agn from the 13h xmm/chandra deep radio/x-ray survey
DESCRIPTION
AGN from the 13H XMM/Chandra deep radio/X-ray survey. Nick Seymour (SSC) NRAO 17th May. AGN from the 13H XMM/Chandra deep radio/X-ray survey. The 13hr core team: Southampton: Ian McHardy, Katherine Gunn, Derek Moss, Tom Dwelly MSSL: Mat Page, Nicola Loaring, Keith Mason - PowerPoint PPT PresentationTRANSCRIPT
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AGN from the 13H XMM/Chandra deep radio/X-ray survey
AGN from the 13H XMM/Chandra deep radio/X-ray survey
Nick Seymour (SSC) NRAO 17th May
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AGN from the 13H XMM/Chandra deep radio/X-ray survey
AGN from the 13H XMM/Chandra deep radio/X-ray survey
Nick Seymour (SSC) NRAO 17th May
The 13hr core team:
• Southampton: Ian McHardy, Katherine Gunn, Derek Moss, Tom Dwelly• MSSL: Mat Page, Nicola Loaring, Keith Mason• Liverpool JM: Andy Newsam• USA: Tim Sasseen, Jamie Kennea, France Cordova• Subaru: Kaz Sekiguchi, T. Takata• Spitzer MIPS team: George Rieke et. al.
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AGN from the 13H XMM/Chandra deep radio/X-ray survey
AGN from the 13H XMM/Chandra deep radio/X-ray survey
The 13hr field
• Location of UK Rosat deep survey. Lowest Galactic NH
• 200ks XMM-Newton• 120ks Chandra mosaic• Deep VLA+MERLIN+GMRT• Deep optical imaging from CFHT + WHT + Subaru• Optical spectroscopy from WHT + CFHT + Keck• Ultra-deep 3.6-170 m imaging with Spitzer• IR imaging from UKIRT (coming next month)
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The 20cm deep radio countsThe 20cm deep radio counts
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The 20cm deep radio countsThe 20cm deep radio counts
• Sub-mJy up-turn known for 2 decades
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The 20cm deep radio countsThe 20cm deep radio counts
• Sub-mJy up-turn known for 2 decades• Successfully modeled from star-burst population
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The 20cm deep radio countsThe 20cm deep radio counts
• Sub-mJy up-turn known for 2 decades• Successfully modeled from star-burst population• Direct evidence is scarce, many faint radio sources remain un-identified (difficult for R ≥ 26)
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The 20cm deep radio countsThe 20cm deep radio counts
• Sub-mJy up-turn known for 2 decades• Successfully modeled from star-burst population• Direct evidence is scarce, many faint radio sources remain un-identified (difficult for R ≥ 26)• models suggest that AGN may still contribute 20% even at the faintest fluxes
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours
1.4GHz R-band 635MHz i´-band
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics• X-ray spectra
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Spectra of NELGs Spectra of NELGs
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
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Spectra of NELGs Spectra of NELGs
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
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Spectra of NELGs Spectra of NELGs
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
Lots of them are absorbed.
Some are not. Some absorbed
and with reprocessed soft component.
![Page 18: AGN from the 13H XMM/Chandra deep radio/X-ray survey](https://reader033.vdocuments.us/reader033/viewer/2022051402/56815876550346895dc5d614/html5/thumbnails/18.jpg)
You can tell the AGN by a combination of properties.
Variable Power law spectra Point-like sources How many sources with L2-10
< 1042 are powered by star formation rather than AGN?
You can tell the AGN by a combination of properties.
Variable Power law spectra Point-like sources How many sources with L2-10
< 1042 are powered by star formation rather than AGN?
Answer is 2. Both have L2-10 <= 1040
The ambiguous region of 1040<LX<1042 is almost entirely AGN.
Answer is 2. Both have L2-10 <= 1040
The ambiguous region of 1040<LX<1042 is almost entirely AGN.
AGN-powered
Star-powered
Star-forming galaxies? Star-forming galaxies?
Page et al. 2006
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics• radio morphology (AGN=compact/lobes, SFGs=galaxy sized)• X-ray spectra• radio spectra/morphology (AGN=flat compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep)
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HzRGs compared to other radio sourcesHzRGs compared to other radio sources
30µJy detection limit
Redshift
Log(L1.4GHz)[W/Hz]
Log(L1.4GHz)[W/Hz]
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HzRGs compared to other radio sourcesHzRGs compared to other radio sources
Redshift
Log(L1.4GHz)[W/Hz]
Log(L1.4GHz)[W/Hz]
Starburst galaxies?
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HzRGs compared to other radio sourcesHzRGs compared to other radio sources
Redshift
Log(L1.4GHz)[W/Hz]
Log(L1.4GHz)[W/Hz]
Radio-loud QSOs
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HzRGs compared to other radio sourcesHzRGs compared to other radio sources
Redshift
Log(L1.4GHz)[W/Hz]
Log(L1.4GHz)[W/Hz]
HzRGs
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HzRGs compared to other radio sourcesHzRGs compared to other radio sources
Redshift
Log(L1.4GHz)[W/Hz]
Log(L1.4GHz)[W/Hz]
??
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics• radio morphology (AGN=compact/lobes, SFGs=galaxy sized)• X-ray spectra• radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep)• Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics• radio morphology (AGN=compact/lobes, SFGs=galaxy sized)• X-ray spectra• radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep)• Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution: cold reservoir of dust for star-formation and hot dust heated by the AGN.
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AGN/SFG DiscriminationAGN/SFG Discrimination• optical morphology/colours• optical spectra - need high S/N for line diagnostics• radio morphology (AGN=compact/lobes, SFGs=galaxy sized)• X-ray spectra• radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep)• Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution: cold reservoir of dust for star-formation and hot dust heated by the AGN. Some redshifts available with IRS spectroscopy
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Photometric redshiftsPhotometric redshifts
One faint source with S=120Jy at 20cm
R z´ Ks
Over an order of magnitude break between R and z´
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Photometric redshiftsPhotometric redshifts
One faint source with S=120Jy at 20cm
R z´ Ks
Over an order of magnitude break between R and z´, hence either
z~1.1 L~1023.5 SFG (v dusty)z~6.4 L~1024.9 AGN (lensed?)
Deep(er) J, H, K and IRAC data is in hand
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ConclusionsConclusions• some AGN are radio loud QSOs at z~1-2• some are hidden in SFGs with L1.4GHz ~ 1022-23 W/Hz• low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered
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ConclusionsConclusions• some AGN are radio loud QSOs at z~1-2• some are hidden in SFGs with L1.4GHz ~ 1022-23 W/Hz• low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered• follow-up in X-ray/optical/IR is crucial (and labour intensive)
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ConclusionsConclusions• some AGN are radio loud QSOs at z~1-2• some are hidden in SFGs with L1.4GHz ~ 1022-23 W/Hz• low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered• follow-up in X-ray/optical/IR is crucial (and labour intensive)• as are wider/deeper radio observations