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Demystifying the IR-Radio Correlation in AGN

This study aims to understand the IR-radio correlation in AGN, focusing on the impact of radio-loud AGN and the possibility of using radio excess as an AGN indicator. The study analyzes high-resolution multiwavelength data to investigate the origin and behavior of the correlation in different types of galaxies.

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Demystifying the IR-Radio Correlation in AGN

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  1. Demystifying the IR - radio correlation with high angular resolution in AGN M. Almudena Prieto (IAC) EWASS 2015

  2. The IR – radio correlation origins • Normal galaxies, starburst, spirals, irregulars follow a tight IR-radio correlation • First reports on a 10 um -1.4GHz correlation relates to Seyfert galaxies (Van de Kruit, 1973), soon extended to starbursts (Van de Kruit, 1975)

  3. The AGN impact on the correlation • Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it • Subtracting the AGN contribution does not always help to bring galaxies back to the correlation • Radio-loud objects getting more dominated by AGN: is their IR being also dominated by the AGN as well ? • Is radio excess an AGN indicator in FIR selected-galaxies ?

  4. PARSEC programMultiwavelengthPARSECS scale study of the centre of the nearest galaxies From X-ray (Chandra) to UV - optical (HST) to IR (VLT diffraction-limit) to mm (SMA/ALMA) to radio-cm (VLBA / ATCA) Achieved angular scales Chandra 10 keV  θ ~ 0.5” HST 0.3 - 0.9 µm  θ< 0.1” VLT /AO 1 - 5 µm  θ< 0.1” ( ~ 1- 20 pc) VLT 10 - 20 µm  θ< 0.4” ALMA/SMA mm  θ < 0.3” VLBA/ ATCA cm  θ< 0.4” For some of the brightest: VLBI 10 µm  θ ~ 0.03“ ( ~ 0.5 pc)

  5. Some of the nearest AGN studied in PARSEC • Lbol • Q/RL 3C273 4x1047 • S1 N3783 2x1044 • S2N1068 8x1043 • RQS1.5 N4151 5x1043 • S2Circinus 8x1042 • RG Cen A2x1042 • LLAGN N3169 9x1041 • LLAGN N10973x1041 • RL LLAGN N1052 3x1041 • LLAGN M 87 1x1041 • LLAGN Sombrero 2x1040 • Prieto et al. 2010, Fernandez-Ontiveros et al. 2012

  6. The AGN impact on the correlation • Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it • Subtracting the AGN contribution does not always help to bring galaxies back to the correlation • Radio-loud objects getting more dominated by AGN: is their IR being also dominated by the AGN as well ? • Is radio excess an AGN indicator in FIR selected-galaxies ?

  7. Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it Radio-galaxies RL Radio-galaxies RL 3C273 M87 N1068 Circinus N1052 N1097 CenA Qso Seyfert RQ Star-forming Qso Seyfert RQ Star-forming Sopp & Alexander 1991 Sopp & Alexander 1991

  8. Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it Radio-galaxies RL 3C273 M87 N1068 Circinus N1052 N1097 CenA Qso Seyfert RQ Star-forming Sopp & Alexander 1991

  9. The AGN impact on the correlation • Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it • Subtracting the AGN contribution does not always help to bring galaxies back to the correlation • Radio-loud objects getting more dominated by AGN: is their IR being also dominated by the AGN as well ? • Is radio excess an AGN indicator in FIR selected-galaxies ?

  10. 3C 273 QSO NGC 5506 Seyfert 1.9 AGN in the IR There are the rulers: 2MASS 2MASS Some AGN dominate the galaxy light regardless of the aperture size

  11. AGNin the IR NGC 1068 Centaurus A …. and the dominated ones: Circinus NGC 1566 2MASS In others, the galaxy dominates the total IR light by orders of magnitude

  12. Modest AGN: their IR luminosity is a few percent of the total IR output S S + low resolution  sub arcsec S RG Prieto+2010

  13. Modest AGN: VLT/VISIR 20 um images, <0.4” resolution, central kpc: the IR excess flux must come large-scale emission in the galaxy NGC1068 - Q Galliano et al. 2006 Reunanen et al. 2008

  14. Modest AGN: … or from circumnuclear star forming regions S1 LLAGN/ S1 S2 NGC 1097 - Q LIR(Ring) = ½ LIR LIR(Ring) =¾ of LIR LIR(Ring) = LIR Reunanen et al. 2008

  15. NGC 1068 Centaurus A Modest AGN: What about the radio emission? Circinus NGC 1566 2MASS 1.4 GHz wide-field maps in contours (Condon 1987; Elmouthie+ 1998)

  16. 3C 273 QSO NGC 5506 Seyfert 2 Dominant AGN the IR 2MASS 2MASS Some AGN dominate the galaxy light regardless of the aperture size

  17. NGC 5506 Seyfert 2 Dominant AGN: their IR luminosity is ~100% of the total Often happens for Lagn > 1044 erg/s QSO S1 S2 2MASS Prieto+2010

  18. The AGN impact on the correlation • Radio-quiet AGN follow the normal “star-forming” correlation, radio-loud galaxies tend to get away from it • Subtracting the AGN contribution does not always help to bring galaxies back to the correlation • Radio-excess objects getting more dominated by AGN: is their IR also dominated by the AGN ? • Is radio excess an AGN indicator in FIR selected-galaxies ?

  19. Low Luminosity RL-AGN: Lagn <1042 erg/s Dominated Intermediate NGC 1097- RQ-RL NGC 4594-RL Dominant 2MASS NGC 1052 - RL NGC 1052 - RL

  20. Low Luminosity RL-AGN: some dominate the total-IR, in others the galaxy dominates the total-IR NGC 1052 - RL Fernandez-Ontiveros et al. 2012

  21. Low Luminosity AGN are jet-dominated objects: should show a IR-radio correlation on their own Fernandez-Ontiveros et al. 2015

  22. Summary • Radio-quiet AGN with Lagn< 10^44 erg/s follow the normal “star-forming” correlation on their own right: they are star-forming dominated objects • Radio-quiet AGN with Lagn> 10^44 erg/s follow the correlation but “as intruders”: IR and Radio are genuinely of AGN origin • Radio-loud objects tend to get away from the correlation: radio excess is an AGN mark • Low luminosity AGN (Lagn<10^42 erg/s) should follow a radio-IR correlation on their own: they are jet-dominated sources from radio to IR

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