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Obscured AGNs and Deep Radio Surveys

Obscured AGNs and Deep Radio Surveys D.R. Ballantyne Center for Relativistic Astrophysics, School of Physics, Georgia Tech. AGN dN/dS as before, but now includes star-formation in the host galaxy. The SFR in Type 2 > SFR Type 1.

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Obscured AGNs and Deep Radio Surveys

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  1. Obscured AGNs and Deep Radio Surveys D.R. Ballantyne Center for Relativistic Astrophysics, School of Physics, Georgia Tech AGN dN/dS as before, but now includes star-formation in the host galaxy. The SFR in Type 2 > SFR Type 1. AGN dN/dS predicted from a synthesis model of the X-ray background. Includes Compton-thick AGN.

  2. Far-IR Properties of z~2 DOGsShane Bussmann, Univ. of ArizonaPoster #22 • 350m and 1mm imaging • Td > 50-60 K • VLA 1.4 GHz imaging Dec. 15th and 18th 24m 24m R R

  3. Do Galaxy Interactions Generate High Velocity Clouds? M81/M82 NGC 2403 1 M81/M82 Group 5 4 NGC 2403 Group 2 3 50 kpc 50 kpc Katie Mae Chynoweth, Vanderbilt & NRAO, Poster #3

  4. 1.7 Myr 0.84 Myr 0.71 Myr < 0.5 Myr Unknown 10 pc 50 pc 100 pc E N Mapping the Recent StarFormation History of the Disk of M51Katie Kaleida, Paul Scowen Arizona State University M51 / NGC 5195 –Hubble WFC/ACS Optical: B, V, and I broadband and Hα • MS Turnoff Age-dating is only effective for a small minority of clusters at this distance and resolution 900+ Potential Stellar Associations This work was supported by NASA/STScI Grant HST-AR 1068401A to Arizona State University.

  5. Resolved Stellar Populations in the Extremely Metal-poor Galaxy CGCG 269-049 Hwihyun Kim (ASU)‏ Fig. 2 - Color-magnitude diagrams of resolved stars within CGCG 269-049. Padua isochrones for these filters and for a metallicity of Z=0.0004 are overlaid. Fig. 1 - HST ACS/HRC color composite of F330W, F550M and F814W images Fig. 4 - HI emission map and velocity field with the GMRT 28x24-arcsec2 resolution (Begum et al. 2006)‏ Fig. 3 - H image in the ACS/HRC F658N filter

  6. Extragalactic Ammonia (NH3) (C. Henkel/MPIfR) 10 K  Tkin1200 K With the EVLA: • Molecular kinetic temperature maps of entire galaxies. • Measurements of the proton-to-electron mass ratio as a function of redshift, location or density  Talk by Karl Menten

  7. steep spec. galaxies faint quasars Complex Resolved Compact flat spec. Results fromcross-correlating large sky surveys bright Amy Kimball Univ. Washington faint Paper: Kimball & Ivezić AJ, 2008, 136, 684 Webpage: www.astro.washington.edu/users/akimball/radiocat

  8. The nature of the radio sources in the FORS Deep Field J. Heidt, J. Pforr, K. Menten , A. Gabasch , S. Wagner (Heidelberg, Portsmouth, Bonn, ESO) Aim:Probing the ~ 100 μJy source population in the 7‘ • 7‘ FORS Deep Field located at α = 1h 6m 3.6s , δ = -25o 45‘ 46“ (2000) Starburst/starforming galaxies vs AGN? Radio data: 1.4GHz (A-configuration) and 5GHz (C-configuration) images of the FDF taken with the VLA  rms noise levels 15μJy (1.4 GHz) and 7.2μJy (5.GHz) • 22 sources (8 L-band, 12 L+C, 2 C-band) exceeding 5 rms Optical data: Very deep UBgRIJKs-images , best image quality 0.5-0.6“ (B and I). 50% completeness limits: 27.7 (B), 26.4 (I), B+I selected catalog contains ~ 8500 galaxies 340 spectra of galaxies up to z = 5, 5500 high-quality photo z‘s and SEDs Discriminator: • Radio luminosities, radio spec. indices and radio SFRs • Photo z‘s and SEDs • 2-dim surface brightness fits • Visual appearance (mergers, radio pos. in spiral arm) • Colors (EROs) Result? Have a look at the poster!!!

  9. Rolling Motions in Extragalactic Spiral Arms Imaginary? Real? What can new EVLA observations of external spiral galaxies tell us about these enigmatic motions in our Milky Way? Roland Kothes DRAO, Herzberg Institute of Astrophysics Brandon U. Tyler Foster Dept. of Physics & Astronomy

  10. 1.2mm Observations of z~2 SWIRE ULIRGs, Carol Lonsdale, NRAO SUMMARY • Spitzer 24um-selected starburst vs AGN-dominated ULIRGs can be reliably separated by IRAC-24um SEDs • IRS spectra confirm this • The band 2 peakers (z~1.7) have very similar SED IRS spectra, which resemble the mean local starburst of Brandl et al (2006) more than local compact ULIRGs: extended SF? • Band 3 peakers (z~2) have lower 1.2mm/24um flux ratios than SMGs, also: • More warm dust • comparable or larger IR/mm luminosities • large stellar masses IRS Observations of 32 4.5µm peakers, Farrah et al 2008 MAMBO 1.2mm observations of 61 Spitzer 5.8µm peakers. They have lower 1.2mm/24µm ratios than “SMGs” and warmer FIR/mm

  11. K. Spekkens (RMC), E. W. Greisen (NRAO) Modelling Extra-Planar HI in NGC 6503 VLA C configuration 14”, 5 km/s resolution NHI > 1.8x1019 cm-2 Intensity -> morphology Colour -> kinematics 1 kpc = 40” Greisen et al. 2009, AJ, submitted

  12. K. Spekkens (RMC), E. W. Greisen (NRAO) Modelling Extra-Planar HI in NGC 6503 V, km/s Dec 100 Position- velocity Channel map 4’ Ropt 0 0’ -100 6’ 9’ R 3’ RA 4’ 0’ 8’ 2 - component models 1 - component models Thin:thick ratio 4:1 Thin disk Thin + truncated thick Thick disk Greisen et al. 2009, AJ, submitted

  13. K. Spekkens (RMC), E. W. Greisen (NRAO) Modelling Extra-Planar HI in NGC 6503 V, km/s Dec 100 Position- velocity Channel map 4’ Ropt 0 0’ -100 6’ 9’ R 3’ RA 4’ 0’ 8’ 2 - component models Thick HI disk extent is correlated with optical disk: feedback at work! Thin:thick ratio 4:1 Thin + truncated thick Greisen et al. 2009, AJ, submitted

  14. HI Imaging of Void Galaxies K. Stanonik1, E. Platen2, M. A. Aragón-Calvo3, J. van Gorkom1, R. van de Weygaert2, J. M. van der Hulst2, K. Kovač4, C.-W. Yip3, J. Peebles5 (1) Columbia University, (2) Kapteyn Institute, (3) Johns Hopkins, (4) ETH Zurich, (5) Princeton

  15. Local Analogs of the First AGNs: GH 10 SDSS VLA 8.5 GHz FOV 5” = 7.5 kpc 0.4 mJy Black holes and galaxies co-evolve First AGNs at z ~ 10 Black hole mass ~ 1e5 Msun Lbol / Ledd ~ 1 “Feedback luminosity” ~ 5 % Lbol GH 10 AGN at z ~ 0.08 Black hole mass ~ 8e5 Msun Lbol / Ledd ~ 2 “Feedback luminosity” ~ 1e43 ergs/s ? Dwarf spheroidal-like host SFR  2 Msun/yr 1.4 GHz power  7e21 W/Hz 5” 7.5 kpc HST I VLA imaging of GH 10 in 2007 Diameter  0.15” = 220 pc Optically-thin synchrotron 1.4 GHz power ~ 3e22 W/Hz Emission dominated by AGN GH 10 like Seyferts with AGN outflows Kinetic luminosities  1e43 ergs/s VLBA imaging of GH 10 in 2009 Resolution ~ 10 pc Outflow structure ? Outflow length scale ? Wrobel, Greene, Ho and Ulvestad 2008, ApJ, 686, 838

  16. VLA Spectra of a High Frequency Selected Sample of Radio GalaxiesBruce Partridge, Haverford College • Radio sources contaminate searches for CMB anisotropies • What are properties of radio sources at frequencies used for CMB work? • Best survey 18 GHz AT20 G (Spring 2009: preliminary results in Sadler et al. 2006)‏ • Alternate approach – look at extreme radio sources • α > 0.4 1.4 GHz to 5 GHz (FIRST vs GB6)‏ • 400 sources chosen to avoid confusion • Simultaneous L, C, X & K band VLA observations • Follow up ~40 at Q band + polarization • Findings (see Partridge et al. 2009 in prep., Lin et al. 2009, arXive:0805.1750)‏ • Little correlation between low freq. and high freq. Spectra • Most spectra turn over > 22 GHz • Polarization low (all <4%0

  17. From Lin et al.

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