AGN driven outflows in dwarf galaxies Christina Manzano-King With - - PowerPoint PPT Presentation

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agn driven outflows in dwarf galaxies
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AGN driven outflows in dwarf galaxies Christina Manzano-King With - - PowerPoint PPT Presentation

Aug 05, 2023 392 likes •557 views

AGN driven outflows in dwarf galaxies Christina Manzano-King With Gabriela Canalizo and Laura V. Sales UC Riverside Small Galaxies, Cosmic Questions 30 July 2019 The background ...and AGN? AGN are present and possibly common in dwarf

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SLIDE 1

AGN driven outflows in dwarf galaxies

Christina Manzano-King

With Gabriela Canalizo and Laura V. Sales

UC Riverside Small Galaxies, Cosmic Questions 30 July 2019

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SLIDE 2
  • AGN are present and possibly

common in dwarf galaxies

(Reines+2013, Moran+2014, Sartori+2015)

  • Theory work suggests AGN

feedback could be important (Silk

2017, Dashyan+2017, Barai+2018, Koudmani+2019)

  • Recent evidence that quiescence

and AGN coexist (Penny+2018,

Bradford+2018, Dickey+2019)

The background

...and AGN?

And Reionization

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SLIDE 3

Our work

  • 50 dwarf galaxies

○

29 AGN (Reines+2013, Moran+2014, Sartori+2015)

○

21 SF (control sample from SDSS)

  • LRIS longslit on Keck I

BPT Diagram AGN Star Forming LMC SMC

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SLIDE 4

The data

  • utflow?
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SLIDE 5

Identifying outflows

σ > 80 km/s

arXiv:1905.09287

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SLIDE 6

9 AGN 4 star forming

13 Dwarfs with Galaxy-Wide Outflows

arXiv:1905.09287

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SLIDE 7

Difgerent Line Profiles

  • Blueshifted
  • Larger fraction (up to 50%) of [O III] flux
  • Symmetrical
  • Smaller fraction (4-8%) of [O III] flux

AGN Star Forming

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SLIDE 8

Difgerent Outflow Origins?

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SLIDE 9

Outflow Ionization

  • utflow

arXiv:1905.09287

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SLIDE 10

Star Forming C

  • m

p

  • s

i t e AGN arXiv:1905.09287

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SLIDE 11

Star Forming C

  • m

p

  • s

i t e AGN Plus, their line profiles tend to be blueshifted

( t

  • f

a i n t )

arXiv:1905.09287

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SLIDE 12

Star Forming C

  • m

p

  • s

i t e AGN Plus, both of their line profiles are symmetric arXiv:1905.09287

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SLIDE 13

Fate of the gas?

  • Points are scaled by % of [O III]

flux in outflow component

  • vesc is an upper limit

1:1

arXiv:1905.09287

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SLIDE 14

Tying outflows to the AGN -- IR

  • Most outflow galaxies hosting AGN have Si[IV]
  • Line ratios strongly exclude shocks as ionizing mechanism for gas in IR
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SLIDE 15

Possible star formation suppression?

arXiv:1905.09287

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SLIDE 16

In Summary,

  • Outflows detected in 9/29 AGN and 4/21 SF dwarfs
  • Differences in line profiles suggest origin

○ Blueshifted outflow implies central source with obscurration ○ Symmetrical outflow implies unobscured sources

  • Emission line diagnostics indicate AGN-like ionization in at least 6 galaxies
  • Outflow velocities exceed escape velocities in all cases
  • Evidence suggestive of feedback:

○ AGN-driven outflows tend to carry a higher fraction of emission line flux than SF (5-50%) vs. (4-8%) ○ Outflows carrying a larger fraction of [OIII] flux tend to populate redder galaxies ○ Placement on color-mass diagram is suggestive of ongoing star formation suppression arXiv:1905.09287