x-ray and radio agn in coma cluster progenitors quyen nguyen hart university of colorado at boulder,...
TRANSCRIPT
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X-ray and Radio AGN in Coma Cluster Progenitors
Quyen Nguyen HartUniversity of Colorado at Boulder, Center for Astrophysics and Space Astronomy
Collaborators
CU-Boulder
John Stocke Erica Ellingson Eric Hallman
U. Of Michigan
Gus Evrard
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Why should we follow this road?
On the Road to Coma
More MassiveCluster
LessMassiveCluster
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On the Road to Coma
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Multi-wavelength Study
• Chandra Archival data• VLA 20-cm maps
(new/archival)• HST archival images• Apache Point
Observatory, 3.5m– Two color imaging
• (g,r) or (r,i)• K-short
– Med. Dispersion spectrograph with red/blue channels (3500 - 9000 Å)
• Additional sources– SDSS– ChaMP– CNOC-1– Literature
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Example of Data
Abell 963, z=0.206
Chandra 0.3-8.0 keV
FIRST SDSS r
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AGN Luminosity LimitsX-ray LF
Sazonov & Revnivtsev (2004)
1 order below knee
Ledlow & Owen 1996
1.4 GHz - Radio LF
2 orders below knee
X-ray 0.3-8 keV 3 1042 erg s-1
Radio 20 cm 1 1023 W Hz1
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Passive Galaxy Spectrum
Ca HK
B-band
Na IMg I
APO DIS spec, r ~ 17th
A-band
G-band
APO DIS spec, r ~ 19th
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Emission-Line Spectrum
APO DIS spec, r ~ 18.5th[O II]
[Ne V]
[Ne III]
Ca HK [O III] H-[N II]
[S II]
z=0.209
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Simple Number Counts
• 12 low-z clusters (0.2 < z < 0.5)
Radio Sources(~40)
X-ray Point Sources(~60)
TWO Radio AGN per Cluster
ONE Xray AGN per Cluster
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Upper/lower limits reached by APO 3.5m spectroscopy
Mr * ~ 20.8
CompositeCOLOR
MAGNITUDE Diagram
Cluster Red Sequence“old, dead, red galaxies”
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Mr * ~ 20.8
X-ray AND Radio AGNWith optical counterparts(N ~ 100)
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Xray AGNCluster Member
Radio AGNCluster Member
Xray AGNNon-member
Radio AGNNon-member
Redshiftunknown
Majority of cluster AGN lies on Cluster Red Sequence (CRS)
Some X-ray AGN have BLUER colors than CRS; emission-line spectra
Host galaxies of Cluster AGN are bright cluster galaxies
Mr * ~ 20.8
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AGN Host Galaxies
• Cluster AGN optical colors representative of old, red, & dead galaxies, ie. Passive ellipticals
• Spectra reveal that in our sample– X-ray AGN: ~75% passive galaxy host– Radio AGN: ~80% passive galaxy host
• In both cases, only a ~few AGN would have been identified optically
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AGN Projected Distance from ICM X-ray Emission Centroid
1 Mpc
750 kpc
500 kpc
250 kpc
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Xray
RadioALL AGN
ClusterRedSequenceGalaxies
ICM EMISSION( - Model)
Rcore
100 kpc400 kpc Cluster AGN are
more centrally concentrated
than red sequence galaxies!
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In Summary
• Road to Coma is unique sample
• Majority of cluster AGN reside within 500 kpc– distributed heating in cluster centers?
• Cluster AGN host galaxies are passive ellipticals (old, red, & dead galaxies!)
• RARE overlap of X-ray and Radio AGN sources– Different modes of AGN activity?
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What’s next…
• AGN population in z>0.5 sample
• X-ray hardness ratios; composite X-ray spectrum
• X-ray and Radio luminosity Functions– Is there an X-ray bi-variate luminosity function similar to
radio?
• Input cluster AGN properties in cosmological simulations
• This research is supported by Chandra Archive/Theory Grant AR8-9013X