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DISSECTING LUMINOUS INFRARED GALAXIES THROUGH MULTI-WAVELENGTH INTEGRAL FIELD SPECTROSCOPY

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

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DISSECTING LUMINOUS INFRARED GALAXIES THROUGH MULTI-WAVELENGTH INTEGRAL FIELD SPECTROSCOPY

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  1. 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

  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 5135. Outflows in supernovae-dominated SF clumps • NGC 3256. Extended hot & cold molecular gas outflows THE STAR-FORMATION LAW ON (SUB)KPC SCALES IN LIRGS • IC4687. KS-law at ΣSFR > 100 M yr-1

  3. U/LIRGS. BASICS 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 numerous @ high-z (dusty IR phase) • SFR (local U/LIRGs) ~ SFR (MS-SFGs @ z~2) NUMBER DENSITY 1” = 200 pc 49% 17% 0.1% 0.01% LIRGS: 1011 ≤ L/L < 1012 ULIRGs: 1012 ≤ L/L < 1013 LIRGS: 1011 ≤ L/L < 1012 ULIRGs: 1012 ≤ L/L < 1013 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

  4. THE MULTI-λ IFS SURVEY OF LOW-Z U/LIRGS IFS data cube • ~ 75 U/LIRGs @ z < 0.2 ( i.e. ~ 0.2-3 kpc/”) • Different dynamics (isolated, interacting, mergers) • 30% AGNs • ANCILLARY: HST Paα & CanariCam/GTC mid-IR imaging

  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

  6. MAPPING THE IONIZATION STRUCTURE

  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

  8. NEAR-IR BPT DIAGRAMS. IDENTIFYING AGN – YOUNG STARS - SNE EXCITATION IN LIRGS HIGH-SURFACE BRIGHTNESS CLUMPS DIFFUSE ISM SNe (8-20 Myr) SF-clumps AGN Young (< 6 Myr) SF-clumps 10 LIRGS, 28000 points Colina+15, A&A in press

  9. THE 2D MULTI-PHASE STRUCTURE OF OUTFLOWS

  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 ~ 1000 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

  11. NGC 3256. THE EXTENDED HOT H2 OUTFLOW 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 + 2014 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)

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

  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 LOW SFE HIGH SFE HIGH SFE FoV = 18” x 18” (6.3.x.6.3 kpc2)

  15. THE STAR-FORMING LAWS @ (SUB)KPC SCALES • IC4687 • - ΣH2 ~30-3000 M pc-2 • - Large dispersion (x100) • in ΣSFRfor 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

  16. FUTURE. VLT - JWST – ALMA SYNERGIES MUSE+AO: 0.46-0.93 μm IFS JWST: 1 – 28 μm IFS (NIRSpec & MIRI combined) 12-16 October 2015

  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 4687. 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 Paα IONIZED GAS [FeII] SUPERNOVAE H-BAND OLD STARS 4 kpc H2 HOT MOLECULAR PAHs + HOT DUST H2 COLD MOLECULAR

  19. NGC 5135. SNE-INDUCED OUTFLOWS IN AGED STAR FORMING CLUMP SPT-lensed sources, Vieira+2013 AzTEC sources in GOODS-N & COSMOS REGION E F(B)/F(N)= 2 F(B)/F(N)= 9 F(B)/F(N)= 0.7 Colina+12 [FeII]: Vmax ~ 370 km s-1 / FWZI ~ 1400 km s-1 / Mass ~5.5x104 M! (preliminary)

  20. EXTRA MATERIAL

  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. 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. 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 GAS Casey et al + 2014

  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

  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. 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 Outflows: low-z U/LIRGs vs. high-z SFGs Arribas+14 Arribas+14

  28. 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) Outflow Mass Loading Factors: η Arribas+14

  29. σ (~ 40-90 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) Local velocity dispersion vs. SFR density Arribas+14

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

  31. 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. 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. 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 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) Ionized+molecular+shocked gas properties (Piqueras-Lopez+12)

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