1 / 20

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

yael
Download Presentation

ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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.

More Related