informed by the galaxy-galaxy lensing profiles, we perform a like-with-like comparison between the observations and the FLAMINGO simulations. By constraining the gas distribution across a range of scales (i.e., kSZ versus X-ray gas fractions), redshifts, and halo masses, we are working towards a complete picture of baryon feedback.
| Primary Theme | Small to large scales |
|---|---|
| Secondary Theme | Past feedback processes to present-day observations |
| Presenter's Name | Jared Siegel |
| Presenter's Email Address | [email protected] |
| Keywords | cosmology, simulations, feedback, weak gravitational lensing |
| Recording Permission | YES |
| Virtual Audience Permission | YES |
| Photography Permission | YES |
| If your talk is not accepted for a contributed talk, would you be interested in presenting a fireslide/lightning talk? | Yes |
| If your fireslide/lighting talk is not accepted, would you be interested in presenting a poster? | Yes |
Author
Co-authors
External references
- 25070007
- acb9573c-32da-487f-a107-181d06fb32dd
