The Role of Environment in Fueling Seyfert AGN
Erin K. S. Hicks University of Alaska Anchorage
Francisco Müller-Sánchez (CASA), Matt Malkan (UCLA), Po-Chieh Yu (UCLA), Richard Davies (MPE)
* Support from NSF AAG under award AST-1008042. UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs.
Potential Seyfert AGN fueling mechanisms:
i. Major mergers
ii. Minor mergers
iii. Accretion of gas streamers
vi. Secular evolution
Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs.
Potential Seyfert AGN fueling mechanisms:
i. Major mergers Several studies suggest not major mergers: ª Over 50% of z~2 AGN in undisturbed ii. Minor mergers host galaxies (Koceviski et al. 2012) ª AGN at z~2 not in galaxies with iii. Accretion of enhanced star formation (Rosario et gas streamers al. 2013)
vi. Secular evolution
Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs.
Potential Seyfert AGN fueling mechanisms:
i. Major mergers ª Minor mergers may be associated with low and intermediate luminosity AGN ii. Minor mergers (Neistein & Netzer 2014) ª Number required to account for iii. Accretion of dust in early type galaxies is gas streamers 250 times greater than predicted (Simões Lopes et al 2007, Martini et al 2013) vi. Secular evolution
Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs.
Potential Seyfert AGN fueling mechanisms:
i. Major mergers
ii. Minor mergers
iii. Accretion of gas streamers We focus on these using circumnuclear H2 kinematics vi. Secular evolution
Erin K. S. Hicks IAU August 2015 UAA Detailed Kinematics Required Physics & Astronomy ² Imaging studies cannot differentiate between the relative roles of minor mergers, gas accretion (due to interactions or streamers), and secular evolution
² Detailed studies of the kinematics are needed
² Also need to look at spatial scales with relevant timescales:
ü AGN duty cycle is 100 Myrs with flickering on scales of 1-10 Myrs (e.g. Hickox et al. 2014) ü At r=100pc v=100-150 km s-1 (Hicks et al. 2013) à Dynamical timescale of 2-3 Myrs, comparable to duty cycle
With local galaxies we can probe the central few hundred parsecs at the resolution needed to accurately measure the nuclear gas and stellar kinematics
Erin K. S. Hicks IAU August 2015 Summary of Observations PSF FWHM ID Galaxy (pc) OSIRIS 1a NGC 6814 18 1q NGC 864 12 UAA 2a NGC 4151 8 2q NGC 5383 32 Matched Sample: Seyfert & Quiescent3a NGCGalaxies 7469 35 Physics & 3q NGC 5614 47 Astronomy 4a NGC 3227 6 Galaxy pairs (from Martini et al. 2003) Summary4q NGC of Observations 2406 -- matched in large scale (>kpc) host galaxy 5a NGC 4593 PSF FWHM-- ID5q NGCGalaxy 5614 (pc)-- properties: SINFONIOSIRIS 1a NGC 32276814 5618 1q ICNGC 5267 864 9012 galaxy type, optical luminosity, angular & 2a NGC 56434151 408 2q NGC 53834030 3287 size, inclination, and distance 3a NGC 74696300 3540
et 2014et al. 3q NGC 56143368 4730 VLT SINFONI: 5 pairs
resolution sample 4q4q NGCNGC 2406628 --28 5a5a NGCNGC 45937743 --50 5q5q NGCNGC 5614357 --97 SINFONI 1a NGC 3227 56 1q IC 5267 90 2a NGC 5643 40 Erin K. S. Hicks 2q NGCIAU 4030 August 201587 3a NGC 6300 40 3q NGC 3368 30 4a NGC 6814 57 4q NGC 628 28 5a NGC 7743 50 5q NGC 357 97 UAA Comparison of Integrated Properties Physics & Astronomy Seyferts systematically have: AGN
(1) a more centrally concentrated nuclear stellar surface brightness (2) a lower central stellar inactive velocity dispersion (r < 200 pc)
Stars traced by CO 2.3µm bandheads
Hicks et al. 2013
Erin K. S. Hicks IAU August 2015 UAA Comparison of Integrated Properties Physics & Astronomy OSIRIS extended high resolution sample Seyferts systematically have: AGN
(1) a more centrally concentrated nuclear stellar surface brightness (2) a lower central stellar inactive velocity dispersion (r < 200 pc)
Stars traced by CO 2.3µm bandheads
Hicks et al. 2013
Erin K. S. Hicks IAU August 2015 The Astrophysical Journal,768:107(17pp),2013May10 Hicks et al.
UAA Comparison of Integrated Properties Physics & Figure 18. Mean uniformly weighted CO velocity dispersion of all pixels within apertures of radius (a) 0–100 pc and (b) 100–250 pc and (c) the ratio of these two. The Astronomy triangles represent Seyfert galaxies while circles are quiescent galaxies. The error bars represent the standard deviation of the dispersion measured in the pixels within the aperture considered. The probability that the two subsamples are drawn from different parent populations based on both the r 0–100 pc and r 100–250 pc apertures is 93.8%. = = Seyferts systematically have: (A color version of this figure is available in the online journal.)
(1) a more centrally AGN concentrated nuclear stellar surface brightness (2) a lower central stellar velocity dispersion inactive (r < 200 pc)
(3) more centrally Hicks et al. 2013 concentrated H2 surface brightness profiles
Figure 19. Mean H2 luminosity as a function of radius (a) intrinsic values and (b) normalized to 250 pc. The error bars are the standard deviations of measurements (4) elevated central within each aperture. The triangles represent Seyfert galaxies while circles are quiescent galaxies. The dashed curves and arrows represent upper limits. The label on the curve for each galaxy is as given in Table 1. Molecular gas (A color version of this figure is available in the online journal.) H2 1-0 S(1) luminosity traced by (r < 250 pc) H2 1-0 S(1)
Erin K. S. Hicks IAU August 2015
Figure 20. Total H2 luminosity in an apertures of radius (a) 0–100 pc and (b) 100–250 pc and (c) the ratio of these two. The triangles represent Seyfert galaxies while circles and upper limits are quiescent galaxies. The error bars represent the 10% systematic uncertainty of the flux calibration. The probability that the two subsamples are drawn from different parent populations based on the r 0–100 pc aperture is 96.9%. = (A color version of this figure is available in the online journal.)
14 The Astrophysical Journal,768:107(17pp),2013May10 Hicks et al.
UAA Comparison of Integrated Properties Physics & Figure 18. Mean uniformly weighted CO velocity dispersion of all pixels within apertures of radius (a) 0–100 pc and (b) 100–250 pc and (c) the ratio of these two. The Astronomy triangles represent Seyfert galaxies while circles are quiescent galaxies. The error bars represent the standard deviation of the dispersion measured in the pixels within the aperture considered. The probability that the two subsamples are drawnOSIRIS from extended different parenthigh populations based on both the r 0–100 pc and r 100–250 pc apertures is 93.8%. resolution sample = = Seyferts systematically have: (A color version of this figure is available in the online journal.)
(1) a more centrally AGN concentrated nuclear stellar surface brightness (2) a lower central stellar velocity dispersion inactive (r < 200 pc)
(3) more centrally Hicks et al. 2013 concentrated H2 surface brightness profiles
Figure 19. Mean H2 luminosity as a function of radius (a) intrinsic values and (b) normalized to 250 pc. The error bars are the standard deviations of measurements (4) elevated central within each aperture. The triangles represent Seyfert galaxies while circles are quiescent galaxies. The dashed curves and arrows represent upper limits. The label on the curve for each galaxy is as given in Table 1. Molecular gas (A color version of this figure is available in the online journal.) H2 1-0 S(1) luminosity traced by (r < 250 pc) H2 1-0 S(1)
Erin K. S. Hicks IAU August 2015
Figure 20. Total H2 luminosity in an apertures of radius (a) 0–100 pc and (b) 100–250 pc and (c) the ratio of these two. The triangles represent Seyfert galaxies while circles and upper limits are quiescent galaxies. The error bars represent the 10% systematic uncertainty of the flux calibration. The probability that the two subsamples are drawn from different parent populations based on the r 0–100 pc aperture is 96.9%. = (A color version of this figure is available in the online journal.)
14 UAA Comparison of Integrated Properties Physics & Astronomy Seyferts systematically have: Ø dynamically cold (in (1) a more centrally comparison to the bulge) concentrated nuclear component of gas and stellar surface brightness stars on scales of hundreds of parsecs in (2) a lower central stellar Seyferts velocity dispersion (r < 200 pc) Ø significant gas reservoir and a relatively young stellar population (3) more centrally concentrated H2 surface Ø nuclear stellar population brightness profiles requires a supply of gas (4) elevated central from which to form à inflow required H2 1-0 S(1) luminosity (r < 250 pc) Hicks et al. 2013
Erin K. S. Hicks IAU August 2015 8 8 Davies et al. Davies et al.
Fueling AGN II: Spatially Resolved Molecular Inflows and Outflows 9
8 Davies et al.
Fig. 3.— Molecular gas as traced by the 1-0 S(1) line in NGCFig. 3.—3227,Molecular showing the gassame as traced region by as the in 1-0 Fig. S(1) 1. line Top in row: NGC observed 3227, showing flux the same region as in Fig. 1. Top row: observed flux distribution, and the residual flux after subtracting ellipticaldistribution, isophotes and centered the residual on the flux nucleus; after the subtracting right panel elliptical shows isop thehotes V-H dustcentered on the nucleus; the right panel shows the V-H dust Fig. 4.— ImagesUAAstructure of the map circumnuclear reproduced ring from in Martini NGC 3227. et al. Left: (2003). H-band Bottom frstructureom row: HST obser map (square-rootved reproduced velocity scaling), from field, Martini disk after model, subtracting et al. and (2003). the a dimodel Bottomfference of row: t betweenhe obser themved velocity field, disk model, and the difference between them bulge and disk derived from larger scales. Right: the CO 2-1 map from Schinnerer, Eckart & Tacconi (2000). Reproduced fromDaviesetal. showing the strong velocity residuals′′ in the central few arcsec.showing This suggests the strongthat velocity a simple residuals disk is in not the an central appropriate few arcsec. model′′ This for this suggests galaxy,that a simple disk is not an appropriate model for this galaxy, (2006). The centraland Fig. rectangle 4 shows indicates an alternative the ∼ 1 of afield disk of with view a ring analysed generated inand that by Fig. a paper, lar 4ge-scale shows which an bar. alternative is significantly The rightmost of a disk sm panelaller with is than a a ring map the generated of 6.5 thefield velocity by we a lar dispersion.ge-scale bar. The rightmost panel is a map of the velocity dispersion. use here. In thisThe and dashed other ellipse figures represents of NGC3227, the locationKinematic the dashed of the elli circumnuclearpse represents TheAnalysis: ring. dashed the Axis location ellipsescales represents of are theInflows in circumnuclear arcsec, the location with a ring. ofconversion the Axis circumnuclear toscales parsec are given;ring. in Axis northscales is are in arcsec, with a conversion to parsec given; north is arcsec; north is up and east is left. Physicsup & and east is left. up and east is left. Astronomy arcsec
No. 1, 2009 ROLE OF MOLECULAR GAS IN AGNs 453 No. 1, 2009 ROLE OF MOLECULAR GASk m IN s- 1 AGNsk m s- 1 453 Fig. 4.— Density (left) and lineFig. of 3.—sightMolecular velocity (right) gas as forFig. traced a hydrodynami 4.— byDensity the 1-0cal S(1) (left) simulation line and in line NGC of of a sight3227, disk velocitywith showing a circumnuclear (right) the same for a region hydrodynami ring as(spiral) in Fig.cal 1. simulation Top row: of observed a disk with flux a circumnuclear ring (spiral) generated by a large scale bar, matchingdistribution, model and D20 the from residual Maciejewskigenerated flux after by (200 subtractinga4). large The scale bar elliptical bar, was matching oriented isophotes 20model◦ west centered D20 of from the on line Maciejewski the of nucleus; nodes, (200and the4). the right The panel bar was shows oriented the V-H 20◦ west dust of the line of nodes, and the vrgscmue sn h etfi ausdtrie from kinematics, determined stellar values the best-fit the from using the computed in determined difference significant averages no angle is there However, possible. when best-fit inclination the with and computed PA all are stated, As properties publication). averaged future a azimuthally in detail more in discussed be from kinematics, determined stellar values the best-fit from the using the computed in determined difference significant averages no angle is 2. there Figure However, possible. when best-fit inclination the with and computed PA all are stated, As properties publication). averaged future a azimuthally in detail more in discussed be 2. Figure 453 453 AGNs IN GAS MOLECULAR OF ROLE AGNs IN GAS MOLECULAR OF ROLE 2009 1, No. 2009 1, No. y y Aclrvrino hsfiuei vial nteoln journal.) online the in available is figure this of version color (A y journal.) online the in available is figure this of version color (A y model has been set at an inclinationstructure and map position reproduced angle matching frommodel Martini NGC has been 3 et227 al. set as (2003). at given an inclination in Bottom Tables row: 3 and and obser position 4. ved velocity angle matching field, disk NGC model, 3227 and as given the di inff Tableserence between3 and 4. them ae nmp fNC32 r lge ln Aof PA a along aligned are 3227 NGC of maps in -axes of PA a along aligned are 3227 NGC of maps in -axes ai n ati otelf.Tecrldcosmrstelcto ftenntla continuum. nonstellar the of location the marks cross circled The left. the to is east and -axis continuum. nonstellar the of location the marks cross circled The left. the to is east and -axis showing the strong velocity residuals² in theH central2 detected few arcsec. Thisin all suggests Seyfertsthat a simple disk is not an appropriate model for this galaxy, and Fig. 4 shows an alternative of a disk with a ring generated by a large-scale bar. The rightmost panel is a map of the velocity dispersion. The dashed ellipse represents the locationand of the 3 circumnuclear of 8 inactive ring. Axis scalesgalaxies, are in arcsec, with a conversion to parsec given; north is w-iesoa aso h H the of maps Two-dimensional H the of maps Two-dimensional up and east is left. all with rotating disk
² At least 4 Seyferts show signatures of inflow Fig. 5.— Molecular gash asydrodynamical traced by the 1-0 S(1)models line in qualitatively NGC 3227, showi ng the same region as in Fig. 2. Top row: observed flux, and the residual after subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust structure map reproduced from Martini et al. (2003).verify Bottom that row: for observed NGC velocity 3227 fiethereld, disk is model, and the difference between them. The strong residuals a few arcsec from the centreFig. 5.— suggestIonised that gas a simple as traced disk by is thenot narrow an appropriate Brγ line model in NGCFig. for 3227, 5.—² thisIonised showing galaxy.Inflow gas The the asalong same rightmost traced region by large panel the as shownnarrow is ascale map previously. Brγ olinefthevelocity in The NGC reg 3227,ion of showing high the same region as shown previously. The region of high
2 2 dispersion. Axisdispersion scales areinflow at in the arcsec, centre in with a should bar a conversion ebthat interpreted settles to parsec cautiously, in given; a since northdispersion in is this up regi andat theon east it centre was is left. not should possible eb interpreted to robustly cautiously, separate the since broad in this and regi narrowon it was not possible to robustly separate the broad and narrow u itiuin eoiy n eoiydseso,fo ett ih,frec efr aayosre ihOII.The OSIRIS. with observed galaxy Seyfert each for right, to left from dispersion, velocity and velocity, distribution, flux The OSIRIS. with observed galaxy Seyfert each for right, to left from dispersion, velocity and velocity, distribution, flux components.nuclear The orange ring ellipse traces the stellar ring as forcomponents. Fig. 17. Axisbars The scales orange in are inellipseat arcsec, least traces with the2 a conversion stellarSeyferts ring to as parsec for Fig. given; 17. A northxis scales is are in arcsec, with a conversion to parsec given; north is up and east is left. up and east is left. Fig. 4.— Density (left)◦ and line of sight velocity (right) for a hydrodynamical simulation◦ of a disk with a circumnuclear ring (spiral) sides of the galaxy centre, assuminggenerated by a PA a large of 120 scale,almost bar,sides matching of the model galaxyHigh D20 velocitycentre, from Maciejewski assuming dispersion a(200 PA and4). of The high120 bar,almost velocity was oriented residuals 20High◦ west velocityof the line dispersion of nodes, and and the high velocity residuals
− − perpendicular to its run inmodel the has central been set parts. at an For inclinationperpendicular this andoccuring position to its angle at run the matching in outskirts the NGC central 3of227 the parts. as givenfield For incan Tables this be caused 3 andoccuring 4. by at the outskirts of the field can be caused by 45 45 Erin K. S. Hicks IAU August 2015
◦ ◦ reason, if we subtract the disk model derived fromreason, stel- if weoutflow subtract superimposed the disk model on rotation derived there. from stel- On the north-outflow superimposed on rotation there. On the north- n hs fNC76 r lgtdaogaP of PA a along alighted are 7469 NGC of those and , of PA a along alighted are 7469 NGC of those and , lar kinematics, then the largest residuals, with amplitudelar kinematics,east then side, the these largest residuals residuals, are cospatial with amplitude with the H2eastflux side, these residuals are cospatial with the H2 flux reaching 100 km/s, are towards the edges of our fieldreaching to- 100residual km/s, about are towards 3′′ from the the edges centre, of our which field may to- traceresidual the about 3′′ from the centre, which may trace the wards both east and west: at radii beyond 2′′ fromwards the bothoutflowing east and west: material. at radii This beyond material 2′′ from is also the seen inoutflowing Hα material. This material is also seen in Hα nucleus, roughly along the minor axis of the galaxy.nucleus, In- roughlyemission along in the the minorF658N axis HST of filter, the galaxy. with a In- blue-shiftedemission in the F658N HST filter, with a blue-shifted terestingly, at the same locations, the velocity dispersioterestingly,n velocity at the same consistent locations, with the our velocity measurement dispersion (Fischervelocity et consistent with our measurement (Fischer et also increases to ∼100 km s−1. also increasesal. 2013). to ∼100 In km another s−1. tracer, the [S III] line at 0.9al.µm, 2013). In another tracer, the [S III] line at 0.9 µm, Fig. 6.— Density (left) and line of sight velocity (right) for a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) h H the H the h retto ftegsds geswt hto h tr.For [O stars. case the ( this of al. that (in with et agrees Dumas disk gas example, the of orientation the For [O stars. case the ( this of al. that (in with et agrees Dumas disk gas example, the of orientation the eta p fasml flclatv n nciegalaxies. inactive and active local of sample a of kpc central galaxies. inactive and active local of sample a of kpc central generated by a large scale bar, matching model S20 from Maciejewski (2004). The bar was oriented 20◦ west of the line of nodes, and the model has been set at an inclination and position angle matching NGC 3227 as given in Tables 3 and 4. 2 2 ieais nlre cls teshv lofudthat found also have others scales, larger On kinematics. that found also have others scales, larger On kinematics. Fig. 5.— Ionised gas as traced by the narrow Brγ line in NGC 3227, showing the same region as shown previously. The region of high dispersion at the centre should eb interpreted cautiously, since in this region it was not possible to robustly separate the broad and narrow components. The orange ellipse traces the stellar ring as for Fig. 17. Axis scales are in arcsec, with a conversion to parsec given; north is up and east is left. iii iii ◦ ]andH ]andH sides of the galaxy centre, assuming a PA of 120 ,almost High velocity dispersion and high velocity residuals perpendicular to its run in the central parts. For this occuring at the outskirts of the field can be caused by − − 2007 2007 48 48 reason, if we subtract the disk model derived from stel- outflow superimposed on rotation there. On the north- β β ◦ ◦ .Inallothermaps,northisalignedwiththe .Inallothermaps,northisalignedwiththe )andstellardiskorientationinthe )andstellardiskorientationinthe lar kinematics, then the largest residuals, with amplitude east side, these residuals are cospatial with the H2 flux ′′ )findagreementbetweenthegas )findagreementbetweenthegas reaching 100 km/s, are towards the edges of our field to- residual about 3 from the centre, which may trace the wards both east and west: at radii beyond 2′′ from the outflowing material. This material is also seen in Hα nucleus, roughly along the minor axis of the galaxy. In- emission in the F658N HST filter, with a blue-shifted Fig. 7.— Ionised gas as traced by the narrowterestingly, Brγ line in at NGC the 3227, same over locations, the same the field velocity of view dispersioas shown previousln velocityy. The region consistent of high with our measurement (Fischer et dispersion at the centre should be interpreted cautiously, since in this region− it1 was not possible to robustly separate the broad and narrow components. The orange ellipse traces the stellaralso ring increases as forFig.4.Axisscalesareinarcsec;northisupandeastisleft to ∼100 km s . al. 2013).. In another tracer, the [S III] line at 0.9 µm,
Figure 2. Two-dimensional maps of the H flux distribution, velocity, and velocity dispersion, from left to right, for each Seyfert galaxy observed with OSIRIS. The Figure 2. Two-dimensional maps of the H 2 flux distribution, velocity, and velocity dispersion, from left to right, for each Seyfert galaxy observed with OSIRIS. The y-axes in maps of NGC 3227 are aligned along2 a PA of 45 , and those of NGC 7469 are alighted along a PA of 48 .Inallothermaps,northisalignedwiththe y-axes in maps of NGC 3227 are aligned along a PA of 45◦, and those of NGC 7469 are alighted along a PA of 48◦.Inallothermaps,northisalignedwiththe y-axis and east is to the left. The circled cross marks the− location◦ of the nonstellar continuum. − ◦ y-axis and east is to the left. The circled cross marks the− location of the nonstellar continuum. − (A color version of this figure is available in the online journal.) (A color version of this figure is available in the online journal.) be discussed in more detail in a future publication). As stated, all the H2 kinematics. On larger scales, others have also found that be discussed in more detail in a future publication). As stated, all the H2 kinematics. On larger scales, others have also found that azimuthallyazimuthally averaged averaged properties properties are are computed computed with the best-fit thethe orientation of the gas disk agrees with that of the stars. For PA and inclination angle determined from the stellar kinematics, example, Dumas et al. (2007)findagreementbetweenthegas PA and inclination angle determined from the stellar kinematics, example, Dumas et al. (2007)findagreementbetweenthegas when possible. However, there is no significant difference in the (in this case [O iii]andHβ)andstellardiskorientationinthe when possible. However, there is no significant difference in the (in this case [O iii]andHβ)andstellardiskorientationinthe averages computed using the best-fit values determined from central kpc of a sample of local active and inactive galaxies. averages computed using the best-fit values determined from central kpc of a sample of local active and inactive galaxies. UAA Kinematic Analysis: Outflows Physics & Astronomy ² At least 4 Seyferts have spatially resolved molecular outflows (+1 with indirect evidence) 10 10 Davies et al. Davies et al.
flux residual (sqrt) arcsec
H 2 1- 0S(1) velocity residual NGC 5643 (Seyfert) arcsec
k m s- 1 k m s- 1
Fig. 6.— Molecular gas as traced by the 1-0Fig. S(1) 6.— lineMolecular in NGC 5643,gas as showing traced by the thesame 1-0 region S(1) line as in in Fig. NGC 1. 5643, Top showing row: observed the same flux region as in Fig. 1. Top row: observed flux distribution, and the residual flux after subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust distribution, and the residual flux after subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust structure map reproduced from Martini et al. (2003). Bottom row: observed velocity field, disk model, and the difference between them structure map reproduced from Martini et al. (2003). Bottom row: observed velocity field, disk model, and the difference between them showing the strong velocity residuals in the central few arcsec.Erin K. The S. rightmHicks ost panel is a map of the velocity dispersion. Magenta lines IAU August 2015 denote the extent of the outflow as measuredshowing from the the 1-0 strong S(1) velocity dispersion residualsand residual in the velocity central fewmaps; arcsec. these The also tracerightm theost outline panel is of a the map of the velocity dispersion. Magenta lines low extinction region in the dust structuredenote map. The the orange extent linesof the tra outflowce the as3 main measured absorption from the features 1-0 S(1) in the dispersion dust structureand residual map. velocityAxis maps; these also trace the outline of the scales are in arcsec, with a conversion to parseclow extinction given; north region is up in and the east dust is structureleft. map. The orange lines trace the 3 main absorption features in the dust structure map. Axis scales are in arcsec, with a conversion to parsec given; north is up and east is left.
Fig. 7.— Density (left) and line of sight velocity (right) for a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) Fig. 7.— Density (left) and line of sight velocity (right) for◦ a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) generated by a large scale bar, matching model D20 from Maciejewski (2004). The bar was oriented 60 from the line of nodes, and the ◦ model has been set at an inclination matchinggenerated NGC 5643 by a as large given scale in Tabl bar,e4,butataPAof-30 matching model D20◦,10 from◦ Maciejewskidifferent to that (200 in4). Table The 3. bar was oriented 60 from the line of nodes, and the model has been set at an inclination matching NGC 5643 as given in Table4,butataPAof-30◦,10◦ different to that in Table 3.
Fig. 8.— Ionised gas as traced by the Brγ line in NGC 5643, showing the same region as shown previously. Magenta and orange lines are is for Fig. 6. Axis scales are in arcsec, withFig. a conversion 8.— Ionised to parsec gas as given traced; north by the is Br upγ andline east in NGC is left. 5643, showing the same region as shown previously. Magenta and orange lines are is for Fig. 6. Axis scales are in arcsec, with a conversion to parsec given; north is up and east is left. As for most of the other AGN in our sample, NGC 6300 abettercomparisonofthelocationsoffeaturesbetween exhibits complex 1-0 S(1) distribution andAs kinematics. for most of the In otherthe AGN various in our maps. sample, The NGC velocity 6300 field showsabettercomparisonofthelocationsoffeaturesbetween a clear gra- this case, we argue that the simplestexhibits interpretation complex is as 1-0 S(1)dient, distribution which is and oriented kinematics. similarly In to thatthe of various the stars maps. on The velocity field shows a clear gra- an edge-on outflow superimposed onthis a rotating case, we disk argue – thatthe the same simplest spatial interpretation scales (shown is as in Fig.dient, 1), as which well as is the oriented similarly to that of the stars on although we have detected at best onlyan edge-on very weak outflow Brγ superimposedlarge scale Honα a(Buta rotating et al. disk 2001) – andthe H I same (Ryder spatial et al. scales (shown in Fig. 1), as well as the emission within the same features. although we have detected1996). at best When only subtracting very weak a Br diskγ model,large for scale which Hα the(Buta et al. 2001) and H I (Ryder et al. The residual flux map in Fig. 9 revealsemission a distinct within bi-the samePA features. was fixed to match that of the stars,1996). the When structures subtracting a disk model, for which the conical feature, aligned roughly north-south.The residual Expecially flux mapin in the Fig. residual 9 reveals velocity a distinct field showbi- aPA clear was blue-shift fixed to to match that of the stars, the structures to the south side, the flux is enhancedconical along feature, the limbs alignedthe roughly north north-south. and red-shift Expecially to the south, followingin the residual the arms velocity field show a clear blue-shift to of this structure. On several of the panelsto the in south the figures, side, the fluxof the is enhanced cross. A along global the gradient limbs in thethe residual north and can red-shift be to the south, following the arms we have drawn a cross corresponding toof it,this which structure. enables On severalan indication of the panels that in the the PA figures, of the diskof model the cross. was incor- A global gradient in the residual can be we have drawn a cross corresponding to it, which enables an indication that the PA of the disk model was incor- Fueling AGN II: Spatially Resolved Molecular Inflows and Outflows 15
Fig. 13.— Dust structure (V-H) map of IC 5267 reproduced from Martini et al. (2003). The field of view of SINFONI, shown in the corresponding Fig. 14, isUAA marked.8 In addition, the same ellipses as shown in some panels of thatDavies figure are et al.overdrawn with dotted lines. Axis scales are in arcsec; north is up and east is left. Fueling AGN II: Spatially Resolved Molecular Inflows and Outflows 17 Inactive Galaxies: Counter Rotation Physics & Astronomy
v Two inactive galaxies with H2 detected have counter rotating molecular components
IC 5267 NGC 3368
- 1 k m s- 1 k m s arcsec arcsec Fig. 14.— Molecular gas as traced by the 1-0 S(1) line in IC 5267. Top row: observed flux distribution, the model comprising 2 rings, and the difference between them (noteFig. that 3.— someMolecular of the diff gaserences as traced may be by due the to 1-0the S(1) model line being in NGCaxisymmetric 3227, showing while the the illuminationsame region of the as in Fig. 1. Top row: observed flux rings may vary between locations).distribution, On the far and right the is residual shown the flux veloci afterty dispersion. subtracting Bottom elliptical row: isop observedhotes velocity centered field, on beforethe nucleus; and after the right panel shows the V-H dust correcting for the double peakedstructure linev profile mapImplies causing reproduced the fingerexternal from of Martini anomalous accretion et al. velocities (2003). extending Bottom of molecular south-west row: obser fromved velocity the gas nucleus field, (see disk text model,AGN for and in the an difference between them details). On the right side areshowing the 2-ring the model, strong and velocity the residual residuals vel inocity the after central subtracting few arcsec. this This model. suggests The twothat ellipses a simple represent disk is thenot 2 an appropriate model for this galaxy, rings (drawn corresponding toand a size Fig. of Radius+FWHM/2,4 shows an alternative as given of a disk in Ta withb. 5, a to ring denote generated the full by extent a lar ofge-scale the two bar. structures). The rightmost Axis scales panel is a map of the velocity dispersion. are in arcsec, with a conversionThe to parsec dashed given; ellipse north represents is up and the east location is left. of the circumnuclear ring. Axis scales are in arcsec, withoff a conversion state? to parsec given; north is up and east is left. v configurations are quasi-stable à a small perturbationTABLE would 5 likely result in significant gas inflow Properties of the two rings in IC 5267
Fig. 15.— Molecular gas as traced by the 1-0 S(1) line in NGC 3368, showing the same region as in Fig. 17 and Fig. 2. Top row: observed Radius FWHM Rel. PA i Menc Vrot τorb ′′ ′′ flux distribution,◦ and◦ the residual flux after−1 subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust ( )()Int.(E of N) ( )(M⊙)(kms)(Myr) structure map reproduced from Martini et al. (2003). Middle row: observed velocity field, disk model, and the difference between them showing the clear counter-rotation centered about 0.4′′ north of the nucleus. Bottom row: zoomed-in view of the flux, velocity and velocity ′′ Erin K. S. Hicksresidual (with respect to the right-most 9 panel in the middle row) of the counter-rotatingIAU condensation August model.2015 The circle is centered 0.4 3.9 3.3 1.0 -4 75 2.5 × 10 139 25 ′′ 0.2a 1.8north 6.2 of the 135 nucleus 73 (near 3 the.0 × peak107 of the66 1-0 S(1) emission 3 in the top left panel) and has a radius of 1 .Althoughthefluxofthisoff-centre knot is compact, the impact of its velocity field can be traced out to ∼1.5′′. Axis scales are in arcsec, with a conversion to parsec given; north is up and east is left. a Because the fit yields a radius of the ring smaller than its width, this can be 8 ′′ considered a disk withalso a rather as 2 flat× inner10 M radial⊙,onlyafactor3–4greater.Assuch, profile, extending out to 1.1 . tion of gas from a streamer. Fig. 4.— Density (left) and line of sight velocity (right) for a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) when the condensation does merge with the galaxy nu- ◦ generated by a large scale bar, matching model D20 from Maciejewski (2004). The bar was oriented6. ARE 20 LUMINOUSwest of the SEYFERTS line of nodes, PERTURBED? and the model has been setcleus, at an inclination it will have and a position marked angle impact. matching Interestingly, NGC 3227 as the given in Tables 3 and 4. model of the condensation requires a compact mass dis- While previous studies have revealed some differences tribution, with a maximum rotation velocity of nearly in the circumnuclear structures present in Seyfert and 90 km s−1 at a radius of 0.3′′.Thiscouldaccountforthe non-active galaxies, none have been to identify conditions high anomalous velocities of the two bright knots of H2 that are required to fuel AGN. For example, no signif- emission noted by Nowak et al. (2010): they light up the icant differences in the presence of circumnuclear bars, most rapidly moving part of the condensation, perhaps boxy and disky isophots, or other non-axisymmetric fea- through thermal or shock heating since the shear at this tures are found by Hunt & Malkan (2004) in a compari- point would be a maximum. son of matched samples of Seyferts and quiescent galax- The counter-rotating condensation here is likely differ- ies. They do, however, report that Seyferts are more ent from the kinematically distinct components (KDCs), likely to show isophotal twisting, suggesting a potential some of which are counter-rotating cores, reported for a increase in the disturbance of the kinematics in these ac- significant fraction of the targets in a survey of 48 early- tive galaxies (we note that this difference is driven by the Fig. 5.— Ionisedtype gas as galaxies traced by (Emsellem the narrow et Br al.γ line 2004, in NGC 2007; 3227, Krajnovi´cet showing the sameSeyfert region 2 as galaxies shown previously. in the sample). The reg Followingion of high the indica- dispersion at the centreal. 2008). should These eb interpreted KDCs were cautiously, measured since in in the this stellar region kine- it was not possibletions from to robustly Sim˜oes separate Lopes et the al. broad (2007) and that narrow the source of components. The orangematics ellipse rather traces than the the stellar molecular ring as gas for kinematics, Fig. 17. Axis as scales seen are ingas arcsec, for with early- a conversion and late-type to parsec hosts given; may north be di isfferent, we up and east is left. here. While both fast and slow rotators in that sample have further split the sample of Hunt & Malkan (2004) sides of the galaxyexhibited centre, assumingkinematic atwists PA of and 120 misalignments,◦,almost theHigh most velocityinto dispersion early- and late-type and high hosts. velocity This residuals shows that the ele- perpendicular tonearly its run all in of the the kinematically central parts. decoupled For this cores wereoccuring seen at thevated outskirts level of of isophotal the field twisting can be is caused found in by Seyferts re- reason, if we subtractin slow the rotators. disk model Emsellem derived et al. from (2007) stel- suggestoutflow that dis- superimposedgardless of on host rotation type. there. This analysis On the north-also reveals that sipationless mergers had a major role in the evolution of there are more late-type quiescent galaxies than late- lar kinematics, then the largest residuals, with amplitude east side, these residuals are cospatial with the H2 flux reaching 100 km/s,these are galaxies. towards That the edgeswe have of observed our field a to- counter-rotatingresidual abouttype 3′′ Seyfertsfrom the with centre, circumnuclear which may bars, trace the the significance condensation in molecular gas argues instead for accre- wards both east and west: at radii beyond 2′′ from the outflowing material.of which is This not clear.material is also seen in Hα As we have alluded, a key result of the comparative nucleus, roughly along the minor axis of the galaxy. In- emission in the F658N HST filter, with a blue-shifted terestingly, at the same locations, the velocity dispersion velocity consistent with our measurement (Fischer et also increases to ∼100 km s−1. al. 2013). In another tracer, the [S III] line at 0.9 µm, 12 Davies et al. Fueling AGN II: Spatially Resolved Molecular Inflows and Outflows 15
Fig. 10.— Molecular gas as traced by the 1-0 S(1) line in NGC 6814, showing the same region as in Fig. 1. Top row: observed flux distribution, and the residual flux after subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust structure map reproduced from Martini et al. (2003). Bottom row: observed velocity field, disk model, and the difference between them showingFig. 13.— the strongDust structure velocity residuals (V-H) map in the of central IC 5267 few reproduced arcsec. The from rightm Martiniost panel et al. is (20 a map03). of The the field velocity of view dispersion. of SINFONI, We note shown that forin the correspondingthis object, the Fig. Brγ 14,flux is extracted marked. from In addition, the same the datacube same ellipses has already as sho beenwn presented in some panels and analysed of thatby figure M¨uller-S´anchez are overdrawn et al. with (2011). dotted Axis lines. Axisscales scales are in are arcsec, in arcsec; with a north conversion is up and to parsec east is given; left. north is up and east is left. 10 8 Davies et al. Davies et al. 8 Davies et al.
UAA Rotating Stellar Disks and
Physics & Complex Molecular Gas Kinematics Astronomy NGC 3227 (Seyfert) NGC 5643 (Seyfert) NGC 7743 (Seyfert) IC 5267 (inactive)
H 2 1- 0S(1) velocity residual
- 1 - 1 - 1 k m s k m s k m s - 1 arcsec arcsec arcsec k m s Fig. 6.— Molecular gas as tracedFig. 3.—by theMolecular 1-0 S(1) gas line as in traced NGC 5643, by the showing 1-0 S(1) the linesame inFig. NGCFig. region 14.— 11.— 3227, asMolecularMolecular showing in Fig. 1. the gas gas Topsame as astraced row: traced regionFig. observed by by 3.— as the the inMolecular 1-0 Fig. 1-0flux S(1) S(1) 1. line Top line gas in row:asin IC NGCtraced 5267. observed 7743, Top by the showingrow: flux 1-0 obser S(1) theved linesame flux in region NGCdistribution, 3227, as in showing Fig. the 1.model Topthe comprisingsame row: region observed 2 rings,as flux in Fig.and 1. Top row: observed flux distribution, and the residualdistribution, flux after subtracting and the residual elliptical flux isop afterhotes subtracting centered on elliptical thethedistribution, nucleus; di isopfferencehotes the and between centered right the panel residual them on the shows (note fluxdistribution, nucleus;Seyfert that the after V-H some the subtractings (8) andright dust of the the panel diInactive residualellipticalfferences shows flux isop themay(8)hotes after V-H be due subtracting dust centered to the on model elliptical the beingnucleus; isop axisymmetrichotes the right centered panel while on shows the the illumination nucleus; the V-H the dust of right the panel shows the V-H dust structure map reproduced fromstructure Martini map et al. reproduced (2003). Bottom from Martini row: obser et al.ved (2003). velocity Bottom field,ringsstructure diskrow: may model, obser map varyved reproduced between and velocity the locations). di fromff field,erencestructure Martini disk between On model, the et map al. far them and reproduced(2003). right the is di Bottom shownfference from the row: Martinibetween veloci obserty et themved dispersion.al.velocity (2003). Bottomfield, Bottom disk row: row: model, obser observed andved the velocity velocity difference field, field, between disk before model, and them after and the difference between them showing the strong velocity residualsshowing in the the strong central velocity few arcsec. residuals The in the rightm centralost panelfew arcsec. iscorrectingshowing a map This of suggests the the for strong the velocitythat double velocity a dispersion. simple peaked residuals diskshowing line is Magenta not profile with the an an strong appropriate causinglines arcsec velocity the of modelthe finger residuals nucleus. for of anomthis in The galaxy,thealous centralrightmost velocities few panel arcsec. extending is This a map south-west suggests of thethat velocity from a simple the dispersion. nucleus disk is(see not The an text red appropriate for model for this galaxy, and Fig. 4 shows an alternative of a disk with a ring generated by a large-scalestellar bar. disk The rightmost panel is a map of the velocity dispersion. denote the extent of the outflow as measured from the 1-0 S(1) dispersion and residual velocitydetails).and blue-shifted maps; On the these velocity right also side residuals trace areand the lie Fig.outline2-ringall along 4 8 shows model, ofthe the minor an and alternative axis, theall residual and 8 of neit a diskher velocity withare spatially aftera ring subtracting generated coincident by this with a lar model. excessge-scale The1-0 bar. S(1) two The flux. ellipses rightmost In contrast, represent panel the is the a map 2 of the velocity dispersion. low extinction region in the dustThe structure dashed ellipse map. represents The orange the lines location trace of the the 3 circumnuclear main absorptionred-shifted ring. features Axisunperturbed residualscales in the is are associated dust in arcsec, structureThe with with dashed a map. ‘hole’ a conversion ellipse Axis in the represents 1-0 to S(1) parsec flux the given; map. location northThe of Br is theγ map circumnuclear for this object ring. shows Axis onlyscales very are weak in arcsec, emission with located a conversion to parsec given; north is up and east isSample left. of 16 galaxies with rings (drawn corresponding to a size of Radius+FWHM/2, as given in Tab. 5, to denote the full extent of the two structures). Axis scales scales are in arcsec, with a conversion to parsec given; north is up and east is left. arewithin in arcsec, an arcsec with north a conversion of the nucleus.up to and parsec Axis east given; scalesis left. north are in is arcsec, up and with east a is conversi left. on to parsec given; north is up and east is left. matched host galaxies: H2 detectionNGC 7743all 8 3 in the bar of NGC 7743. rotating disk all 8 all 3 The velocity field also has significant structure and is 8 Seyfert & The detailed structures in the 1-0 S(1) flux map be-TABLEdominated 5 by non-circular motions. Two spiral arms come clearer once elliptical isophotes haveProperties been sub- of the two(one rings blue in IC and 5267 one red) can be traced in the velocity 8 inactive galaxies inflow at least 4 ◦ tracted. As Fig. 11 shows, this has a strong resemblence field: the blue arm winds from about PA∼−45 at small Radius FWHM Rel. PA i Menc ◦Vrot τorb to the V −H dust structure map′′ from which′′ Martini et◦ al. radii◦ to PA∼ 200 at− the1 outskirts of the FOV, while the outflow at( )(least 4)Int.(E of N) ( )(M⊙)(kms)(Myr) (2003) classified the circumnuclear region of NGC 7743 as red arm is not so well defined. Such a structure should alooselywoundspiral.Theonlyfeaturenottracedby accompany a density wave of a 2-arm morphology (e.g. perturbed 2 9 3.9 3.3 1.0 -4Davies 75 2.5 et× 10 al. 2009),139 and we 25 can attempt to understand the H2 emission is the arm thata continues almost straight 7 out to the south-east. Outside0.2 this spiral1.8 structure, 6.2 Moi- 135it 73 in 3 terms.0 × 10 of inflow66 driven 3 by a circumnuclear spiral, Fig. 4.— Density (left) and line of sight velocity (right)seev, for a hydrodynami Vald´es,& Chavushyancal simulation (2004)Fig. of a 4.— disk reportDensity with atwo circumnuclear (left) dust and lanes line ring of sight (spiral)often velocity present (right) inside for a the hydrodynami straightcal shocks simulation in the of bar, a disk and with a circumnuclear ring (spiral) Fig. 7.— Density (left) and line of sightErin velocity K. S. (right) Hicks for a hydrodynami cal simulation of a disk with a circumnucleara ring (spiral)◦ IAU August 2015 ◦ generated by a large scale bar, matching model D20 from Maciejewski (2004).◦ The bar wasgenerated orientedBecause 20 the bywest a fit large yields of scalethe a lineradius bar, of matching nodes,of the ring and model smallerthe D20 than from its Maciejewski width, this (200 can4). be The bar was oriented 20 west of the line of nodes, and the generated by a large scale bar, matching model D20 from Maciejewski (2004). The bar was oriented 60 from the line of nodes, and the ′′ model has been set at an inclination and position angle matching NGC 3227 as given in Tables 3 and 4. model has been set at an inclination matching NGC 5643 as given in Table4,butataPAof-30◦,10◦ different to thatconsideredmodel in Table has 3. a been disk set with at a an rather inclination flat inner and radial position profile, angle exte matchingnding out NGC to 1.1 3227. as given in Tables 3 and 4.
Fig. 5.— Ionised gas as traced by the narrow Brγ line in NGC 3227, showing the same regionFig. as 5.— shownIonised previously. gas as traced The reg byion the of narrow high Brγ line in NGC 3227, showing the same region as shown previously. The region of high Fig. 8.— Ionised gas as traceddispersion by the atBrγ theline centre in NGC should 5643, eb interpreted showing the cautiously, same region since as in shown this regi previously.on it was notMagent possibleadispersion and to orange robustly at the lines separate centre should the broad eb interpreted and narrow cautiously, since in this region it was not possible to robustly separate the broad and narrow are is for Fig. 6. Axis scales arecomponents. in arcsec, with The a orange conversion ellipse to traces parsec the given stellar; north ring is as up for and Fig. east 17. is A left.xis scales are in arcsec,components. with a conversion The orange to parsec ellipse given; traces north the stellar is ring as for Fig. 17. Axis scales are in arcsec, with a conversion to parsec given; north is As for most of the other AGNup and in east our is sample, left. NGC 6300 abettercomparisonofthelocationsoffeaturesbetweenup and east is left. exhibits complex 1-0 S(1) distributionsides of the galaxyand kinematics. centre, assuming In athe PA various of 120◦,almost maps. The velocityHigh velocityfield showssides dispersion a of clear the gra-galaxyand high centre, velocity assuming residuals a PA of 120◦,almost High velocity dispersion and high velocity residuals this case, we argue that theperpendicular simplest interpretation to its run in is theas centraldient, parts. which For is oriented this similarlyoccuring to at that theperpendicular outskirts of the stars of the on to field its run can in be the caused central by parts. For this occuring at the outskirts of the field can be caused by an edge-on outflow superimposedreason, if on we a subtract rotating the disk disk – modelthe derived same spatial from stel- scales (shownoutflow in superimposed Fig. 1),reason, as well on if asrotation we the subtract there. the On disk the model north- derived from stel- outflow superimposed on rotation there. On the north- although we have detectedlar at kinematics, best only then very the weak largest Brγ residuals,large with scale amplitude Hα (Buta eteast al. 2001) side, andthese H residualslar I (Ryder kinematics, are et al.cospatial then the with largest the residuals, H2 flux with amplitude east side, these residuals are cospatial with the H2 flux emission within the same features.reaching 100 km/s, are towards the1996). edges of When our field subtracting to- residual a disk about model, 3′′reaching forfrom which the 100 centre, the km/s, which are towards may trace the edges the of our field to- residual about 3′′ from the centre, which may trace the The residual flux map inwards Fig. both 9 reveals east and a distinct west: atbi- radiiPA beyond was 2 fixed′′ from to the match thatoutflowing of the stars,material.wards the structures This both material east and is west: also at seen radii in beyond Hα 2′′ from the outflowing material. This material is also seen in Hα conical feature, aligned roughlynucleus, north-south. roughly along Expecially the minor axisin of the the residual galaxy. velocity In- fieldemission show in a the clearnucleus, F658N blue-shift HST roughly to filter, along with the a minor blue-shifted axis of the galaxy. In- emission in the F658N HST filter, with a blue-shifted to the south side, the fluxterestingly, is enhanced at the along same the locations, limbs thethe velocity north dispersio and red-shiftn tovelocity the south, consistent followingterestingly, with the our arms at measurement the same locations, (Fischer the etvelocity dispersion velocity consistent with our measurement (Fischer et − − of this structure. On severalalso of increases the panels to in∼100 the km figures, s 1. of the cross. A global gradiental. 2013). in In the another residualalso increases tracer, can be theto ∼ [S100 III] km line s 1. at 0.9 µm, al. 2013). In another tracer, the [S III] line at 0.9 µm, we have drawn a cross corresponding to it, which enables an indication that the PA of the disk model was incor- Fueling AGN II: Spatially Resolved Molecular Inflows and Outflows 15
Fig. 13.— Dust structure (V-H) map of IC 5267 reproduced from Martini et al. (2003). The field of view of SINFONI, shown in the corresponding Fig. 14, is marked. In addition, the same ellipses as shown in some panels of that figure are overdrawn with dotted lines. 10 Davies et al. Axis scales are in arcsec; north is up and east is left.
UAA Linking Small Scales with Environment 10 DaviesPhysics et al. & Astronomy V-H dust structure H gas velocity 2 V-H dust structure H2 gas velocity Martini et al. (2003)
NGC 5643 IC 5267 k m s- 1 k m s- 1 Fig. 6.— Molecular gas as traced by the 1-0 S(1) line in NGC 5643, showing the sameFig. region 14.— asMolecular in Fig. 1.gas Top as traced row: by observed the 1-0 flux S(1) line in IC 5267. Top row: observed flux distribution, the model comprising 2 rings, and distribution, and the residual flux after subtractingFig. 1.—Continued elliptical isophotes centeredFig. 1.— onContinued the di nucleus;fference the between right them panelFig. 1.—Continued (note shows that the some V-H of dust theFig. di1.—fferencesContinued may be due to the model being axisymmetric while the illumination of the structure map reproduced from Martini et al. (2003). Bottom row: observed velocity field, disk model, and the difference between them ² All undisturbed galaxies withoutFig. 1.—Continuedrings circumnuclear may vary betweenmolecular locations). On disks the far are right inactive. is shown the velocity dispersion. Bottom row: observed velocity field, before and after showing the strong velocity residuals in the central few arcsec. The rightmost panel iscorrecting a map of for the the velocity double dispersion. peaked line Magenta profile causing lines the finger of anomalous velocities extending south-west from the nucleus (see text for denote the extent of the outflow as measured from the360 1-0 S(1) dispersion and residual360 details). velocity On maps; the these right also side360 trace are the the 2-ring outline model, of the and360 the residual velocity after subtracting this model. The two ellipses represent the 2 low extinction region in the dust structure² map.Isolated The orange or otherwise lines trace the undisturbed 3 main absorptionrings (drawnAGN features have corresponding in circumnuclear the dust to structure a size of Radius+FWHM/2,map.molecular Axis disks as given in Tab. 5, to denote the full extent of the two structures). Axis scales scales are in arcsec, with a conversion to parsec given; north is up and east is left. and dust structures classified369 asare spirals in arcsec, (and with a a conversion large scale to parsec bar given; to drive north isit): up and east is left. secular inflow.
² Seen in late type galaxies where the gas supply is plentiful TABLE 5 Properties of the two rings in IC 5267 Fig. 6.— Molecular gas as traced by the 1-0 S(1) line in NGC 5643, showing the ²sameG regionalaxies as inwith Fig. chaotic 1. Top row: circumnuclear observed flux dust structures (which may be Radius FWHM Rel. PA i Menc Vrot τorb distribution, and the residual flux after subtracting elliptical isophotes centered on the nucleus; the right panel shows the V-H dust ′′ ′′ ◦ ◦ −1 superimposed on an H2 disk) are in groups with ~10-15 (members)()Int.(: E of N) ( )(M⊙)(kms)(Myr) structure map reproduced from Martini et al. (2003). Bottom row: observed velocity field, disk model, and the difference between them showing the strong velocity residuals in the central few arcsec. The rightmost panel is a mapexternal of the velocityaccretion dispersion.. Magenta lines denote the extent of the outflow as measured from the 1-0 S(1) dispersion and residual velocity maps; these also trace the outline of the 3.9 3.3 1.0 -4 75 2.5 × 109 139 25 low extinction region in the dust structure map. The orange lines trace the 3 main absorption² featuresMost easily in the dustdetected structure in map. early Axis type galaxies lacking0.2 theira own1.8 gas 6.2 supply 135 73 3.0 × 107 66 3 scales are in arcsec, with a conversion to parsec given; north is up and east is left. Fig. 7.— Density (left) and line of sight velocity (right) for a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) ◦ a Because the fit yields a radius of the ring smaller than its width, this can be generated by a large scale bar, matching model D20 from Maciejewski (2004). The bar was oriented 60 from the line of nodes, and the ′′ model has been set at an inclination matchingErin K. NGC S. Hicks 5643 as given in Tabl e4,butataPAof-30 ◦,10◦ different to thatconsidered in Table a 3. disk withIAU aAugust rather flat 2015 inner radial profile, extending out to 1.1 .
Fig. 7.— Density (left) and line of sight velocity (right) for a hydrodynamical simulation of a disk with a circumnuclear ring (spiral) generated by a large scale bar, matching model D20 from Maciejewski (2004). The bar was oriented 60◦ from the line of nodes, and the model has been set at an inclination matching NGC 5643 as given in Table4,butataPAof-30◦,10◦ different to that in Table 3. Fig. 8.— Ionised gas as traced by the Brγ line in NGC 5643, showing the sameFig. region1.—Continued as shown previously. Magenta and orange lines are is for Fig. 6. Axis scales are in arcsec, with a conversion to parsec given; north is up and east is left. As for most of the other AGN in our sample, NGC 6300 abettercomparisonofthelocationsoffeaturesbetween exhibits complex 1-0 S(1) distribution and kinematics. In the various360 maps. The velocity field shows a clear gra- this case, we argue that the simplest interpretation is as dient, which is oriented similarly to that of the stars on an edge-on outflow superimposed on a rotating disk – the same spatial scales (shown in Fig. 1), as well as the although we have detected at best only very weak Brγ large scale Hα (Buta et al. 2001) and H I (Ryder et al. emission within the same features. 1996). When subtracting a disk model, for which the The residual flux map in Fig. 9 reveals a distinct bi- PA was fixed to match that of the stars, the structures conical feature, aligned roughly north-south. Expecially in the residual velocity field show a clear blue-shift to to the south side, the flux is enhanced along the limbs the north and red-shift to the south, following the arms Fig. 8.— Ionised gas as traced by the Brγ lineof this in NGC structure. 5643, showing On several the same of the region panels as shown in the previously. figures, Magentofa the and cross. orange A lines global gradient in the residual can be are is for Fig. 6. Axis scales are in arcsec, withwe a conversionhave drawn to parseca cross given corresponding; north is up to and it, east which is left. enables an indication that the PA of the disk model was incor- As for most of the other AGN in our sample, NGC 6300 abettercomparisonofthelocationsoffeaturesbetween exhibits complex 1-0 S(1) distribution and kinematics. In the various maps. The velocity field shows a clear gra- this case, we argue that the simplest interpretation is as dient, which is oriented similarly to that of the stars on an edge-on outflow superimposed on a rotating disk – the same spatial scales (shown in Fig. 1), as well as the although we have detected at best only very weak Brγ large scale Hα (Buta et al. 2001) and H I (Ryder et al. emission within the same features. 1996). When subtracting a disk model, for which the The residual flux map in Fig. 9 reveals a distinct bi- PA was fixed to match that of the stars, the structures conical feature, aligned roughly north-south. Expecially in the residual velocity field show a clear blue-shift to to the south side, the flux is enhanced along the limbs the north and red-shift to the south, following the arms of this structure. On several of the panels in the figures, of the cross. A global gradient in the residual can be we have drawn a cross corresponding to it, which enables an indication that the PA of the disk model was incor- UAA Early versus Late Type Galaxies Physics & Astronomy External accretion is seen more easily in early-types without a plentiful supply of gas. Implications: (i) a source for the gas, in the form of a group with 10-15 members (ii) paucity of gas in inactive galaxies vs presence of gas in AGN (iii) gas & stars should sometimes be counter-rotating
Dumas et al. 2007 & Westoby et al. 2012 samples: Early Type 11 AGN: all with gas detections Hosts 8 also with stellar rotation: 5 co-rotating gas 3 counter-rotating gas 6 inactive: gas detected in only 2
Secular inflow requires a large scale disk to supply the gas (i.e. late type host). Implications: (i) presence of gas in both active & inactive galaxies (ii) gas & stars should always be co-rotating
Dumas et al. 2007 & Westoby et al. 2012 samples: Late Type 10 AGN: gas & stars co-rotating in all (some misalignments) Hosts 8 inactive: gas detected in 6, co-rotating with stars
Erin K. S. Hicks IAU August 2015 UAA Linking Small Scales with Environment Physics & Astronomy dust molecular nuclear driver of predicted host type structure gas activity activity environment
none none none … early or late isolated
disk secular spiral either late type isolated rotation processes chaotic either, but (e.g. external more easily groups with 10- chaotic either counter accretion detectable in 15 members rotating) early type
IC 5267 NGC 3227 NGC 5643 NGC 7743
Martini et al. (2003) Fig. 1.—Continued Fig. 1.—Continued Fig. 1.—Continued Fig.Fig.1.—1.—ContinuedContinued Fig. 1.—Continued Erin K. S. Hicks IAU August 2015 360
369 369 360381 384
Fig. 1.—Continued
360 UAA Probing Kinematics via HST Dust Maps Physics & Astronomy IC 5267 NGC 3227 NGC 5643 NGC 7743
Martini et al. (2003) Fig. 1.—Continued Fig. 1.—Continued Fig. 1.—Continued Fig.Fig.1.—1.—ContinuedContinued Fig. 1.—Continued
v Martini et360 al. 2003 classified the nuclear dust structures of 123
369 galaxies369 imaged with 360HST381 384
v A subset of these form a matched sample from which little was found to correlate with nuclear activity.
v Hunt & Malkan 2004 did a similar analysis with 250 galaxies imaged with HST and also found little correlated with nuclear activity.
Erin K. S. Hicks IAU August 2015
Fig. 1.—Continued
360 UAA Probing Kinematics via HST Dust Maps Physics & Astronomy Quantifying environment by determining the distance to the 4th nearest neighbor (e.g. McGee 2013, Peng et al. 2010).
Use a subsample of tracer galaxies from 2MASS Redshift Survey (Huchra et al. 2012) that have KS < -24.3 and a line of sight v±500 km/s from the target galaxy
Erin K. S. Hicks IAU August 2015 UAA Larger Sample: Improved Statistics Physics & future integral field spectroscopy + AO samples Astronomy
² Sample of 20 active + 20 inactive with SINFONI AO (Davies et al. 2015)
² Volume limited sample of nearby active galaxies selected by their 14–195 keV luminosity
² Stellar population also characterized using XShooter data
² KONA (Keck OSIRIS Nearby AGN) Survey (Hicks, Müller Sánchez, Malkan, et al.)
² Sample of 40 nearby AGN: 21 Seyfert 1s + 19 Seyfert 2s ** Posters: KONA details at poster S319p.11 first results at Erickson, P. (DJp2.11), Kade, K. (DJp2.18), Smits, H. (DJp2.23)
HST imaging is available for about half of the galaxies in these two samples and the rest we hope will be obtained in the near future to solidify the correlation of nuclear dust structure with NGC 3227 inflow mechanism.
Erin K. S. Hicks IAU August 2015