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

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

Jul 24, 2023 216 likes •803 views

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

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Gaseous Galaxy Halos

Josh Peek Columbia / Hubble Fellow

with

Mary Putman Columbia Ryan Joung Columbia

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Gaseous Galaxy Halos

Josh Peek Columbia / Hubble Fellow

with

Mary Putman Columbia Ryan Joung Columbia

Look up here if you get lost!

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SLIDE 3

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

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SLIDE 4

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

FB

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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

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Disks require accretion, especially of low-Z gas

Chiappini, Matteucci, Gratton 97; Fraternali & Binney 08

G-Dwarf Problem

[Fe/H] # G Dwarfs

  • 1 -0.5 0

Data

˙ σinf Ψ = 40%

Lagging Disk-Halo Interfaces ˙ Macc ˙ MSF

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no wind

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with wind

Springel & Hernquist 2003

Simulations require feedback to make reasonable disks*

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no wind

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with wind

Springel & Hernquist 2003

Simulations require feedback to make reasonable disks*

FB

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0.5% 3.5% 23.0% 73.0% Dark Energy Dark Matter Plasma & Gas Stars etc.

Universe Mass- Energy Budget

Most baryons are in a diffuse component -- perhaps halos?

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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

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SLIDE 11

W e’ve known about neutral gas in the halo for a long time

Muller, Oort, Raimond 1963 Oort 1970

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SLIDE 12

W e’ve known about neutral gas in the halo for a long time

Muller, Oort, Raimond 1963 Oort 1970

FB

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HVCs are seen across the Milky W ay sky

–350 +350 C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 180º 90º +45º AC shell LMC SMC M31 M33 +175
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MS C WE VLSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

Putman, JEGP, & Joung 2012

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SLIDE 14 +45º 0º +45º MS AC GCN S WA WB M C K H 0º –45º –45º 0º –90º 0º +90º –90º LMC SMC M31 M33 MS C WE LA WD C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 270º 90º 270º 90º 180º 180º 180º 90º +45º AC shell AC shell LMC SMC M31 M33 MS C WE –250 +250 +125
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VGSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

HVCs are seen across the Milky W ay sky

Putman, JEGP, & Joung 2012

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W e find distances to HVCs with absorption lines

Thom, JEGP+ 08

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W e now know where most of the HVC gas is in 3D!

Putman, JEGP, Joung 12; Thom+ 08; Wakker in prep

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HVCs avoid the cone above and below the Galactic center

30° 50% of volume

JEGP, in prep?

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HVCs avoid the cone above and below the Galactic center

FB

30° 50% of volume

JEGP, in prep?

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SLIDE 19 M31 NGC 891 LMC SMC LMC SMC LMC SMC LMC SMC HVCs 10 kpc Observed H I Disk Magellanic system Observed H I Putman, JP, Joung 12 Westmeier, Bruns, Kerp 08 Oosterloo,Fraternali, Sancisi 07

M31 NGC891 MW MW

M31 and NGC891 have somewhat richer halos to the MW

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Other disks also have limited neutral halo gas

Heald+ 10

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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

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W e also see lots of warm halo gas (circles, diamonds, Hα)

–350 +350 C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 180º 90º +45º AC shell LMC SMC M31 M33 +175
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MS C WE VLSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

Putman, JEGP, & Joung 2012

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W e model HVCs and find accretion rate < SFR

Putman, JEGP, & Joung 12

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km/s [M33 systemic] HI 21-cm 1 1 1 1 1 1 Hot Accretion Warm Accretion TB [K] Normalized Flux Si II 1264 S II 1253 S II 1250 S II 1259 Si IV 1402 Si IV 1393

M33 shows central warm accretion, rather than outflow

James Green/COS GTO JEGP, Putman, Werk

Warm-Hot Accretion
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SLIDE 25 15 10 5
  • 600 -400 -200 0 200 400 600
km/s [M33 systemic] HI 21-cm 1 1 1 1 1 1 Hot Accretion Warm Accretion TB [K] Normalized Flux Si II 1264 S II 1253 S II 1250 S II 1259 Si IV 1402 Si IV 1393

M33 shows central warm accretion, rather than outflow

FB

James Green/COS GTO JEGP, Putman, Werk

Warm-Hot Accretion
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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

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W e also see associated OVI: warm-hot gas

–350 +350 C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 180º 90º +45º AC shell LMC SMC M31 M33 +175
  • 175
MS C WE VLSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

Putman, JEGP, & Joung 12

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SLIDE 28 +45º 0º +45º MS AC GCN S WA WB M C K H 0º –45º –45º 0º –90º 0º +90º –90º LMC SMC M31 M33 MS C WE LA WD C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 270º 90º 270º 90º 180º 180º 180º 90º +45º AC shell AC shell LMC SMC M31 M33 MS C WE –250 +250 +125
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VGSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

There is +velocity OVI upwards, not with associated HI

Putman, JEGP, & Joung 12

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SLIDE 29 +45º 0º +45º MS AC GCN S WA WB M C K H 0º –45º –45º 0º –90º 0º +90º –90º LMC SMC M31 M33 MS C WE LA WD C L LA WD WA WB MS AC M A H GCN K S –45º 0º +45º –45º 0º 360º 270º 180º 90º 360º 270º 270º 90º 270º 90º 180º 180º 180º 90º +45º AC shell AC shell LMC SMC M31 M33 MS C WE –250 +250 +125
  • 125
VGSR (km s–1) OVI SiII, SiIII IHVCs HI CHVCs

There is +velocity OVI upwards, not with associated HI

FB

Putman, JEGP, & Joung 12

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W e can inspect other galaxies in OVI now with COS

Observed Wavelength [Å]

3

O VI

Tumlinson+ 11

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Impact parameter [kpc]

Unexpectedly, there is lots of OVI around SF galaxies

Tumlinson+ 11

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B A

Are there lots of metals in halos? Ionization is key.

Tumlinson+ 11

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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

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Studying the truly hot halo (in X-rays) is very, very hard

Anderson & Bregman 2011

NGC 1961

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SLIDE 35 1.0 1.5 2.0 2.5 3.0 3.5 log(D/kpc) 2 4 6 8 log(MHI/MSolar) BooI Coma SegueI Her LeoIV LeoI Scl Sex Tuc Car For Cet BooII CVnI CVnII UMaI UMaII WillI LeoII UMi Draco Sgr LeoV AndI AndII AndIII AndV AndVI AndVII AndIX AndX AndXIV AndXV AndXVI AndXVII NGC147 NGC185 NGC205 Phe Ant DDO210 LGS3 PegDIG LeoT IC10 UGCA 092 LeoA SexB SexA GR8 SagDIG IC5152 UGCA 438 M32 IC1613 WLM

HI deficit in dwarf galaxies inside R_vir are a clue

Grcevich & Putman 2009

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SLIDE 36 Right ascension (J2000) Galactic longitude (°) NHI and velocity Galactic latitude (°) Declination (J2000) –35° 30’ –48 –46 –44 –42 –35° 00’ –34° 30’ –34° 00’ –32° 30’ –32° 00’ –31° 30’ –31°00’ 1h 58m 7h 00m 6h 58m 56m 54m 164 162 160 158 156 56m 54m Velocity (km s–1) (GSR) NHI (1018 cm–2) 75 150 –278 –290 –265 –252 –240

The shape (and pressure) of HVCs indicate a hot halo

Putman, JEGP, & Joung 2012

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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

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SLIDE 38 ~ disk ~3 kpc Warm ionized medium Hot ionized medium Rotating neutral gas

Cool, warm, and hot gas interact in the Disk-Halo interface

Putman, JEGP, & Joung 2012

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Ford, Lockman,& McClure-Griffiths 2010

HI clouds are lofted kpc above the bar by star formation

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Ford, Lockman,& McClure-Griffiths 2010

HI clouds are lofted kpc above the bar by star formation

FB

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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

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An AMR simulation lends intuition for the multiphase halo

Putman, JP, Joung 12; Fernández+ 12; Joung+, JP in prep

MHI,Halo 108M ˙ MHI 0.2M/yr

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log(T) [K] log(n) [cm-3]

s P Disk gas

Putman, JEGP, & Joung 2012

The union of spatial and phase space lends much insight

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log(T) [K] log(n) [cm-3]

s P Disk gas background halo gas

Putman, JEGP, & Joung 2012

A lot of the halo gas is hot, diffuse, and largely static

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log(T) [K] log(n) [cm-3]

s P Disk gas Hot outflow

Putman, JEGP, & Joung 2012

Hot outflows have high entropy, but are not symmetric

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log(T) [K] log(n) [cm-3]

s P Disk gas Hot outflow

FB

Putman, JEGP, & Joung 2012

Hot outflows have high entropy, but are not symmetric

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SLIDE 47 7 4 6 5
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log(T) [K] log(n) [cm-3]

s P Disk gas Hot outflow

Putman, JEGP, & Joung 2012

Hot outflows have high entropy, but are not symmetric

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log(T) [K] log(n) [cm-3]

s P Disk gas Hot outflow Satellite gas

Putman, JEGP, & Joung 2012

Satellite gas is cool and merges into the halo

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log(T) [K] log(n) [cm-3]

s P Disk gas L
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s i n f l
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s Hot outflow Satellite gas

Putman, JEGP, & Joung 2012

Low entropy distant regions are the source of inflows

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log(T) [K] log(n) [cm-3]

s P Disk gas L
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s i n f l
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s Hot outflow H e a t i n g i n f l
  • w

Putman, JEGP, & Joung 2012

Some of these flows shock and heat

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SLIDE 51 7 4 6 5
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log(T) [K] log(n) [cm-3]

s P Disk gas Low s inflows Hot outflow H e a t i n g i n f l
  • w
C
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i n g i n f l
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Putman, JEGP, & Joung 2012

but a fraction cool instead

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SLIDE 52 R [kpc] dMZ/dt [M /yr] dM/dt [M /yr] dMH/dt [M /yr] (a) (b) (c)

10 1 0.1 0.01 10 1 0.1 0.01 0.001 t [Gyr] 250 200 150 100 50 R [kpc]

tcool tcomp tcool < tcomp tcool > tcomp Total T > 5.5 T < 5.5

Joung+ 2012

Two-temperature flows feed the galaxy, with hot dominating

hot warm-hot warm, cool

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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

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Gaseous Galaxy Halos are big (cool, warm, warm-hot, and) hot messes Halo kinematics signatures are easier to study than thermodynamic states The halo does seem to be aware of the feedback state of the disk, on many scales

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Thanks!

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