1. LUIS COLINA (CAB/CSIC, SPAIN)
DISSECTING LUMINOUS INFRARED GALAXIES THROUGH MULTI-WAVELENGTH INTEGRAL FIELD SPECTROSCOPY
LUIS COLINA (CAB/CSIC, SPAIN)
J. Piqueras-Lopez, M. Pereira-Santaella, S. Arribas, S. García-Burillo, B. Emonts, A. Alonso-Herrero, E. Bellocchi, S. Cazzoli
R. Riffel, R.A Riffel, A. Rodriguez-Ardila, T. Storchi-Bergmann 1

2. OUTLINE MOTIVATION THE MULTI-λ IFS SURVEY OF LOW-Z U/LIRGS
MAPPING THE IONIZATION STRUCTURE IN LIRGS
Spatially resolved near-IR BPT diagrams: AGNs, young stars & SNe
THE 2D MULTI-PHASE STRUCTURE OF OUTFLOWS IN LIRGS
NGC Outflows in supernovae-dominated SF clumps
NGC Extended hot & cold molecular gas outflows
THE STAR-FORMATION LAW ON (SUB)KPC SCALES IN LIRGS
IC KS-law at ΣSFR > 100 M yr-1 2

3. U/LIRGS. BASICS most luminous low-z galaxies
49%
17%
0.1%
0.01%
LIRGS: ≤ L/L < 1012
ULIRGs: ≤ L/L < 1013
NUMBER DENSITY
LUMINOSITY CONTRIBUTION
U/LIRGS (LIR > 1011 L)
most luminous low-z galaxies
from regular star-forming disks to interaction/merging of gas-rich galaxies
sites of massive star formation > 20 M yr-1
extreme cases of the starburst+AGN activity
sites of powerful AGN & SF-outflows
More high-z (dusty IR phase)
SFR (local U/LIRGs) ~ SFR z~2)
1” = 200 pc
6 kpc
UNIQUE LABORATORIES TO INVESTIGATE MOST EXTREME & LUMINOUS STARBURSTS (+ AGNS) & THEIR IMPACT ON AMBIENT ISM ON SCALES OF HUNDRED OF PARSECS
CLOSEST ANALOGS TO HIGH-Z SF-GALAXIES 3

4. THE MULTI-λ IFS SURVEY OF LOW-Z U/LIRGS
IFS data cube
~ 75 U/LIRGs @ z < ( i.e. ~ kpc/”)
Different dynamics (isolated, interacting, mergers)
30% AGNs
ANCILLARY: HST Paα & CanariCam/GTC mid-IR imaging
TELESCOPE
IFS
FoV
(arcsec)
Sampling. (´´/spaxel)
 Range
(m)
Spectral
Resolution (R)
Number of Targets
4.2m/WHT
INTEGRAL
12x16
0.90
1400 22
3.5m/CAHA
PMAS
16x16
1.00
1200 14
8.0m/VLT
VIMOS
27x27
0.67
2650 42
SINFONI
8x8
0.25
H, K
ALMA
18 X 18
0.33
CO(2-1) 4 4

5. MAPPING THE 2D MULTI-PHASE STRUCTURE OF THE ISM USING NEAR-IR IFS (SINFONI)
ionized hot molecular highly ionized coronal shocks
Young SC dense gas Young SC AGN SNe 5

6. MAPPING THE IONIZATION STRUCTURE6

7. NGC5135. 2D NEAR-IR BPT DIAGRAMS
Colina+15, A&A in press
2D NEAR-IR BPT DIAGRAM
AGN, young (< 6 Myr) and aged (8-20 Myr) star-forming regions occupy different regions in the near-IR BPT diagram
Diffuse ISM: complex, mixture of excitation sources 7

8. NEAR-IR BPT DIAGRAMS. IDENTIFYING AGN – YOUNG STARS - SNE EXCITATION IN LIRGS
HIGH-SURFACE BRIGHTNESS CLUMPS DIFFUSE ISM
Young (< 6 Myr)
SF-clumps
SNe (8-20 Myr)
AGN 8
10 LIRGS, points
Colina+15, A&A in press

9. THE 2D MULTI-PHASE STRUCTURE OF OUTFLOWS9

10. SNE-INDUCED OUTFLOWS: HIGH SPEED EXTENDED HOT MOLECULAR OUTFLOW
HOT H2-OUTFLOW
SNe ~ 0.1 per year
M(hot-H2) ~ 440 M
SIZE ~ 400 pc
Vmax ~ 240 km s-1
FWZI ~ km s-1
WAITING FOR ALMA CYCLE 2:
WOULD BE FIRST DETECTION OF
HIGH-SPEED COLD MOLECULAR OUTFLOW
INDUCED BY SNE.:
SF QUENCHING BY SNe 10

11. NGC 3256. THE EXTENDED HOT H2 OUTFLOW
MA ~ 630 M
MB ~ 570 M
MA+B ~ 1200 M
Size ~ 1.3 kpc
Opening A.: 40deg
Vmax ~ 450 km s-1
FWZI ~ 1200 km s-1
Casey et al 11
Emonts+14, A&A

12. NGC 3256. THE HOT & COLD MOLECULAR OUTFLOW. NEAR-IFS & ALMA COMBINED
SINFONI: Emonts+14
ALMA/Cy0: Sakamoto+14
COLD & HOT H2 OUTFLOW
Same spatial structure (collimated, narrow, size)
Same kinematics (amplitude, blue- & redshifted)
Mass ratio of ~6x 10-5 (hot-to-cold) 12

13. THE STAR-FORMATION LAW ON (SUB)KPC SCALES13

14. IC 4687. THE STAR-FORMING LAW @ (SUB)KPC SCALES
ALMA CO(2-1) FWHM ~0.35” (120 pc) HST Paα FWHM ~0.25”
LOW SFE
HIGH SFE
FoV = 18” x 18” (6.3.x.6.3 kpc2) 14

15. THE STAR-FORMING LAWS @ (SUB)KPC SCALES
IC4687
- ΣH2 ~ M pc-2
- Large dispersion (x100)
in ΣSFR for a given ΣH2
- Star-formation law
flatter than KS-law
SFE higher (x10-100)
than that of spirals &
local AGNs of similar ΣH2
- Depletion times ~ 20 to
200 Myr
Leroy: SF in spirals
Casasola: circumnuclear SF in low-z AGNs 15

16. FUTURE. VLT - JWST – ALMA SYNERGIES
MUSE+AO: μm IFS
JWST: 1 – 28 μm IFS (NIRSpec & MIRI combined)
12-16 October 2015 16

17. SUMMARY
Multi-wavelength IFS survey of local U/LIRGs underway: study of the excitation sources, kinematics of the different phases of ISM and outflows, and SF-law at sub)kpc scales.
Excitation sources and near-IR 2D BPT diagrams (Colina+15)
- AGN, young (< 6 Myr) and SNe (8-20 Myr) SF-clumps occupy different regions
in the near-IR BPT diagram
- Diffuse ISM a complex mixture of AGN/ionizing stars/shocks
Multi-phase outflows in LIRGs (Emonts+14; Piqueras-López+ work in progress)
- NGC 5135: SNe induced outflows in SF clump with velocities up to 1000 km/s (FWZI). Expected detecttion of cold molecular outflow with ALMA
NGC 3256: Hot and cold molecular gas with similar kinematics & kpc-structure
IC SF law on sub-kpc scales (Pereira-Santaella+, in progress) PRELIMINARY
- Large dispersion (x100) in the star formation for a given molecular gas density
Star-formation law appears flatter than standard KS-law
Star formation efficiency higher (x10-100) than that of spirals and local AGNs
at similar molecular gas densities

18. IC 4687. STAR FORMATION IN LIRGS ON ~ 200 pc SCALES.
ALMA + NEAR- & MID-IR SUB-ARCSEC VIEW
H-BAND OLD STARS
Paα IONIZED GAS
[FeII] SUPERNOVAE
4 kpc
H2 COLD MOLECULAR
H2 HOT MOLECULAR
PAHs + HOT DUST 18

19. NGC 5135. SNE-INDUCED OUTFLOWS IN AGED STAR FORMING CLUMP
AzTEC sources in GOODS-N & COSMOS
SPT-lensed sources, Vieira+2013
REGION E
F(B)/F(N)= 9
F(B)/F(N)= 2
F(B)/F(N)= 0.7
[FeII]: Vmax ~ 370 km s-1 / FWZI ~ km s-1 / Mass ~5.5x104 M! (preliminary)
Colina+12

20. EXTRA MATERIAL 20

21. IONIZED GAS. INTEGRATED GAS KINEMATICS
IFS data cube
Integrated spectrum
2 Components (Hα –[NII]):
Narrow: Ambient systemic ISM
Broad: Outflow Vmax = Δv + FWHM/2
Velocity field removed + S/N optimization => well constrained fits
Optimization for detection of faint broad outflows
Similar methodology as high-z (Shapiro+09, Newman+12)
Then: same tracer (Hα) , integrated spectra, 2 Gaussian fitting
Arribas+14

22. AGN & STAR FORMATION IMPACT
AMBIENT IONIZED GAS.
AGN & STAR FORMATION IMPACT
Gas more turbulent than spirals:
σ ~1.5-4 x σspirals (~25 kms-1;Epinat+09)
Weak dependence with increased SF:
σ ~ SFR0.12±0.03
σ range similar to z~2 SFGs
(Forster-Schreiber+09)
Arribas+14

23. AGN & STAR FORMATION IMPACT ON Vmax
IONIZED GAS OUTFLOWS.
AGN & STAR FORMATION IMPACT ON Vmax
Outflows universal
Vmax(non-AGN) ~ SFR0.24±0.05
Vmax (AGN) ~ 2x (non-AGN)
Mass(AGN) ~ 1.4x (non-AGN)
AGNs do not dominate Lbol but
dominate the ionized outflows
Arribas+14

24. NGC 5135. SNE-INDUCED OUTFLOWS. HOT MOLECULAR & PARTIALLY IONIZED GAS24
Casey et al

25. NEAR-IR IFS. EXPLORING MULTI-PHASE ISM
Kinematics of
stars ionized molecular high ion coronal shocks
Stellar pop Young SC dense gas Young SC AGN SNe
VELOCITY
VELOCITY DISPERSION 25

26. IONIZED GAS OUTFLOWS. DOES IT ESCAPES?
Vescape
NO!
Only galaxies with
Mdyn < 2.5x1010 M
are able to expel gas
i.e. Vmax > Vesc
Arribas+14
Mdyn from Bellocchi+13

27. Outflows: low-z U/LIRGs vs. high-z SFGs
Ionized outflows in low-U/LIRGs can be directly compared with high-z work (Shapiro+09, Genzel+11, Newman+12, Harrison+12):
same tracer (Hα), methods, ~ linear scales (when high-z with AO)
Similar trends with SFR, presence of AGNs
Similar properties if samples at similar SFRs
F(B)/F(N) vs. Σ (SFR) plane
Low-z U/LIRGs coverage includes z~2 SFGs (Newman+12)
No ΣSFR threshold for strong outflows at low-z, while for high-z claims of ΣSFR > 1
(Newman+12)
high-z stacked
Arribas+14
Arribas+14

28. Outflow Mass Loading Factors: η
Generally, η < 1 (i.e., no efficient
feedback)
Similar to η (neutral gas)
For (non-AGN) LIRG discs,
η lower than predicted
by models, but similar trends
(i.e., slope)
Arribas+14

29. Local velocity dispersion vs. SFR density
σ (~ kms-1) is larger than in lower luminosity local SFGs (~25 kms-1;Epinat+09)
σ doesn’t seem to be driven by SF (If so, dots in the gray zone, Lehnert+09)
σ similar to z~2 SFGs (Forster-Schreiber+09)
Similar trend in the Σ SFR – σ plane as found for high-z SFGs (Genzel+11)
Arribas+14

30. Local velocity dispersion vs. dynamical phase
Observed trend
Due to SF
Isolated
discs
Wide
pairs
Close
pairs
Mergers
Arribas+14
Dynamical Phase
Gravitational energy release associated to interactions and mergers important for driving sigma

31. DEPENDENCE ON SF COMPACTNESS Σ (SFR)?
IONIZED GAS OUTFLOWS.
DEPENDENCE ON SF COMPACTNESS Σ (SFR)?
z~2, Newman+12
F(B)/F(N) ~ Σ (SFR) +0.12
with large scatter
Low-z U/LIRGs coverage
includes z~2 SFGs’
No clear Σ (SFR) threshold
for launching strong outflows
at low-z
Arribas+14

32. MAPPING EXTENDED HOT MOLECULAR GAS FLOWS
ULIRGS.
MAPPING EXTENDED HOT MOLECULAR GAS FLOWS
HOT-H2 OUTFLOWS ULIRGs
(preliminary)
Common: 4 out of 4
Size ~2-3 kpc
FWZI ~ 1000 km s-1
Mhot ~ few thousand M
Mhot ~10-4 to 10-5 Mcold
IRAS17208, COLD CO /PDBI / Garcia-Burillo+14 in prep.
OUTFLOW
1% H2 MASS
ROTATION
99% H2 MASS

33. EXCITATION STRUCTURE OF THE HOT H2 OUTFLOW
NGC 3256.
EXCITATION STRUCTURE OF THE HOT H2 OUTFLOW
Compatible with thermal processes
Close to LTE with T ~2000 K
More complex than LTE
No/minor differences between broad & narrow 33
Emonts+14, submitted

34. IFS SURVEY. SPATIALLY RESOLVED PROPERTIES
2D SF distribution
(Rodriguez-Zaurin+11)
Extra-nuclear ionization
(Monreal-Ibero+10)
Extinction structure
(Piqueras-López+13)
2D Neutral gas outflows
(Cazzoli+14)
SNe ([FeII]) gas outflows
(Colina+12)
Spatially resolved kinematics
(Bellocchi+13)
for our sample.
Ionized+molecular+shocked gas properties
(Piqueras-Lopez+12)