Extended X-ray Emission in Compton Thick AGN with Deep Chandra Observations
Mackenzie L Jones, K. Parker, G. Fabbiano, M. Elvis, W. P. Maksym, A. Paggi, J. Ma, M. Karovska, A. Siemiginowska, J. Wang
DDraft version January 29, 2021
Typeset using L A TEX twocolumn style in AASTeX61
EXTENDED X-RAY EMISSION IN COMPTON THICK AGN WITH DEEP
CHANDRA
OBSERVATIONS
Mackenzie L. Jones, Kieran Parker,
2, 1
G. Fabbiano, Martin Elvis, W. P. Maksym, A. Paggi, Jingzhe Ma, M. Karovska, A. Siemiginowska, and Junfeng Wang Center for Astrophysics — Harvard & Smithsonian, 80 Garden St, Cambridge, MA 02138, USA Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ, UK INAF-Osservatorio Astrofisica di Torino, Via Osservatorio 20, 10025 Pino Torinese, Italy Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138, USA Department of Astronomy, Xiamen University, Xiamen, 361005, China
ABSTRACTWe present the spatial analysis of five Compton thick (CT) active galactic nuclei (AGNs), including MKN 573,NGC 1386, NGC 3393, NGC 5643, and NGC 7212, for which high resolution
Chandra observations are available. Foreach source, we find hard X-ray emission ( > ∼ kpc scales along the ionization cone, and for somesources, in the cross-cone region. This collection represents the first, high-signal sample of CT AGN with extendedhard X-ray emission for which we can begin to build a more complete picture of this new population of AGN. Weinvestigate the energy dependence of the extended X-ray emission, including possible dependencies on host galaxyand AGN properties, and find a correlation between the excess emission and obscuration, suggesting a connectionbetween the nuclear obscuring material and the galactic molecular clouds. Furthermore, we find that the soft X-rayemission extends farther than the hard X-rays along the ionization cone, which may be explained by a galactocentricradial dependence on the density of molecular clouds due to the orientation of the ionization cone with respect tothe galactic disk. These results are consistent with other CT AGN with observed extended hard X-ray emission (e.g.,ESO 428-G014 and the Ma et al. 2020 CT AGN sample), further demonstrating the ubiquity of extended hard X-rayemission in CT AGN. Keywords: galaxies: active; X-rays: galaxies a r X i v : . [ a s t r o - ph . GA ] J a n INTRODUCTIONRecent
Chandra observations of nearby, Comptonthick (CT) active galactic nuclei (AGNs) have uncov-ered kiloparsec-scale extended hard X-ray and Fe K α line emission regions that have challenged our under-standing of the origin and extent of high energy photonsand what impact they may have on their host galaxies(e.g., Circinus , Ar´evalo et al. 2014; NGC 1068, Baueret al. 2015; ESO 428-G014, Fabbiano et al. 2017; NGC7212, Jones et al. 2020).In the classical picture, the hard X-ray continuum andfluorescent Fe K lines that are observed in AGN are gen-erated by the excitation of the obscuring material in theinner parsecs. Observing this characteristic energeticemission on host galaxy scales is unexpected. The pres-ence of extended emission outside of this inner regionhas interesting consequences for AGN feedback and itsimpact on the surrounding medium.The first well-studied case of hard X-ray emissionobserved outside of the nuclear region was in the CTAGN, ESO 428-G014 (Fabbiano et al. 2017, 2018a,b,2019). ESO 428-G014 exhibits extended emission pre-dominately in the soft X-ray band, but also has sig-nificant extent in the hard X-rays, including the bandaround Fe K α (6 . − . ∼ kpc scales, including NGC 7212.NGC 7212 is the farthest of these sources examined thusfar ( z = 0 . Chandra observa- tions for seven CT AGN, not previously known to haveextended emission and compared them with ESO 428-G014 and NGC 7212. They demonstrate that the ex-tended hard X-ray emission, including that from Fe K α ,is a characteristic feature of these obscured sources. Fur-thermore, this emission can contribute between ∼ −
36% of the total observed emission in 3 − Chandra observations anddata reduction for these CT AGN are described in Sec-tion 2. For each source we report on the spatial extentof the X-ray emission in Section 3, and discuss the im-plications of this population of extended X-ray AGN inSection 4. Our findings and conclusions are summarizedin Section 5. OBSERVATIONSOur sample consists of five CT AGN (log N H > − ) with archival Chandra aim point observations(Table 1). These observations were reprocessed with
Chandra-repro and analyzed using CIAO 4.11 (Frus-cione et al. 2006) and CALDB 4.8.2 and inspected forhigh background flares ( > σ ). Each individual ob-servation for each source was exposure-corrected andmerged , . We visually inspected each observation usingthe CIAO image analysis tools available in SAOImageds9 and enabled 1 / . (cid:48)(cid:48) ) to improve the spatial resolution of these ob-servations (as in e.g., Tsunemi et al. 2001; Wang et al.2011). From the merged observations for each source, wegenerated a full band (0.3-8.0 keV) adaptively smoothedimage (using dmimgadapt from the ds9 CIAO package )to investigate the detailed morphology of our CT AGN.The smoothing parameters used in this analysis werechosen to highlight the extended emission: 0 . −
15 pixelscale with 5 counts under the gaussian kernel for 30 it-erations, unless otherwise indicated.2.1.
MKN 573 http://cxc.harvard.edu/ciao/threads/combine/ http://cxc.harvard.edu/ciao/threads/merge all/ http://ds9.si.edu http://cxc.harvard.edu/ciao/gallery/smooth.html Table 1.
Chandra
ACIS-S Observation Log
Source ObsID t exp (ks) PI DateMKN 573 7745 38.08 Bianchi 2006-11-1812294 9.92 Wang 2010-09-1613124 52.37 Wang 2010-09-1713125 16.83 Wang 2010-09-19NGC 1386 4076 19.64 Kraemer 2003-11-1912289 17.32 Wang 2011-04-1313185 29.67 Wang 2011-04-1313257 33.82 Wang 2011-04-14NGC 3393 4868 29.33 Levenson 2004-02-2812290 69.16 Wang 2011-03-1220496 48.25 Maksym 2019-04-0420497 39.54 Maksym 2018-03-1920498 44.52 Maksym 2018-03-1821039 44.47 Maksym 2019-04-0921047 95.84 Maksym 2018-03-2321048 40.43 Maksym 2018-07-2322077 47.15 Maksym 2019-03-1122078 79.06 Maksym 2019-08-06NGC 5643 17031 72.12 Fabbiano 2015-05-2117664 41.53 Fabbiano 2015-12-26NGC 7212 4078 19.9 Kraemer 2003-07-2220372 49.42 Fabbiano 2018-08-0821668 51.38 Fabbiano 2018-08-1121672 27.21 Fabbiano 2018-09-07
MKN 573 is an SAB0 type galaxy at RA=01:43:57.80(25.991 ° ), Dec=+02:20:59.65 (2.350 ° ), and z = 0 . lum ∼
72 Mpc), with a double radio source (Nagaret al. 1999). The AGN ( M BH = 2 × M (cid:12) , Bian& Gu 2007; L x, − keV = 2 . × erg s − , RamosAlmeida et al. 2009) is optically classified as a Seyfert 2,but Ramos Almeida et al. (2008) finds evidence that anarrow-line Seyfert 1 is hiding beneath the CT obscuringmaterial ( N H > . × cm − ; Guainazzi et al. 2005).MKN 573 has been previously shown to have extended,biconical soft X-ray emission on kpc scales (Gonzalez-Martin et al. 2010; Paggi et al. 2012). We extend thisanalysis to the harder X-rays, focusing specifically onthe spatial extent of the 6 to 7 keV band where we ex-pect to find Fe K α line emission. The full-band (0 . − . NGC 1386 e-06 0.21 1.1 4.5 18 7 . . . : : . . . . e-06 0.21 1.1 4.5 18 7 NE1:44:00.0 59.0 58.0 57.0 43:56.0 . . . : : . . . . : . NE ″ Mkn 573 c o n e c r o ss - c o n e cts/px Figure 1.
Merged 0 . − . Chandra
ACIS image ofMKN 573 with applied adaptive gaussian smoothing ( dmin-gadapt ; 0 . −
15 pixel scales, 5 counts under kernel, 30 itera-tions) on image pixel = 1 / (cid:48)(cid:48) × (cid:48)(cid:48) (29.12 × (cid:48)(cid:48) (0.546 kpc) circularregion and cone/cross-cone quadrants used in our analysis ofthe X-ray extent. NGC 1386 is an SB0 type galaxy at RA=03:36:46.18(54.192 ° ), Dec=-35:59:57.87 (-35.999 ° ), and z = 0 . lum ∼
12 Mpc), with a water-megamaser (Schulz &Henkel 2003) and jet (Nagar et al. 1999). The AGN(log L x, − keV = 41 .
84 erg s − , Brightman et al. 2015)is optically classified as a Seyfert 2 (e.g., Brightman &Nandra 2011) with a Compton thick AGN ( N H = 5 . × cm − ; Brightman et al. 2015). The full band (0 . − . III narrow lines (e.g., Schmittet al. 2003) aligned along the north-south direction andcoincident with our defined “cone” region as shown inFigure 2. 2.3.
NGC 3393
NGC 3393 is an SBab type galaxy at RA=10:48:23.46(162.098 ° ), Dec=-25:09:43.4 (-25.162 ° ), and z = 0 . lum ∼
61 Mpc), with a triple-lobed radio source andextended ionization cones oriented along the north-eastdirection (e.g., Cooke et al. 2000). The AGN is opticallyclassified as a Seyfert 2 with a Compton thick obscura-tion ( N H = 1 . × cm − ; Marchesi et al. 2018; seealso Maiolino et al. 1998; Guainazzi et al. 2005; Burlonet al. 2011; Koss et al. 2015; Maksym et al. 2017). The e-06 0.059 0.3 1.2 5 2 - : : . . - : : . . e-06 0.059 0.3 1.2 5 2 NE49.0 48.0 47.0 3:36:46.0 45.0 44.0 43.0 - : : . . . . - : : . . . . NE ″ NGC 1386 c r o ss - c o n e c o n e cts/px Figure 2.
Merged 0 . − . Chandra
ACIS image ofNGC 1386 with applied adaptive gaussian smoothing ( dmin-gadapt ; 0 . −
15 pixel scales, 5 counts under kernel, 30 itera-tions) on image pixel = 1 / (cid:48)(cid:48) × (cid:48)(cid:48) (4.96 × (cid:48)(cid:48) (0.093 kpc) circular re-gion and cone/cross-cone quadrants used in our analysis ofthe X-ray extent. full band (0 . − . ° that wedesignate the “cone region”, as shown in Figure 2.2.4. NGC 5643
NGC 5643 is an SABc type galaxy at RA=14:32:40.74(218.170 ° ), Dec=-44:10:27.86 (-44.174 ° ), and z =0 . lum ∼
21 Mpc), with a water maser (Green-hill et al. 2003) and ultra-luminous X-ray source (e.g.,Annuar et al. 2015; Pintore et al. 2016). The AGN( L x, − keV = (0 . − . × erg s − , Annuar et al.2015) is optically classified as a Seyfert 2 (Cid Fer-nandes et al. 2001) with Compton thick obscuration( N H = 1 . × cm − ; Marchesi et al. 2018; see alsoRisaliti et al. 1999; Guainazzi et al. 2004; Maiolino et al.1998; Bianchi et al. 2006; Matt et al. 2013; Annuar et al.2015) likely from a nuclear rotating obscuration disk(Alonso-Herrero et al. 2018). The full band (0 . − .
015 0.11 0.53 2.2 9 3 : . . - : : . .
015 0.11 0.53 2.2 9 3
NE26.0 25.0 24.0 10:48:23.0 22.0 21.0 : . . . . . - : : . . . ″ NGC 3393 NE cts/px Figure 3.
Merged 0 . − . Chandra
ACIS image ofNGC 3393 with applied adaptive gaussian smoothing ( dmin-gadapt ; 0 . −
15 pixel scales, 10 counts under kernel, 30 itera-tions) on image pixel = 1 / (cid:48)(cid:48) × (cid:48)(cid:48) (21.28 × (cid:48)(cid:48) (0.399 kpc) circularregion and cone/cross-cone quadrants used in our analysis ofthe X-ray extent. line region ionization cone and kpc-scale radio lobes(Morris et al. 1985; Schmitt et al. 1994; Fischer et al.2013; Cresci et al. 2015) which forms the basis for ourcone/cross-cone regions (as indicated in Figure 4).2.5. NGC 7212
NGC 7212 is located at RA=22:07:01.30 (331.755 ° ),Dec:+10:13:52 (10.231 ° ), and z = 0 . lum ∼ M bh = 7 . L/L
Edd = − .
55; Hern´andez-Garc´ıa et al. 2015) isoptically classified as a Seyfert 2, with a kpc-scale ex-tended narrow line region (ENLR; e.g., Wasilewski 1981;Falcke et al. 1998; Schmitt et al. 2003; Cracco et al. 2011;Congiu et al. 2017), and typical characteristics of Comp-ton thick obscuration ( N H = 1 . × cm − ; March-esi et al. 2018; see also Risaliti et al. 2000; Guainazziet al. 2005; Levenson et al. 2006; Bianchi et al. 2006;Singh et al. 2011; Severgnini et al. 2012; Hern´andez-Garc´ıa et al. 2015). The full band (0 . − . . (cid:48)(cid:48) ; Falcke et al. 1998; Drake et al.2003). e-05 0.044 0.22 0.93 3.8 1 - : : . . . : . e-05 0.044 0.22 0.93 3.8 1 NE44.0 43.0 42.0 41.0 14:32:40.0 39.0 38.0 37.0 : . . . . . . : . NE ″ NGC 5643 c o n e c r o ss - c o n e cts/px Figure 4.
Merged 0 . − . Chandra
ACIS image ofNGC 5643 with applied adaptive gaussian smoothing ( dmin-gadapt ; 0 . −
15 pixel scales, 5 counts under kernel, 30 itera-tions) on image pixel = 1 / (cid:48)(cid:48) × (cid:48)(cid:48) (6.88 × (cid:48)(cid:48) (0.129 kpc) circular re-gion and cone/cross-cone quadrants used in our analysis ofthe X-ray extent.3. SPATIAL ANALYSISThe detailed morphologies that we are able to extractby capitalizing on the sub-pixel resolution of
Chandra enable a thorough investigation of the significance ofthe extended emission. Likewise, our sample is madeof sources with > ° quadrants (the biconical cone and cross-cone re-gions). Of the five sources, NGC 7212 is the only one tonot exhibit a strong azimuthal dependence.Using SAOImage ds9, we filtered our sources in eightenergy bands and generated concentric annuli withineach quadrant starting at the nucleus ( r = 0 . (cid:48)(cid:48) ) andworking radially outward, increasing the width as nec-essary to maintain a minimum of 10 counts, until theregions became noise and background dominated (typ-ically around 30 (cid:48)(cid:48) to 50 (cid:48)(cid:48) ). The surface brightness pro-files were extracted from these energy-and-quadrant-dependent regions (excluding obvious point sources) andbackground subtracted, before being compared to the Chandra
Point Source Functions (PSF) for the givenenergy band and regions (PSFs were created from an e-05 0.058 0.29 1.2 4.9 2 . . . . : : . . . : . e-05 0.058 0.29 1.2 4.9 2 NE04.0 03.0 02.0 01.0 22:07:00.0 . . . . : : . . . : . NE ″ NGC 7212 c r o ss - c o n e c o n e cts/px Companion Galaxy
Figure 5.
Merged 0 . − . Chandra
ACIS image ofNGC 7212 with applied adaptive gaussian smoothing ( dmin-gadapt ; 0 . −
15 pixel scales, 5 counts under kernel, 30 itera-tions) on image pixel = 1 / (cid:48)(cid:48) × (cid:48)(cid:48) (44.48 × (cid:48)(cid:48) (0.834 kpc) circularregion and cone/cross-cone quadrants used in our analysis ofthe X-ray extent. absorbed power-law spectrum typical for an AGN usingChaRT (Γ ∼ . N H =0 . × cm − ) and MARX5.4.0 , and following the CIAO simulation threads ).There are known uncertainties introduced when sim-ulating the Chandra
PSF with ChaRT and MARX ,specifically, for energies > − − (cid:48)(cid:48) and 100 (cid:48)(cid:48) ) based on the analy-sis “Wings of the Chandra
PSF” . An extent of 100 (cid:48)(cid:48) iswell outside of our area of interest that typically extendsonly to ∼ (cid:48)(cid:48) − ∼ (cid:48)(cid:48) before becoming noise dominated.For energies 2.4 − (cid:48)(cid:48) is ∼ .
2, and at 100 (cid:48)(cid:48) is ∼ .
7. For energies6.4 − (cid:48)(cid:48) is ∼ . http://cxc.harvard.edu/ciao/PSFs/chart2/ https://space.mit.edu/cxc/marx/ http://cxc.harvard.edu/ciao/threads/psf.html http://cxc.harvard.edu/ciao/threads/marx sim/ https://cxc.harvard.edu/ciao/PSFs/chart2/caveats.html https://cxc.harvard.edu/ccw/proceedings/02 proc/presentations/t gaetz . . . . . E x t e n t ( k p c ) Energy (keV) E x t e n t ( a r c s ec ) NGC1386ConeCross-ConePSF— FWHM--- 1 % SB . . . . . . . E x t e n t ( k p c ) Energy (keV) E x t e n t ( a r c s ec ) NGC3393ConeCross-ConePSF— FWHM--- 1 % SB . . . . . . . . . E x t e n t ( k p c ) Energy (keV) E x t e n t ( a r c s ec ) NGC5643ConeCross-ConePSF— FWHM--- 1 % SB . . . . . . . . E x t e n t ( k p c ) Energy (keV) E x t e n t ( a r c s ec ) NGC7212ConeCross-ConePSF— FWHM--- 1 % SB . . . . . . . . . E x t e n t ( k p c ) Energy (keV) E x t e n t ( a r c s ec ) MKN573ConeCross-ConePSF— FWHM--- 1 % SB Figure 6.
Emission extent as a function of energy calculated from the radial profiles for both the cone (red) and cross-cone(blue) regions of each CT AGN in our sample. The extent of the corresponding
Chandra
PSF is shown in grey. Solid lines: Fullwidth at half maximum surface brightness. Dashed lines: Full width at 1% of the peak surface brightness. 1-sigma errors areshown. at 100 (cid:48)(cid:48) is ∼ .
8. Taking this extreme factor into ac-count, we confirm that the 6.0 − > σ ) in both thecone and cross-cone regions. However, we expect errorsin the simulated PSF introduced by this method to beless than a factor of 2.8 at high energies and large ex-tent. Additional discrepancies between the simulatedand observed PSF associated with this method are mit-igated using the recommended AspectBlur in MARX of0.25 (cid:48)(cid:48) for ACIS-S observations. Despite these knownuncertainties, we observe a significant difference in thesource extent by cone angle, as described in the follow-ing sections, that cannot be solely attributed to poorlysimulating the Chandra
PSF.The
Chandra
PSFs were energy filtered and normal-ized to the source counts in the nuclear ( < . (cid:48)(cid:48) ) regionbefore being subtracted from the source radial profiles todetermine the quantity of total excess counts outside ofthe nuclear 0.5 (cid:48)(cid:48) region as a function of energy. We thencalculate the “total excess fraction” by dividing the totalexcess counts by the total counts (not PSF subtracted)over the entire region of interest. Similarly, we quantifyan extended excess by adding up the PSF subtractedcounts outside of a 1.5 (cid:48)(cid:48) region as a function of energy.By increasing the radius to 1.5 (cid:48)(cid:48) from 0.5 (cid:48)(cid:48) , we are fur-ther limiting any potential contamination from the CTAGN. We then calculate the “extended fraction” by di-viding the extended excess counts by the total counts(not PSF subtracted) over the entire region of interest.To better compare the extent in each energy band, wethen calculate the full width at half maximum (FWHM)and the full width at 1% of the surface brightness (inlog space) for each radial profile (following, e.g., Fab-biano et al. 2018a; Jones et al. 2020). This not onlynormalizes the brightness of each energy band, it alsominimizes the bias between each source in our sampleof five CT AGN caused by variations in signal-to-noise.These width calculations are made by fitting the radialprofiles with a spline approximation (or for profiles withless than four points, a gaussian curve) with errors de-rived from a bootstrap Monte Carlo analysis.3.1. MKN 573
MKN 573 exhibits extended emission with an az-imuthal dependence along the designated “cone” regionthat transitions into a circular blob at the higher ener-gies (Figure 13). The surface brightness in the cone andcross-cone lies predominately above the
Chandra
PSF,and exhibits bumps and waves outside of ∼ (cid:48)(cid:48) thatmay correspond to point sources that were unaccountedfor in the radial profile extraction. For 0 . − . ±
59 counts at > . (cid:48)(cid:48) above the Chandra
PSF in the cone region, and 978 ±
31 in cross-cone region(Table 2). Between 6 − ± ± . − . . ± . . ± . − . ± . . ± . . − . . ± . . ± . − . ± . . ± . ∼ . ∼ .
25 kpc farther than in the harder X-rays,respectively, although the slope of this extent as a func-tion of energy is fairly shallow, especially above ∼ ∼ . NGC 1386
Compared to MKN 573, NGC 1386 presents a morechallenging picture due to additional point sources pri-marily aligned with the cone region, even at the harderX-rays (Figure 15). Despite this, we successfully ex-tracted the radial profiles in each energy band (Figure16) and find, unsurprisingly, that the central region isdominated by the point source. Outside of ∼ − (cid:48)(cid:48) however, the surface brightness falls at a gentler slope.We calculate the excess counts above the PSF at > . (cid:48)(cid:48) and find, for 0 . − . ±
58 in the cone and886 ±
30 excess counts in the cross-cone region (Table3). Compared to the total counts in this energy band,we find a total excess fraction of 71 . ± . . ± . Table 2. MKN 573 − Excess counts over the
Chandra
PSF (normalized to the central 0.5 (cid:48)(cid:48) ) for select energy bands.
Energy Total Counts Counts > . (cid:48)(cid:48) Counts > . (cid:48)(cid:48) Extended Fraction Total Excess Fraction(kev) Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone0.3-1.5 5377 ±
73 3138 ±
56 3399 ±
56 774 ±
28 2312 ±
48 404 ±
20 43 . ± . . ± . . ± . . ± . ±
24 477 ±
22 261 ±
16 81 ± ±
14 69 ± . ± . . ± . . ± . . ± . ±
11 82 ± ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
10 107 ±
10 29 ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
79 4037 ±
64 3483 ±
59 978 ±
31 2562 ±
51 529 ±
23 40 . ± . . ± . . ± . . ± . X-rays between 6 − ± σ ) in the coneand 34 ± . ± . . ± . (cid:48)(cid:48) , we find a total extended fractionof 49 . ± . . ± . . − . − . ± . . ± . σ result.The radial profile FWHM as a function of energy forNGC 1386 is similar to what was found for MKN 573(Figure 6; top, right). The cone and cross cone are moreextended at soft energies than hard energies with a dif-ference of 0 . ∼ .
04 kpc, respectively, but re-main relatively flat above ∼ ∼ . NGC 3393
NGC 3393 is elongated in the “cone” region (Figure17) and continues to have an azimuthal dependence evenin the hard X-rays, although to a lesser extent. The ra-dial profiles (Figure 17) that we extract are peaky near-est the central point source before exhibiting a bumpoutside of ∼ (cid:48)(cid:48) in the cone region, similar to MKN573 and NGC 1386.From these radial profiles, we calculate the excesscounts above the Chandra
PSF and find the most countsout of our entire sample, 13080 ±
114 counts in the coneand 3785 ±
62 in the cross cone for 0 . − . − ±
14 excess counts in the cone and 169 ± . ± . . ± . . − . . ± . . ± . − . ± . . ± . . ± . . ± . > > . > ∼ . NGC 5643
NGC 5643 has an azimuthal dependence, as in theother CT AGN discussed thus far, however, this de-pendence is not symmetric around the central pointsource (Figure 19). There exists an interesting soft X-ray excess in the East-cone region. As the energy in-creases, this asymmetry lessens and even transitions toa slight excess in the West-cone region in the hard en-ergy bands. The radial profiles are consistent with thispicture and show lopsided curves surrounding the cen-tral point source (Figure 20).The total excess counts in the 0 . − . ±
54 in the cone region and 1052 ±
32 in the crosscone region (Table 5). At the 6 − ±
10 counts in the cone 38 ± . ± . . ± . Table 3. NGC 1386 − Excess counts over the
Chandra
PSF (normalized to the central 0.5 (cid:48)(cid:48) ) for select energy bands.
Energy Total Counts Counts > . (cid:48)(cid:48) Counts > . (cid:48)(cid:48) Extended Fraction Total Excess Fraction(kev) Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone0.3-1.5 3747 ±
61 1520 ±
39 2783 ±
53 713 ±
27 2022 ±
45 438 ±
21 53 . ± . . ± . . ± . . ± . ±
22 200 ±
14 298 ±
17 93 ±
10 172 ±
13 58 ± . ± . . ± . . ± . . ± . ±
12 40 ± ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
12 38 ± ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
68 1846 ±
43 3352 ±
58 886 ±
30 2313 ±
48 523 ±
23 49 . ± . . ± . . ± . . ± . Table 4. NGC 3393 − Excess counts over the
Chandra
PSF (normalized to the central 0.5 (cid:48)(cid:48) ) for select energy bands.
Energy Total Counts Counts > . (cid:48)(cid:48) Counts > . (cid:48)(cid:48) Extended Fraction Total Excess Fraction(kev) Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone0.3-1.5 10019 ±
100 2839 ±
53 9550 ±
98 2531 ±
50 7764 ±
88 1554 ±
39 77 . ± . . ± . . ± . . ± . ±
53 1047 ±
32 2434 ±
49 781 ±
28 1952 ±
44 530 ±
23 69 . ± . . ± . . ± . . ± . ±
22 261 ±
16 375 ±
19 154 ±
12 297 ±
17 117 ±
11 64 . ± . . ± . . ± . . ± . ±
18 244 ±
16 166 ±
13 58 ± ±
11 45 ± . ± . . ± . . ± . . ± . ±
17 281 ±
17 102 ±
10 82 ± ± ± . ± . . ± . . ± . . ± . ±
26 555 ±
24 203 ±
14 169 ±
13 82 ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
122 5375 ±
73 13080 ±
114 3785 ±
62 10400 ±
102 2254 ±
48 70 . ± . . ± . . ± . . ± . cone for 0 . − . . ± . . ± . − . ± . . ± . . − . . ± . . ± . − < ∼ . ∼ .
38 kpc farther than the cross-cone at 1% of the sur-face brightness. 3.5.
NGC 7212
Unlike the other CT AGN in this sample, NGC 7212does not exhibit a strong azimuthal dependence (Figure21), thus we select the “cone” region to align with theoptically classified extended narrow line emission region(e.g., Congiu et al. 2017). Extracting the radial profileswas made more challenging due to contamination fromthe companion galaxies in the North-cone region and thesoft X-ray filaments that connect them. They exhibit a similar “bump” to the other CT AGN in the inner ∼ (cid:48)(cid:48) ,but due to its distance, these potential wings are notwell resolved (Figure 22).The excess counts above the PSF in 0 . − . ±
37 in the cone and 731 ±
27 in the cross cone(Table 6). This corresponds to a total excess fractionof 54 . ± . . ± . . ± . . ± . − ± ± . ± . . ± . − . ± . . ± . ∼ . ∼ .
45 kpc difference in theextent between the soft and the hard X-rays. The cross-cone region, however, is much more consistent. At 1%of the surface brightness, the extent is flatter for the0
Table 5. NGC 5643 − Excess counts over the
Chandra
PSF (normalized to the central 0.5 (cid:48)(cid:48) ) for select energy bands.
Energy Total Counts > . (cid:48)(cid:48) > . (cid:48)(cid:48) Extended Fraction Total Excess Fraction(kev) Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone0.3-1.5 2288 ±
48 812 ±
29 2013 ±
45 588 ±
24 1762 ±
42 477 ±
22 77 . ± . . ± . . ± . . ± . ±
26 376 ±
19 481 ±
22 198 ±
14 424 ±
21 190 ±
14 64 . ± . . ± . . ± . . ± . ±
15 147 ±
12 126 ±
11 70 ± ±
10 61 ± . ± . . ± . . ± . . ± . ±
14 197 ±
14 109 ±
10 76 ± ± ± . ± . . ± . . ± . . ± . ±
12 110 ±
11 71 ± ± ± ± . ± . . ± . . ± . . ± . ±
16 256 ±
16 93 ±
10 38 ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
62 1950 ±
44 2880 ±
54 1052 ±
32 2448 ±
50 856 ±
29 64 . ± . . ± . . ± . . ± . cross-cone than the cone region, especially above 3 keV.The cone is ∼ . DISCUSSION4.1.
Spatial Extent at 1% Surface Brightness
As discussed in Section 3, we use the radial profilewidth at 1% of the surface brightness as a proxy mea-surement for the X-ray extent of our CT AGN. For thecone region, we find that the CT AGN with the largestmeasured extent is NGC 3393 with extent = 2 . extent = 2 . . .
67 kpc (NGC 5643), and 0 . . . . . .
19 kpc (NGC 1386).To better compare the slopes of these extent-energyrelationships, we renormalized the extent of each sourcein kpc to the softest X-ray band (Figure 7), and fit theslopes with a simple line model. We find that the coneregions exhibit steeper drops in the X-ray extent withincreasing energy, averaging a ∼
50 % drop by 6 − ∼
10 %, on average, by 6 − ),black hole mass, X-ray luminosity (2 −
10 keV), and1
Table 6. NGC 7212 − Excess counts over the
Chandra
PSF (normalized to the central 0.5 (cid:48)(cid:48) ) for select energy bands.
Energy Total Counts > . (cid:48)(cid:48) > . (cid:48)(cid:48) Extended Fraction Total Excess Fraction(kev) Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone Cone Cross-cone0.3-1.5 868 ±
30 631 ±
25 552 ±
24 328 ±
18 339 ±
18 172 ±
13 39 . ± . . ± . . ± . . ± . ±
26 429 ±
21 393 ±
20 141 ±
12 221 ±
15 75 ± . ± . . ± . . ± . . ± . ±
16 181 ±
13 119 ±
11 80 ± ± ± . ± . . ± . . ± . . ± . ±
15 153 ±
12 101 ±
10 35 ± ± ± . ± . . ± . . ± . . ± . ±
14 147 ±
12 73 ± ± ± ± . ± . . ± . . ± . . ± . ±
14 180 ±
13 54 ± ± ± ± . ± . . ± . . ± . . ± . ± ± ± ± ± ± . ± . . ± . . ± . . ± . ±
50 1760 ±
42 1359 ±
37 731 ±
27 751 ±
27 331 ±
18 30 . ± . . ± . . ± . . ± . Table 7.
Total combined excess fraction and observed properties of our CT AGN.Total Excess Fraction log N H (a) d log M BH (c) log L x, − keV (d) log νL ν, µm (e) λ Edd (f)
Source Cone+Cross-cone (cm − ) (kpc) (M (cid:12) ) (erg s − ) (erg s − )MKN 573 43 . ± . > . . ± .
06 7 .
37 41 .
54 43 . ± .
08 0.0105NGC 1386 65 . ± . . ± .
09 5 . ± .
004 7 .
24 41 .
60 42 . ± .
09 0.0010NGC 3393 83 . ± . . +0 . − . . ± .
02 7 .
48 41 .
29 42 . ± .
08 0.0018NGC 5643 68 . ± . . +0 . − . . ± .
004 6 .
30 40 .
87 42 . ± .
12 0.0121NGC 7212 49 . ± . . +0 . − . . ± .
09 7 .
54 42 .
60 43 . ± .
15 0.0092
Note — (a) Guainazzi et al. 2005; Brightman et al. 2015; Marchesi et al. 2018; (b) de Vaucouleurs et al. 1991; (c)
Bian & Gu2007; Kondratko et al. 2008; Hern´andez-Garc´ıa et al. 2015; (d)
Gonz´alez-Mart´ın et al. 2015; Hern´andez-Garc´ıa et al. 2015; (e)
Asmus et al. 2014; (f) λ Edd = νL ν, µm /L Edd , where L Edd = 1 . × ∗ M BH and νL ν, µm is used as a proxy for L bol . Energy (keV) . . . . . . . . R e n o r m a li z e d E x t e n t MKN573 NGC1386 NGC3393 NGC5643 NGC7212— CONE
Energy (keV) . . . . . . . . R e n o r m a li z e d E x t e n t MKN573 NGC1386 NGC3393 NGC5643 NGC7212— CROSS-CONE
Figure 7.
Renormalized extent (kpc) at 1% of the surface brightness for our sample of five CT AGN as a function of energy:(left) cone regions (right) cross-cone regions. . . . . . . . . log vL v, µm (erg s ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone . . . . . . . . log vL v, µm (erg s ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ .
00 41 .
25 41 .
50 41 .
75 42 .
00 42 .
25 42 . log L X, (erg s ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone .
00 41 .
25 41 .
50 41 .
75 42 .
00 42 .
25 42 . log L X, (erg s ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ . . . . . . . log M BH (M ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone . . . . . . . log M BH (M ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ d (kpc) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone d (kpc) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ . . . . . . . . . log N H (cm ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone . . . . . . . . . log N H (cm ) . . . . . . . . S l o p e o f E x t e n t v s . E n e r g y MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ Figure 8.
Best-fit slope of the extent at 1% of the surface brightness versus energy in the cone and cross-cone regions (Figure7) for each of the five CT AGN as a function of observed properties: (top to bottom) log N H , d , log M BH , log L x, − keV ,log νL ν, µm . For each characteristic property, we find that the extent in the cross-cone region is less likely to be influenced byenergy (i.e., the slope is consistent with 0). We observe a potentially interesting trend with black hole mass in the cone region(center, left). µm Luminosity (Table 7; Figure 8). For each charac-teristic property, we find little to no slope in the cross-cone region. In the cone region, the slopes are morediverse. Interestingly, the slope for NGC 3393 is verysteep, deviating from a possible trend made by the otherfour sources in N H , d , log L x, − , and log νL ν, µm .For all five sources, however, there may exist an inter-esting correlation between M BH and the slope of the ex-tent as a function of energy, such that for higher blackhole masses, the soft X-ray extent dominates the hardX-rays.4.2. Spatial Extent as a Function of Observables
Since our sample is made up of “nearby” CT AGN, theavailability of multiwavelength data provides a uniqueadvantage to probe the X-ray extent as a function ofAGN and host galaxy properties (Table 7). We split oursample into their respective cone and cross-cone regionsand then calculate the total excess fraction for theseregions in the wide-band 0 . − . . − . (cid:48)(cid:48) in 0 . − . . − . Column Density
We first probe the dependence of the X-ray extent onthe obscuring column density (Figure 9). We calculatethe Pearson coefficient of this dependence in each re-gion for each energy band, noting that our sources onlycover a limited range in column density clustered aroundlog N H ∼
24 and more sources with diverse column den-sities are required to better probe this correlation. In0 . − . . − . N H and the total excesshard X-ray fraction that is stronger than that found withthe Ma et al. (2020) sources alone (coefficient of 0.42), al-though the strength of this correlation is mostly drivenby NGC 1386. In the cross-cone region for both thewider 0 . − . . − . https://docs.scipy.org/doc/scipy/reference/generated/scipy.stats.pearsonr.html -0.26 (0.34 including the Ma et al. 2020 sources), respec-tively. This suggests that the nuclear obscuration maybe correlated with the abundance of molecular clouds inthe disk. The cross-cone region, however, does not ex-hibit this trend. This may be explained by a torus withobscuration that dominates in this plane over any effectsfrom molecular clouds, or more simply that molecularclouds are not coupled with obscuration of the torus inthe disk plane.4.2.2. Host Galaxy Diameter
For each source, we compare the excess fraction withthe d diameter measure of the host galaxy from the Third Reference Catalog of Bright Galaxies (de Vau-couleurs et al. 1991), as shown in Figure 10. We cal-culate the Pearson coefficient of this dependence in eachregion for each energy band. In both the full-band andhard-band cone region, we find the excess fraction shal-lowly decreases with increasing d (Pearson coefficientsof -0.62 and -0.64, respectively). This may imply thatthe extent of the galaxy is uncoupled from the extent ofthe AGN emission, such that as the host galaxy increasesin size, there is not any additional energy from the cen-tral source imparted into the host galaxy to maintain aconstant excess fraction. This may be further compli-cated by evolutionary effects, such that in the presenceof strong outflows, the bicone may be more spatiallydeveloped. As with N H , there is no significant trendobserved in the cross-cone region (Pearson coefficientsof -0.04 and -0.36 in 0 . − . . − . Black Hole Mass
The black hole masses for our sources are calculatedfrom independent dynamical measurements (Bian & Gu2007; Hern´andez-Garc´ıa et al. 2015 and determined fromwater maser observations (NGC 3393; Kondratko et al.2008); Table 7). While the masses are not well con-strained, we do not see a strong dependence on the to-tal excess fraction with black hole mass for either en-ergy band or region (Figure 11). The Pearson coeffi-cients of these dependences are -0.18 (cone) and -0.26(cross-cone) in 0 . − . . − . “Extended” X-ray Luminosity We then explore whether there is a correlationbetween the nuclear luminosity (for which we use12 µmL IR as a proxy) with the luminosity of the ex-tended emission (Figure 12). We calculate the extendedluminosity using the extended counts (PSF subtractedcounts > . (cid:48)(cid:48) ; Tables 2,3,4,5,6) multiplied by 4 πd ,where d is the distance in cm. We find a positive4 . . . . . . . log N H (cm ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212
Ma+ 2020 (0.3 . . . . . . . log N H (cm ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212
Ma+ 2020 (3.0 . . . . . . . log N H (cm ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212
Ma+ 2020 (0.3 ⇥ . . . . . . . log N H (cm ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212
Ma+ 2020 (3.0 ⇥ Figure 9.
Total excess fraction in the cone (left) and cross-cone (right) regions for each of the five CT AGN as a functionof column density (log N H ; Table 7) for both the wide-band (0 . − . . − . . − . d (kpc) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72120.3 d (kpc) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72120.3 ⇥ d (kpc) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72123.0 d (kpc) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72123.0 ⇥ Figure 10.
Total excess fraction in the cone (left) and cross-cone (right) regions for each of the five CT AGN as a function ofhost galaxy diameter (d ; Table 7) for both the wide-band (0 . − . . − . for the cone region, but none in the cross-coneregion. . . . . . . . log M BH (M ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72120.3 . . . . . . . log M BH (M ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72120.3 ⇥ . . . . . . . log M BH (M ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72123.0 . . . . . . . log M BH (M ) T o t a l E x ce ss F r a c t i o n ( % ) MKN573 NGC1386 NGC3393 NGC5643 NGC72123.0 ⇥ Figure 11.
Total excess fraction in the cone (left) and cross-cone (right) regions for each of the five CT AGN as a function ofblack hole mass (log M BH ; Table 7) for both the wide-band (0 . − . . − . M BH , influences the total excess fraction in either energy band, but the cone region is more dispersedthan the cross-cone region. . . . . . . . . log ⌫L ⌫, µm (erg s ) l og L e x t e n d e d ( c t s c m ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone . . keV . . . . . . . . log ⌫L ⌫, µm (erg s ) l og L e x t e n d e d ( c t s c m ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cone . . keV . . . . . . . . log ⌫L ⌫, µm (erg s ) l og L e x t e n d e d ( c t s c m ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ . . keV . . . . . . . . log ⌫L ⌫, µm (erg s ) l og L e x t e n d e d ( c t s c m ) MKN573 NGC1386 NGC3393 NGC5643 NGC7212Cross-Cone ⇥ . . keV Figure 12.
Luminosity of the extended emission in the cone (left) and cross-cone (right) regions for each of the five CT AGNas a function of the nuclear luminosity for both the soft energy band (0 . − . . − . νL ν, µm ; Table 7). We find enhanced extended luminosities athigher nuclear luminosities, likely due to the increased availability of nuclear photons. . − . . − . CONCLUSIONWe have analyzed and compared the spatial extent offive CT AGN that exhibit extended X-ray emission in
Chandra observations .1. We find extended emission in the cone region forall five CT AGN in our sample, MKN 573, NGC1386, NGC 3393, NGC 5643, and NGC 7212. Thisemission is significant across all three of our met-rics, including, counts over the PSF, the total ex-cess fraction, and the extended fraction for boththe full X-ray band (0 . − . α line (6 − Chandra
PSF, total excessfraction, and extended fraction for the entire sam-ple from 0 . − . − > σ sig-nificance in the extended fraction (although counts > . (cid:48)(cid:48) and total excess fraction are significant).3. We show that the extent as a function of energy at1% of the surface brightness in the cone region ofour CT AGN exhibits a steeper relationship com-pared to the cross-cone region (with the exceptionof NGC 3393 that exhibits a similar cone-cross-cone slope). This may be explained by an inclina-tion effect, in which the orientation of the ioniza-tion cone with respect to the galactic disk molec-ular clouds impacts the extent to which the softX-rays propagate through the ISM. We further in-vestigate these slopes as a function of galaxy prop-erties and find for the cone region that the slopedecreases as the mass of the black hole increases. 4. We compare the extent of our sample at 1% of thesurface brightness with the column densities forboth the cone and cross-cone region. In the coneregion, we find a positive trend between N H andthe X-ray extent that may indicate that nuclearobscuration along the ionization cone is correlatedwith the disk molecular clouds. The cross-conedoes not exhibit a trend, suggesting that the nu-clear torus is the dominant obscurer.5. We do not find a clear correlation between theexcess fraction and black hole mass for our sam-ple, despite finding that as the black hole massincreases, the soft X-rays extend farther than thehard X-rays. We do find, however, a shallow trendin the excess fraction of our five CT AGN in thecone region with host galaxy extent (d ), but notrend in the cross-cone region.6. We use L IR as a proxy for the nuclear luminosityand investigate how luminosity impacts the lumi-nosity of the extended X-rays. To do this, we usethe counts ∗ πd as a proxy for the extended lu-minosity. We find that as the nuclear luminosityincreases, the extended luminosity also increases,likely due to the heightened availability of AGNphotons.We would like to thank the referee for constructivecomments and suggestions to improve this paper. Theanalysis of NGC 3393 was in part, the Master thesisof K. Parker at University of Southampton, UK. Thiswork makes use of data from the Chandra data archive,and the NASA-IPAC Extragalactic Database (NED).The analysis makes use of CIAO and Sherpa, devel-oped by the
Chandra
X-ray Center; SAOImage ds9;XSPEC, developed by HEASARC at NASA-GSFC; andthe Astrophysics Data System (ADS). JW acknowledgessupport by the National Key R&D Program of China(2016YFA0400702) and the NSFC grants (U1831205,11473021, 11522323). This work was supported by theChandra Guest Observer programs, grant no. GO5-16101X GO7-18112X, GO8-19099X, GO8-19096X (PI:Maksym); GO8 − A. X-RAY EXTENT AS A FUNCTION OF ENERGYWe have appended the adaptively smoothed images of our five CT AGN, each divided into six energy bins between0 . − . . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e . . . : : . . . . NE10 ″ c o n e c r o ss - c o n e cts/px cts/pxcts/pxcts/pxcts/px cts/px Figure 13.
Adaptively smoothed images of MKN 573 in the indicated energy bands on image pixel = 1/8 ACIS pixel( dmingadapt ; 0 . −
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.546 kpc) circularregion and cone/cross-cone regions.9
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.546 kpc) circularregion and cone/cross-cone regions.9
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone4.0-5.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone6.0-7.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone4.0-5.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone6.0-7.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone0.3-1.5 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone1.5-3.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone3.0-4.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone0.3-1.5 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone1.5-3.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone3.0-4.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone0.3-8.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone0.3-8.0 keVChandra PSF
Mkn 573 Mkn 573
Figure 14.
Background subtracted radial profiles of MKN 573 for the indicated energy bands compared to the
Chandra
PSFwhich has been re-normalized to the 0.5 (cid:48)(cid:48) (0.182 kpc) nuclear region for both the cone and cross-cone regions (as labeled“Cone” and “XCone”, respectively). Each bin contains a minimum of 10 counts and is shown with 1 σ error. We include adashed horizontal line to indicate the level of background emission and note that points below this line are valid data since thebackground has already been subtracted. Downward arrows indicate a region at or below the background. - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e - : : . . - : : . . NE10 ″ c r o ss - c o n e c o n e cts/px cts/pxcts/pxcts/pxcts/px cts/px Figure 15.
Adaptively smoothed images of NGC 1386 in the indicated energy bands on image pixel = 1/8 ACIS pixel( dmingadapt ; 0 . −
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.093 kpc) circularregion and cone/cross-cone regions.
20 0 20 40
R (arcsec) c t s / p i x e l Cone0.3-1.5 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone1.5-3.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone3.0-4.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone0.3-1.5 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone1.5-3.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone3.0-4.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone4.0-5.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone6.0-7.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l Cone4.0-5.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l Cone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone6.0-7.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l Cone0.3-8.0 keVChandra PSF
20 0 20 40
R (arcsec) c t s / p i x e l XCone0.3-8.0 keVChandra PSF
NGC 1386 NGC 1386
Figure 16.
Background subtracted radial profiles of NGC 1386 for the indicated energy bands compared to the
Chandra
PSF which has been re-normalized to the 0.5 (cid:48)(cid:48) (0.031 kpc) nuclear region for both the cone and cross-cone regions (as labeled“Cone” and “XCone”, respectively). Each bin contains a minimum of 10 counts and is shown with 1 σ error. We include adashed horizontal line to indicate the level of background emission and note that points below this line are valid data since thebackground has already been subtracted. Downward arrows indicate a region at or below the background. : . . - : : . . ″ cross-cone coneNE : . . - : : . . ″ cross-cone coneNE : . . - : : . . ″ cross-cone coneNE : . . - : : . . ″ cross-cone coneNE e-06 0.025 0.13 0.53 2.1 8. : . . - : : . . ″ cross-cone coneNE e-05 0.034 0.17 0.71 2.9 1 : . . - : : . . ″ cross-cone coneNE cts/px cts/pxcts/pxcts/px cts/pxcts/px Figure 17.
Adaptively smoothed images of NGC 3393 in the indicated energy bands on image pixel = 1/8 ACIS pixel( dmingadapt ; 0 . −
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.399 kpc) circularregion and cone/cross-cone regions.
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone0.3-1.5 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone1.5-3.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone3.0-4.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone0.3-1.5 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone1.5-3.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone3.0-4.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone4.0-5.0 keVChandra PSF
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R (arcsec) c t s / p i x e l XCone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l XCone6.0-7.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone4.0-5.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone6.0-7.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone0.3-8.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone0.3-8.0 keVChandra PSF
NGC 3393 NGC 3393
Figure 18.
Background subtracted radial profiles of NGC 3393 for the indicated energy bands compared to the
Chandra
PSF which has been re-normalized to the 0.5 (cid:48)(cid:48) (0.133 kpc) nuclear region for both the cone and cross-cone regions (as labeled“Cone” and “XCone”, respectively). Each bin contains a minimum of 10 counts and is shown with 1 σ error. We include adashed horizontal line to indicate the level of background emission and note that points below this line are valid data since thebackground has already been subtracted. Downward arrows indicate a region at or below the background. - : : . . . : . ″ c o n e c r o ss - c o n e NE - : : . . . : . ″ c o n e c r o ss - c o n e NE - : : . . . : . ″ c o n e c r o ss - c o n e NE - : : . . . : . ″ c o n e c r o ss - c o n e NE - : : . . . : . ″ c o n e c r o ss - c o n e NE e-08 0.015 0.073 0.31 1.2 4. - : : . . . : . ″ c o n e c r o ss - c o n e NE cts/px cts/pxcts/pxcts/pxcts/px cts/px Figure 19.
Adaptively smoothed images of NGC 5643 in the indicated energy bands on image pixel = 1/8 ACIS pixel( dmingadapt ; 0 . −
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.129 kpc) circularregion and cone/cross-cone regions.
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone0.3-1.5 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone1.5-3.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone3.0-4.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone0.3-1.5 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone1.5-3.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone3.0-4.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone4.0-5.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone5.0-6.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone6.0-7.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone4.0-5.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone5.0-6.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone6.0-7.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l Cone0.3-8.0 keVChandra PSF
20 0 20 40 60
R (arcsec) c t s / p i x e l XCone0.3-8.0 keVChandra PSF
NGC 5643 NGC 5643
Figure 20.
Background subtracted radial profiles of NGC 5643 for the indicated energy bands compared to the
Chandra
PSF which has been re-normalized to the 0.5 (cid:48)(cid:48) (0.043 kpc) nuclear region for both the cone and cross-cone regions (as labeled“Cone” and “XCone”, respectively). Each bin contains a minimum of 10 counts and is shown with 1 σ error. We include adashed horizontal line to indicate the level of background emission and note that points below this line are valid data since thebackground has already been subtracted. Downward arrows indicate a region at or below the background. . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE . . . . : : . . . : . ″ c r o ss - c o n e c o n e NE cts/px cts/pxcts/pxcts/pxcts/px cts/px Figure 21.
Adaptively smoothed images of NGC 7212 in the indicated energy bands on image pixel = 1/8 ACIS pixel( dmingadapt ; 0 . −
15 pixel scales, 2 − (cid:48)(cid:48) × (cid:48)(cid:48) . Also shown are the 1.5 (cid:48)(cid:48) (0.834 kpc) circularregion and cone/cross-cone regions.
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone0.3-1.5 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone1.5-3.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone3.0-4.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone0.3-1.5 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone1.5-3.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone3.0-4.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone4.0-5.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone5.0-6.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone6.0-7.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone4.0-5.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone5.0-6.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone6.0-7.0 keVChandra PSF
10 0 10 20 30
R (arcsec) c t s / p i x e l Cone0.3-8.0 keVChandra PSF
10 0 10 20
R (arcsec) c t s / p i x e l XCone0.3-8.0 keVChandra PSF
NGC 7212 NGC 7212
Figure 22.
Background subtracted radial profiles of NGC 7212 for the indicated energy bands compared to the
Chandra
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