1 / 13

ULIRGs: IR-Optical-X-ray properties

ULIRGs: IR-Optical-X-ray properties. Valentina Braito. ULIRGs: IR-Optical-X-ray properties. Results from XMM observations of 10 ULIRGs Searching possible multi wavelength diagnostics Results on L band observations (P.I. Risaliti). Background.

soren
Download Presentation

ULIRGs: IR-Optical-X-ray properties

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. ULIRGs: IR-Optical-X-ray properties Valentina Braito

  2. ULIRGs: IR-Optical-X-ray properties • Results from XMM observations of 10 ULIRGs • Searching possible multi wavelength diagnostics • Results on L band observations • (P.I. Risaliti)

  3. Background ULIRGs are a class of sources with LIR>1012L comparable to QSO luminosities. ULIRGs are predominantly powered by heavily dust enshrouded AGN or circumnuclear starbursts? ULIRGs classification strongly depends on the energy band Starburst dominated ULIRGs revealing an obscured AGN when observed in the X-rays (i.e. NGC6240) With this survey all the ULIRGs of Genzel sample (complete at F60m>5.4 Jy and LFIR~1012L ) will have X-ray data

  4. Main goals characterize the hard X-ray continuum investigate the presence of AGN activity • AGN activity is present in 1/3 of the observedsources • AGN-ULIRGs have hard X-ray luminosity lower than typical QSO luminosity • We found 2 ULIRG with high X-ray luminosity & deeply absorbed (Superantennae; Mkr231) • SB-ULIRGs have LX(2-10 keV)  1041-1042ergs/s

  5. absorbed power law (AGN) ~1.7-2 or a flat power law (X-ray binaries) E1-e-E/Ec Ec=8 keV Thermal emission X Ray Spectral properties

  6. X-ray & FIR emission Thermal vs FIR luminosity • No evident correlation between X-ray thermal and FIR luminosity • No evident difference between SB and AGN ULIRGs • X-ray AGN-ULIRGs • X-ray SB-ULIRGs

  7. X-ray & FIR emission 2-10 keV luminosity vs FIR luminosity AGN SB • X-ray AGN-ULIRGs • X-ray SB-ULIRGs

  8. Arp 299 Comparison with local SBs SB-ULIRGs Our results confirm that for ULIRGs without a dominant AGN component, the 2-10 keV emission is a good SFR indicator (Persic et al. 2004).

  9. X-ray & FIR emission The observed hard X-ray emission can be used to highlight AGNs in LIRGs • X-ray AGN-ULIRGs • X-ray SB-ULIRGs

  10. Optical-IR-X-ray Compton-thin Compton-thick SB REGION AGN REGION Work in progress…

  11. The waveband coverage allows to determine of the 3-4 m continuum level a correct estimate of the PAH strength PAH at 3.3m with low EW typical of AGN dominated sources Results from L band spectroscopy P.I. Guido Risaliti IRAS 19254-7245 Broad absorption feature at 3.4m indicative of heavily absorbed AGN see poster by Risaliti for all the spectra

  12.  vs PAH EW A possible dignostic diagram PAH EW vs LIR PURE SB AGN-dominated Composite SB AGN SB-dominated AGN Risaliti et al. in prep

  13. Conclusion and future • LX(2-10) keV as a SFR indicator or to preselect AGN in IR sources • the Fx/FIR vs FOIII /FIR diagram allows to select heavily absorbed AGN in composite sources like ULIRGs • check the peculiar sources in this diagram • complete the Genzel sample (IRAS22491-1808 and IRAS 20100-4156) in L band • spectra of the 4-5 brightest ULIRGs at 4-5 m

More Related