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Science-Technology

Published on August 29, 2007

Author: GenX

Source: authorstream.com

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Nearby Dwarf Galaxies as Tracers of Dark Matter:  Nearby Dwarf Galaxies as Tracers of Dark Matter the good, the bad, and the ugly Beth Willman, Irvine, March 2007 Slide2:  Made by D.W. Hogg from SDSS images The least luminous galaxies known are all nearby:  The least luminous galaxies known are all nearby Slide4:  Image courtesy J. Diemand Slide5:  Image courtesy J. Diemand How can we use nearby dwarfs to learn about the density, mass spectrum, abundance, and/or spatial distribution of dark matter on small scales? Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs:  Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs Figure from: Diemand, Kuhlen, andamp; Madau 2007 Mass spectrum predicted for CDM sub-halos:  Figure from: Diemand, Kuhlen, andamp; Madau 2007 All sub-halos within r200, in the highest resolution simulation All sub-halos within r200, in a 1/27th resolution simulation Same, but within 0.1r200 Mass spectrum predicted for CDM sub-halos Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs:  Figure from: Diemand, Kuhlen, andamp; Madau 2007 Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs:  Figure from: Diemand, Kuhlen, andamp; Madau 2007 Plenty of physics to render low mass halos dark: Reionization Stellar feedback Atomic cooling efficient to only 104 K Toomre-stable (Verde et al 02, Jimenez et al 97, Taylor andamp; Webster 05) Abundance predicted for CDM sub-halos vs. observed for Milky Way dwarfs Cosmological model + baryonic physics =andgt; Expected number and mass of nearby dwarfs? Lots of people have done this with both semi-analytic and numerical models: Benson et al, Bullock, Kravtsov andamp; Weinberg, Somerville (2002), Stoehr et al, Hayashi et al (2003), Kravtsov, Gnedin, andamp; Klypin (2004), Moore et al (2006), Governato, Willman et al (2006) Slide10:  Figure from Tassis, Kravtsov andamp; Gnedin 2007 Read, Pontzen andamp; Viel (2006), Tassis, Kravtsov, andamp; Gnedin (2007), Governato, Willman et al (in prep) all predict a sharp decrease in the stellar content of dark matter halos near some transition mass Take Home Messages:  Take Home Messages Number of nearby dwarfs is broadly consistent with CDM + baryonic physics models. Models may need to allow for upwards of 100 luminous DM sub-halos 'Lower limit' and spectrum of inferred dwarf masses is not at odds with CDM + BP models. Suppression of small scale power below baryonic building blocks may be OK for dwarf number. Spatial distribution of Milky Way dwarf galaxies:  Spatial distribution of Milky Way dwarf galaxies Image from Belokurov et al. 2007 Slide13:  Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005 also investigated r.d.s Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Taylor andamp; Babul 2004, Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Slide14:  Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005 also investigated r.d.s Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005, Kravtsov, Klypin andamp; Gnedin 2004 Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Taylor andamp; Babul 2004, Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Slide15:  Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Taylor andamp; Babul 2004, Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Slide16:  Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005 also investigated r.d.s Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005, Kravtsov, Klypin andamp; Gnedin 2004 Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Taylor andamp; Babul 2004, Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Slide17:  Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005 also investigated r.d.s Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Moore et al 2005, Kravtsov, Klypin andamp; Gnedin 2004 Update of Willman et al 04; simulation data from Diemand, Kuhlen andamp; Madau; Taylor andamp; Babul 2004, Moore et al 2006, Kravtsov, Klypin andamp; Gnedin 2004 Take Home Messages:  Take Home Messages Number of nearby dwarfs is broadly consistent with CDM + baryonic physics models. Models may need to allow for upwards of 100 luminous DM sub-halos 'Lower limit' and spectrum of inferred dwarf masses is not at odds with CDM + BP models. Suppression of small scale power below baryonic building blocks may be OK for dwarf number. Observed dwarfs are biased tracers of DM sub-halos. They are not consistent with the most massive z=0 sub-halos. Sub-halos andgt; 30 km/sec at any point in their history provide a good match to MW and M31 satellites radial distributions, and possibly abundance Slide19:  Willman et al, Zucker et al, Belokurov et al, Martin et al, Majewski et al Slide20:  Slide21:  Take Home Messages:  Take Home Messages Number of nearby dwarfs is broadly consistent with CDM + baryonic physics models. Models may need to allow for upwards of 100 luminous DM sub-halos 'Lower limit' and spectrum of inferred dwarf masses is not at odds with CDM + BP models. Suppression of small scale power below baryonic building blocks may be OK for dwarf number. Observed dwarfs are biased tracers of DM sub-halos. They are not consistent with the most massive z=0 sub-halos. Sub-halos andgt; 30 km/sec at any point in their history provide a good match to MW and M31 satellites radial distributions, and possibly abundance Lots of caveats - do the newly discovered satellites belong to the same underlying population as those known before? Slide23:  Made by D.W. Hogg from SDSS images

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