how to start an agn: the role of host galaxy environment rachel gilmour (eso chile & ifa,...
TRANSCRIPT
![Page 1: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/1.jpg)
How to start an AGN:
the role of host galaxy
environmentRachel Gilmour (ESO Chile & IfA, Edinburgh)
Philip Best (Edinburgh), Omar Almaini & Meghan Gray (Nottingham)
or stop
![Page 2: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/2.jpg)
Why do some galaxies have AGN?
Gas -> black hole = AGN
Internal: size, morphology, star-formation
Historical: previous activity -- depletion,
feedback
External: mergers, close encounters, tidal
field, strangulation, ram-pressure stripping
No AGN
0.01%
30%
![Page 3: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/3.jpg)
External effects on galaxies
Morphology: spirals -> S0s
Star-formation rate: high -> low
Q1 – Do the frequency and properties of AGN
depend on the external environment?
Q2 – Can this be explained by the changes in the
type of host galaxies?
![Page 4: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/4.jpg)
Where are AGN found?
Miller '03, Wake '05
Kauffmann '04, Coldwell '02
Dressler '99
Eckart '05
Ruderman '05
Johnson '03Porciani '04
Ledlow & Owen '96
Reddy '04
Best '04
Best '02
Galaxy density / AGN clustering
Red
shif
t
~0.8
~0.1
Optical
Radio
X-ray
![Page 5: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/5.jpg)
My projects
1. AGN in the A901/2 supercluster• Detailed study
• X-ray detected AGN
• Includes groups, clusters, filaments, field etc.
2. Statistical survey of AGN in > 100 galaxy clusters• X-ray detected AGN
• Find statistical excess of sources compared to “blank” field
• Split sample by cluster properties and redshift
![Page 6: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/6.jpg)
A901
A901aA901b
A902
Filament
SW group
The A901/2 supercluster (z=0.17)
Optical data (from COMBO-17 team)• Deep R-band imaging
• 17-band photometric redshifts for ~18000 objects (m
R<24)
• 1240 supercluster galaxies found
• 282 supercluster spectra from 2dF
• Weak lensing map
Spitzer data• MIPS 24-micron sources
X-ray data• 12 ksec ROSAT images (HRI)
• 90 ksec XMM-Newton image
People: Meghan Gray, Chris Wolf + COMBO-17 team, Bell and Papovich, Andy Taylor.
![Page 7: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/7.jpg)
A901
A901a
A902
A901b
SW groupz=0.5 cluster
Emission
A901/2: Finding the supercluster AGN
• Identify point sources Sources- wavelet detection on images from 3 cameras 150
- remove uncertain and extended sources 139
![Page 8: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/8.jpg)
A901/2: Finding the supercluster AGN
• Identify point sources Sources- wavelet detection on images from 3 cameras 150
- remove uncertain and extended sources 139• Match with optical sources
- R-band, using likelihood ratios from 14000 random sources
- also Spitzer 24-micron data to resolve uncertainties
88
![Page 9: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/9.jpg)
A901/2: Finding the supercluster AGN
• Identify point sources Sources- wavelet detection on images from 3 cameras 150
- remove uncertain and extended sources 139• Match with optical sources
- R-band, using likelihood ratios from 14000 random sources
- also Spitzer 24-micron data to resolve uncertainties
88• Determine supercluster membership
- COMBO-17 photometric redshifts and 2dF spectra 11
- Manual check for AGN contaminated sources 12
![Page 10: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/10.jpg)
• Identify point sources Sources- wavelet detection on images from 3 cameras 150
- remove uncertain and extended sources 139• Match with optical sources
- R-band, using likelihood ratios from 14000 random sources
- also Spitzer 24-micron data to resolve uncertainties
88• Determine supercluster membership
- COMBO-17 photometric redshifts and 2dF spectra 11
- Manual check for AGN contaminated sources 12• Find out which are AGN
- check for low-mass X-ray binaries using fx/fB 12
- check for star-forming galaxies using Lx, hardness ratios, fx/fR,
star-formation rates from OII lines and OIII/Hβ line ratios 11
A901/2: Finding the supercluster AGN
![Page 11: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/11.jpg)
A901/2: Finding the non-AGN
Aim: Compare the AGN environments with control samples of galaxies
which have:• no AGN• similar magnitudes• similar colours• where AGN could be detected
Method:• 100 samples of 66 galaxies• equal number of galaxies in
each 0.5 magnitude bin• exclude cluster centres • use K-S and Kuipers tests
![Page 12: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/12.jpg)
A901/2: AGN host galaxies
RESULT 1 : All of the AGN
lie in galaxies with mR < 20
RESULT 2 : ~5% of bright
supercluster galaxies contain
X-ray detected AGN (~1%
optically detected)
RESULT 3 : Brighter galaxies
have equal luminosity or
fainter AGN (92%)
![Page 13: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/13.jpg)
A901/2: Separating the Environments
Define by hand:
• Clusters (A901a, A901a,
A901b, A902)
• Groups
• Outskirts of large clusters and groups
• Filaments
![Page 14: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/14.jpg)
Two parameter
separation for
environments:
(1.5' = 250 kpc)
Local density:
clusters & field
Local colour:
groups & edges
filaments & clusters
1.5'
A901/2: Separating
the Environments - 2
![Page 15: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/15.jpg)
A901/2: Separating the environments:
Does it work for all galaxies?
Cluster
Red group / Edge
Blue group
Filament
Field
![Page 16: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/16.jpg)
cluster
filament
field
group
edge
A901/2: Environments of AGN
3.3% - AGN match
control in 2D
space
18% -AGN match
control in edge
and group
4% - AGN match
control in 1D
space along
cluster line (30%
in density only)
>98%-Lx
decreases along
the cluster line
direction
Cluster line
![Page 17: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/17.jpg)
A901/2: Conclusions
1. ~5% of bright supercluster galaxies contain X-ray detected AGN.
2. All of the AGN lie in galaxies with mR < 20. more gas, larger black hole
3. The lack of AGN in fainter galaxies is not due to a LX – mR
correlation. no correlation or large galaxies are more stable
4. Compared to other similar galaxies, those with AGN lie in group or
edge like environments – moderate density and bluer than average.suppression in centre, triggering on outskirts, tracing star-formation, more smaller galaxies
5. AGN in more cluster like environments are fainter.galaxies with more gas need less disturbance, strangulation reduces available gas
![Page 18: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/18.jpg)
Where are AGN found?
Miller '03, Wake '05
Kauffmann '04, Coldwell '02
Dressler '99
Eckart '05
Ruderman '05
Johnson '03Porciani '04
Ledlow & Owen '96
Reddy '04
Best '04
Best '02
Galaxy density / AGN clustering
Red
shif
t
A901/2
~0.8
~0.1
Optical
Radio
X-ray
![Page 19: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/19.jpg)
Chandra Clusters: Method
• Find sources in fields of galaxy clusters
• Predict source distribution assuming no cluster AGN
• Compare flux and radial distributions of excess sources
AGN
Abell 1689
HST Credit: NASA / N. Benitez
![Page 20: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/20.jpg)
Chandra Clusters: The sample
Secure redshift and z > 0.1Exposure > 10 ksecX-ray detected cluster (after data reduction)
=== 139 good cluster fields ===
+ 8 with z > 1
Redshift distributionMorphology
89 'relaxed' 23 'disturbed' 19 'contaminated' 8 high redshift
(z > 1)
Luminosity
z
0.1 – 70 x 1044 erg/sec
![Page 21: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/21.jpg)
Chandra Clusters: PredictionBlank fields – deep surveys (22) and high redshift QSOs (22)Sensitivity map – background, size, exposure, accuracy + errors
Background
Source size Good region
Exposure time
Sensitivity
map
![Page 22: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/22.jpg)
Chandra Clusters: Lensing
Lensing changes background sources : flux increases
number density decreases
Net result: lensing causes ~ 10% reduction in the central 0.5 Mpc
INPUTS:
• Background AGN redshift distribution (3 used)
• Cluster model (SIS now, NFW in future)
• Cluster luminosity => mass
N
Lx
Model = Blank fields + Sensitivity map + Lensing
![Page 23: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/23.jpg)
Chandra Clusters: Radial position
AGN lie between 0.5 and 1 Mpc
from the cluster centre.
Excess of 1 or 2
sources per cluster
Radial trend seen in
physical distance (Mpc)
Lack of AGN in central
regions is not due to
the intra-cluster
emission
![Page 24: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/24.jpg)
Chandra Clusters: Suppression?
AGN appear to be suppressed
in moderate redshift clusters
NX(flux) NX(Cl,flux)
NOpt(>L*) NOpt(Cl,>L*) =
25 galaxies > L*
5 galaxies > L*
1 galaxy > L*
Clusters with low LX (~1x1044) have ~6 galaxies > L*
(De Propris 2004)
(Excess per average field = excess per square degree x average field size)
![Page 25: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/25.jpg)
Chandra Clusters: Evolution
The evolution of AGN in clusters
is faster than in the field
25 gal.
25 gal.
25 gal.25 galaxies
5 galaxies
Redshift samples < 1 have
similar luminosity &
morphology distributions
![Page 26: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/26.jpg)
Chandra Clusters: Radial Evolution
High redshift clusters have more
AGN at larger radii
![Page 27: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/27.jpg)
Chandra Clusters: Morphology
Disturbed clusters have more
low luminosity sources
Disturbed clusters also have excess at higher radius
![Page 28: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/28.jpg)
Chandra Clusters: Results
AGN lie between 0.5 and 1 Mpc from the cluster centre.
AGN appear to be suppressed in moderate redshift
clusters.
The evolution of AGN in clusters is faster than in the field.
High redshift clusters have more AGN at larger radii.
Disturbed clusters have more low luminosity sources.
![Page 29: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/29.jpg)
Where are AGN found?
Miller '03, Wake '05
Kauffmann '04, Coldwell '02
Dressler '99
Eckart '05
Ruderman '05
Johnson '03Porciani '04
Ledlow & Owen '96
Reddy '04
Best '04
Best '02
Galaxy density / AGN clustering
Red
shif
t
~0.8
~0.1
Optical
Radio
X-ray
A901/2
![Page 30: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/30.jpg)
AGN lie between 0.5 and 1 Mpc
from the cluster centre.
AGN appear to be suppressed in
moderate redshift clusters.
The evolution of AGN in clusters
is faster than in the field.
High redshift clusters have more
AGN at larger radii.
Disturbed clusters have more low
luminosity sources.
Results~5% of bright supercluster
galaxies contain X-ray detected
AGN. All are in galaxies with mR < 20.
The lack of AGN in fainter galaxies is not due to a LX – mR
correlation.
Compared to similar galaxies,
those with AGN lie in group or
edge like environments –
moderate density and bluer.
AGN in more cluster like
environments are fainter.
![Page 31: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/31.jpg)
AGN lie between 0.5 and 1 Mpc
from the cluster centre.
AGN appear to be suppressed in
moderate redshift clusters.
The evolution of AGN in clusters
is faster than in the field.
High redshift clusters have more
AGN at larger radii.
Disturbed clusters have more low
luminosity sources.
AGN in more massive clusters
have a larger radial spread.
Results~5% of bright supercluster
galaxies contain X-ray detected
AGN. All are in galaxies with mR < 20.
The lack of AGN in fainter galaxies is not due to a LX – mR
correlation.
Compared to similar galaxies,
those with AGN lie in group or
edge like environments –
moderate density and bluer.
AGN in more cluster like
environments are fainter.
![Page 32: How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray](https://reader036.vdocuments.site/reader036/viewer/2022062423/56649e975503460f94b9a8e9/html5/thumbnails/32.jpg)
Chandra Clusters: Cluster size
AGN in more massive clusters
have a larger radial spread
Expect mass to go as
Lx M4/3
Expect radius to go as
R ~Lx 0.3