The Far-‐‑IR View of an Ultra-‐‑Hard X-‐‑ray - Herschel

The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
Mrk 704
ESO197-­‐‑G027
Taro Shimizu (UMDCP)
Richard MushoIky (UMDCP)
Marcio Melèndez (UMDCP)
Amy Barger (U. Wisconsin)
Len Cowie (IfA Hawaii)
Mike Koss (IfA Hawaii)
NGC 5674
“The Universe Explored by Herschel”
October 16, 2013
ESA/ESTEC Noordwijk, Netherlands
The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
Motivation
• 
Close connection between supermassive black hole (SMBH) and host galaxy properties (MBH-­‐‑σ, MBH-­‐‑Mbulge, etc.)
• 
Points to coevolution of galaxy and SMBH
• 
Active Galactic Nuclei (AGN) feedback invoked to explain coevolution
•  Far-­‐‑IR (FIR) emission = Star Formation heated dust. What is the AGN contribution to FIR?
• 
Need reference AGN sample with high angular resolution (Herschel) in FIR to determine true AGN contribution
The Herschel-­‐‑BAT Sample
•  313 AGN selected from Swift/Burst Alert Telescope (BAT) 58 month catalog (14-­‐‑195 keV)
•  z < 0.05
•  Greatly reduces selection bias •  Flux-­‐‑limited sample
149 Sy 1-­‐‑1.5 (Sy 1)
155 Sy 1.8 – 2 (Sy 2)
5 LINER
4 “Other” AGN
LBAT ~ 1041 – 1045 ergs s-­‐‑1 Herschel Observations
•  PACS: 70 and 160 µμm in mini-­‐‑scan mode
•  Two 3’ scan legs, 4” step, 70° and 110° scan angles
•  20”/sec speed – 3’x1’ images •  SPIRE: 250, 350, and 500 µμm in small-­‐‑map mode
• 
• 
• 
• 
•  30”/sec speed, 2 orthogonal scan angles, 5’ homogeneous coverage
Data reduced to Level 1 using HIPE v8
Images created with Scanamorphos v19 (Roussel 2013)
Pixel sizes of 1.4”, 2.85”, 4.5”, 6.25”, 9” for 70-­‐‑500 µμm images
Pixel size = ¼ * PSF FWHM
NGC 6221
PACS 70
PACS 160
SPIRE 250
SPIRE 350
SPIRE 500
Flux Extraction
•  Aperture photometry using annularSkyAperturePhotometry task within HIPE or DS9 “Funcnts” tool
•  Concentric annulus to estimate background
•  All sources < 5σ considered non-­‐‑detections and only upperlimits reported
• 
• 
• 
• 
• 
70 µμm: 94% detected
160 µμm: 83% detected
250 µμm: 85% detected
350 µμm: 69% detected
500 µμm: 46% detected
PACS: Melèndez et al in prepSPIRE: Shimizu et al in prep The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
LFIR-­‐‑LBAT Correlations
•  Tested correlations using partial Kendall tau test and survival analysis
•  Takes into account correlation with distance and upper limits
•  Type 1 AGN correlated at ALL Herschel wavebands with BAT luminosity
•  Type 2 AGN NOT correlated at 10
ANY Herschel waveband with 10
BAT luminosity
45
Blue dots = Sy 1
Red squares = Sy 2
Green triangles = LINER
Black stars = “Other” AGN
Melendez et al in prep
L70 [ergs s−1 ]
44
1043
1042
1041 41
10
1042
1043
LBAT [ergs s−1 ]
1044
1045
Number of Sources
F70 /F160
7
6
5
4
3
2
1
0
0.0
0.5
1.0
KINGFISH: Dale et al 2012
3.0
2.5
2.0
1.5
1.0
0.5
0.0
0.0
0.5
1.0
K-S = 0.04
PACS Color Not Different than “Normal Galaxies” SPIRE Colors Different
Number of Sources
1.5
F70 /F160
1.5
2.0
1.2
BAT AGN
HRS
Normalized Counts
Normalized Counts
0.8
K-­‐‑S < 5%
0.6
0.4
0.2
0.0
0.5
3.0
3.5
HRS: Ciesla et al. 2012
Melèndez et al in prep.
2.5
3.0
3.5
/F160
FF7070/F
160
1.2K-­‐‑S = 2e-­‐‑06
1.0
2.5
= 31%
Blue: KINGFISHK-­‐‑SK-S
= 0.31
Grey: BAT
1.6
1.4
2.0
1.0
1.5
2.0
2.5
3.0
3.5
1.0
0.8
0.6
BAT AGN
HRS
K-­‐‑S = 0.07
K-­‐‑S = 7%
0.4
0.2
0.0
0.5
1.0
F250 /F350
F250/F350
1.5
2.0
2.5
F350 /F500
Shimizu et al in prep
3.0
3.5
F350/F500
4.0
FIR Colors: Comparison to “Normal” Galaxies
3.5
BAT
3.0
F250 /F350
2.5
2.0
1.5
1.0
0.5
0.0
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350 /F500
Shimizu et al in prep
FIR Colors: Comparison to “Normal” Galaxies
3.5
BAT
HRS
3.0
What are these sources?
F250 /F350
2.5
2.0
1.5
1.0
But much larger dispersion…
0.5
Majority AGN same as HRS galaxies (~70%) 0.0
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350 /F500
HRS: Ciesla et al 2012
Shimizu et al in prep
FIR Colors: Comparison to “Normal” Galaxies
3.5
3.0
F250 /F350
2.5
BAT
HRS
β = 1.5
β=2
2.0
1.5
1.0
Fν ~ ν^β*B(T) (ie “greybody”)
β = 1.5 – 2
T = 20 – 50 K
0.5
0.0
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350 /F500
HRS: Ciesla et al 2012
Shimizu et al in prep
FIR Colors: Comparison to “Normal” Galaxies
What are these sources?
3.5
3.0
F250 /F350
2.5
BAT
HRS
β = 1.5
β=2
2.0
1.5
1.0
0.5
0.0
0.5
But much larger dispersion…
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350 /F500
HRS: Ciesla et al 2012
Shimizu et al in prep
FIR = SF + Jet?
•  Hypothesis: Increasing radio loudness causes change in FIR colors
•  Use radio loudness parameter, R = log(L6cm/L70µμm)
FIR = SF + Jet?
3.0
F250/F350
2.5
2.0
1.5
R < −6
−6 < R < −5
−5 < R < −4
−4 < R < −3
R > −3
1.0
0.5
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350/F500
•  Determined R from archival radio fluxes (NVSS, SUMSS)
•  Radio loudness only explains most extreme sources (yellow and red)
FIR = SF + Jet?
3.0
3C 111
Pictor A
F250/F350
2.5
2.0
1.5
R < −6
−6 < R < −5
−5 < R < −4
−4 < R < −3
R > −3
1.0
0.5
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350/F500
•  Determined R from archival radio fluxes (NVSS, SUMSS)
•  Radio loudness only explains most extreme sources (yellow and red)
FIR = SF + Jet?
3.0
F250/F350
2.5
2.0
1.5
R < −6
−6 < R < −5
−5 < R < −4
−4 < R < −3
R > −3
1.0
0.5
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
F350/F500
•  Determined R from archival radio fluxes (NVSS, SUMSS)
•  Radio loudness only explains most extreme sources (yellow and red)
The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
The Far-­‐‑IR View of an Ultra-­‐‑Hard X-­‐‑ray Selected Sample of AGN
1.  Motivation, sample, and flux extraction
• 
• 
Large unbiased, low-­‐‑z sample of AGN Aperture photometry to extract fluxes
2.  LAGN-­‐‑LFIR correlations, FIR colors and comparison to “normal” SF galaxies
• 
• 
All wavebands correlated with AGN lum. for Sy 1
SPIRE FIR colors indicate presence of radio jet
3.  SFR density of AGN
• 
• 
Almost all sources have majority of FIR flux from point source
SFR density for large fraction of AGN above threshold for SF-­‐‑
driven winds
Point Source Contribution to FIR
120
Number of Sources
100
80
60
70 µm
160 µm
Nearly all sources have Fpoint/Ftotal > 50%
40
20
0
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
Fpoint /Ftotal
Fpoint = Flux within small point source aperture
6” for 70 µμm, 12” for 160 µμm
MushoIky et al 2013 (in prep)
Measuring SFR density
PACS 70
Mrk 704
ESO197-­‐‑G027
NGC 5674
•  Used GALFIT (Peng+ 2002) with Gaussian model or aperture radius to estimate FIR sizes of sources
•  Upper limits for point sources determined by increasing FWHM of Gaussian until Δχ2 = 3σ
•  Monochromatic SFR calibrations from Calze€i et al. 2010
•  SFR ~ 0.1 – 100 Msun yr-­‐‑1
Starburst-­‐‑driven Winds in AGN?
ΣSFR,160 [Msun yr−1 kpc−2]
100
10−1
10−2
10−3 −3
10
10−2
MushoIky et al 2013 (in prep)
10−1
100
101
ΣSFR,70 [Msun yr−1 kpc−2]
70 µμm: 35 – 55% > 0.1 Msun yr-­‐‑1 kpc-­‐‑2 (Heckman 2002 threshold)
160 µμm: 20 – 30% > 0.1 Msun yr-­‐‑1 kpc-­‐‑2
Large fraction of AGN could be living in nuclear starburst
Summary and Future Work
•  Measured the FIR (70 – 500 µμm) fluxes of a large, unbiased sample of AGN using Herschel Space Observatory
•  FIR luminosities correlated with BAT luminosity for Sy 1 suggesting an AGN contribution to FIR
•  SPIRE colors can separate galaxies based on increased radio loudness
•  SFR density > Heckman 2002 threshold for large fraction of AGN
Work in progress…
• 
• 
Full SED modeling to determine AGN contribution
Determination of AGN bolometric corrections