THE EMISSION AND DISTRIBUTION OF DUST OF THE TORUS OF NGC 1068

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THE EMISSION AND DISTRIBUTION OF DUST OF THE TORUS OF NGC 1068 ENRIQUE LOPEZ RODRIGUEZ Instrument Scientist (HAWC+) Stratospheric Observatory For Infrared Astronomy (SOFIA) / NASA

1 THE EMISSION AND DISTRIBUTION OF DUST OF THE TORUS OF NGC 1068 ENRIQUE LOPEZ RODRIGUEZ Instrument Scientist (HAWC+) Stratospheric Observatory For Infrared Astronomy (SOFIA) / NASA elopezrodriguez@nasa.gov COLLABORATORS: Alonso-Herrero, A. (CSIC) Efstathiou, A. (U. of Cyprus) Fuller, L. (UT San Antonio) Ichikawa, R. (Columbia U.) Levenson, N. (STScI) Nikutta R. (NOAO) Packham, C. (UT San Antonio) Radomski, J. (SOFIA) Ramirez, E. (INAOE) Ramos Almeida C. (IAC) and HAWC+ Science Team

2 2 THE TORUS ACTIVE GALACTIC NUCLEI

3 ACTIVE GALACTIC NUCLEI: SPECTRAL ENERGY DISTRIBUTION 3

4 ACTIVE GALACTIC NUCLEI: PHYSICAL STRUCTURES 4 log(radius) Host Galaxy Disk Bulge Bicones Warped mol. disk Dusty wind 2000 K Dusty molecular torus 20 K ~10 7 M 1 pc kpc kpc pc pc Failed wind Ionized Wind Accretion disk continuum 100 r s Nucleus Compton Wind 10 Relativistic Jet perpendicular to disk Black Hole 1 symmetry Bicones Extended NELR OIII, Coronal lines FIR cont 100µm CO H 2 MIR cont N NELR Hα [OIII] Coronal lines NIR cont JHK Low Ionization Broad Emission Lines LoBELs MgII, Balmer, Paschen series High Ionization Broad Emission Lines HiBELs CIV HeII OVI Coronal lines? UV continuum Big Blue Bump X-ray source 10 6 M : ~10 12 cm ~0.3 µpc 10 9 M : ~10 15 cm ~0.3 mpc Martin Elvis, September 2007

5 ACTIVE GALACTIC NUCLEI: INFRARED EMISSION Scale of Quasar/AGN Components log(radius) Host Galaxy Disk Bulge Warped mol. disk Dusty wind Bicones 2000 KFailed wind Dusty molecular torus 20 K ~10 7 M 1 pc kpc kpc pc pc Ionized Wind Accretion disk continuum 100 r s Nucleus Compton Wind 10 Relativistic Jet perpendicular to disk Black Hole 1 symmetry 5 FIR cont 100µm CO H 2 MIR cont N Bicones NELR Extended NELR Hα [OIII] OIII, Coronal Coronal lines lines NIR cont JHK Low Ionization Broad Emission Lines LoBELs MgII, Balmer, Paschen series High Ionization Broad Emission Lines HiBELs CIV HeII OVI Coronal lines? UV continuum Big Blue Bump X-ray source 10 6 M : ~10 12 cm ~0.3 µpc 10 9 M : ~10 15 cm ~0.3 mpc Martin Elvis, September 2007

6 THE TORUS AS THE CORNERSTONE STRUCTURE OF UNIFICATION 6 Beckman & Shrader et al. (2012)

7 ACTIVE GALACTIC NUCLEI: THE CLUMPY TORUS 7

8 AGN TORUS: CLOUD DISTRIBUTION 8 FACE-ON EDGE-ON 45 O EDGE-ON Credit: Nikutta R.

9 AGN TORUS: DUST EMISSION DISTRIBUTION FACE-ON 9 45 O 1 EDGE-ON Credit: Nikutta R. 2 3

10 CLUMPY TORUS SED 10 - The isolated emission from the nucleus using 10-m class telescopes can be reproduced using CLUMPY torus models. NGC 1068 Alonso-Herrero et al. (2011) Torus models using CLUMPY (Nenkova et al. 2002, 2008a,b)

11 HIGH-ANGULAR RESOLUTION NUCLEAR SED OF AGN: CLUMPY TORUS MODEL 11 Alonso-Herrero et al. (2011)

12 AGN SED: LACK OF FIR OBSERVATIONS WITH MODERATED RESOLUTIONS 12 Alonso-Herrero et al. (2011)

13 Fuller et al. (2016) AGN SED: FILLING THE FAR-INFRARED GAP WITH FORCAST/SOFIA um imaging observations of AGN using FORCAST

14 AGN SED: FILLING THE FAR-INFRARED GAP WITH SOFIA um observations: - Characterize the warm dust of the torus. - Sample the peak emission of the torus, suggesting to occurs in the um range. - Reduce the uncertainties of the inferred family of CLUMPY torus models Fuller et al. (2016)

GOAL: FIR OBSERVATIONS OF NGC 1068 15 Characterizing the warm/cold dust in the AGN torus: Lack of 20-100 um coverage at

15 GOAL: FIR OBSERVATIONS OF NGC Characterizing the warm/cold dust in the AGN torus: Lack of um coverage at moderate angular resolutions: - Missing warm and cold dust in the torus - How this affect the torus emission and morphology?

16 16 FORCAST & HAWC+ IMAGING OBSERVATIONS EMISSION AND DISTRIBUTION OF DUST IN THE TORUS OF NGC 1068 Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

17 17 17

18 THE RESOLVED TORUS OF NGC 1068: ALMA OBSERVATIONS 18 Torus size ~ 12x5 pc Orientation of the torus ~ 110 o Highly inhomogeneous molecular torus Garcia-Burrillo et al. (2016) Gallimore et al. (2016) Imanishi et al. (2018) Garcia-Burrillo et al. (2016)

19 THE RESOLVED TORUS OF NGC 1068: ALMA OBSERVATIONS 19 Torus size ~ 12x5 pc Orientation of the torus ~ 110 o Highly inhomogeneous molecular torus Garcia-Burrillo et al. (2016) Gallimore et al. (2016) Imanishi et al. (2018) Lack of moderate angular resolution observations in the FIR.

SOFIA: 2.5-m telescope 20 WAVELENGTH RANGE: 0.3-300 microns INSTRUMENTS: 7 First generation instruments: cameras, spectrometers & highspectrometers.

20 SOFIA: 2.5-m telescope 20 WAVELENGTH RANGE: microns INSTRUMENTS: 7 First generation instruments: cameras, spectrometers & highspectrometers. New instrument: imager-polarimeter at microns (HAWC+) AIRSPEED: Mach 0.85 (560 mph ~ 901 kmh) OBSERVING ALTITUDE: 37,000-45,000 ft ONBOARD STAFF: Flight crew 3; Mission crew 2-6, Scientist 1-3, Educators 5-15 AVERAGE SCIENCE FLIGHT LENGTH: 10 hours overnight

21 SOFIA OBSERVATIONS: FIR IMAGING AND POLARIMETRY INSTRUMENTS 21 HAWC+ HAWC+ observes total and polarized emission of dust grains at four different wavelengths in the range of micrometers. The far-infrared emission, detected by HAWC+, samples different dust temperatures in the range of 10K to 100K. PI: Darren Dowell (JPL) FORCAST FORCAST observes total emission of dust grains in the range of 5-40 micrometers. The infrared emission, detected by FORCAST, samples different dust temperatures in the range of 100K to 600K. PI: Terry Herter (Cornell University)

22 OBSERVATIONS: MICRONS IMAGING 22 HAWC+ FORCAST PI: Darren Dowell (JPL) PI: Terry Herter (Cornell University)

23 FORCAST & HAWC+ OBSERVATIONS: NGC 1068 & PSF 23 Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

24 RESIDUALS: NGC MODEL 24 Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

25 NUCLEAR SED EMISSION: CLUMPY TORUS MODELS 25 We combined SOFIA (FORCAST & HAWC+) observations with 1-20 um imaging and spectroscopy, ALMA, and Spitzer observations. - SED using moderate (>1 ) and high (PSF-fitting) angular flux measurements of the core of NGC 1068 Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

26 NUCLEAR SED EMISSION: CLUMPY TORUS MODELS 26 Star forming regions dominates at wavelengths > 50 um. Dust emission at ~10 um arises from polar emission and its characterized with a blackbody components dominating at ~200 K at scales > 10 pc. The torus emission of the torus peaks in the um range. - This is the first detection and characterization of the AGN torus peak emission. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

27 NUCLEAR SED EMISSION: CLUMPY VS SMOOTH TORUS MODELS 27 CLUMPY torus models best describe the high-resolution um observations Smooth CLUMPY Smooth torus model under-estimates the FIR emission. - If we force the smooth torus models to go through the FIR emission, then smooth models overestimate the torus size and cold dust emission. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

28 NUCLEAR SED EMISSION: CLUMPY VS SMOOTH TORUS MODELS 28 CLUMPY torus models best describe the high-resolution um observations Smooth CLUMPY Smooth torus model under-estimates the FIR emission. - If we force the smooth torus models to go through the FIR emission, then smooth models overestimate the torus size and cold dust emission. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

29 NUCLEAR SED EMISSION: SED COVERAGE We inferred the best CLUMPY torus model using different SED coverages um: The full extend of the torus cannot be constrained um: Turn-over of the torus emission occurs um: Probe the full bulk of dust emission in the torus by accounting the warm/cold dust. 29 Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

30 AGN TORUS: DUST EMISSION DISTRIBUTION USING CLUMPY TORUS MODELS FACE-ON O 1 EDGE-ON Credit: Nikutta R. 2 3

31 NUCLEAR SED EMISSION: 2D CLUMPY TORUS IMAGES um SED coverage underestimates the cold dust in the torus -> Torus is small and very compact, and the SED underestimates the FIR and sub-mm observations um + ALMA SED coverage overestimates the cold dust in the torus -> Torus is slightly bigger and has small angular width. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

32 NUCLEAR SED EMISSION: 2D CLUMPY TORUS IMAGES um SED coverage underestimates the cold dust in the torus -> Torus is small and very compact, and the SED underestimates the FIR and sub-mm observations um + ALMA SED coverage overestimates the cold dust in the torus -> Torus is slightly bigger and has small angular width. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

33 NUCLEAR SED EMISSION: 2D CLUMPY TORUS IMAGES um SED coverage underestimates the cold dust in the torus -> Torus is small and very compact, and the SED underestimates the FIR and sub-mm observations um + ALMA SED coverage overestimates the cold dust in the torus -> Torus is slightly bigger and has small angular width. Lopez-Rodriguez et al. (2018, ApJ, 859, 99)

34 THE RESOLVED TORUS OF NGC 1068: ALMA OBSERVATIONS 34 Torus size ~ 12x5 pc Orientation of the torus ~ 110 o Highly inhomogeneous molecular torus Garcia-Burrillo et al. (2016) Gallimore et al. (2016) Imanishi et al. (2018) Inferred torus using CLUMPY torus models Results: - The inferred torus size, dust distribution and dust emission is well described by the um SED. - Dust distribution is best described by the 432 um observations

35 NUCLEAR SED EMISSION: 2D CLUMPY TORUS IMAGES VS IR INTERFEROMETRY 35 Best inferred dust emission using CLUMPY torus models (Lopez-Rodriguez+2018) Best inferred dust emission using IR interferometry (Lopez-Gonzaga+2014) um nuclear SED 12 um MIDI/VLTI uv-plane and correlated flux

36 SUMMARY 36 - The torus is the cornerstone of the unification model of active galaxies. - The torus absorbs radiation from the active nucleus and re-emits it at IR wavelengths. - This structure has been extensively study in the 1-13 um (1500K-100K) and recently in the sub-mm range with ALMA. - The torus is thought to be clumpy, dusty and with sizes <10 pc. This structure is not resolved with current single-dish telescopes. - Current studies lack of moderate resolution observations in the range of um. - This wavelength range is thought to be where the peak emission of the torus occurs and where the warm/cold dust of the torus can be traced. - We report um imaging observations of NGC 1068 using FORCAST AND HAWC+ onboard SOFIA. - Star forming regions dominate at scales of 700 pc at >100 um. - Dust emission at scales > 10 pc in the polar direction dominates at 10 um. - The torus emission is isolated from these two regions and their peak is found to be in the um range. - Using CLUMPY torus models, we found that: - The 1-20 um range is not able to probe the full extent of the torus. - The morphology of the emission in the 1-20 um range shows an elongated morphology perpendicular to the cloud distribution. - The cloud distribution is characterized by observations in the sub-mm range.

37 Thank you 37

IR Instrumentation & AGN: Revealing Inner Secrets. Chris Packham University of Florida 7 th October, 2011

IR Instrumentation & AGN: Revealing Inner Secrets Chris Packham University of Florida 7 th October, 2011 Presentation Outline T λ" i m e! Instrumentation past, present, and near future INGRID MMT-POL T-ReCS,