Hot Dust in RadioLoud AGNs Wolfram Freudling Space

Hot Dust in Radio-Loud AGNs Wolfram Freudling Space Telescope – European Coordinating Facility • ISOCAM Survey of 3 C galaxies • Questions: – – How do SEDs of various AGNs types differ? Are dust SEDs consistent with Unified Schemes? What heats the dust (AGN vs SB contribution) What do we expect at higher redshifts? • Publications: Freudling, Siebenmorgen, Haas, 2003, Ap. J Letters 599, 13; Siebenmorgen, Freudling, Krügel, Haas, 2003, A&A, submitted 10/2/2020 Hot Dust in Radio-Loud AGNs 1

ISOCAM 3 C Survey Siebenmorgen, Freudling, Krügel, Haas, 2003, A&A, submitted • • • 88 fields in ISOCAM archive include 3 C source All fields homogenously co-added and calibrated About 50% NLRGs, 25% QSOs, 25% BLRGs 71 3 CR sources detected In 60 of them evidence for dust 10/2/2020 Hot Dust in Radio-Loud AGNs 2

ISOCAM Images of 3 C Sources 10/2/2020 Hot Dust in Radio-Loud AGNs 3

ISOCAM pixel size HST imaging by Martel et al, 1999, Ap. JS 122, 88 10/2/2020 Hot Dust in Radio-Loud AGNs 4

Results: SEDs 10/2/2020 Hot Dust in Radio-Loud AGNs 5

Freudling, Siebenmorgen, Haas 2003, Ap. J Letters 599, L 13 Mean SEDs Type 1 Type 2 10/2/2020 Hot Dust in Radio-Loud AGNs 6

Dust Heating in AGNs Model 1 (e. g. Farrah et al. 2003, MNRAS 345, 585 ; Rowand-Robinson 2000, MNRAS 316, 575) SB Cool heats dust local 50 K dust clouds AGN Hot heats dust 300 K torus 10/2/2020 Hot Dust in Radio-Loud AGNs 7

HST imaging of Galactic Nuclei Martel et al. 2000, Ap. JS 130, 267 10/2/2020 Hot Dust in Radio-Loud AGNs 8

Dust Heating in AGNs Model 2 (AGN effects throughout host galaxy) 10/2/2020 Hot Dust in Radio-Loud AGNs 9

Spherical Dust model Model parameters: • radius • AGN luminosity • extinction Av 10/2/2020 Hot Dust in Radio-Loud AGNs 10

Freudling, Siebenmorgen, Haas 2003, Ap. J Letters 599, L 13 Mean SEDs Type 1 Type 2 10/2/2020 Hot Dust in Radio-Loud AGNs 11

Radius of dust sphere Best fit radius=2 kpc 10/2/2020 Best fit radius=4 kpc Hot Dust in Radio-Loud AGNs 12

Conclusions 1 • AGNs can heat dust throughout the host • The presence of cold dust does not necessarily imply a SB component do not use SEDs to identify starburst contribution to dust heating 10/2/2020 Hot Dust in Radio-Loud AGNs 13

Differences between AGN and SB heating Hard radation by AGN distroys PAHs Siebenmorgen et al. 2003 10/2/2020 Hot Dust in Radio-Loud AGNs 14

Mean SEDs of local (z<~1) AGNs ISO data suggest Type 1 that dust throughout the host is heated by Type 2 SE Ds PA the central engine pre d ict H sp ec tra Freudling, Siebenmorgen, Haas 2003, Ap. JL 599, L 13 10/2/2020 Hot Dust in Radio-Loud AGNs 15

PAH spectra by AGN type ISOPHOT spectra of PG QSOs by Haas et al. 2003 A&A 402, 87 ISOPHOT spectra of four 3 CR sources extracted from archive Freudling et al. 2003 ISOPHOT spectra of Seyfert 2 s by Clavel et al. 2000 A&A 357, 839 10/2/2020 Hot Dust in Radio-Loud AGNs 16

Dust in high-z QSOs Redshifted local QSOs Freudling et al. 2003, Ap. JL 599, L 13 High-z QSOs Bertoldi et al. 2003, AA 406, L 55 10/2/2020 Hot Dust in Radio-Loud AGNs 17

Summary & Conclusions • ISOCAM detected most of the 3 C sources within its field of view, mostly because of dust emission. • There is a clear correlation between the AGN type and the peak of the SEDs: – type 1 peak around 40 m – 2 100 m • PAHs emmission is stronger in type 2 AGNs with same dust luminosity as their type 1 counterparts • AGN can heat dust throughout the host 10/2/2020 Hot Dust in Radio-Loud AGNs 18

The End 10/2/2020 Hot Dust in Radio-Loud AGNs 19

The End 10/2/2020 Hot Dust in Radio-Loud AGNs 20

Dust Heating in AGNs Model 2 (AGN effects throughout host galaxy: 10/2/2020 Hot Dust in Radio-Loud AGNs 21

Fitting Procedure Plot data synchrotron stellar dust 10/2/2020 Hot Dust in Radio-Loud AGNs 22

Example M 82 log L= 10 Av= 25 R=2 kpc Krügel & Siebenmorgen, 1994, AA 288, 929: log L= 10. 5 Av=25 R=1 kpc 10/2/2020 Hot Dust in Radio-Loud AGNs 23

NO 10/2/2020 Hot Dust in Radio-Loud AGNs 24

0. 05 < z < 0. 4 10/2/2020 Hot Dust in Radio-Loud AGNs 25