Quenching in the Green Valley (Preliminary Work) Joanna Woo Advisor: Avishai Dekel Hebrew University...
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Transcript of Quenching in the Green Valley (Preliminary Work) Joanna Woo Advisor: Avishai Dekel Hebrew University...
Quenching in the Green Valley(Preliminary Work)
Joanna WooAdvisor: Avishai Dekel
Hebrew University of Jerusalem
Motivation
Galaxy Bimodality Presumably BC galaxies are quenched and form
RS galaxies Then GV galaxies are still being quenched
What can the GV tell us about quenching mechanisms?
Quenching in GalICS
Hybrid N-body (DM) + SAM Each galaxy has 3 components: disc, bulge, burst Stars form as a function of M
cold / t
dyn
Quenching happens in two ways: During mergers and periods of disc instability, stars
+ gas from the disc move to the burst and then to the bulge (causes bulge to grow, and depletes disc of gas) → BULGE QUENCHING
If a halo grows above 2x1012 M⊙ all SF is shutdown by hand → HALO QUENCHING
Questions
Which quenching mechanisms dominate in which eras?
How does the GalICS SAM compare with the real universe? (SDSS, AEGIS)
Green Valley
The galaxy bimodality is characterised by two sequences: the Red Sequence and the Star Forming sequence
Define GV to be those that are NOT in the RS, and not in the SF sequence
Data
SDSS: Colours: KCORRECT on ugriz (Cooper et al. 2007) SFR: GALEX (Salim et al. 2007) M
*: (Kauffmann et al 2002)
C=R90/R50: sdss website M
halo: (Yang et al. 2008)
AEGIS: Colours: KCORRECT on BRI from Coil et al. 2004 (Cooper et al.
2007) SFR: GALEX (Salim et al. 2009) M
*: SED fits to optical/NIR photometry (Bundy et al. 2006)
B/T: (Simard et al 2002 – kindly provided by David Koo)
Summary of Preliminary Results
At z~0, bulge-quenching is the dominant quenching mechanism in the GV Affects smaller galaxies The GalICS SAM and the SDSS agree
At z~1, halo-quenching was the dominant quenching mechanism in the GV Affects larger galaxies True in GalICS, not enough data in AEGIS
Still to Think About
Better GV sample? In GalICS, bulge-quenching resulted from both
mergers and disc-instability Easy to separate in GalICS. How about in data?
Halo masses for AEGIS? Apply Yang et al method?