Gaseous Galaxy Halos Josh Peek Columbia / Hubble Fellow w ith - PowerPoint PPT Presentation

Gaseous Galaxy Halos Josh Peek Columbia / Hubble Fellow w ith Mary Putman Columbia Ryan Joung Columbia

Look up here if you get lost! Gaseous Galaxy Halos Josh Peek Columbia / Hubble Fellow w ith Mary Putman Columbia Ryan Joung Columbia

I’ll refer to this paper a lot; if you doze o ff , read this at home

I’ll refer to this paper a lot; if you doze o ff , read this at home FB

An outline: A leetle motivation Observations of low-z halos (MW and beyond) Cool gas (<T4) warm gas (T4-T5) warm-hot gas (T5-T6) hot gas (>T6) Disk - Halo interface Simulations/theory of multiphase low-z halos

Disks require accretion, especially of low - Z gas G-Dwarf Problem Lagging Disk-Halo Interfaces Data ˙ σ inf = 40% Ψ # G Dwarfs -1 -0.5 0 M acc � ˙ ˙ M SF [Fe/H] Chiappini, Matteucci, Gratton 97; Fraternali & Binney 08

Simulations require feedback to make reasonable disks* x [ h -1 kpc ] x [ h -1 kpc ] -10 -5 0 5 10 -10 -5 0 5 10 2 2 z [ h -1 kpc ] z [ h -1 kpc ] 2 2 -10 -5 0 5 10 2 2 2 -10 -5 0 5 10 2 1 1 1 1 1 1 0 0 0 0 0 0 0 0 -1 -1 -1 -1 -1 -1 -2 -2 -2 -2 -10 -10 -5 -5 0 0 5 5 10 10 -2 -2 -2 -10 -10 -5 -5 0 0 5 5 10 10 -2 10 10 10 10 10 10 5 5 5 5 5 5 y [ h -1 kpc ] y [ h -1 kpc ] 0 0 0 0 0 0 -5 -5 -5 -5 -5 -5 -10 -10 -10 -10 -10 0 -1 no wind with wind -10 -10 -5 -5 0 0 5 5 10 10 -10 -10 -5 -5 0 0 5 5 10 10 -10 -5 0 5 10 -10 -5 0 5 10 x [ h -1 kpc ] x [ h -1 kpc ] Springel & Hernquist 2003

Simulations require feedback to make reasonable disks* FB x [ h -1 kpc ] x [ h -1 kpc ] -10 -5 0 5 10 -10 -5 0 5 10 2 2 z [ h -1 kpc ] z [ h -1 kpc ] 2 2 -10 -5 0 5 10 2 2 2 -10 -5 0 5 10 2 1 1 1 1 1 1 0 0 0 0 0 0 0 0 -1 -1 -1 -1 -1 -1 -2 -2 -2 -2 -10 -10 -5 -5 0 0 5 5 10 10 -2 -2 -2 -10 -10 -5 -5 0 0 5 5 10 10 -2 10 10 10 10 10 10 5 5 5 5 5 5 y [ h -1 kpc ] y [ h -1 kpc ] 0 0 0 0 0 0 -5 -5 -5 -5 -5 -5 -10 -10 -10 -10 -10 0 -1 no wind with wind -10 -10 -5 -5 0 0 5 5 10 10 -10 -10 -5 -5 0 0 5 5 10 10 -10 -5 0 5 10 -10 -5 0 5 10 x [ h -1 kpc ] x [ h -1 kpc ] Springel & Hernquist 2003

Most baryons are in a di ff use component -- perhaps halos? Universe Mass- Energy Budget 23.0% 73.0% 3.5% 0.5% Dark Energy Dark Matter Plasma & Gas Stars etc.

An outline: A leetle motivation Observations of low-z halos (MW and beyond) Cool gas (<T4) warm gas (T4-T5) warm-hot gas (T5-T6) hot gas (>T6) Disk - Halo interface Simulations/theory of multiphase low-z halos

W e’ve known about neutral gas in the halo for a long time Muller, Oort, Raimond 1963 Oort 1970

W e’ve known about neutral gas in the halo for a long time Muller, Oort, Raimond 1963 FB Oort 1970

HVCs are seen across the Milky W ay sky M V LSR (km s –1 ) K C +350 WA L +45º +45º A C WB +175 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE GCN LMC -175 –45º –45º O VI SMC MS Si II , Si III IHVCs MS –350 H I CHVCs Putman, JEGP, & Joung 2012

HVCs are seen across the Milky W ay sky M V GSR (km s –1 ) K +250 C WA L +45º +45º A C WB +125 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE LMC GCN -125 –45º –45º SMC MS O VI MS Si II , Si III –250 IHVCs 270º 270º H I CHVCs LA WE WD LMC WB 0º 0º SMC 0º 0º WA –45º –45º AC +45º +45º AC shell MS +90º –90º –90º 180º 180º M GCN K MS C S M33 C M31 H Putman, JEGP, & Joung 2012 90º 90º

W e find distances to HVCs with absorption lines Thom, JEGP+ 08

W e now know where most of the HVC gas is in 3D! Putman, JEGP, Joung 12; Thom+ 08; Wakker in prep

HVCs avoid the cone above and below the Galactic center 50% of volume 30° JEGP, in prep?

HVCs avoid the cone above and below the Galactic center FB 50% of volume 30° JEGP, in prep?

M31 and NGC891 have somewhat richer halos to the MW M31 NGC 891 M31 NGC891 Observed H I Observed H I 10 kpc SMC SMC LMC LMC LMC LMC SMC SMC MW MW Putman, JP, Joung 12 HVCs Westmeier, Bruns, Kerp 08 Disk Magellanic system Oosterloo,Fraternali, Sancisi 07

Other disks also have limited neutral halo gas Heald+ 10

An outline: A leetle motivation Observations of low-z halos (MW and beyond) Cool gas (<T4) warm gas (T4-T5) warm-hot gas (T5-T6) hot gas (>T6) Disk - Halo interface Simulations/theory of multiphase low-z halos

e also see lots of warm halo gas ( circles, diamonds, H α ) W M V LSR (km s –1 ) K C +350 WA L +45º +45º A C WB +175 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE GCN LMC -175 –45º –45º O VI SMC MS Si II , Si III IHVCs MS –350 H I CHVCs Putman, JEGP, & Joung 2012

W e model HVCs and find accretion rate < SFR Putman, JEGP, & Joung 12

M33 shows central warm accretion, rather than outflow 15 HI 21-cm 10 T B [K] 5 0 S II 1259 Warm Accretion 1 0 S II 1253 1 0 S II 1250 Normalized Flux 1 0 Si II 1264 1 0 Si IV 1402 Hot Accretion Warm-Hot Accretion 1 0 Si IV 1393 1 James Green/COS GTO 0 -600 -400 -200 0 200 400 600 JEGP, Putman, Werk km/s [M33 systemic]

M33 shows central warm accretion, rather than outflow 15 HI 21-cm 10 T B [K] 5 FB 0 S II 1259 Warm Accretion 1 0 S II 1253 1 0 S II 1250 Normalized Flux 1 0 Si II 1264 1 0 Si IV 1402 Hot Accretion Warm-Hot Accretion 1 0 Si IV 1393 1 James Green/COS GTO 0 -600 -400 -200 0 200 400 600 JEGP, Putman, Werk km/s [M33 systemic]

An outline: A leetle motivation Observations of low-z halos (MW and beyond) Cool gas (<T4) warm gas (T4-T5) warm-hot gas (T5-T6) hot gas (>T6) Disk - Halo interface Simulations/theory of multiphase low-z halos

W e also see associated OVI: warm - hot gas M V LSR (km s –1 ) K C +350 WA L +45º +45º A C WB +175 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE GCN LMC -175 –45º –45º O VI SMC MS Si II , Si III IHVCs MS –350 H I CHVCs Putman, JEGP, & Joung 12

There is +velocity OVI upwards, not with associated HI M V GSR (km s –1 ) K +250 C WA L +45º +45º A C WB +125 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE LMC GCN -125 –45º –45º SMC MS O VI MS Si II , Si III –250 IHVCs 270º 270º H I CHVCs LA WE WD LMC WB 0º 0º SMC 0º 0º WA –45º –45º AC +45º +45º AC shell MS +90º –90º –90º 180º 180º M GCN K MS C S M33 C M31 Putman, JEGP, & Joung 12 H 90º 90º

There is +velocity OVI upwards, not with associated HI M V GSR (km s –1 ) K +250 FB C WA L +45º +45º A C WB +125 360º 360º 270º 270º 180º 180º 90º 90º WD AC shell H LA 0º 0º 0 S M31 AC M33 WE LMC GCN -125 –45º –45º SMC MS O VI MS Si II , Si III –250 IHVCs 270º 270º H I CHVCs LA WE WD LMC WB 0º 0º SMC 0º 0º WA –45º –45º AC +45º +45º AC shell MS +90º –90º –90º 180º 180º M GCN K MS C S M33 C M31 Putman, JEGP, & Joung 12 H 90º 90º

W e can inspect other galaxies in OVI now with COS O VI Observed Wavelength [Å] 3 Tumlinson+ 11

Unexpectedly, there is lots of OVI around SF galaxies Impact parameter [kpc] Tumlinson+ 11

Are there lots of metals in halos? Ionization is key. A B Tumlinson+ 11

An outline: A leetle motivation Observations of low-z halos (MW and beyond) Cool gas (<T4) warm gas (T4-T5) warm-hot gas (T5-T6) hot gas (>T6) Disk - Halo interface Simulations/theory of multiphase low-z halos

Studying the truly hot halo ( in X - rays ) is very, very hard NGC 1961 Anderson & Bregman 2011

log(M HI /M Solar ) HI deficit in dwarf galaxies inside R_vir are a clue 0 2 4 6 8 1.0 SegueI UMaII M32 1.5 Sgr WillI NGC205 AndIX Coma AndXVII AndI BooI UMi BooII AndIII Draco Scl Sex UMaI 2.0 Car AndV NGC147 AndX For log(D/kpc) Her CVnII LeoIV AndXIV AndXV LeoV AndII LeoII NGC185 CVnI AndVII LeoI AndXVI AndVI LGS3 2.5 LeoT Phe PegDIG UGCA 092 Cet IC1613 LeoA IC10 DDO210 Tuc Grcevich & Putman 2009 WLM 3.0 SagDIG UGCA 438 Ant SexB SexA GR8 IC5152 3.5

The shape ( and pressure ) of HVCs indicate a hot halo –31°00’ N H I (10 18 cm –2 ) Velocity (km s –1 ) (GSR) 150 75 –31° 30’ 0 –290 –278 –265 –252 –240 N H I and velocity –32° 00’ –42 Declination (J2000) –32° 30’ 1 h 58 m 56 m 54 m Galactic latitude (°) –44 –34° 00’ –46 –34° 30’ –35° 00’ –48 –35° 30’ 7 h 00 m 6 h 58 m 56 m 54 m 164 162 160 158 156 Right ascension (J2000) Galactic longitude (°) Putman, JEGP, & Joung 2012