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ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION

ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION. L. COLINA, IEM/CSIC. S. ARRIBAS, STSCI & CSIC D. CLEMENTS, IMPERIAL COLLEGE A. MONREAL, IAC M. GARCIA-MARIN, IEM/CSIC. OUTLINE. SAMPLE OF LOW-Z ULIRGs AND INSTRUMENTATION ARP 220: STRUCTURE OF THE EXTENDED WARM IONIZED GAS

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ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION

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  1. ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION L. COLINA, IEM/CSIC S. ARRIBAS, STSCI & CSIC D. CLEMENTS, IMPERIAL COLLEGE A. MONREAL, IAC M. GARCIA-MARIN, IEM/CSIC

  2. OUTLINE • SAMPLE OF LOW-Z ULIRGs AND INSTRUMENTATION • ARP 220: STRUCTURE OF THE EXTENDED WARM IONIZED GAS • 2D KINEMATICAL PROPERTIES OF ULIRGS • DYNAMICAL MASS TRACERS • IMPLICATIONS FOR HIGH-Z GALAXIES: SFR AND MASS • CONCLUSIONS

  3. SAMPLE OF LOW-Z ULIRGS REDSHIFT LUMINOSITY ACTIVITY MERGING PHASE Z < 0.2 11.8 < log(LIR/L) < 12.6 HII - Sy1 EARLY/LATE

  4. Mode FoV (”x”) Ø (”) SB1 7.80x6.40 0.45 SB2 16.0x12.3 0.90 SB3 33.6x29.4 2.70 INTEGRAL FIELD SPECTROSCOPY OF ULIRGS INTEGRAL on WHT Arribas et al. 1998 3 fiber bundles:

  5. ARP 220: INTEGRAL FIELD SPECTROSCOPY (I)* SB3 BUNDLE 6000 s 18000 s 28 X 15 Kpc 15000 s * Colina, Arribas & Clements, 2004, ApJ 602

  6. ARP 220: INTEGRAL FIELD SPECTROSCOPY (II) 350 spectra 4500 - 7500 A Log F(H) > -17 erg cm-2 s-1 arcec-2

  7. ARP 220: HST vs IFS STELLAR STRUCTURE WFPC2 F814W INTEGRAL SB3 *

  8. ARP 220: 2D IONIZED GAS STRUCTURE NW PLUME W LOBE E LOBE SE PLUME

  9. Galaxy log LIR (L) LH /LIR (xE-5) LX/LIR (xE-5) Extent (kpc) Arp 220 Plumes 12.16 0.14 0.6 7 Arp 220 Lobes 12.16 0.16 0.3 24 NGC 253 10.46 0.37 1.5 1.3 NGC 3079 10.49 2.7 6.2 3 ARP 220: ORIGIN OF EXTENDED IONIZED GAS* STARBURST-INDUCED SUPERWINDS OR MERGER-INDUCED SHOCKS Distance (Mpc) 77.6 77.6 3.0 3.0 16 M82 10.52 16 2.6 2.4 * Colina, Arribas, Clements 2004, ApJ 602

  10. ARP 220: ORIGIN OF EXTENDED IONIZED GAS MERGER-INDUCED STRUCTURES? SIMULATION (S. LAMB) - Gas-rich galaxies - Comparable-mass - Low impact velocity - Face-on collision McDowell et al. 2003, ApJ 591

  11. ARP 220: VELOCITY vs STELLAR AND GAS STRUCTURES - Peak-to-peak V of 600 km/s - Vel. Deviations of 300 km/s - Vel gradients of 50 km/s/kpc - Associated with the stellar envelope - Average velocities of E and W lobes: +8 and -79 km/s - Not dominated by central, starburst-driven wind - Average velocities of E and W lobes consistent with merger simulations (to first order) GAS STRUCTURE STELLAR STRUCTURE STELLAR STRUCTURE

  12. 2D KINEMATICAL PROPERTIES OF ULIRGS (I) HST F160W CONT. H VELOCITY DISP. VELOCITY FIELD

  13. 2D KINEMATICAL PROPERTIES OF ULIRGS (II) HST F160W CONT. H VELOCITY DISP. VELOCITY FIELD

  14. 2D KINEMATICS OF ULIRGS: SUMMARY • Velocity field on scales of few to several kpc does not correspond in general to that of an ordered, rotating system • Peak-to-peak velocity amplitudes of up to 600 km/s are detected in tidally induced structures: tails and extranuclear star-forming regions • The peak of the velocity dispersion in 60% of the ULIRGs studied does not coincide in position with the stellar nucleus • Velocity dispersions associated with extranuclear, diffuse ionized gas are large: 150 to 250 km/s • Velocity dispersion associated with the less massive, secondary nucleus in pairs is not distinguishable from that of the extended, diffuse gas • Extended ionized gas velocities on scales of few to several kpc are not wind-related but merger-induced

  15. MASS TRACER: CENTRAL VELOCITY AMPLITUDE IF ROTATION: MASS  V2 R HOWEVER VELOCITY AMPLITUDE DOES NOT TRACE ROTATION, IN GENERAL : stars : cold gas VELOCITY AMPLITUDE IS NOT A RELIABLE TRACER OF DYNAMICAL MASS

  16. MASS TRACER: CENTRAL VELOCITY DISPERSION : Central velocity dispersion Re: Effective radius MASS  2 Re VELOCITY DISPERSION IS A RELIABLE TRACER OF DYNAMICAL MASS : stars : cold gas ULIRG MASSES 0.1m* < m < 1.1m* m= 0.4  0.3 m* m*= 1.4E+11 M

  17. IMPLICATIONS FOR HIGH-Z GALAXIES: SFR and MASS • LIRGS and ULIRGs carry a large fraction oof SF at z> 1 • SPITZER and HERSCHEL most likely to detect LIRGs at high-z • KEY PARAMETERS  SFR AND DYNAMICAL MASS  H line • H line shifts into the near and mir-IR (1 to 10 micron) for z> 1 • near-IR multi-slit spectrographs NOT GOOD ENOUGH •  • MISLEADING DERIVATIONS OF SFRs AND MASSES • IN HIGH-Z LUMINOUS DUST-ENSHROUDED STARBURST Strong differential extinction effects Decoupled ionized & stellar structuresINTEGRAL FIELD SPECTROSCOPY Complex 2D velocity field

  18. IMPLICCATIONS FOR HIGH-Z GALAXIES (I) Av (C)= 5.6 mag Av (D)= 2.2 mag García-Marín, Colina & Arribas, see poster

  19. IMPLICATIONS FOR HIGH-Z GALAXIES (II) NIRCam Z=2.5 HST F814W NIRSpec IFU H INTEGRAL H 1 2 SFR(1)/SFR(2)= 2 m(1)/m(2)=0.25 García-Marín, Colina & Arribas, see poster

  20. IMPLICATIONS FOR HIGH-Z GALAXIES: SUMMARY IF most high-z galaxies are merging systems such as low-z ULIRGs THEN • H velocity amplitudes should not be used in general to estimate Mdyn • H central velocity dispersions are a more reliable tracer of the Mdyn, provided the true nucleus is known from near-IR imaging • H-based star formation rates can be underestimated, factors 2 or 3 in some systems, even if corrected by strong differential extinction effects • Long-slit spectroscopy could give misleading results. IFS desirable.

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