J.Wagner:The cosmological Cheshire cat
Posted: Fri 19 Jun 2020 16:11
VIA lecture by Jenny Wagner "The cosmological Cheshire cat -- how to characterize dark matter halo shapes without seeing them" was given on 19.06.2020. Its presentation is attached and the record is in VIA library
http://viavca.in2p3.fr/jenny_wagner.html
The following questions were put in the course of the talk:
Shantanu: Please clarify: what is PIEMD?
Shantanu: Do you assume substructure in your halo model?
Shantanu: which of these cases corresponds to dwarf spheroidals?
Shantanu: 1. Within this formalism can you explain the empirical observation of constant surface density of dark matter haloes found by Donato et al (2009) or Kormendy & Freeman (2004)?
Shantanu: I presume you assumed Newtonian gravity? How easy it is to extend this formalism to non-Newtonian gravity theories
Sotiris Loucatos: On p 6 in the various profiles, what is the reason of strong fluctuations at large r?
Shantanu: Since Prof. Liliya Williams is also on the online, would you like to answer the first question? (either within this model or on basis of the model you mentioned in your VIA talk many years ago)
Shantanu: I will write the reference
https://academic.oup.com/mnras/article/397/3/1169/1074365
Vlad: What if the structure is built by substructures as halo stars show?
Liliya Williams: Hi, what is the question? Modified gravity? In our formalism, gravity comes in in the equation that connects kinetic and potential energy and the total energy, so whichever way modified gravity will change that will affect our result for differential energy distribution.
Shantanu: No, my first question is whether this model can explain the constant surface density of dark matter haloes first found by Kormendy & Freeman (2004) and also by Donato et al (2009) (reference to MNRAS provided above)
Shantanu: what about self-interacting DM?
You are welcome to continue discussion of this topic in replies to this post
http://viavca.in2p3.fr/jenny_wagner.html
The following questions were put in the course of the talk:
Shantanu: Please clarify: what is PIEMD?
Shantanu: Do you assume substructure in your halo model?
Shantanu: which of these cases corresponds to dwarf spheroidals?
Shantanu: 1. Within this formalism can you explain the empirical observation of constant surface density of dark matter haloes found by Donato et al (2009) or Kormendy & Freeman (2004)?
Shantanu: I presume you assumed Newtonian gravity? How easy it is to extend this formalism to non-Newtonian gravity theories
Sotiris Loucatos: On p 6 in the various profiles, what is the reason of strong fluctuations at large r?
Shantanu: Since Prof. Liliya Williams is also on the online, would you like to answer the first question? (either within this model or on basis of the model you mentioned in your VIA talk many years ago)
Shantanu: I will write the reference
https://academic.oup.com/mnras/article/397/3/1169/1074365
Vlad: What if the structure is built by substructures as halo stars show?
Liliya Williams: Hi, what is the question? Modified gravity? In our formalism, gravity comes in in the equation that connects kinetic and potential energy and the total energy, so whichever way modified gravity will change that will affect our result for differential energy distribution.
Shantanu: No, my first question is whether this model can explain the constant surface density of dark matter haloes first found by Kormendy & Freeman (2004) and also by Donato et al (2009) (reference to MNRAS provided above)
Shantanu: what about self-interacting DM?
You are welcome to continue discussion of this topic in replies to this post