Low Luminosity AGNs: The Power of JWST. Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Dillon Berger (GMU), Sara Ellison(UVIC)

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1 Low Luminosity AGNs: The Power of JWST Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Dillon Berger (GMU), Sara Ellison(UVIC)

2 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?

3 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!)

4 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

5 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

6 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

7 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

8 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)

9 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

10 Optically Identified AGNs: Almost all in Massive Bulge-dominated Hosts (Kauffmann et al. 2003) Optical studies don t tell the full story

11 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

12 Limitations with X-ray Diagnostics HLXs (Walton et al. 2011) Separation (kpc) LLAGNs have X-ray luminosities comparable to ULXs At z= = 5 kpc More significant in starburst galaxies X-ray observations alone not sufficient to confirm low luminosity AGNs

13 Limitations of MIR Color Selection 1.4M AGN - Secrest et al. (2015)

14 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

15 Transmitted Continuum Model SED of 5 Myr starburst

16 Transmitted Continuum AGN heats dust to high T Obscuration-independent diagnostic

17 Transmitted Continuum Less effective when L AGN < 50% L tot

18 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.

19 Limitations with MIR Color Selection AGN demarcation (Jarret et al ) 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

20 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

21 Limitations with with MIR Selection

22 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)

23 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

24 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

25 AGN Detection Rate vs. Hubble Type Detection rate of ~ 30% at 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

26 Tip of the Iceberg: Weak AGNs not found with WISE Bulgeless AGNs with [NeV] emission

27 Tip of the Iceberg: Weak AGNs not found with WISE Bulgeless AGNs with [NeV] emission NGC 1042 He 2-10 NGC 3621 NGC 4178

28 What can we learn with JWST? AGN bolometric luminosity Relation to disk, nuclear star cluster, or any other galaxy property? Secrest et al AGN/SF connection True SMBH occupation fraction?

29 What can we learn with JWST? Black Hole Mass? NeV NeVI R s (10 5 M )~ 0.01 at 10Mpc

30 What can we learn with JWST? Black Hole Mass? NeV NeVI Species Transition Wavelngth IP(eV) [MgVII] 3P2-3P [KVI] 3P2-3P [MgV] 3P1-3P [AlVIII] 3P1-3P [CaVII] 3P1-3P [SiVII] 3P0-3P [NeVI] 2P3/2-2P1/ [FeVII] 3F4-3F [NaVI] 3P2-3P [KVI] 3P1-3P [MgVII] 3P1-3P [AlVI] 3P0-3P [FeVII] 3F3-3F [FV] 2P3/2-2P1/ [MgV] 3P0-3P [NeV] 3P2-3P [NaVI] 3P1-3P [NeV] 3P1-3P

31 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

32 Elusive AGN Conference June 12-15, 2017, George Mason University Abstract submission deadline: March 20th Website: agnjwst.cos.gmu.edu

Challenges in Finding AGNs in the Low Luminosity Regime. Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Amrit Singh (GMU), Sara Ellison(UVIC)

Challenges in Finding AGNs in the Low Luminosity Regime Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Amrit Singh (GMU), Sara Ellison(UVIC) Motivation and Overview Why are low luminosity AGNs important?