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. 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! Brent Groves
Stellar View of Andromeda Ultraviolet Optical Near-IR
Dust & Gas! PACS 160 μ m H α data: Winkler et al. SPIRE 500 μ m CO data: Nieten et al. (2006) Brent Groves
Integrated Andromeda Brent Groves
Integrated Andromeda Brent Groves
Integrated Andromeda Brent Groves
Quenching in Progress? • Nearby (780 kpc) L * galaxy • Early type inclined (70 o ) spiral • Occupies “green valley” log M * ~10.8 M o Brinchmann et al. (2004) Brent Groves
Quenching in Progress? • Nearby (780 kpc) L * galaxy • Early type inclined (70 o ) spiral • Occupies “green valley” log M * ~10.8 M o Brinchmann et al. (2004) Brent Groves
Mass outward Tamm et al. (2012) Brent Groves
Mass outward Tamm et al. (2012) Brent Groves
Mass outward log 10 M 200 = 12.3 Fardal et al. (2013) Tamm et al. (2012) 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? Brent Groves
Streams of Stars The Pan-Andromeda Archaeological Survey Colour shows stellar surface density McConnachie et al. (2009)
Streams of Stars The Pan-Andromeda Archaeological Survey Colour shows stellar surface density M33 McConnachie et al. (2009)
Streams of Stars The Pan-Andromeda Archaeological Survey Colour shows stellar surface density And XIX M33 McConnachie et al. (2009)
Streams of Stars The Pan-Andromeda Archaeological Survey Colour shows stellar surface density And XIX M33 log 10 M 200 = 12.3 Fardal et al. (2013) McConnachie et al. (2009)
Quenched by Harassment? Stars Dust
Quenched by Harassment? Stars Dust
Quenched by Harassment?
Quenched by Harassment?
Extended HI - Starvation? • HI still extended around M31 • but shows interaction with M33 Lewis et al. (2013)
Quiescence
Quiescence
Quiescence
Quiescence? • SED suggests no M bulge ~ 10 10 M o SFR (< 10 -2 M o /yr) • sSFR < 0.01 Gyr -1 • Extremely old (>6 Gyr) • Dust heated predominantly by old stars! Groves et al. (2013)
There is gas... • M dust ~ 10 5 M o • M gas ~10 6.8 M o • most of this in cool phase PACS100 H α Kapala et al. (in prep) 0 14 29 43 58 72 87 101 116 130 145
There is gas... • M dust ~ 10 5 M o • M gas ~10 6.8 M o • most of this in cool phase PACS100 H α Kapala et al. (in prep) 0 14 29 43 58 72 87 101 116 130 145
There is gas... • M dust ~ 10 5 M o • M gas ~10 6.8 M o • most of this in cool phase Melchior et al. (2011) PACS100 H α Kapala et al. (in prep) 0 14 29 43 58 72 87 101 116 130 145
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 H α
Gas heating • Ionized gas follows dust • but shows LINER-like ratios (R. Singh’s talk) Ciardullo et al. (1988) • Shocks may be present, but not dominant based on line widths H α
UV heating? Rosenfield et al. (2012) • Resolved stars (& UV light) dominated by extreme horizontal branch
UV heating? Rosenfield et al. (2012) F336W F275W • Resolved stars (& UV light) dominated by extreme horizontal branch
UV heating? Rosenfield et al. (2012) 4 . 0 3 . 5 F336W 3 . 0 log L ( L ) 2 . 5 F275W 2 . 0 1 . 5 1 . 0 5 . 0 4 . 5 4 . 0 3 . 5 log T eff ( K ) • Resolved stars (& UV light) dominated by extreme horizontal branch
X-ray heating Li & Wang (2009) • Large number of low mass X-ray binaries • Diffuse X-ray gas heated by SNI
X-ray heating Li & Wang (2009) Bogdán & Gilfanov(2008) (& A. Bogdan, and M. • Large number of low mass X-ray binaries Gilfanov’s talk) • Diffuse X-ray gas heated by SNI
Keeping • X-rays will provide diffuse heating deep in the gas (X-ray ionization) it hot? • 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)
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 Brent Groves
• Bulge stars so old s r (red) a t S Unattenuated stellar spectrum Dust absorption cross-section Bulge dust heating SED Brent Groves
• Bulge stars so old s r (red) a t S Unattenuated stellar spectrum Dust absorption cross-section • Even with Steep dust t s u opacity D Bulge dust heating SED Brent Groves
• Bulge stars so old s r (red) a t S Unattenuated stellar spectrum Dust absorption cross-section • Even with Steep dust t s u opacity D t s u • Optical light D dominates dust X s heating r a Bulge dust heating SED t S Brent Groves
Bulge Heating? 1 • Steep inner T dust slope ν bulge ∝ ( r/r b )(1+ r/r b ) 3 suggests bulge dominated U ∗ = ν bulge ⊗ 1 /r 2 heating • Optical-UV colours T dust,U suggest old pop. and little 0.8 T dust,U dust (as shown by IR) pixel number density • Assume • optically thin T dust (K) • constant M/L • diffuse dust • T d ∝ U * 1/6 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) 13 Lauer et al. (1993) 14 Kent (1983) 15 Walterbos & Kennicutt (1987) 16 17 Global Light Profile 18 Disk 19 20 Bulge 21 22 23 24 0.001 0.01 0.1 1 10 100 Brent Groves
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