Low Luminosity AGNs: The Power of JWST Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Dillon Berger (GMU), Sara Ellison(UVIC)
Low Luminosity AGNs: The Power of JWST Why are LLAGN important? Why JWST is crucial to find them? What can JWST tell us about them?
Motivation and Overview Why are low luminosity AGNs important? Finding low mass SMBHs (L Edd ~10 42 ergs s -1 for M BH =10 4 M ) insight into SMBH seeds Understanding BH growth in minor mergers (~3 x more frequent than major mergers) Understanding of merger-free pathways to BH growth Link between active and quiescent galaxies (only 1% of galaxies are highly accreting!)
Motivation and Overview Why are low luminosity AGNs important? Crucial to understanding of the origin of SMBHs and their connection to galaxy evolution Difficulty: Low Luminosity AGNs are difficult to find
Limitations with Optical Diagnostics Dust obscuration (LLAGN can have very high N H ; Annuar et al. in prep, Ricci et al. 2015) Optical lines dominated by SF Overlap in low metallicity AGNs with SF on BPT (Trump et al. 2015) More significant in low mass galaxies
Limitations with Optical Diagnostics Dust obscuration (LLAGN can have very high N H ; Annuar et al. in prep, Ricci et al. 2015) Optical lines dominated by SF Overlap in low metallicity AGNs with SF on BPT (Trump et al. 2015) More significant in low mass galaxies
Limitations with Optical Diagnostics Dust obscuration (LLAGN can have very high N H ; Annuar et al. in prep, Ricci et al. 2015) Optical lines dominated by SF Overlap in low metallicity AGNs with SF on BPT (Trump et al. 2015) More significant in low mass galaxies
Limitations with Optical Diagnostics Type II SNe can look like AGNs L Hα from broad lines comparable to SNe (e.g. Greene & Ho 2007) Majority of broad lines in dwarfs fade within a few years (Baldassare et al. 2016) (Fillipenko 1987)
Limitations with Optical Diagnostics Type II SNe can look like AGNs L Hα from broad lines comparable to SNe (e.g. Greene & Ho 2007) Majority of broad lines in dwarfs fade within a few years (Baldassare et al. 2016) (Fillipenko 1987) Optical diagnostics limited in finding low luminosity AGNs
Optically Identified AGNs: Almost all in Massive Bulge-dominated Hosts (Kauffmann et al. 2003) Optical studies don t tell the full story
Limitations with X-ray Diagnostics (Mineo et al. 2014) (Fragos et al. 2013) Contamination by XRBs X-ray enhancement with metallicity More significant in low mass galaxies
Limitations with X-ray Diagnostics HLXs (Walton et al. 2011) Separation (kpc) LLAGNs have X-ray luminosities comparable to ULXs At z=0.35 1 = 5 kpc More significant in starburst galaxies X-ray observations alone not sufficient to confirm low luminosity AGNs
Limitations of MIR Color Selection 1.4M AGN - Secrest et al. (2015)
Integrated Modeling Approach Theoretical model of predicted line and continuum from a starburst and AGN Key Goals Explore diagnostic potential of multiwavelength studies of LLAGN Pre-selection strategy for JWST See poster by Nick Abel
Transmitted Continuum Model SED of 5 Myr starburst
Transmitted Continuum AGN heats dust to high T Obscuration-independent diagnostic
Transmitted Continuum Less effective when L AGN < 50% L tot
Transmitted Continuum Less effective when L AGN < 50% L tot
Limitations with MIR Color Selection AGN demarcation (Jarret et al. 20011) SDSS AGNs identified through BPT classification (Kewely et al. 2001) Only 9% in AGN mid-ir color selection wedge Most optically identified AGNs are not identified as AGNs through mid-ir color selection Mid-IR color selection selects only dominant AGNs
Limitations with MIR Color Selection Question: Can a pure starburst theoretically produce MIR colors like an AGN? 2.5% of optically classified star forming galaxies have AGNlike in mid-ir colors
Limitations with with MIR Selection
Limitations with MIR Color Selection Extreme starbursts can look like an AGN in mid-ir colors (Satyapal et al, in prep) Galaxies with extreme SF more affected (Satyapal et al. 2014, 2017, Sartori et al 2015, Hainline et al. 2016)
Mid Infrared Spectroscopic Diagnostics THE POWER OF JWST MIRI NeV NeV Insensitive to extinction Insensitive to dilution by SF No confusion with XRBs, ULXs Robust way to find low luminosity AGNs
Mid Infrared Spectroscopic Diagnostics THE POWER OF JWST MIRI NeV NeV Insensitive to extinction Insensitive to dilution by SF No confusion with XRBs, ULXs Robust way to find low luminosity AGNs
AGN Detection Rate vs. Hubble Type Detection rate of ~ 30% at 10 38 ergs s -1 Roughly 4 times the detection rate of optical studies! Optically studies significantly miss AGNs in late-type hosts (Satyapal et al. 2007, 2008, 2009) NGC 3621 NGC 4178
Tip of the Iceberg: Weak AGNs not found with WISE Bulgeless AGNs with [NeV] emission
Tip of the Iceberg: Weak AGNs not found with WISE Bulgeless AGNs with [NeV] emission NGC 1042 He 2-10 NGC 3621 NGC 4178
What can we learn with JWST? AGN bolometric luminosity Relation to disk, nuclear star cluster, or any other galaxy property? Secrest et al. 2012 AGN/SF connection True SMBH occupation fraction?
What can we learn with JWST? Black Hole Mass? NeV NeVI R s (10 5 M )~ 0.01 at 10Mpc
What can we learn with JWST? Black Hole Mass? NeV NeVI Species Transition Wavelngth IP(eV) [MgVII] 3P2-3P1 5.5032 186.51 [KVI] 3P2-3P1 5.575 82.66 [MgV] 3P1-3P2 5.60985 109.24 [AlVIII] 3P1-3P0 5.85 241.44 [CaVII] 3P1-3P0 6.154 108.78 [SiVII] 3P0-3P1 6.4922 205.05 [NeVI] 2P3/2-2P1/2 7.6524 126.21 [FeVII] 3F4-3F3 7.8145 99.1 [NaVI] 3P2-3P1 8.61059 138.39 [KVI] 3P1-3P0 8.8299 82.66 [MgVII] 3P1-3P0 9.009 186.51 [AlVI] 3P0-3P1 9.116 153.83 [FeVII] 3F3-3F2 9.5267 99.1 [FV] 2P3/2-2P1/2 13.432 87.14 [MgV] 3P0-3P1 13.5213 109.24 [NeV] 3P2-3P1 14.3217 97.12 [NaVI] 3P1-3P0 14.3964 138.39 [NeV] 3P1-3P0 24.3175 97.12
Key Points Low Luminosity AGNs are crucial in understanding origin of BH and BH/Galaxy evolution Optical studies limited by extinction and dilution by SF X-ray studies limited by XRB/ULX contamination Mid-IR color selection limited by dilution by SF
Elusive AGN Conference June 12-15, 2017, George Mason University Abstract submission deadline: March 20th Website: agnjwst.cos.gmu.edu