The Baryon Content of Dark Matter Halos: Hsiao-Wen Chen. (University of Chicago)
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1 The Baryon Content of Dark Matter Halos: Hsiao-Wen Chen (University of Chicago)
2 Mapping the Dark Universe
3 Mapping the Dark Universe Absorption spectrum of a distant quasar
4 Mapping the Dark Universe Absorption spectrum of a distant quasar
5 Mapping the Dark Universe probing halo gas on kpc scales M31 Thilker+ 04 ~ 10 kpc Absorption spectrum of a distant quasar
6 Properties of MgII absorbers prominent doublet features at λ=2796, 2803 A ; observable in the optical window at z =
7 Properties of MgII absorbers prominent doublet features at λ=2796, 2803 A ; observable in the optical window at z = photo-ionized gas of T ~ 10,000 K; probing warm gas in the ISM and galactic halos (Bergeron & Stasinska 86)
8 Properties of MgII absorbers prominent doublet features at λ=2796, 2803 A ; observable in the optical window at z = photo-ionized gas of T ~ 10,000 K; probing warm gas in the ISM and galactic halos (Bergeron & Stasinska 86) multi-component features with the absorption equivalent width W number of components (Petitjean & Bergeron 90; Churchill & Vogt 01; Prochter +06) W => underlying gas kinematics
9 Properties of MgII absorbers prominent doublet features at λ=2796, 2803 A ; observable in the optical window at z = photo-ionized gas of T ~ 10,000 K; probing warm gas in the ISM and galactic halos (Bergeron & Stasinska 86) multi-component features with the absorption equivalent width W number of components (Petitjean & Bergeron 90; Churchill & Vogt 01; Prochter +06) association with luminous galaxies at ρ 100 h -1 kpc (Lanzetta & Bowen 90; Steidel +94; Kacprzak +08)
10 Probing halo gas with MgII absorbers High Velocity Clouds in the Milky Way Halo
11 Probing halo gas with MgII absorbers High Velocity Clouds in the Milky Way Halo unknown distances
12 Probing halo gas with MgII absorbers Rao et al. (2006) High Velocity Clouds in the Milky Way Halo unknown distances
13 Probing halo gas with MgII absorbers Rao et al. (2006) High Velocity Clouds in the Milky Way Halo unknown distances High velocity MgII cloud along PG v = km s -1 Sembach+04 sensitive to low column density clouds
14 Empirical Constraints from a Random Sample of Foreground Galaxies Chen & Tinker (2008)
15 Empirical Constraints from a Random Sample of Foreground Galaxies Chen & Tinker (2008) z = ρ = 16 h -1 kpc 3C336 W=1.55 Å 0.892
16 Empirical Constraints from a Random Sample of Foreground Galaxies Chen & Tinker (2008) z = ρ = 16 h -1 kpc z = ρ = 31 h -1 kpc 3C336 W=1.55 Å PKS W=0.85 Å 0.892
17 Empirical Constraints from a Random Sample of Foreground Galaxies Chen & Tinker (2008) z = ρ = 16 h -1 kpc z = ρ = 31 h -1 kpc z = ρ = 76 h -1 kpc 3C336 W=1.55 Å PKS W=0.85 Å PKS W=0.42 Å 0.892
18 Extent of Gaseous Halos and Covering Fraction 23 galaxies at z= Chen & Tinker (2008)
19 Extent of Gaseous Halos and Covering Fraction 23 galaxies at z= Chen & Tinker (2008)
20 Extent of Gaseous Halos and Covering Fraction 23 galaxies at z= The extent of Mg + ions scales with galaxy luminosity, Rgas = 91x(LB/LB*) The gas covering fraction is κg ~ 100% around galaxies of > 0.2 L*, and < 50% around fainter galaxies. Chen & Tinker (2008)
21 The Origin of Halo Clouds: fuel for star formation or wind remnant? Chen & Tinker (2008)
22 The Origin of Halo Clouds: fuel for star formation or wind remnant? Chen & Tinker (2008) photoionization
23 The Origin of Halo Clouds: fuel for star formation or wind remnant? Chen & Tinker (2008) Chen+ 01 CIV comparable extent between C 3+ and Mg +
24 The Origin of Halo Clouds: fuel for star formation or wind remnant? Chen & Tinker (2008) two-phase medium: pressure confined cold clouds in hot halos Mo & Miralda-Escudé 96; Maller & Bullock 04 MgII profiles Chen+ 01 CIV profiles CIV comparable extent between C 3+ and Mg +
25 The Origin of Halo Clouds: fuel for star formation or wind remnant? Chen & Tinker (2008) two-phase medium: pressure confined cold clouds in hot halos Mo & Miralda-Escudé 96; Maller & Bullock 04 MgII profiles Chen+ 01 CIV profiles CIV comparable extent between C 3+ and Mg +
26 Constraining halo gas content over a broad mass range luminous red galaxies vs. MgII Absorbers at z = Visualization of SDSS DR5 Courtesy of Mark SubbaRao
27 Constraining halo gas content over a broad mass range luminous red galaxies vs. MgII Absorbers at z = Visualization of SDSS DR5 Courtesy of Mark SubbaRao
28 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. Tinker & Chen (2008)
29 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. Prochter et al. (2006) Steidel & Sargent (1992) DATA frequency distribution function + 2-pt clustering amplitude Tinker & Chen (2008)
30 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. DATA frequency distribution function + 2-pt clustering amplitude Bouché et al. (2006) Tinker & Chen (2008)
31 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. DATA frequency distribution function + 2-pt clustering amplitude MODEL known dark matter halos + gaseous halo profile Tinker+ 06 Tinker & Chen (2008)
32 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. density profile : (r 2 +a 2 ) -1 gaseous extent : Rg=1/3 R200 mass dependence : Mh 1/3 DATA frequency distribution function + 2-pt clustering amplitude W (s M) = W R 0 σ cl f g 2 s2 g M cl 0 ρ( s 2 + l 2 )dl MODEL known dark matter halos + gaseous halo profile s dl Tinker & Chen (2008)
33 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. density profile : (r 2 +a 2 ) -1 gaseous extent : Rg=1/3 R200 mass dependence : Mh 1/3 DATA frequency distribution function + 2-pt clustering amplitude MODEL known dark matter halos + gaseous halo profile P(log M W) RESULTS P(W Mh): incidence and extent of cold gas vs. DM halo mass Tinker & Chen (2008)
34 Halo Occupation of Dark Baryons An empirical mapping between DM halos and baryons through a statistical approach. density profile : (r 2 +a 2 ) -1 gaseous extent : Rg=1/3 R200 mass dependence : Mh 1/3 DATA frequency distribution function + 2-pt clustering amplitude P(log M W) the data demand a transition in the halo gas content MODEL known dark matter halos + gaseous halo profile RESULTS P(W Mh): incidence and extent of cold gas vs. DM halo mass Tinker & Chen (2008)
35 Comparisons with Theoretical Expectations The growth of hot halos vs. halo mass Keres et al Tinker & Chen 08
36 Summary A self-consistent model is established to characterize the origin of absorption systems uncovered in QSO spectra. A larger galaxy-absorber pair sample allows a detailed investigation of κg vs. LB (a proxy of Mh) and κg vs. ρ.
37 Summary A self-consistent model is established to characterize the origin of absorption systems uncovered in QSO spectra. A larger galaxy-absorber pair sample allows a detailed investigation of κg vs. LB (a proxy of Mh) and κg vs. ρ. individual probes A MagE survey of MgII in SDSS galaxies J.-R. Gauthier, J. Helsby, J. Tinker, S. Shectman, I. Thompson
38 Summary A self-consistent model is established to characterize the origin of absorption systems uncovered in QSO spectra. A larger galaxy-absorber pair sample allows a detailed investigation of κg vs. LB (a proxy of Mh) and κg vs. ρ. individual probes A MagE survey of MgII in SDSS galaxies 2D map of individual halos M31 J.-R. Gauthier, J. Helsby, J. Tinker, S. Shectman, I. Thompson Thilker+ 04 ~ 10 kpc
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