Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.mrao.cam.ac.uk/galevol/salberts_cambridge_conference.pdf Äàòà èçìåíåíèÿ: Sun Oct 6 18:31:40 2013 Äàòà èíäåêñèðîâàíèÿ: Fri Feb 28 00:15:56 2014 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: iceland

Stacey Alberts Department of Astronomy

Galaxy Evolution over Five Decades Cambridge, England September 2013

The Evolution of Dust-Obscured Star Formation Activity in Galaxy Clusters over the Last 9 Billion Years
Alberts et al., MNRAS, submitted

With Collaborators: Alex Pope (Umass), Mark Brodwin (UMKC), David Atlee (NOAO), Yenting Lin (ASIAA), Arjun Dey (NOAO) Peter Eisenhardt (JPL), Dan Gettings (Uflorida), Anthony Gonzalez (UFlorida), Buell Jannuzi (Steward), Conor Mancone (UFlorida), John Moustakas (Siena), Greg Snyder (CFA), Adam Stanford (UCDavis), Dan Stern (JPL), Ben Weiner (Steward), Greg Zeimann (UCDavis)
Image credit: NASA, ESA, J. Richard (Center for Astronomical Research/Observatory of Lyon, France), and J.-P. Kneib (Astrophysical Laboratory of Marseille, France)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


· · · · · · ·

The Emerging Picture of Cluster Galaxy Evolution Mancone+10
Cluster cores in the local Universe are generally red and dead. increased star forming fraction toward cluster cores at z>1.4 (e
+10, Tran+10, Hayashi+11, Fassbender+11) .g. Hilton

m*

evolution of 4.5um luminosity function of cluster galaxies -> rapid mass assembly at z>1.3 (Mancone+10) increased fraction of AGN in clusters
(Galametz+09, Martini+13)

Redshift
Post-starburst Galaxies
Muzzin+11

excess post-starburst fraction at z~1
(Muzzin+12)

Color and scatter of Red Sequence consistent with extended SFH and rapid red sequence growth (Snyder+12) rapid transition from active formation to passive evolution from z=1.5 to z=1 (Brodwin+13)

Sunday, October 6, 2013


·
·
· · · ·

Goal: explore star formation in cluster galaxies over long redshift baseline (z=0.3-1.5) in large cluster sample Large, uniform cluster sample High redshift SF hidden behind dust need IR SF tracer Stacking looks at average population, can probe down the luminosity function

IRAC Shallow Cluster Survey (Eisenhardt+08)
9 square degrees, 274 clusters with uniform mass (~1014 M) rest-frame near-IR overdensities spec-z or photo-z and stellar mass estimates mass limited cluster and field samples (M 1010 M

·

Herschel SPIRE 250um data from HerMES (Oliver+12)

Sunday, October 6, 2013


Stacking Procedure
1. Cluster and field galaxies binned in redshift and stacked

·

variance-weighted stacking and bootstrap resampling errors

Credit: H. Dole/IAS/ Arizona/ NASA/JPLCaltech

2. source blending/clustering bias correction 3. field galaxy contamination correction 4. Stacked 250m flux converted to LIR/SFR

·

empirical template based on z~1 star forming galaxies (Kirkpatrick+12)

5. SSFRs calculated

Sunday, October 6, 2013


Stacking Cluster Galaxies
UDS Field Galaxies (Viero+13)

Average SFR [M yr

asdfa

In the Cluster Cores (r<0.5 Mpc)

Complete stellar mass limited cluster and field galaxy samples -includes both SFing and passive galaxies

Sunday, October 6, 2013


Stacking Cluster Galaxies
UDS Field Galaxies (Viero+13)

Average SFR [M yr

asdfa

In the Cluster Cores (r<0.5 Mpc)

·

As a function of cosmic time:

· · ·

y = et e-folding times: 1.5 Gyr for cluster galaxies and 2.4 Gyr for field galaxies timescales consistent with ram pressure stripping...?

Sunday, October 6, 2013


Stacking Cluster Galaxies
Main Sequence

Average SSFR [Gyr

asdfa

asdfa

In the Cluster Cores (r<0.5 Mpc)
Sunday, October 6, 2013


Stacking Cluster Galaxies
Average SFR [M yr

asdfa

·

Enhanced SF over the field level

·

mergers among infalling galaxies??

Including the Outskirts (r<1 Mpc)

Sunday, October 6, 2013


Stacking Cluster Galaxies
asdfa

·

Enhanced SF over the field level

Which types of galaxies are driving

·

mergers among infalling these trends? galaxies??

Including the Outskirts (r<1 Mpc)

Sunday, October 6, 2013


Stacking Cluster Galaxies - By Mass
asdfa

asdfasd

Lower Mass

Higher Mass

Lower mass: 1.3x1010-6.3x1010 M Higher Mass: >6.3x1010 M
Sunday, October 6, 2013

In the Cluster Cores (r<0.5 Mpc)

asdfasd


Stacking Cluster Galaxies - Blue Galaxies
Haines+13 cluster and field stacks

asdfa

asdfa

In the Cluster Cores (r<0.5 Mpc)
Sunday, October 6, 2013


Stacey Alberts Department of Astronomy

Galaxy Evolution over Five Decades Cambridge, England September 2013

Putting it all together
· · · ·
Cluster galaxies are quenched below the field up to z~1.2, after which they show field-like SF on average. Exact transition epoch probably depends on cluster properties, such as mass. Enhanced SF (mergers!) in cluster outskirts at z1.4. Ongoing mass assembly at these epochs. Trends depend on galaxy mass and type. Blue galaxies show a weaker evolution compared to the field, but still below field level. Rapid growth of red sequence? Timescales consistent with ram pressure stripping? major mergers prominent at high redshifts (see paper for discussion!)

Sunday, October 6, 2013


Stacey Alberts Department of Astronomy

Galaxy Evolution over Five Decades Cambridge, England September 2013

Putting it all together
· · · ·
Cluster galaxies are quenched below the field up to z~1.2, after which they Lookwor paper e SF on sho f field-lik Paper submitted! average. Exact transitionin the near future. epoch probably depends on on astro-ph cluster properties, such as mass. Enhanced SF (mergers!) Future work: in cluster outskirts at z1.4. Ongoing Deep PACS imaging of 11 mass assembly at these epochs. ISCS clusters from z=1-2!! Trends depend on galaxy mass and type. Blue galaxies show a weaker evolution compared to the field, but still below field level. Rapid growth of red sequence? Timescales consistent with ram pressure stripping? major mergers prominent at high redshifts (see paper for discussion!)

Sunday, October 6, 2013


Cluster at z=1.75

SPIRE 250m
Sunday, October 6, 2013

PACS 100m