The impact of chemistry on the internal structure and ......The impact of chemistry on the internal...
Transcript of The impact of chemistry on the internal structure and ......The impact of chemistry on the internal...
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The impact of chemistry on the internal structure
and emission from high-redshift galaxies.
Andrea Pallottini
in collaboration with:
A. Ferrara, S. Gallerani, L. Vallini, R. Maiolino, S. Carniani, S. Bovino, C. Behrens, S. Salvadori
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Search and characterization of high-z galaxies
Optical/NIR surveys Observed UV luminosity functions e.g. Bouwens+16
Additional probes are needed to characterize high-z galaxies(metallicity, dust, feedback, outflow, ...)
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FIR line as a tool to characterize high-z galaxies
Why should we use the [C II]�2
P3/2 ! 2P1/2
�line at 157.74 µm?
Major coolant of the ISMDalgarno&McCray 1972
Among the strongest FIR line(LCII ⇠ 0.1%� 1%LFIR) Stacey 1993
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[C II] observations in the local Universe
Local dwarf and starburst galaxies: a [C II]-SFR relation is in place e.g. De Looze+14, Cormier+15
Can we use ALMA capabilities to study [C II] from high-z galaxies?
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[C II] observations from high-z galaxies
ALMA [C II] observations from the first cycles: see Carniani+17b for an updated collection
Why does the [C II]-SFR relation seem different at high-z?What can we learn from detections and upper limits?
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Modelling [C II] emission at high-z
Emission of [C II] from the multi-phase ISM: Vallini+15
V15: log(LCII) = 7.0 + 1.2 log(SFR) + 0.021 log(Z ) + see also Yue+2015, Pallottini+15, Olsen+15
+ 0.012 log(SFR) log(Z )� 0.74 log(Z )
Yue+15; Pallottini+15
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Predicting [C II] from high-z galaxies
Using cosmological metal enrichment simulation and V15 model Vallini+15(mdm ' 5 ⇥ 105M�; �x ' 1 ckpc/h ' 200pc @ z = 6)
Pallottini+14
�22 �20 �18 �16 �14 �12MUV
�6
�5
�4
�3
�2
�1
log(�
UV/m
ag/M
pc3)
Luminosity functionat z = 6
simulated
observed
Schechter fit
Pallottini+15
�22.5 �20.0 �17.5 �15.0 �12.5MUV
�5.0
�2.5
0.0
2.5
5.0
log(Fpeak/µ
Jy)
[CII] flux - MUV relation
simulated (z = 6)fit from simulationMaiolino et al. 2015 (z � 7)Capak et al. 2015 (z � 5.5)Willott et al. 2015 (z � 6)
We predict a [C II]-MUV that is in agreement with observationsfit from simulation: log(Fpeak/µJy) = �27.205 � 2.253MUV � 0.038 MUV
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Observing the structure of high-z galaxy
The example of BDF3299: spatial offsets and velocity shifts Maiolino+15,Carniani+17a
see e.g. Capak+15, for offsets/shifts in other galaxies
7.07.58.08.59.09.5
logL[CII]/L�
[CII] clump
atclum
plocation
optical/UV
location
0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5logG/G0
7.07.58.08.59.09.5
logL[O
III]/L�
[OIII] clump-I
atclum
plocation
optical/UV
location
6.8
7.2
7.6
8.0
8.4
8.8
9.2
9.6
10.0
logM
gas/M�
Indication of in-situ star formation/merging event(s) e.g. Carniani+17a, Vallini+17
and/or inomhogeneous radiation field and/or photoevaporation e.g. Decataldo+17,Katz+17,Vallini+17
and/or inomhogeneous dust/metal distribution? e.g. Behrens+18
To attack the problem we have to model the internal structure of high-z galaxies.
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Introducing Dahlia: a prototypical LBG galaxy at z ⇠ 6
Dahlia characteristics (at z=6)
dark matter Mdm ⇠ 1011M�
size rvir ' 15 kpc re↵ ' 0.5 kpc
stars SFR ⇠ 100M�/yr M? ⇠ 1010M�
gas MH ⇠ 1010M� MH2 ⇠ 108
M�metals Z ' 0.5Z� MD ⇠ 107
M�
Resolution
gas mass mg ' 104M�
AMR ⇠ 80 � 0.1 ckpc/hat z = 6 �x ' 30 pc
Model main features
AMR code RAMSES Teyssier 2002 zoom-in IC MUSIC Hahn 2011
H2 based star formation (SK relation) Krumholz+09 Stellar tracks from STARBURST99 Leitherer+10
Thermal and kinetic energy (e.g. Agertz&Kravtsov 2015)
GRACKLE 2.1 cooling module Bryan+14 Kinetic energy dissipation Mac Low 1999; Teyssier+13
SN explosions, OB/AGB winds & radiation pressure (e.g. Agertz+13, Hopkins+14)
Subgrid modelling for blastwaves Ostriker&McKee 1988
Pallottini+17a
nomination for best image set for Wikimedia EestiEuropean Science Photo Competition 2015
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Formation of an high-z galaxy
Density field evolution from z ' 10 to z ' 9more movies: https://www.researchgate.net/profile/Andrea_Pallottini
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Dynamical properties: gas kinematics
Slice of density and velocity fieldsVelocity PDF as a function of distance
ALMA suggests outflow in z ⇠ 5.5 galaxies
Outflow rate: Mout ⇠ 50M�/yr
flow rate definition: M =R
vr⇢dA Gallerani+18
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Dynamical properties: metal outflows
Slice with metallicity and velocityVelocity PDF as a function of distance
ALMA suggests outflow in z ⇠ 5.5 galaxies
Metal outflow rate: MoutZ ⇠ 0.1M�/yr
flow rate definition: MZ =R
vr Z⇢dA Gallerani+18
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Physical properties of Dahlia at z = 6
Density Metallicity H2 structure
1) molecular disk of mass ' 108.5M�, radius 0.5 kpc and scale height 200 pc
2) composed by dense (n ⇠ 102cm
�3) relatively metal rich (Z ' 0.5Z�) gasPallottini+17a
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Looking at the [C II] emission structure
C II abundance [C II] emission H2 structure
1) ' 95% of the [C II] emission arises from the molecular disk Pallottini+17a, cfr with Olsen+17
2) Diffuse gas contains 30% of C II, but the emission is suppressed see also da Cunha+13; Pallottini+15
L[CII] ⇠�
n
103 cm�3
� ⇣Z
Z�
⌘⇣M
M�
⌘L� for the actual model see Vallini+13; Vallini+15
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Looking at the [C II] emission structure (edge-on view)
C II abundance [C II] emission H2 structure
1) ' 95% of the [C II] emission arises from the molecular disk Pallottini+17a, cfr with Olsen+17
2) Diffuse gas contains 30% of C II, but the emission is suppressed see also da Cunha+13; Pallottini+15
L[CII] ⇠�
n
103 cm�3
� ⇣Z
Z�
⌘⇣M
M�
⌘L� for the actual model see Vallini+13; Vallini+17
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Star formation history
For Dahlia, SFR and M? are compatible with high-z galaxy observations Pallottini+17a,b
sSFR ' 39.7Gyr�1 to sSFR ' 4.1Gyr
�1 as galaxy grows older Gonzalez+10; Stark+13; Jiang+16
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Schmidt-Kennicutt relation
Schmidt-Kennicutt relation in the Krumholz+12 formulation ⌃? � ⌃/t↵ Pallottini+17b
Dahlia is on the “high-z main sequence”However, Dahlia is off the Schmidt-Kennicutt relationHow can we improve our models?
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Improved model for the formation of H2
Molecular fraction (fH2) benchmark: Pallottini+17b
equilibrium (Krumholz+09) vs non-equilibrium (Grassi+14) model
high-z environment(Z ' 0.5Z�; G ' 100 G0):equilibrium model n >⇠ 102
cm�3 (Dahlia)
non-equilibrium model n >⇠ 103cm
�3 (Althæa)
MW environment(Z = Z�; G = G0):both models fH2
>⇠ 0.5 at n >⇠ 25 cm�3
aa
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Schmidt-Kennicutt relation
With the improved model, gas must be denser to be molecular Pallottini+17b
Althæa is nicely sits on the Schmidt-Kennicutt relation
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Star formation history
Both galaxies are compatible with observation of main sequence at high-z Pallottini+17b
Difference within a factor ⇠ 2 for both M? and SFRAlthæa has a more bursty nature than Dahlia
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ISM of high-z galaxies: the impact of chemistry
FIR (ALMA) and Mid-IR (SPICA) synthetic observations Pallottini+17b
Althæa is denser then Dahlia (⇥6.8), but has a lower molecular mass (⇥3.5)Althæa is more clumpy and compact
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Observing the ISM of high-z galaxies
FIR (ALMA) and Mid-IR (SPICA) synthetic observations Pallottini+17b, see Spinoglio+17 for SPICA
Chemical modelling does matter: ' 7 (15) factor increase in luminosity of [C II] (H2)
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Reproducing the properties of high-z galaxies
CII-SFR relation Schmidt-Kennicutt relation
Better modelling gives simulations in closer agreement with current observations. Pallottini+17b
Whether or not the CII-SFR relation applies at high-z remains as an open question. see also Carniani+17b
How can we have a more complete picture?
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Modelling CO emission in high-z galaxy
Accounting for the structure of Molecular Clouds Vallini+18
combined with CLOUDY emission models
GMCdensityPDF
COlineemissionfromGMC
derive
from simulation
from simulation
parameter
determine
Simulation cell
Internal structureR
adiative transfer
G0, Z, n, NH
clumpproperties
contribution to CO(1-0) from a MC withRGMC = 15 pc, n0 = 102
cm�3
M = 5, t/t↵ = 0.4log G/G0 = 2, Z = Z�
see also Munoz&Furlanetto+12, Popping+16
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CO emission from of Althæa
Vallini+18
Conversion factor
h↵COi = (1.54 ± 0.9)M�/(Kkms�1
pc2)
little spatial variation due to density fluctuationssee also Narayanan+12
CO SLED
CO SLED boosted by the CMBand by high turbulence in Althæa
cfr with da Cunha+13
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CO observability for ALMA
Vallini+18
LCO(7�6) = 107.1L� ' 116L[C II]
To resolve (detect) the CO(7-6) line with at 5�an ALMA observing time of ' 38 h (' 13 h) is required.
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Conclusions
1) Our typical z ' 6 LBG form a H2 disk of mass of ⇠108
M�, radius ' 0.5 kpc, and scale height ' 200pc
2) The total [C II] luminosity is ⇠ 108L�, and 95% of the
emission arises from the H2 disk.
3) CO(7-6) shines at ⇠ 107L�: detection is challenging
but possible with ALMA.
4) Such galaxies have indication of outflows that can bedetected by deeper observations.