Feedback in the Nuclei of Mrk 273 Luminous Infrared Galaxies (not - - PowerPoint PPT Presentation

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Jul 16, 2023 182 likes •388 views

Feedback in the Nuclei of Mrk 273 Luminous Infrared Galaxies (not to scale) Vivian U Chancellors Postdoctoral Fellow UC Riverside / UC Irvine GalFRESCA2017, Caltech Observation Feedback Theory Galaxy mergers are prime targets to

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Feedback in the Nuclei of Luminous Infrared Galaxies

Vivian U

Chancellor’s Postdoctoral Fellow UC Riverside / UC Irvine GalFRESCA2017, Caltech

Mrk 273 (not to scale)

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Observation ß Feedback à Theory

Galaxy mergers are prime targets to investigate how SMBHs

grow and coalesce.

Small-scale gas dynamics in the nuclei of mergers trace BH

growth and feedback processes as a function of merger sequence.

Observations and simulations of comparable spatial

resolution work hand-in-hand to help us understand the physical processes in detail.

SLIDE 3

e.g. Sanders+88, Hopkins+08

Post-starbursts

Me Merger-dr driven n scena nario

f galaxy evo volution

Early-stage mergers Late-stage mergers Post mergers / Quasars

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e.g. Sanders+88, Hopkins+08

Post-starbursts Early-stage mergers Late-stage mergers Post mergers / Quasars Star Formation Rate Black Hole Growth

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Galactic Ecosystem

AGN / nuclear SF Supernovae Expel gas / Quench SF ISM/GMC Star Formation Outflows / Winds Cool gas Inflows / Turbulence

Giant Molecular Clouds = Stellar Nursery Supernova Galactic winds in M82 Gas inflows AGN

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Black holes ← Gas → Galaxies

Feeding: gas fuels central nuclear activity
How do SMBH grow in the heart of merging systems?

➤ SMBH grow rapidly (~109 M¤) in gas-rich mergers (Medling, U+ 2015b)

Feedback: fate of outflowing gas or winds
How does gas feedback affect subsequent nuclear star formation?

Ke Key Questions

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How feedback transforms galaxies

Large-scale galactic winds are prevalent in ULIRGs.
Still lack conclusive evidence on their origin and effect at small

scales – key to understanding how galaxies evolve. à Need observations of spatially-resolved gas dynamics!

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The Keck OSIRIS AO LIRGs Analysis (KOALA) Survey

Our goal is to study nuclear gas dynamics in a statistical sample of galaxy mergers in order to trace black hole growth and feedback processes as a function of the merger sequence.

Leads: Vivian U (UCR/UCI), Anne Medling (ANU/Caltech)

Co-Is: Lee Armus (Caltech/IPAC), Jeff Rich (Carnegie), George Privon (PUC/UF), Dave Sanders (UH), Claire Max (UCSC), Aaron Evans (UVa/NRAO), Jake Borish (UVa), Gaby Canalizo (UCR), Lisa Kewley (ANU), Joe Mazzarella (Caltech/IPAC), Jason Surace (Caltech/IPAC), Hanae Inami (Lyon), Sabrina Stierwalt (NRAO), and the GOALS Team

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Our sample consists of nearby galaxy mergers at a redshift of z < 0.08, or ~350 Mpc.

MCG+08 IR03359 NGC6090 NGC2623 IR20351 CGCG436 UGC8387 IIIZw035 IR01364 VV340a UGC5101 UGC8696 IR17207 UGC8058

NGC7674

NGC7469 IR6076 NGC6670 IR15250 IR22491

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OSIRIS: near-infrared integral field spectrograph (IFS)

x y λ

AO-assisted
Sampling at 0.020" – 0.1" / px; 0.035"/px à 20-60 pc/px

(for comparison, HST WFC3: 0.13" / px in the IR)

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CO bandheads H2 H2 H2 Brγ HeI H2 [Si VI] H2 Brδ CaI

Typical K-band spectrum for (U)LIRGs

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Late-stage merging ULIRG
Multi-clump system with (at least) 1 AGN

Case study: Mrk 273

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Mrk 273

(K band; U+ 2013, ApJ, 775, 115)

N SW SE

400 pc

X

0.5"

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Mrk 273: H2

Direct observational evidence for biconical molecular outflows

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Mrk 273: H2 outflow properties

V ~ 200 km/s
MH2 = 7.7 x 103 M¤
Age of outflow ~ 3.3 Myr
Outflow power ~ 1.3 x 1043 erg/s

Quantitative comparisons to simulations

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Excitation Mechanisms of H2

U+ 2017 (in prep.)

Thermal Nonthermal Temperature

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What effect does feedback have on the ISM?

IR luminosity Shock-excited H2 Turbulent H2 Nuclear Star Formation Rate