The HI-to-H2 Transition in Galaxy Star-Forming Regions · The HI-to-H2 Transition in Galaxy...
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The HI-to-H2 Transition in Galaxy Star-Forming Regions
Amiel SternbergSackler School of Physics & AstronomyTel Aviv UniversityISRAEL
Life Cycle of Gas in Galaxies31 August 2015
Sunday, September 6, 15
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The HI-to-H2 Transition in Galaxy Star-Forming Regions
Amiel SternbergSackler School of Physics & AstronomyTel Aviv UniversityISRAEL
Life Cycle of Gas in Galaxies31 August 2015
Sunday, September 6, 15
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The Multi-Phased Interstellar Medium (ISM) and Star-Formation:
hot ionized medium (HIM) T = 105 - 106 K
warm neutral medium (WNM) T ~ 104 K
<density> = 1 cm-3
but very inhomogeneous
warm ionized medium (WIM) T ~ 104 K
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The Multi-Phased Interstellar Medium (ISM) and Star-Formation:
hot ionized medium (HIM) T = 105 - 106 K
warm neutral medium (WNM) T ~ 104 K
<density> = 1 cm-3
but very inhomogeneous
CNMcold neutral medium T < 200 K
[multi-phased,pressure-equilibrium]
warm ionized medium (WIM) T ~ 104 K
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The Multi-Phased Interstellar Medium (ISM) and Star-Formation:
hot ionized medium (HIM) T = 105 - 106 K
warm neutral medium (WNM) T ~ 104 K
Interstellar gas exposed to
starlightshock wavesenergetic particles (cosmic-rays)magnetic fields
Global ISM heated and energized by stars(outflows, radiation, and supernova explosions).
Turbulent!
Total Galactic ISM mass = 5x109 M
Mid-plane thermal pressure = 2.5x103 cm-3 K(at Solar circle)
most of mass in cold neutral hydrogen phasemost of volume in warm/hot ionized phase.
<density> = 1 cm-3
but very inhomogeneous
CNMcold neutral medium T < 200 K
[multi-phased,pressure-equilibrium]
warm ionized medium (WIM) T ~ 104 K
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The Multi-Phased Interstellar Medium (ISM) and Star-Formation:
hot ionized medium (HIM) T = 105 - 106 K
warm neutral medium (WNM) T ~ 104 K
Interstellar gas exposed to
starlightshock wavesenergetic particles (cosmic-rays)magnetic fields
Global ISM heated and energized by stars(outflows, radiation, and supernova explosions).
Turbulent!
Total Galactic ISM mass = 5x109 M
Mid-plane thermal pressure = 2.5x103 cm-3 K(at Solar circle)
most of mass in cold neutral hydrogen phasemost of volume in warm/hot ionized phase.
<density> = 1 cm-3
but very inhomogeneous
stars form in cold molecular (H2) clouds:Galactic star-formation rate ~3 M yr-1
CNMcold neutral medium T < 200 K
[multi-phased,pressure-equilibrium]
HI to H2 conversion:star-formation!
Herschel views Aquila
warm ionized medium (WIM) T ~ 104 K
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Talk Outline:
• motivation.• HI-to-H2 transition, some radiative transfer computations.• analytic formula for the HI column density.• self-regulated media.• observations: from Perseus to galaxies.
2014 ApJ 790 10
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Kennicutt-Schmidt Relation:Schmidt 1959 ApJ 129 253Kennicutt 1998 ApJ498 541 Genzel et al. 2010 MNRAS 407 2091 [“SINS(VLT)/IRAM” projects]
e.g., Bigiel+ 2008
apparentthreshold:10 M☉ pc-2
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M83 Crosthwaite+ 2002 ApJ 123 1892
HI as a Photodissociation Product in Molecular Spiral Arms:
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I am going to be juggling many parameters - keep your eye on them!
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HI to H2 Transition in Dense Star-Forming Molecular Clouds:
Stellar ultraviolet “Lyman-Werner” radiation11.2 - 13.6 eV
H2 formation (by grain catalysis) versus far-UV photodissociation.
Shielding required.“PDR”
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HI to H2 Transition in Dense Star-Forming Molecular Clouds:
Stellar ultraviolet “Lyman-Werner” radiation11.2 - 13.6 eV
H2 formation (by grain catalysis) versus far-UV photodissociation.
Shielding required.
parameters:
• effective LW-band photon flux: wF0 cm-2 s-1 • gas density: n = n1 + 2n2 cm-3
• H2 (grain) formation rate coefficient: R cm3 s-1
• dust-grain attenuation cross section: σg cm2
• metallicity Z’ (Z’=1 is “solar”)•
“PDR”
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Effe
ctiv
e P
oten
tial E
nerg
y
Internuclear Separation
Ene
rgy
H2 Photodissociation in the Lyman-Werner bands (912-1108 Å):
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LW
Pumping
“Spontaneous Radiative Dissociation”
Effe
ctiv
e P
oten
tial E
nerg
y
Internuclear Separation
Ene
rgy
H2 Photodissociation in the Lyman-Werner bands (912-1108 Å):
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LW
Pumping
“Spontaneous Radiative Dissociation”
Effe
ctiv
e P
oten
tial E
nerg
y
Internuclear Separation
Ene
rgy
(Cosmologists call this “feedback”!)
H2 Photodissociation in the Lyman-Werner bands (912-1108 Å):
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LW
Pumping
“Spontaneous Radiative Dissociation”
Effe
ctiv
e P
oten
tial E
nerg
y
Internuclear Separation
Ene
rgy
(Cosmologists call this “feedback”!)
H2 Photodissociation in the Lyman-Werner bands (912-1108 Å):
H2 dissociation rate: D0 = 5.8 x 10-11 s-1
in the unit “free-space” (Draine) interstellar field.
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Lyman-Werner Radiative Transfer:
S+ 2014 [“Meudon PDR code”]
Characteristic multi-line H2absorption spectrum, and“self-shielding”.
Dust absorption cross-sectionper hydrogen nucleus:
Numerical radiative transfer on a fine frequency grid with a spectral resolution ~ 105.
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Curve-of-Growth for the “H2 Dust-Limited Dissociation Bandwidth”: [integrated over all LW lines]
Sternberg+ 2014 [“Meudon PDR code”]
The bandwidth (Hz) of radiationabsorbed in H2 line dissociations ina dusty and fully molecular cloud.
“H2 dust” versus “H2 lines”
low metallicity
high metallicity
Z’ “little w”
Universal: independent of radiation field intensity,or cloud gas density, etc.
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“Universal” Total H2 Dust Limited Dissociation Bandwidth:
Universal: independent of radiation field intensity,or cloud gas density, etc.
high Z’low Z’solar
“Effective Dissociation Flux”
Total LW Flux:
Sternberg+ 2014
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dust grain
H
H
H2
H2 Formation:
H + e → H- + photon
H- + H → H2 + e
time scale for equilibrium
In the absence of dust:
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Basic Theory Question:
What is the total HI column density (cm-2)or HI mass surface density (M pc-2)in far-UV irradiated systems?
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Dimensionless Parameter: Sternberg 1988; McKee & Krumholz 2010; Sternberg+ 2014
or:
HI-dust absorption rate of the effective dissociation flux free space H2 photodissociation rate
Physical Meaning:
self-shielded H2 dissociation rate H2 rate formation rate
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Sternberg Parameter: Sternberg 1988; McKee & Krumholz 2010; Sternberg+ 2014
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Sternberg Parameter: Sternberg 1988; McKee & Krumholz 2010; Sternberg+ 2014
...so can be small “weak-field” or large “strong-field”
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H2 lines H2 lines + H2 dust
HI dustαG >> 1 “strong-field”
αG << 1 “weak-field”Z’ ≳ 1 “high-metallicity”
αG << 1 “weak-field”Z’ ≲ 1 “low-metallicity”
Three-Way Competition for the FUV Absorption:
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HI-to-H2 Transition Profiles: Z’=1 (solar metallicity)
weak-field: most of the HI built up inside the H2 zone, “gradual profiles”
FUV attenuation dominated by H2 lines plus “H2 dust”
strong-field: most of the HI built up in an outer layer, “sharp profiles”
FUV attenuation dominated by “HI-dust”
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HI-to-H2 Transition Profiles: Z’=1 (solar metallicity)
weak-field: most of the HI built up inside the H2 zone, “gradual profiles”
FUV attenuation dominated by H2 lines plus “H2 dust”
strong-field: most of the HI built up in an outer layer, “sharp profiles”
FUV attenuation dominated by “HI-dust”
For a given Z’, the profile shapes depend on the dimensionless parameter αG.
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For a given αG the profile “scale lengths” are determined by Z’.
E.g., HI profiles for αG/2 ≈ 1
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General Purpose Analytic Formula for the Total HI Column Density:
Valid for all regimes:
• weak and strong fields• gradual to sharp transitions• arbitrary metallicity
[note: no reference to the H2 linephotodissociation cross sections!]
weak-field strong-field
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Weak-Field Limit:
weak-field strong-field
formation rate per unit area = effective dissociation flux
(a “Strömgren Relation”)
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Strong-Field Limit:
weak-field strong-field
(neglecting the logarithmic term)
makes sense: When HI-dust dominates the attenuationof the far-UV field, the HI-column is “self-limited” and
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Heavy-Element Abundances “Metallicity”:
H2 formation rate coefficient and dust absorption cross-sectionboth proportional to metallicity.
weak-field strong-field
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Heavy-Element Abundances “Metallicity”:
H2 formation rate coefficient and dust absorption cross-sectionboth proportional to metallicity.
weak-field strong-field
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General Purpose Analytic Formula for the Total HI Column Density: S+ 2014
• useful for interpreting 21cm observations
• incorporation into hydrodynamics simulations
• application to “self-regulated” media
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HI Thermal Phases in Self-Regulated Media:
reduced SFR
P/k = nT
enhanced SFR
Field, Goldsmith & Habing 1969 ApJ 155 149
Wolfire, McKee & Hollenbach 2003Sternberg, McKee & Wolfire 2002
Ansatz:Krumholz, McKee & Tumlinson 2009
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HI Thermal Phases in Self-Regulated Media:
reduced SFR
P/k = nT
WNMLyαT=8000°K
CNM[CII] 157 µmT≤200°K
enhanced SFR
Field, Goldsmith & Habing 1969 ApJ 155 149
Wolfire, McKee & Hollenbach 2003Sternberg, McKee & Wolfire 2002
Ansatz:Krumholz, McKee & Tumlinson 2009
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HI Column Density for Self-Regulated Media:
remarkable!
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HI Column Density for Self-Regulated Media:
remarkable!
independent of radiation field intensity and/or gas density.
characteristic HI photodissociation masssurface density in self-regulated systems
“transition” total gas mass surface density...star-formation threshold...galaxies.
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HI-to-H2 in Perseus: Perseus Cloud distance 300 pc
2MASS AV and ICO CfA & COMPLETE surveys Dame+ 2001 Ridge+ 2006
Lee et al. 2012; 2015
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HI-to-H2 in Perseus: Perseus Cloud distance 300 pc
2MASS AV and ICO CfA & COMPLETE surveys Dame+ 2001 Ridge+ 2006
dark clouds &low-mass star-forming regions:
B1B1EB5NGC1333IC348
Lee et al. 2012; 2015
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HI-to-H2 in Perseus: Lee+ 2012, 2015 Peek+ 2011 GALFA HI Survey (Arecibo 4arcmin)
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HI-to-H2 in Perseus:
Fits using S+14:
Bialy, Sternberg, Lee, Le Petit & Roueff 2015 ApJ 809 122
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HI-to-H2 in Perseus: Bialy+ 2015
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HI-to-H2 in Perseus: Bialy+ 2015
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HI-to-H2 in Perseus: Bialy+ 2015
CNM
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HI-to-H2 in Perseus: Bialy+ 2015
Galactic interstellar LW radiation field:F0 ≈ 2 x 107 photons cm-2 s-1
Conclusions: αG ≈ 5 to 50
• FUV absorption dominated by HI-dust
• nHI ≈ 10 to 2 cm-3
• probably a UNM/CNM multiphase
CNM
Sunday, September 6, 15
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Galaxies:
e.g. Bigiel+ 08
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Galaxies:
e.g. Bigiel+ 08
Caveat: This interpretation requires typically “one” primary cloud per line-of-sight.
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To Conclude:
2014 ApJ 790 10 arXiv:1404.5042
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