WISDOM: Weighing Supermassive Black Holes Across the Hubble Sequence - PowerPoint PPT Presentation

WISDOM: Weighing Supermassive Black Holes Across the Hubble Sequence Martin Bureau, Oxford University WISDOM Team (Leo Blitz, Michele Cappellari, Timothy Davis, Satoru Iguchi, Lijie Liu, Eve North, Kyoko Onishi, Marc Sarzi, Mark Smith) Poster - North: WISDOM: Do we have it to constrain SMBH masses? Poster - Smith: WISDOM: Modelling molecular gas observations in NGC4429 and NGC4501 to measure the SMBH mass Plans: Introduction: M BH - σ ★ correlation, SMBH signature SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations Martin Bureau, University of Oxford

WISDOM: Weighing Supermassive Black Holes Across the Hubble Sequence Martin Bureau, Oxford University WISDOM Team (Leo Blitz, Michele Cappellari, Timothy Davis, Satoru Iguchi, Lijie Liu, Eve North, Kyoko Onishi, Marc Sarzi, Mark Smith) Poster - North: WISDOM: Do we have it to constrain SMBH masses? Poster - Smith: WISDOM: Modelling molecular gas observations in NGC4429 and NGC4501 to measure the SMBH mass Plans: Introduction: M BH - σ ★ correlation, SMBH signature SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations Martin Bureau, University of Oxford

M Ÿ - σ ★ Relation: Status SMBH Masses: M Ÿ - σ ★ : ≈ 80 masses, all local • All require medium resolution spectro • at high spatial resolution Basis for all indirect estimates • (reverberation mapping, line widths, virial/X-ray/radio FP, pitch angle, … ) Underlies staggering amount of • theoretical work (McConnell & Ma 13) Essential to framework of (high-mass) • galaxy formation ⇒ Central to much current astrophysics (AGN feedback) Martin Bureau, University of Oxford

M Ÿ - σ ★ Relation: Biases Weaknesses: M Ÿ - σ ★ : Still relatively few measurements • Handful of methods • Each method has own weaknesses • and systematics Methods çè targets highly correlated • ⇒ Different systematics across relation ( σ ★ , mass, Hubble type, … ) ⇒ Highly biased sample (McConnell & Ma 13) (compact cores / high SB) ⇒ Need for unique method (all types), conceptually simple (no systematics), easily scalable (rapid) Martin Bureau, University of Oxford

M Ÿ - σ ★ Relation: Biases Weaknesses: M Ÿ - σ ★ : Still relatively few measurements • Handful of methods • Each method has own weaknesses • and systematics Methods çè targets highly correlated • ⇒ Different systematics across relation ( σ ★ , mass, Hubble type, … ) (van den Bosch) ⇒ Highly biased sample (compact cores / high SB) ⇒ Need for unique method (all types), conceptually simple (no systematics), easily scalable (rapid) Martin Bureau, University of Oxford

(Dark) Mass Measurements Basis: Dark matter (galaxies): F = m a G M m / R 2 = m v 2 / R è M α v 2 R è v α M ½ / R ½ Ø Need tracer(s) over large range of radii Martin Bureau, University of Oxford

(Dark) Mass Measurements Basis: Black holes (nuclei): F = m a G M m / R 2 = m v 2 / R è M α v 2 R è v α M ½ / R ½ Ø Need very high angular resolution Martin Bureau, University of Oxford

(Dark) Mass Measurements Basis: Dark matter + black holes: F = m a G M m / R 2 = m v 2 / R è M α v 2 R è v α M ½ / R ½ Ø Need very high angular resolution Martin Bureau, University of Oxford

WISDOM: Weighing Supermassive Black Holes Across the Hubble Sequence Martin Bureau, Oxford University WISDOM Team (Leo Blitz, Michele Cappellari, Timothy Davis, Satoru Iguchi, Lijie Liu, Eve North, Kyoko Onishi, Marc Sarzi, Mark Smith) Poster - North: WISDOM: Do we have it to constrain SMBH masses? Poster - Smith: WISDOM: Modelling molecular gas observations in NGC4429 and NGC4501 to measure the SMBH mass Plans: Introduction: M BH - σ ★ correlation, SMBH signature SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations Martin Bureau, University of Oxford

CO: NGC 4526 SMBH mass (Davis et al. 2013) HST WFC3 NUV-optical data: SDSS colour image: (Kaviraj et al.) (SDSS) BIMA low-res (4.5”) data: Martin Bureau, University of Oxford

CO: NGC 4526 SMBH mass (Davis et al. 2013) CARMA high-res (0.25” = 20 pc) data: NGC4526: High resolution (0.25”) • CARMA CO(2-1) data Regular (central) disk • kinematics Free M/L ★ and M Ÿ • BIMA low-res (4.5”) data: ⇒ Strong constraints on M Ÿ (M Ÿ = 4.1 x 10 8 M ¤ ) (consistent with M Ÿ - σ ★ ) ⇒ Great prospects across Hubble sequence with ALMA … Martin Bureau, University of Oxford

CO: NGC 4526 SMBH mass (Davis et al. 2013) Model PVD and major-axis trace: Velocity Position Martin Bureau, University of Oxford

CO: WISDOM SMBH “Pipeline”: HST image: IRAM 30m spectrum: 1) Identify promising targets (HST optical imaging) 2) Verify CO content (CO single-dish) 3) Obtain moderate CARMA CO: resolution CO imaging (mm interferometry) 4) Pursue (very) high resolution CO imaging (mm interferometry) ⇒ Get SMBH masses via dynamical modelling (See also work of Barth et al. on massive galaxies) Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass (Davis et al. 2017b) HST optical data: ALMA high-res data: V CO CO CO(2-1) σ CO SMBH: ALMA: • M Ÿ ≈ 1.5 x 10 8 M ¤ CO(3-2) • 0.18” x 0.14” (13 pc) (consistent with M Ÿ - σ ★ ) • ² Strong constraint on spatially varying stellar M/L ratio Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass (Davis et al. 2017b) ALMA CO PVD - Models: SMBH: ALMA: • M Ÿ ≈ 1.5 x 10 8 M ¤ CO(3-2) • 0.18” x 0.14” (13 pc) (consistent with M Ÿ - σ ★ ) • ² Strong constraint on spatially varying stellar M/L ratio Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass (Davis et al. 2017b) Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass (Davis et al. 2017b) Formal uncertainty on M Ÿ and stellar M/L M/L ★ ~ 1% M BH Martin Bureau, University of Oxford

ALMA Cycle 3 Massive: Normal: Dwarfs: Martin Bureau, University of Oxford

CO: NGC 4697 SMBH mass (Davis et al. 2017a) ALMA moderate -res (0.53” = 29 pc) data: Martin Bureau, University of Oxford

CO: NGC 4697 SMBH mass (Davis et al. 2017a) ALMA moderate -res (0.53” = 29 pc) data: NGC4697: ⇒ Strong constraints on M Ÿ Moderate resolution ALMA • (M Ÿ = 1.3 x 10 8 M ¤ ) CO(2-1) ⇒ Essentially independent of Regular disk kinematics • M/L ★ and all galaxy parameters Free M/L ★ and M Ÿ • Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass (North et al., in prep.) Radio: large ALMA: HL Tau Radio: small HST: small ? ALMA PVD prediction: Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass (North et al., in prep.) ALMA: HL Tau ALMA: CO(2-1) ALMA: velocity 0.13” (43 pc) Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass (North et al., in prep.) ALMA: HL Tau ALMA: CO(2-1) ALMA: velocity 0.13” (43 pc) ALMA PVD: 0.13” (43 pc) Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass (North et al., in prep.) ALMA: HL Tau ALMA: CO(2-1) ALMA: velocity 0.13” (43 pc) ALMA PVD: stars only BH + stars BH only Martin Bureau, University of Oxford

ALMA Cycle 3 + 4 V CO CO Martin Bureau, University of Oxford

ALMA Cycle 3 + 4 CO V CO Martin Bureau, University of Oxford

ALMA Cycle 3 + 4 CO V CO Martin Bureau, University of Oxford

WISDOM: Weighing Supermassive Black Holes Across the Hubble Sequence Martin Bureau, Oxford University WISDOM Team (Leo Blitz, Michele Cappellari, Timothy Davis, Satoru Iguchi, Lijie Liu, Eve North, Kyoko Onishi, Marc Sarzi, Mark Smith) Poster - North: WISDOM: Do we have it to constrain SMBH masses? Poster - Smith: WISDOM: Modelling molecular gas observations in NGC4429 and NGC4501 to measure the SMBH mass Plans: Introduction: M BH - σ ★ correlation, SMBH signature SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations Martin Bureau, University of Oxford

SMBHs: GMC studies (free!) (Utomo et al. 15) Cloud identification: Spatially-resolved MDFs: GMC populations: Cloud statistics / MDFs • Larson relations • Support / timescales Larson relations: • Shear / rotation • KS law / star formation • … • ⇒ Milky Way-like studies in Dynamics: Support: external galaxies ⇒ Comparison to other galaxies (expanded parameter space) Martin Bureau, University of Oxford

Molecular Gas (CO) SMBH Measurements Arguments: PVDs: Applicable across Hubble sequence, • active and non-active galaxies • Conceptually simple Rapid (ALMA) • • Proof of concept / pilot studies done ⇒ Method ripe for large-scale exploitation Statistics: ALMA: ⇒ 100s measurements trivial (>10 5 possible ; same systematics) ⇒ Revolution in studies of M Ÿ - σ ★ relation (BHs and galaxies co-evolution) Martin Bureau, University of Oxford