I’m at the Dark Matter Probe Combination workshop at KICP this week, let’s try conference skeeting for the first time since coming over to blue sky! Will use #KICPDM as the tag and try to thread…
September 2, 2026 at 2:24 PM
I’m at the Dark Matter Probe Combination workshop at KICP this week, let’s try conference skeeting for the first time since coming over to blue sky! Will use #KICPDM as the tag and try to thread…
Julian Munoz: the UV luminosity function of high-z galaxies also constrains power spectrum (lots of degeneracies as M_UV closer to SFR the Mstar, can partially break with clustering). With JWST/GLIMPSE can reach k~30 #KICPDM
September 3, 2026 at 4:33 PM
Julian Munoz: the UV luminosity function of high-z galaxies also constrains power spectrum (lots of degeneracies as M_UV closer to SFR the Mstar, can partially break with clustering). With JWST/GLIMPSE can reach k~30 #KICPDM
Vera Gluscevic starts with "read this paper for everything I won't get to" arxiv.org/abs/2607.28564 #KICPDM
Dark Matter Constraints from Small-Scale Cosmic Structure
Small-scale cosmic structure provides a powerful test of the fundamental nature of dark matter (DM). A wide range of DM models impact matter clustering on small scales, including warm, fuzzy, and (sel...
arxiv.org
September 2, 2026 at 7:31 PM
Vera Gluscevic starts with "read this paper for everything I won't get to" arxiv.org/abs/2607.28564 #KICPDM
Mariangela Lisanti reviews three examples of dark sector interactions. CDM is quite unusual, no standard model equivalent. p-n scattering >> self-interacting dark matter, hydrogen atom >> disspiative/atomic dark matter, EM plasma >> dark plasma #KICPDM
September 3, 2026 at 2:17 PM
Mariangela Lisanti reviews three examples of dark sector interactions. CDM is quite unusual, no standard model equivalent. p-n scattering >> self-interacting dark matter, hydrogen atom >> disspiative/atomic dark matter, EM plasma >> dark plasma #KICPDM
Last day of #KICPDM is the best day, dwarf galaxies! :D This thread is Ting Li, Jiaxuan Li, Andrew Pace, Kaia Atzberger, and Alyson Brooks. I am chairing so let’s see how I do with the skeeting..
September 4, 2026 at 2:12 PM
Last day of #KICPDM is the best day, dwarf galaxies! :D This thread is Ting Li, Jiaxuan Li, Andrew Pace, Kaia Atzberger, and Alyson Brooks. I am chairing so let’s see how I do with the skeeting..
Gluscevic: particle theories predict P(k), but for now it's better to think about features: P(k) cutoff, plateau, enhancement. Cutoffs are very well-understood (e.g. WDM, IDM, FDM) and suppress structure; astrophysics is very constraining here #KICPDM
September 2, 2026 at 7:40 PM
Gluscevic: particle theories predict P(k), but for now it's better to think about features: P(k) cutoff, plateau, enhancement. Cutoffs are very well-understood (e.g. WDM, IDM, FDM) and suppress structure; astrophysics is very constraining here #KICPDM
@spacewsarah.bsky.social : stellar streams probe DM with subhalo perturabtions, host halo shapes, and stream frequency. Perturbations to globular cluster streams is one of the most exciting topics because it could probe star-free DM halos. #KICPDM
September 2, 2026 at 3:57 PM
@spacewsarah.bsky.social : stellar streams probe DM with subhalo perturabtions, host halo shapes, and stream frequency. Perturbations to globular cluster streams is one of the most exciting topics because it could probe star-free DM halos. #KICPDM
Crumrine: in the LSST era, will discover both dwarf galaxies and star clusters. A unified model of the whole stellar system population is able to recover dark matter bounds (as long as the star clusters are not too bad) #KICPDM
September 2, 2026 at 8:07 PM
Crumrine: in the LSST era, will discover both dwarf galaxies and star clusters. A unified model of the whole stellar system population is able to recover dark matter bounds (as long as the star clusters are not too bad) #KICPDM
Wendy Crumrine: using existing limits on dark matter, can generalize this to new particle physics models that have similar power spectra; e.g. extended to mixed dark matter with a fraction of DM interacting with photons, neutrinos, baryons, or fuzzy DM arxiv.org/abs/2606.10006 #KICPDM
Mixed Dark Matter: Limits from the Milky Way Satellite Galaxies
The Standard Model of particle physics contains a diverse set of particle species, motivating the possibility of a similarly complex dark sector. Here we study two-component dark matter (DM) mixtures,...
arxiv.org
September 2, 2026 at 8:01 PM
Wendy Crumrine: using existing limits on dark matter, can generalize this to new particle physics models that have similar power spectra; e.g. extended to mixed dark matter with a fraction of DM interacting with photons, neutrinos, baryons, or fuzzy DM arxiv.org/abs/2606.10006 #KICPDM
Niusha Ahvazi implements constrained MW with LMC into Galacticus. This could make a difference in the satellite radial distribution, but surprisingly there is almost no difference in the theoretical radial distribution, only ~15%. Observational incompleteness explains current observations #KICPDM
September 2, 2026 at 8:17 PM
Niusha Ahvazi implements constrained MW with LMC into Galacticus. This could make a difference in the satellite radial distribution, but surprisingly there is almost no difference in the theoretical radial distribution, only ~15%. Observational incompleteness explains current observations #KICPDM
Alyson Brooks: LMC/SMC mass galaxies have a diversity of rotation curves, some steeply rising some slowly rising. LCDM can do one or the other, but seemed hard to do both. However, Marvelous Massive Dwarf Zoom simulations can make things spanning the full range of diversity #KICPDM
September 4, 2026 at 3:12 PM
Alyson Brooks: LMC/SMC mass galaxies have a diversity of rotation curves, some steeply rising some slowly rising. LCDM can do one or the other, but seemed hard to do both. However, Marvelous Massive Dwarf Zoom simulations can make things spanning the full range of diversity #KICPDM
Andrew Pace: infer density profiles with 400-2000 stars hard to distinguish core-to-cusp. Chang+Necib: need at least 10k stars to do it. No one did it for a while, so he decided to do it himself :) crazy campaign now has ~7600 new unique stars -> 8300 total numbers #KICPDM
September 4, 2026 at 2:45 PM
Andrew Pace: infer density profiles with 400-2000 stars hard to distinguish core-to-cusp. Chang+Necib: need at least 10k stars to do it. No one did it for a while, so he decided to do it himself :) crazy campaign now has ~7600 new unique stars -> 8300 total numbers #KICPDM
Tyler Smith simulates SIDM at z>6, can see its effect even at z~15. SIDM makes subhalos disrupt 4-5x more (maybe can feed gas to host halo for starburst). SIDM core-collapse has been proposed for LRD formation but is prevented by lots of mergers stopping collapse. #KICPDM
September 3, 2026 at 5:02 PM
Tyler Smith simulates SIDM at z>6, can see its effect even at z~15. SIDM makes subhalos disrupt 4-5x more (maybe can feed gas to host halo for starburst). SIDM core-collapse has been proposed for LRD formation but is prevented by lots of mergers stopping collapse. #KICPDM
Forecasts for which streams should have the most impacts highlight the Jet stream (one of my favorite!) as a prime candidate with >5 expected impacts! :O arxiv.org/abs/2608.19321 #KICPDM
Detectable subhalo impacts in Milky Way streams
Dark matter subhalos leave gravitational imprints in the stellar streams of the Milky Way. Observing individual strong impacts of subhalos offers a compelling way to constrain and discover potentially...
arxiv.org
September 2, 2026 at 4:21 PM
Forecasts for which streams should have the most impacts highlight the Jet stream (one of my favorite!) as a prime candidate with >5 expected impacts! :O arxiv.org/abs/2608.19321 #KICPDM
Li: ex with Boo3, need to throw in an NFW halo with Mhalo ~ 1e6 Msun in order to explain low velocity dispersion. Same with Crater II. #KICPDM
September 4, 2026 at 2:27 PM
Li: ex with Boo3, need to throw in an NFW halo with Mhalo ~ 1e6 Msun in order to explain low velocity dispersion. Same with Crater II. #KICPDM
Jiaxuan Li: host-to-host scatter and different environment may affect SMHM inference. No one would say galaxy formation does not depend on environment :) a promising environment is around dwarfs #KICPDM
September 4, 2026 at 2:31 PM
Jiaxuan Li: host-to-host scatter and different environment may affect SMHM inference. No one would say galaxy formation does not depend on environment :) a promising environment is around dwarfs #KICPDM
Pace: velocity dispersion profile is flat, can measure kurtosis with 100 stars per bin, difference dynamics between metallicity bins. New surveys are finally coming, but the future is here too :) #KICPDM
September 4, 2026 at 2:51 PM
Pace: velocity dispersion profile is flat, can measure kurtosis with 100 stars per bin, difference dynamics between metallicity bins. New surveys are finally coming, but the future is here too :) #KICPDM
Atzberger: major challenge is models are giving different predictions for what cored and cusped halos predict for stream width :( however cosmological simulations predict we should get more of these if we could go fainter. Now looking at total mass loss as a constraint. #KICPDM
September 4, 2026 at 3:03 PM
Atzberger: major challenge is models are giving different predictions for what cored and cusped halos predict for stream width :( however cosmological simulations predict we should get more of these if we could go fainter. Now looking at total mass loss as a constraint. #KICPDM
Brooks: with CDM only, see correlation with surface brightness. If you add SIDM in this model, you *lose* diversity because it cores everything...SIDM changes galaxy gas disk sizes, masses, and symmetry. In this mass range can probe halo shape. Mock observations add even more scatter #KICPDM
September 4, 2026 at 3:17 PM
Brooks: with CDM only, see correlation with surface brightness. If you add SIDM in this model, you *lose* diversity because it cores everything...SIDM changes galaxy gas disk sizes, masses, and symmetry. In this mass range can probe halo shape. Mock observations add even more scatter #KICPDM
Ting Li: Sgr Ant2, Boo3, Cra2, and Tuc3 are the 5 MW satellites with unusually large sizes and small velocity dispersions (low density, below MW density). All of them have clear tidal features. Ting got impatient with the theorists to model these so she has done it herself :) #KICPDM
September 4, 2026 at 2:19 PM
Ting Li: Sgr Ant2, Boo3, Cra2, and Tuc3 are the 5 MW satellites with unusually large sizes and small velocity dispersions (low density, below MW density). All of them have clear tidal features. Ting got impatient with the theorists to model these so she has done it herself :) #KICPDM
Kaia Atzberger: Crater II has large size and low sigma_v, hard to make form an NFW halo, but can do it with cored profile. Need to understand how much mass is lost and in tidal tails. Using CaHK metallicity filter to remove contamination (36 mag/sq arcsec), >25% stellar mass loss. #KICPDM
September 4, 2026 at 3:00 PM
Kaia Atzberger: Crater II has large size and low sigma_v, hard to make form an NFW halo, but can do it with cored profile. Need to understand how much mass is lost and in tidal tails. Using CaHK metallicity filter to remove contamination (36 mag/sq arcsec), >25% stellar mass loss. #KICPDM
Nierenberg: Euclid/LSST/Roman will get 100k's of new galaxy-galaxy lenses! Overall hints of very dense perturbers relative to CDM, interesting to see similar to streams #KICPDM
September 3, 2026 at 7:23 PM
Nierenberg: Euclid/LSST/Roman will get 100k's of new galaxy-galaxy lenses! Overall hints of very dense perturbers relative to CDM, interesting to see similar to streams #KICPDM