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The Role of Environment in Fueling Seyfert AGN

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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 <PSF FWHM>=58±25 pc 4a NGC 32276814 576 Daives Hicks et al.2013 Summary4q NGC of Observations 2406628 28-- Keck OSIRIS: 3 pairs <PSF FWHM>=23±16 pc 5a NGC 45937743 PSF FWHM50-- ID5q NGCGalaxy 5614357 (pc)97-- OSIRISSINFONI 1a1a NGCNGC 68143227 1856 1q1q NGCIC 5267 864 1290 2a2a NGCNGC 41515643 408 2q2q NGCNGC 53834030 3287 3a3a NGCNGC 74696300 3540 3q3q NGCNGC 56143368 4730 4a4a NGCNGC 32276814 576 extended extended high 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.
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    Galaxies- Please Read CH 1 in! • What is a galaxy? – Observationally S+G – Theoretically • Observationally – A lot of matter in 'one' place • historically matter was traced by ellipticals optical light (due mostly to stars) • Now can find and study galaxies spirals by radio and mm emission from ionized gas, IR emission from dust and by x-ray emission from their ISM+ black holes • Theoretically – A bound system with a mass between Galaxies come in a huge range 6 that of a globular cluster (~10 M of shapes and sizes and a group of galaxies ~1013 M ) Generically divided into 3 – Most of the mass (>65%) is dark matter (>10x more DM than stars) generalized morphologies • e.g. compact condensation of spirals baryons near the center of dark ellipticals 1 matter halos(https://en.wikipedia.org/ wiki/Dark_matter_halo) irregulars Welcome! • What is this course about? • Logistics – Textbook, web pages – Pre-requisites – Assignments, exams, grading – Academic integrity – Semester plan • Discussion – galaxies the big picture 2 Textbook & web pages • Required text: Galaxies in the Universe: An Introduction (2nd Edition) by L. Sparke & J. Gallagher Authors web page http://www.astro.wisc.edu/~sparke/book/galaxybook.html • Secondary book: Galaxy Formation & Evolution (very complete but dense) Mo, van den Bosch and White http://www.physics.utah.edu/~vdbosch/astro5580.html – the first two chapters of MBW are on-line at http://www.astro.umass.edu/~hjmo/astro330/htmldir/ reading.pdf For reference Galactic Dynamics (2nd Edition) by J. Binney & S. Tremaine Course web page: – Information, syllabus, lecture schedule – Assignments – Past lectures • Lectures will be posted on the web page after they are given 3 Other books Extragalactic Astronomy and Cosmology: An Introduction by P.
  • Seen Galaxies Count Ref1 Ref2 Con Visual Scale Mag SBR SIZE M Distance Rv Dist COMMENTS

    Seen Galaxies Count Ref1 Ref2 Con Visual Scale Mag SBR SIZE M Distance Rv Dist COMMENTS

    Seen galaxies Count ref1 ref2 con visual_scale mag SBR SIZE_M Distance Rv dist COMMENTS 1. NGC 224 M 31 AND 5 3.4 13.5 189 2.6 -14 Very large and bright 2. NGC 3031 M 81 UMA 4 6.9 13.2 24.9 12 -3 Fine large galaxy 3. NGC 598 M 33 TRI 3 5.7 14.2 68.7 2.8 -10 Large faint glow in square of stars 4. NGC 4594 M 104 VIR 3 8.0 11.6 8.6 30 48 Moon therefore little detail 5. NGC 221 M 32 AND 3 8.1 12.4 8.5 2.6 -10 Small but easy to see 6. NGC 4472 M 49 VIR 3 8.4 13.2 9.8 53 43 Lovely fuzzy galaxy 7. NGC 3034 M 82 UMA 3 8.4 12.5 10.5 12 13 Could make out bright and dark patches 8. NGC 4258 M 106 CVN 3 8.4 13.6 17.4 24 21 Fine large oval galaxy. So much brighter than most I have been looking at recently. 9. NGC 4826 M 64 COM 3 8.5 12.7 10.3 24 21 Easy galaxy to see 10. NGC 4486 M 87 VIR 3 8.6 13 8.7 51 57 Bright ball 11. NGC 4649 M 60 VIR 3 8.8 12.9 7.6 54 49 Lovely view with three galaxies visible. M60 is the brightest of the three. A nice bright ball of stars 12. NGC 3115 MCG - 1-26- 18 SEX 3 8.9 11.9 7.3 33 29 Bright spindle 13.