Transcript SIMULATIONS

Dust effects in the SEDs of simulated gala
the GRASIL-3D code and some applicatio
Rosa Domínguez-Tenreiro
Universidad Autónoma de Madrid, Spain
A. OBREJA (UAM, Spain)
G.L. GRANATO (INAF, Trieste, Italy)
I. SANTOS (UAM, Spain)
C. A. BROOK (UAM, Spain)
G. STINSON (MPIA, Heidelberg, Germany)
L. SILVA (INAF, Trieste, Italy)
A. SERNA (UMH,Spain)
S. GOTTLOBER, Y. HOFFMAN, G. YEPES & CLUES
Collaboration
Dust Effects in galaxy SEDs
Galaxy formed in a hydro simulation
Z=6
t/t_U=0.066
DECREASING UV optical // INCREASING
IR submm L
DUST reradiates the overall bolometric luminosity
SED has been calculated with GRASIL3D code
(D-T et al, 2014)
Simulations: information on 6D phase
space, ages, composition, gas density and
temperature.
Observations: light
Testing simulations (theories & models)
against observations demands
SOFTWARE TELESCOPES:
Simulation outputs ----> SEDs, images
DUST EFFECTS: FUNDAMENTAL
ROLE in GALAXY SEDs
GRASIL-3D
Application I.- Testing G-3 local galaxies
Application II.- IR-submm emission from
CLUES Local Group dwarfs
Application III.- The MS and the
Fundamental Plane of star-forming galaxies
GRASIL-3D:
An extension of GRASIL to arbitrary
geometries and galaxy evolutionary
histories
(D-T+ 14)
RADIATIVE TRANSFER
THROUGH DUST
SUNRISE (Jonsson 04,05; +09)
RADISHE (Chakrabarti+08; & Whitney09)
ART2
(Li + 07; Yajima+12)
MCarlo solve RT for Simu outputs
GRASIL assumes
Equatorial & axial symmetry for galaxies
SAMS
PEGASE (Fioc & Rocca-Volmerage 1997)
CIGALE (Burgarella + 14) Parameter determination
SKIRT (Baes+ 03, 11)
GRASIL(-3D) PARTICULARITIES
Separately treats RT in MCs and in cirrus,
different dust composition
Age-dependent dust reprocessing of stellar
populations: younger *s in denser ISM embeded
in MC until destruction
Detailed non-equilibrium calculation for dust
grains with diameter a < 250 A
---> Proper PAH treatment
RT solved in a grid, rather than MCarlo
CHARGE VARIABLES to a GRID
MC & CIRRUS DISTRIBUTION
Based on sub-resolution PDF
(Wada+07 ; Federrath + 12)
Choose a density threshold for MC rho_thres
Choose a 2 parameter log-normal PDF for the
cold gas f_pd(rho_0, sig)
For the ith particle
Identify <rho>_V = rho_gas(i) (**)
→ Calculate the MC mass fraction at ¨i¨
Calculate cirrus mass fraction at ¨i
(**) provides a link between PDF parameters
and simulation outputs ---> PDF sig
AGE DEPENDENT DUST
REPROCESSING OF SP
Light fraction that can escape the StarBurst region,
mimicking MC destruction,
f(t) = 1 if t<t_0
0 if t>2t_0
2-t/t_0 in other cases
DUST CONTENT
k-th GAS PARTICLE
d(Z_k) = Z_gas,k /(110 x Z_sun)
PARAMETERS
GRASIL 3D
Grid size simulation resolution
rho_mc,thres 10 – 100 H/ cm^3 (Obs + simu)
1 PDF parameter sig 2 – 3 in simulations
---> cirrus & MC mass fraction f_mc
GRASIL
Dust model
Escape-time-scale t_0 2.5-8 or 18-50 Myrs (N,SB)
Individual MC log(m_mc) = 5 -6 M_o; r_mc= 10-50 pc
SIMULATION: SHAPE, EVOLUTION MODEL, SFRH
I
TESTING GRASIL-3D
LOCAL GALAXIES
SIMULATIONS

P-DEVA AP3M-SPH

Entropy conserving; mutual neighbors




(Martínez-Serrano+ 08)
OK
Chemical evolution tracks the full dependence of
metal production on the detailed chemical
composition of * particles (Q_ij formalism, Talbot+ 73)
Feedback: implicitely through (inefficient) SF
parameters (Agertz+ 11)
GASOLINE SPH
(Wadsley + 04,Brook + 11)
Feedback: blastwave formalism (Stinson+ 06) from
Sne & massive stars (Stinson+ 13). Effective coupling
with gas 1%
Blast-wave scenario
Face- and edge on images of g1536_L*
Box 50 kpc side, resolution and pixel = 312,5 pc
OBSERVATIONAL SAMPLES
GRASIL-3D TESTING
ISO Key Project on the ISM of Normal Galaxies
ISO & IRAS broad-band fluxes
FIR active, quiescent and intermediate (Vega+05)
Helou+96; Dale+ 00
Aromatic Features in Emission 6.2,7.7,8.6 & 11.3 micron
(Lu+03; a subsample of Dale+00)
Spitzer IR Normal Galaxy Survey (SINGS
; Kennicutt+03; Dale+05)
Non-tidally perturbed & non-interacting galaxies
(Smith+07, a SINGS subsample & Lanz+13 from KINGFISH)
Key Insights on Nearby Galaxies: FIR Survey w Herschel
(KINGFISH, Kennicutt+11)
All normal types 61 galaxies imaged with PACS and SPIRE (Dale+12)
MOLECULAR and ATOMIC HYDROGE
& STELLAR CONTENT
A test for the MC model in GRASIL-3D
Simulations vs COLD GASS survey
(Saintonge+11)
OK
IRAS
flux density ratios: simulated (color) vs real
(Gray: Dale+00) galaxies
LEFT: Merger
RIGHT:
Normal
FIR active, quiescent and intermediate (Vega+05)
Lines join consecutive results for HD-5103B along a merger phase
AFE Rel Strengths vs FIR/blue
At z=0 and around a MM
Gray points: data Lu+03
FIR-active,intermediate,quiescent
Color: simulations 8 gal. z=0 BLUE
And merger phase
Different parameter Sets
Codes as in previous Fig.left
Observational results recovered
Aromatic Features in Emission 6.2,7.7,8.6 & 11.3 micron
(Lu+03; a subsample of Dale+00)
Spitzer IRAC & MIPS non-interacting
Histograms:
Smith+07 sample from SINGS
Points
Averages over parameter sets
Spitzer IR Normal Galaxy Survey
(SINGS ; Kennicutt+03; Dale+05)
Non-tidally perturbed & non-interacting galaxies
(Smith+07, a SINGS subsample & Lanz+13 from KINGFISH)
HERSCHEL BANDS non-interacting
Gray: Lanz+13
Color: 8 simulated galaxies,
averages & dispersions over parameter sets
Key Insights on Nearby Galaxies: FIR Survey w Herschel
(KINGFISH, Kennicutt+11)
All normal types 61 galaxies imaged with PACS and SPIRE (Dale+12)
Non-tidally perturbed & non-interacting galaxies
(Smith+07, a SINGS subsample & Lanz+13 from KINGFISH)
UV and optical flux density ratios
Non-interacting
Gray: data Dale+07
Color: 8 simulated galaxies,
averages & dispersions over parameter sets
GRASIL-3D
DISCUSSION
Find encouranging results
when comparing with
disk galaxies in detail
Changing rho_mc_thres and PDF sig
Parameter variations: not remarkable
effects when kept within their ranges
II
IR-submm
EMISSION from DWARF
GALAXIES
The CLUES project LOCAL GROUP
(Isabel Santos +, in prep)
THE CLUES PROJECT
CLUES: Constrained I.C.
(Hoffman +Ribak 92)
** Observational data imposed as constraints
on the IC → local Universe skeleton at Mpc
** Random at sub-Mpc
SIMULATION:
GASOLINE
LCDM
Grav.softening = 220 pc
m_DM, m_*, m_gas 30, 2, 6 x10^4 M_sun
Feedback ERIS simulation (Guedes+11)
Includes chemical evolution
RESULTS:
Luminosity – color
BLUE, CYAN: SF dwarfs
RED: ¨dead¨ dwarfs
Data from Mateo 1998
some relations
Iron vs luminosity
Black Simulated D galaxies
Red Data McConnachie+12
Dwarfs are low Z systems
RESULTS:
velocity disp. vs M_*
RESULTS: half-light radii vs M_V
RESULTS: SEDs for low M* & Z
SF galaxies
Simulations + GRASIL →
Two dust components,
as observations demand
Galametz+09
RESULTS: Irr low M* SF galaxy
Ks
FUV
MIPS160
SFRH
SPIRE500
III
GRASIL-3D as a test bed for
MASS and SFRH DETERMINATION
in
SPIRAL GALAXIES
Obreja et al., 14
MAGICC
Project, Brook & Stinson 2012
Www.star.uclan.ac.uk/Cbb/magicc
MOTIVATION
Constraining galaxy formation scenarios
through
MS: correlation SFR vs M_*
MZ: M_* vs metallicities
(Wuyts + 11)
Gas phase
Stars
(Garnett + 02; Tremonti + 04)
(Cowie & Berger 08; Pérez-Montero + 09)
Projections of a fundamental relation?
Ellison +08
COMPARING SIMU OUTPUTS TO OBSERVATIONAL DATA
OBSERVATIONS: M_* & SFR determined from light (SEDs)
SIMULATIONS: need to apply the same recipees !!
NEED
SEDS as close to observed ones as possible
SOFTWARE
TELESCOPES
Figure 1 from Galaxy Structure and Mode of Star Formation in the SFR-Mass Plane z ~ 2.5 to z
~ 0.1
Stijn Wuyts et al. 2011
Constant slope
Zero point ---> high-z galaxies form stars faster
than local ones with same M_*
Scatter independent of z
Increases at lower M_*
SIMULATIONS
METHODS
Disk gal. from the MaGICC project
(Brook + 12;
Stinson + 13)
GRASIL-3D post-processing
Face-on SB in r-band ----> Petrosian radii R_p (Blanton + 01)
** Luminosities, fluxes & colors from SEDs within 2R_p
ready to apply observational
techniques
including dust effects
MIMIC
OBSERVATIONS
¨observed¨as they evolve from z=3.5 upto
z=0 (324 snapshots)
METHODS
STELLAR MASS
DETERMINATION
Color dependent mass-to-light relations B- and
V-band (McGaugh et al. in prep)
GLOBAL SFR
IR-corrected far UV tracer of Hao + 11:
FUV flux corrected using the total IR emission
WARNING
Test that simulated galaxy
** B-V and M_V are within those of the sample used for calibration
** IRX vs FUV -NUV used for calibration
RESULTS:
M_*
Testing observational methods
M_* assembly history, scatter is shown
Black: as predicted by simulations
Blue: B-band mass-to-light ratios
Green: V-band
RESULTS: THE GLOBAL SFRH
¨Observational¨ SFRs vs real ones
OK
BLACK: SFRHs predicted by simulations
BLUE: SFRHs from IR-corrected FUV
RESULTS: SCATTER IN THE MS
Independent of redshift
Decreases with increasing M_*
May trust simulations !!
---> Reflects bursting/variable SFR
in the SF population
RESULTS:
THE FUNDAMENTAL METALLICITY RELATION
M_* - SFR – (O/H) in gas (Lara-López + 10)
**
**
**
**
Tight correlation
Same scatter as obs
Same coefficients
0.09 dex lower normalization
GREY POINTS: simulated at z<3.5
RED POINTS: simulations in equally populated M_* bins
BLUE LINES: solid - linear fit with slope 1, as in Lara-López + 10
Dashed – 0.16 dex scatter
BLACK LINES: solid & dashed - fit Lara-López data & scatter
CONCLUSIONS
APPLICATION III
GRASIL-3D METHOD to test out
the observational methods to determine M_*
and the SFRH in star forming galaxies
Consistency observations -simulations
The MS and MZ relation for star forming galaxies
Are projections of the Fundamental Plane
M_*-SFR-O/H (Mannucci+ 10; Lara-López+ 10)
Prediction: the FP holds also for lower M_* starforming galaxies
GENERAL CONCLUSIONS
GRASIL-3D particular strengths follow GRASIL (Silva+ 98; 99)
General applicability to systems with arbitrary geometry, in
particular those produced in hydrodynmical simulations
(evolutionary history, SFRH ..)
Subresolution PDF formalism to describe MC/cirrus density
field
Comparison to observations of local galaxy samples are
encouraging, particularly remarkable for PAH features
Detailed analysis of parameter space from literature gives
consistent results
Many specific applications possible: different predictions on
individual & statistical galaxy properties, directly
comparable to observations
Applications so far give encouraging results
STAR FORMATION
d rho_g/dt = - e_ff rho_g/t_ff , rho_g>rho_t (K-S-like)
A few parsec resolution
Sne II E_II = 10^51 (mass/10 M_sun) erg injected in the ISM
after 10 Myear a 8 – 40 M_sun star is formed
Sne Blast wave in adiabatic expansion if parsec-scale resolution
(McKee & Ostriker 1977; Stinson et al. 2006; Brook 2010 . 2011)
SnIa
E_I = E_II, but with slower timescale
+ metals
UNRESOLVED ISM (a few 100 pc for discs)
mimic through tuning resolved physics: H_2 formation, small-scale
turbulence, radiative effects
free parameters, based upon core-scale physics : stocastic model
(Katz 1992; parameter testing in Agertz et al. 2011)
RESULTS: SOME
IMAGES
FUV, Ks, SPIRE 500
SFRH
SNE BLAST WAVE MODEL
** Sne explosions large volumes of hot, low-densitygas
McKee & Ostriker analytical blast wave model
** Mimic its effect in SPH codes:
Sne feedback from m_* >8M_o
(Thacker & Couchman 2000; Stinson et al. 2006; Brook et al. 2011)
Energy from massive stars prior to their explosions (Stinson+ 13)
weak coupling of stellar energy to the sorrounding gas 1%
 Flow outwards + SFR regulated
GASOLINE
RUNS: 3 galaxies
m_bar = 2 and 0.25 x 10^5 M_o
e_g =
312,5 pc - 156,2 pc
M_* = 2.3 - 0.6 x 10^10 M_o
Disk & bulge scales, kine, B/D consistent with observations