Nearby Galaxies as measures of Feedback Brent Groves (MPIA) - - PowerPoint PPT Presentation

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Nearby Galaxies as measures of Feedback Brent Groves (MPIA) - - PowerPoint PPT Presentation

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Nearby Galaxies as measures of Feedback Brent Groves (MPIA) Quenching & Quiescence MPIA, Heidelberg July 14-18, 2014 Why Nearby? In nearby galaxies we can resolve the physics of feedback processes (J. Gallaghers talk)

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Nearby Galaxies as measures of Feedback

Brent Groves (MPIA)

Quenching & Quiescence MPIA, Heidelberg July 14-18, 2014

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Brent Groves

Why Nearby?

  • In nearby galaxies we can resolve the physics of

feedback processes (J. Gallagher’s talk)

  • Proximity means faint structures can be seen (T.

Davis’ Talk)

  • Measure the gas reservoir, stars, star formation, and

winds directly

  • See Quenching in progress
  • See how Quiescence is maintained
  • Nearest example: M31!
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SLIDE 3

Stellar View of Andromeda

Ultraviolet Optical Near-IR

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SLIDE 4

Brent Groves

Dust & Gas!

CO data: Nieten et al. (2006) Hα data: Winkler et al.

PACS 160μm SPIRE 500μm

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SLIDE 5

Brent Groves

Integrated Andromeda

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SLIDE 6

Brent Groves

Integrated Andromeda

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SLIDE 7

Brent Groves

Integrated Andromeda

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SLIDE 8

Brent Groves

Quenching in Progress?

  • Nearby (780 kpc) L* galaxy
  • Early type inclined (70o) spiral
  • Occupies “green valley”

Brinchmann et al. (2004)

log M* ~10.8 Mo

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SLIDE 9

Brent Groves

Quenching in Progress?

  • Nearby (780 kpc) L* galaxy
  • Early type inclined (70o) spiral
  • Occupies “green valley”

Brinchmann et al. (2004)

log M* ~10.8 Mo

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SLIDE 10

Brent Groves

Mass outward

Tamm et al. (2012)

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SLIDE 11

Brent Groves

Mass outward

Tamm et al. (2012)

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SLIDE 12

Brent Groves

Mass outward

Tamm et al. (2012)

log10 M200 = 12.3

Fardal et al. (2013)

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SLIDE 13

Brent Groves

Cause of Quenching?

  • M31* hosts a SMBH
  • no indication of activity over

last ~ Myr

  • Suggested major merger ~5

Gyrs ago (Hammer et al. (2013)

  • Other indications?
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SLIDE 14

Streams of Stars

The Pan-Andromeda Archaeological Survey Colour shows stellar surface density

McConnachie et al. (2009)

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SLIDE 15

Streams of Stars

The Pan-Andromeda Archaeological Survey

M33

Colour shows stellar surface density

McConnachie et al. (2009)

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SLIDE 16

Streams of Stars

The Pan-Andromeda Archaeological Survey

M33 And XIX

Colour shows stellar surface density

McConnachie et al. (2009)

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SLIDE 17

Streams of Stars

The Pan-Andromeda Archaeological Survey

M33 And XIX

Colour shows stellar surface density

McConnachie et al. (2009)

log10 M200 = 12.3

Fardal et al. (2013)

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SLIDE 18

Quenched by Harassment?

Stars Dust

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SLIDE 19

Quenched by Harassment?

Stars Dust

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SLIDE 20

Quenched by Harassment?

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SLIDE 21

Quenched by Harassment?

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SLIDE 22

Extended HI - Starvation?

  • HI still extended

around M31

  • but shows

interaction with M33

Lewis et al. (2013)

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SLIDE 23

Quiescence

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SLIDE 24

Quiescence

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SLIDE 25

Quiescence

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Quiescence?

  • SED suggests no

SFR (< 10-2 Mo/yr)

  • sSFR < 0.01 Gyr-1
  • Extremely old (>6

Gyr)

  • Dust heated

predominantly by

  • ld stars!

Groves et al. (2013)

Mbulge ~ 1010 Mo

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SLIDE 27 14 29 43 58 72 87 101 116 130 145

There is gas...

Hα

  • Mdust ~ 105 Mo
  • Mgas ~106.8 Mo
  • most of this in cool phase

PACS100

Kapala et al. (in prep)

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SLIDE 28 14 29 43 58 72 87 101 116 130 145

There is gas...

Hα

  • Mdust ~ 105 Mo
  • Mgas ~106.8 Mo
  • most of this in cool phase

PACS100

Kapala et al. (in prep)

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SLIDE 29 14 29 43 58 72 87 101 116 130 145

There is gas...

Hα

  • Mdust ~ 105 Mo
  • Mgas ~106.8 Mo
  • most of this in cool phase

Melchior et al. (2011)

PACS100

Kapala et al. (in prep)

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SLIDE 30

Gas heating

  • Ionized gas follows

dust

  • but shows LINER-like

ratios (R. Singh’s talk)

  • Shocks may be

present, but not dominant based on line widths

Hα

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SLIDE 31

Gas heating

  • Ionized gas follows

dust

  • but shows LINER-like

ratios (R. Singh’s talk)

  • Shocks may be

present, but not dominant based on line widths

Hα

Ciardullo et al. (1988)

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SLIDE 32

UV heating?

  • Resolved stars (& UV light)

dominated by extreme horizontal branch

Rosenfield et al. (2012)

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SLIDE 33

UV heating?

F336W F275W

  • Resolved stars (& UV light)

dominated by extreme horizontal branch

Rosenfield et al. (2012)

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SLIDE 34

UV heating?

3.5 4.0 4.5 5.0

log Teff (K )

1.0 1.5 2.0 2.5 3.0 3.5 4.0

log L (L )

F336W F275W

  • Resolved stars (& UV light)

dominated by extreme horizontal branch

Rosenfield et al. (2012)

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X-ray heating

  • Large number of low mass X-ray binaries
  • Diffuse X-ray gas heated by SNI

Li & Wang (2009)

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X-ray heating

  • Large number of low mass X-ray binaries
  • Diffuse X-ray gas heated by SNI

Bogdán & Gilfanov(2008) (& A. Bogdan, and M. Gilfanov’s talk) Li & Wang (2009)

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Keeping it hot?

  • X-rays will provide diffuse heating deep in

the gas (X-ray ionization)

  • P-AGB and EHB provide a low level EUV

field to also ionize (P. Marigo & winds.. J. Bregman’s talk)

  • CO line widths suggest dynamically hot...

Li & Wang (2009)

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Brent Groves

QnQ in M31

  • Nearby galaxies can give insight into the physical

processes proposed for quenching galaxies and keeping them quiescent

  • M31 appears to be in the process of being quenched
  • The bulge of M31 is a perfect test bed for some of

the processes of keeping galaxies dead

Quenching & Quiescence

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SLIDE 39

Brent Groves

Unattenuated stellar spectrum Dust absorption cross-section Bulge dust heating SED

S t a r s

  • Bulge stars so old

(red)

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Brent Groves

Unattenuated stellar spectrum Dust absorption cross-section Bulge dust heating SED

S t a r s D u s t

  • Bulge stars so old

(red)

  • Even with Steep dust
  • pacity
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Brent Groves

Unattenuated stellar spectrum Dust absorption cross-section Bulge dust heating SED

S t a r s D u s t S t a r s X D u s t

  • Bulge stars so old

(red)

  • Even with Steep dust
  • pacity
  • Optical light

dominates dust heating

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SLIDE 42

Brent Groves

Bulge Heating?

  • Steep inner Tdust slope

suggests bulge dominated heating

  • Optical-UV colours

suggest old pop. and little dust (as shown by IR)

  • Assume
  • optically thin
  • constant M/L
  • diffuse dust
  • Td∝U*1/6

νbulge ∝

1 (r/rb)(1+r/rb)3

U∗ = νbulge ⊗ 1/r2

Tdust,U 0.8 Tdust,U Tdust (K) pixel number density

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Brent Groves

Central Stars and Outer Disk

  • M31 bulge dominated in inner ~2kpc
  • Only at blue-UV and 8m (dust) is outer ring clearly visible

Courteau et al. (2011) Geehan et al. (2006)

Bulge Disk Lauer et al. (1993) Kent (1983) Walterbos & Kennicutt (1987) Global Light Profile

0.001 0.01 0.1 1 10 100 24 23 22 21 20 19 18 17 16 15 14 13