Download (if any) Galaxy Properties Depend on Environment at High Redshift?

What (if any) Galaxy Properties
Depend on Environment
at High Redshift?
Casey Papovich
Texas A&M University
George P. and Cynthia Woods Mitchell
Institute for Fundamental Physics and Astronomy
Lalitwadee (Nancy) Kawinwanichakij
(Texas A&M)
Ryan Quadri (Texas A&M)
and collaborators on CANDELS and
ZFOURGE teams
High-z Protoclusters
Observatoire de Paris
2016 Oct 5
star-formation — density relation out to z~1.8
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
…galaxies with quenched [star-formation] … reside
in dense environments out to at least z~1.8. …
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
…galaxies with quenched [star-formation] … reside
in dense environments out to at least z~1.8. …
galaxy density
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
…galaxies with quenched [star-formation] … reside
in dense environments out to at least z~1.8. …
Darvish+16
galaxy density
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
…galaxies with quenched [star-formation] … reside
in dense environments out to at least z~1.8. …
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
… environmental quenching of [star formation has
… ] similar efficiency on all galaxies regardless of
stellar mass. …
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
star-formation — density relation out to z~1.8
… environmental quenching of [star formation has
… ] similar efficiency on all galaxies regardless of
stellar mass. …
Casey Papovich
galaxy
density
High-z (proto)-clusters
2016 Oct 5
Questions I would like to see discussed:
– How does the SF-density relation evolve?
– Is environmental quenching efficiency invariant
with galaxy mass?
– What drives these relations? Gain insight by:
– testing for galaxy properties that vary with
environment?
– When (at what epoch) do they manifest?
– over what timescale(s) do the effects act?
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
Straatman, Labbé, and ZFOURGE team (2016, ApJ)
http://zfourge.tamu.edu
Ks in three CANDELS HST fields (COSMOS,
Ks CDFS,
• Deep (K~25.5-26 AB mag) imaging
UDS) w/Medium-band filters (J1J2J3 HsHl Ks) to provide R~10 “spectroscopy”.
• Includes wealth of ancillary data (Spitzer/Herschel, X-ray, radio).
• Stellar mass limit, >2 x 109 solar masses at z < 2.
• Measure precise redshifts for 1 < z < 4 (Δz/1+z = 1%; or Δv = 2000 km s—1)
• Exceptional image quality in near-IR (median FWHM < 0.5”)
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
Properties of Centrals and Satellites: 1 < z < 3
Random Field
Central Galaxy
Nancy Kawinwanichakij, CP, Quadri et al 2014, ApJ, 792, 103
Properties of Centrals and Satellites: 1 < z < 3
Random Field
Central Galaxy
1<z<3
Mc > 3e10 M⊙
Nancy Kawinwanichakij, CP, Quadri et al 2014, ApJ, 792, 103
Cumulative number of satellites for 1 < z < 3 centrals
Nancy Kawinwanichakij, CP, Quadri et al 2014, ApJ
Properties of Centrals vs. Satellites: Conformity to z < 2.5
Kawinwanichakij, Quadri, CP, et al 2016, ApJ, 817, 9
Including data from ZFOURGE, UltraVISTA (Muzzin+), and NMBS(Whitaker+)
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
galaxy density:
log(1+δ)3
Including data from ZFOURGE in CDFS, COSMOS, and UDS
quiescent galaxies
star-forming galaxies
lower mass quenched galaxies live in
regions of higher galaxy density
(at least to z~1.5)
Nancy Kawinwanichakij, CP, Quadri et al., (2016) in prep
quiescent fraction, fQ
lower
density
quartile
galaxy density in ZFOURGE
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
highest
density
quartile
quenching efficiencies
evolution of mass quenching and environmental
quenching efficiency in ZFOURGE
stellar mass
SDSS/zCOSMOS from Peng+2010, Kovač+2014
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
mass quenching efficiency
environmental quenching
efficiency
SDSS/zCOSMOS from Peng+2010, Kovač+2014
decreasing redshift
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
mass quenching efficiency
environmental quenching
efficiency
SDSS/zCOSMOS from Peng+2010, Kovač+2014
decreasing redshift
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
environmental quenching
efficiency
mass quenching efficiency
mass quenching efficiency
increases with time for all galaxies.
SDSS/zCOSMOS from Peng+2010, Kovač+2014
decreasing redshift
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
environmental quenching
efficiency
mass quenching efficiency
mass quenching efficiency
increases with time for all galaxies.
SDSS/zCOSMOS from Peng+2010, Kovač+2014
decreasing redshift
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
environmental quenching efficiency:
constant for higher-mass galaxies;
increases with time for lower-mass
galaxies.
environmental quenching
efficiency
mass quenching efficiency
mass quenching efficiency
increases with time for all galaxies.
SDSS/zCOSMOS from Peng+2010, Kovač+2014
decreasing redshift
Kawinwanichakij, CP, Quadri et al. (2016) in prep
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
sersic index, n
LDE = lowest density environ.
HDE = highest density environ.
Kawinwanichakij, CP, Quadri
et al., in prep
effective radius, reff / kpc
sersic index, n
Environmental Quenching has
no measurable effect on
morphology….
LDE = lowest density environ.
HDE = highest density environ.
Kawinwanichakij, CP, Quadri
et al., in prep
effective radius, reff / kpc
preprocessing
high z
see, for example, Lister, Weinmann et al. 2013, MNRAS, 432, 1162
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
preprocessing
accretion
merging
preprocessing
mass loss
assembly
bias
moderate z
high z
see, for example, Lister, Weinmann et al. 2013, MNRAS, 432, 1162
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
preprocessing
accretion
accretion
merging
preprocessing
mass loss
assembly
bias
low z
moderate z
high z
see, for example, Lister, Weinmann et al. 2013, MNRAS, 432, 1162
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
Abell 2744
0.3 < z < 0.6
Morishita, Abrahsom, Treu+(GLASS), 2016, arxiv:1607.00384
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
Abell 2744
0.3 < z < 0.6
Morishita, Abrahsom, Treu+(GLASS), 2016, arxiv:1607.00384
Casey Papovich
High-z (proto)-clusters
2016 Oct 5
0.3 < z < 1.0
Kawinwanichakij, CP, Quadri et al., in prep
1.0 < z < 1.5
low-mass quiescent galaxies show
correlation between effective radius
and U-V color (age)
0.3 < z < 1.0
Kawinwanichakij, CP, Quadri et al., in prep
1.0 < z < 1.5
Environmental Quenching observed out to z~2.5
– ZFOURGE shows (Kawinwanichakij+2016, in prep):
– Mass quenching efficiency increases with decreasing redshift,
and increasing galaxy stellar mass.
– near constant environmental quenching for massive galaxies;
increasing quenching at lower-redshifts for low-mass galaxies.
– Environmental quenching appears to change morphologies:
– quiescent galaxies in high density regions (even at ow
masses) have (statistically) identical morphologies to
quiescent galaxies in low density regions.
– However, evidence that low-mass quiescent galaxies have a
relation between effective radius and U-V color (age) to z ~< 1.5.
– Implies galaxy accretion and environmental quenching
happens at high redshifts, with “preprocessing” in groups,
consistent with predictions from models.
Casey Papovich
High-z (proto)-clusters
2016 Oct 5