Picturing Feedback in Action in the Milky Way
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1 Picturing Feedback in Action in the Milky Way ADistantEchoofMilkyWayCentralActivityclosesthe Galaxy s Baryon Census F. Nicastro 1,2,F.Senatore [1,3], Y. Krongold 4,S.Mathur [5,6], M. Elvis 2 Nicastro (OAR-INAF) F. Senatore, Y. Krongold, M. Elvis, S. Mathur 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 1
2 Three Main Results Million-degree Gas permeates both the Disk and Halo of our Galaxy A spherically symmetric structure in the density profile of the million-degree halo gas tracks the current position of a shock-front generated 6 Million years ago by an energetic outflow powered by an AGN-like accretion episode The Mass of the OVII-bearing Gas is sufficient to close the Galaxy s Baryon Census 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 2
3 The Galaxy Missing Baryons Problem Cosmological Baryon Fraction f b = The baryon deficit is more severe in smaller galaxies è Less massive objects are unable to retain baryons (and metals?) due to feedback processes (winds)? è Are these baryons in the surrounding CGM/IGM? 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 3
4 The Milky Way s Baryon Problem (M b ) Obs = 6.5x10 10 M (McMillian & Binney, 2012) M DM = (1-2)x10 12 M (Boylan-Kolchin+12) f b = (The Plank Collaboration, 2015) è M b /(M b ) Obs M b Missing (1.5-3)x10 11 M 5/27/16 Vulcano Workshop 2016 (F. Nicastro) 4
5 The Hot z=0 Absorber(s) Nicastro+02 Williams+05 Highly Ionized, Warm and Cold Medium seen in all directions (e.g. Bregman+07, Gupta+11, Fang+13) Location Not Known 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 5
6 Low-Density: Locates the gas at >50 kpc Local Group? Local WHIM filament? CGM? The OVI Problem (Williams+05) 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 6
7 All the X-ray Spectral Signatures of the Milky Way Nicastro+16a /26/16 Vulcano Workshop 2016 (F. Nicastro) 7
8 The Optimal OVII Sample Differs from previous (e.g. Gupta+12, Miller&Bregman13): - HGL + LGL for the first time - Complete to SNRE>10 at 22 Å - Remove NOVII-b Degeneracy 18/20 (90%) LGL have OVII, but only 14 known distance (1 contaminated) 52 HGL; 9 contaminated + 3 Instr.Feat.; 34/39 (87%) have OVII, but only 18 Kα & Kβ è 13 LGL (XRBs) + 18 HGL (AGNs) = 31 LoS 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 8
9 Adopted Density Profiles ξ(r) = LoS coordinate, with R 2 = ξ 2 + R 2 2ξR cos(b)cos(l) n(r) =n 0 e R R s /R c ; (Exponential Sphere) n(r) =n 0 e (ρ/ρ c ) 2 +(z h s )/h c ) 2 ; (Exponential Disk) n(r) =n 0 [1 + (R R s ) 2 /R 2 c] 3β/2 ; (β-sphere) n(r) =n 0 [1 + ρ 2 /ρ 2 c +(z h s) 2 /h 2 c ] 3β/2. (β-cylinder) R s and h s = Offset Radius and Height 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 9
10 Separate LGL & HGL N OVII -(l,b) Fits Model Model n 0 R c or ρ c h c R s Halo Size Mass chi 2 (dof) Name Type (10 2 cm 3 ) (kpc) (kpc) (kpc) (kpc) (10 9 M HGL M1 Exp-SS N/A > (15) LGL M2 Exp-CS N/A N/A (10) LGL: χ 2 flat (dof) = 12.8(10) vs χ2 Sph (dof) = 22.5(11) LGL to HLG: χ 2 (dof) = 373(18)!!! HGL to LGL: χ 2 (dof) = 147(13)!!! LGL trace the Galaxy s Disk: M OVII (Disk) 1.4x10 8 M 2 distinct components or compromising solution 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 10
11 Combined LGL+HGL N OVII -(l,b) Fits Model Model n 0 R c β R s Halo Size Mass chi 2 (dof) Name Type (10 2 cm 3 ) (kpc) (kpc) (kpc) (10 11 M A β-ss > (27) B M2 + β-ss /8 > M3 M2 + β-ss (frozen) 0 (frozen) > M4 β-ss (frozen) 0 (frozen) > (27) (29) (29) Model A: peak density at 6 kpc Model B: empty central 6-kpc sphere P(A;M4) = 99.8% ; P(A;M3) = 91.3% /25/16 Vulcano Workshop 2016 (F. Nicastro) 11
12 Why an Offset Radius? Model A Model A Model M4 Model M4 Model B Model B Model M3 Model M3 HGL (AGNs) LGL (XRBs) HGL (AGNs) LGL (XRBs) HGL (AGNs) LGL (XRBs) HGL (AGNs) LGL (XRBs) /25/16 Vulcano Workshop 2016 (F. Nicastro) 12
13 OVII Emission Measure In 1-sr around l=90 0, b=60 0 : EM = cm -6 pc (McCammon+02) EM(A; b 60 0 ;30 0 <l<150 0 )= cm 6 pc EM(B; b 60 0 ;30 0 <l<150 0 )= cm 6 pc. Toward the Galactic Center at b <20 0 and across the Fermi Bubbles: EM = ( ) cm -6 pc (Kataoka+15) EM(A; b 20 0 ;340 0 <l<20 0 )= cm 6 pc EM(B; b 20 0 ;340 0 <l<20 0 )= cm 6 pc, 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 13
14 The 6-kpc Central Cavity (other pieces of evidence) Size and shape similar to Fermi Bubbles (gamma-rays) and Plank Haze (microwave): Dobler+10; Su+10 Seen in Hα and IR emission: Bland-Hawthorn+03 Seen in modulation of X-ray EM across edges of Fermi Bubbles: Kataoka+15 Resolved in moderate-ionization double-peaked (nearand far-side of the bubble) metal absorption suggesting expansion v 1000 km/s: Fox+15 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 14
15 A Distant Echo of Central Activity A fast moving piston powered by a period of activity of our supermassive black hole moves outwards and compresses the ambient gas while pushing (a fraction of) it outwards (i.e. Davè+11; Faucher-Giguère & Quataert, 2012, Lapi+05) Nuclear energy-conserving outflows with v in km/s produce shock traveling at v s 1000 km/s (Faucher- Giguère & Quataert, 2012) At this rate it would take 6 Myrs for the OVII-traced shock to reach its current position at 6 kpc (6 ± 2) Myr is also the age of 2 stellar disks in the innermost 0.2 pc of the Milky Way, thought to be a relic of a gaseous accretion disk (Paumard+06; Levin, Beloborodov 03) 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 15
16 Checking the Energetic For a simple isothermal sphere ΔM/M 1/2ΔE/E (Lapi+05) è M Bubble = M ( M/M) Bubble E/E E ((kt Hot )/kev ) 5/2 For T Hot (0.6-1)x10 6 K è E ( )x10 59 ergs è ΔE (0.1-4)x10 57 ergs = 1/2ΔM<v 2 > è <v> km/s ΔE<<E AGN (Δt=4-8 Myr) (2.5-5)x10 58 ergs ergs 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 16
17 Closing the Galaxy s Baryon Census Closes the Milky Way Baryon Census Sizes: R(A)>61 kpc R(B)>190 kpc Masses at R vir : M(A)=( )x1011 M M(A)=( )x1011 M 1.5 Model B Actual Solution probably in between 1 Model A /25/16 Vulcano Workshop 2016 (F. Nicastro) 17
18 Conclusions Million-degree Gas permeates both the Disk and Halo of our Galaxy A spherically symmetric structure in the density profile of the million-degree halo gas tracks the current position of a shock-front generated 6 Million years ago by an energetic outflow powered by an AGN-like accretion episode The Mass of the OVII-bearing Gas may be sufficient to close the Galaxy s Baryon Census 5/25/16 Vulcano Workshop 2016 (F. Nicastro) 18
A Dist ant Echo of M ilky Way Cent ral A ct ivity closes t he Galaxy s B aryon Census
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