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

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

Jul 12, 2023 249 likes •566 views

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 -

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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: MBH - σ★ correlation, SMBH signature

SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations

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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: MBH - σ★ correlation, SMBH signature

SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations

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Martin Bureau, University of Oxford

MŸ- σ★ Relation: Status

MŸ- σ★:

SMBH Masses:

  • ≈ 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

  • Essential to framework of (high-mass)

galaxy formation ⇒ Central to much current astrophysics (AGN feedback)

(McConnell & Ma 13)

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Martin Bureau, University of Oxford MŸ- σ★:

Weaknesses:

  • 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 (compact cores / high SB) ⇒ Need for unique method (all types), conceptually simple (no systematics), easily scalable (rapid)

MŸ- σ★ Relation: Biases

(McConnell & Ma 13)

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Martin Bureau, University of Oxford MŸ- σ★:

(van den Bosch)

Weaknesses:

  • 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 (compact cores / high SB) ⇒ Need for unique method (all types), conceptually simple (no systematics), easily scalable (rapid)

MŸ- σ★ Relation: Biases

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Martin Bureau, University of Oxford

(Dark) Mass Measurements

Basis:

F = m a G M m / R2 = m v2 / R è M α v2 R è v α M½ / R½

Dark matter (galaxies):

Ø Need tracer(s) over large range of radii

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Martin Bureau, University of Oxford

(Dark) Mass Measurements

Basis:

F = m a G M m / R2 = m v2 / R è M α v2 R è v α M½ / R½

Black holes (nuclei):

Ø Need very high angular resolution

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Martin Bureau, University of Oxford

(Dark) Mass Measurements

Basis:

F = m a G M m / R2 = m v2 / R è M α v2 R è v α M½ / R½

Dark matter + black holes:

Ø Need very high angular resolution

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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: MBH - σ★ correlation, SMBH signature

SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations

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Martin Bureau, University of Oxford HST WFC3 NUV-optical data: BIMA low-res (4.5”) data:

CO: NGC 4526 SMBH mass

(Davis et al. 2013)

SDSS colour image:

(SDSS) (Kaviraj et al.)

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Martin Bureau, University of Oxford

NGC4526:

  • High resolution (0.25”)

CARMA CO(2-1) data

  • Regular (central) disk

kinematics

  • Free M/L★ and MŸ

⇒ Strong constraints on MŸ (MŸ = 4.1 x 108 M¤) (consistent with MŸ - σ★) ⇒ Great prospects across Hubble sequence with ALMA… BIMA low-res (4.5”) data: CARMA high-res (0.25” = 20 pc) data:

CO: NGC 4526 SMBH mass

(Davis et al. 2013)

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Martin Bureau, University of Oxford

Position Velocity

Model PVD and major-axis trace:

CO: NGC 4526 SMBH mass

(Davis et al. 2013)

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Martin Bureau, University of Oxford HST image: CARMA CO:

SMBH “Pipeline”:

1) Identify promising targets (HST optical imaging) 2) Verify CO content (CO single-dish) 3) Obtain moderate resolution CO imaging (mm interferometry) 4) Pursue (very) high resolution CO imaging (mm interferometry) ⇒ Get SMBH masses via dynamical modelling

CO: WISDOM

IRAM 30m spectrum:

(See also work of Barth et al. on massive galaxies)

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Martin Bureau, University of Oxford

CO VCO σCO

ALMA:

  • CO(3-2)
  • 0.18” x 0.14” (13 pc)

CO: NGC 4429 SMBH mass

(Davis et al. 2017b)

ALMA high-res data:

CO(2-1)

SMBH:

  • MŸ ≈ 1.5 x 108 M¤

(consistent with MŸ- σ★)

² Strong constraint on spatially

varying stellar M/L ratio HST optical data:

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Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass

(Davis et al. 2017b)

ALMA CO PVD - Models:

ALMA:

  • CO(3-2)
  • 0.18” x 0.14” (13 pc)

SMBH:

  • MŸ ≈ 1.5 x 108 M¤

(consistent with MŸ- σ★)

² Strong constraint on spatially

varying stellar M/L ratio

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Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass

(Davis et al. 2017b)

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Martin Bureau, University of Oxford

CO: NGC 4429 SMBH mass

(Davis et al. 2017b)

Formal uncertainty

  • n MŸ and stellar M/L

~ 1% MBH M/L★

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Martin Bureau, University of Oxford

ALMA Cycle 3

Massive: Normal: Dwarfs:

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Martin Bureau, University of Oxford

CO: NGC 4697 SMBH mass

(Davis et al. 2017a)

ALMA moderate-res (0.53” = 29 pc) data:

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Martin Bureau, University of Oxford NGC4697:

  • Moderate resolution ALMA

CO(2-1)

  • Regular disk kinematics
  • Free M/L★ and MŸ

ALMA moderate-res (0.53” = 29 pc) data:

CO: NGC 4697 SMBH mass

(Davis et al. 2017a)

⇒ Strong constraints on MŸ (MŸ = 1.3 x 108 M¤) ⇒ Essentially independent of M/L★ and all galaxy parameters

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Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass

(North et al., in prep.)

HST: small Radio: large Radio: small ALMA PVD prediction: ALMA: HL Tau

?

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Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass

(North et al., in prep.)

ALMA: velocity ALMA: CO(2-1) ALMA: HL Tau

0.13” (43 pc)

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Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass

(North et al., in prep.)

ALMA: velocity ALMA: CO(2-1) ALMA: HL Tau ALMA PVD:

0.13” (43 pc)

0.13” (43 pc)

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Martin Bureau, University of Oxford

CO: NGC 383 SMBH mass

(North et al., in prep.)

ALMA: velocity ALMA: CO(2-1) ALMA: HL Tau ALMA PVD:

BH + stars stars only BH only

0.13” (43 pc)

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Martin Bureau, University of Oxford

ALMA Cycle 3 + 4

CO

VCO

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Martin Bureau, University of Oxford

ALMA Cycle 3 + 4

CO

VCO

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Martin Bureau, University of Oxford

ALMA Cycle 3 + 4

CO

VCO

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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: MBH - σ★ correlation, SMBH signature

SMBHs: Pilot observations, ALMA and WISDOM Conclusions: SMBHs prospects, GMC populations

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Martin Bureau, University of Oxford Larson relations:

Spatially-resolved GMC populations:

  • Cloud statistics / MDFs
  • Larson relations
  • Support / timescales
  • Shear / rotation
  • KS law / star formation
  • …

⇒ Milky Way-like studies in external galaxies ⇒ Comparison to other galaxies (expanded parameter space) Cloud identification:

SMBHs: GMC studies (free!)

(Utomo et al. 15)

Support: Dynamics: MDFs:

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Martin Bureau, University of Oxford PVDs:

Arguments:

  • 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

ALMA:

⇒ 100s measurements trivial (>105 possible ; same systematics) ⇒ Revolution in studies of MŸ - σ★ relation (BHs and galaxies co-evolution)

Molecular Gas (CO) SMBH Measurements

Statistics: