Obscured AGNs and Deep Radio Surveys D R
Obscured AGNs and Deep Radio Surveys D. R. Ballantyne Center for Relativistic Astrophysics, School of Physics, Georgia Tech AGN d. N/d. S predicted from a synthesis model of the X-ray background. Includes Compton-thick AGN d. N/d. S as before, but now includes star-formation in the host galaxy. The SFR in Type 2 > SFR Type 1.
Far-IR Properties of z~2 DOGs Shane Bussmann, Univ. of Arizona Poster #22 • 350 m and 1 mm imaging • Td > 50 -60 K • VLA 1. 4 GHz imaging Dec. 15 th and 18 th 24 m R
Do Galaxy Interactions Generate High Velocity Clouds? M 81/M 82 NGC 2403 1 M 81/M 82 Group� 5 4 NGC 2403 Group 2 50 kpc 3 50 kpc Katie Mae Chynoweth, Vanderbilt & NRAO, Poster #3
Mapping the Recent Star Formation History of the Disk of M 51 Katie Kaleida, Paul Scowen Arizona State University 1. 7 Myr 0. 84 Myr 0. 71 Myr < 0. 5 Myr Unknown 10 pc 50 pc 100 pc N E M 51 / NGC 5195 –Hubble WFC/ACS Optical: B, V, and I broadband Hα • MS Turnoff Age-dating is only effective for a small minority of clusters at this distance and resolution 900+ Potential Stellar Associations
Resolved Stellar Populations in the Extremely Metal-poor Galaxy CGCG 269 -049 Hwihyun Kim (ASU) Fig. 1 - HST ACS/HRC color composite of F 330 W, F 550 M and F 814 W images Fig. 2 - Color-magnitude diagrams of resolved stars within CGCG 269049. Padua isochrones for these filters and for a metallicity of Z=0. 0004 are overlaid. Fig. 3 - H image in the ACS/HRC F 658 N filter Fig. 4 - HI emission map and velocity field with the GMRT 28 x 24 -arcsec 2 resolution (Begum et al. 2006)
Extragalactic Ammonia (NH 3) (C. Henkel/MPIf. R) With the EVLA: (1) Molecular kinetic (2) (3) temperature maps of entire galaxies. (2) Measurements of the (3) proton-to-electron (4) mass ratio as a function of redshift, location or density (5) (6) Talk by Karl Menten 10 K Tkin 1200 K
steep spec. flat spec. galaxies quasars Amy Kimball Univ. Washington faint Paper: Kimball & Ivezić AJ, 2008, 136, 684 Compact Resolved Complex faint Results from crosscorrelating large sky surveys bright Webpage: www. astro. washington. edu/users/akimball/radiocat
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 = 1 h 6 m 3. 6 s , δ = -25 o 45‘ 46“ (2000) Starburst/starforming galaxies vs AGN? Radio data: 1. 4 GHz (A-configuration) and 5 GHz (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 UBg. RIJKs-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!!!
Rolling Motions in Extragalactic Spiral Arms Real? Imaginary? 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 Tyler Foster Dept. of Physics & Astronomy Brandon U.
1. 2 mm Observations of z~2 SWIRE ULIRGs, Carol Lonsdale, NRAO SUMMARY • Spitzer 24 um-selected starburst vs AGN-dominated ULIRGs can be of IRS Observations 32 4. 5µm peakers, reliably separated by IRAC-24 um SEDs Farrah et al 2008 • IRS spectra confirm this • The band 2 peakers (z~1. 7) have very similar SED IRS spectra, which 1. 2 mm observations resemble the mean local. MAMBO starburst of Brandl et al (2006) more than of 61 Spitzer 5. 8µm peakers. local compact ULIRGs: extended SF? They have lower 1. 2 mm/24µm ratios than “SMGs” and • Band 3 peakers (z~2) have lower 1. 2 mm/24 um flux ratios than SMGs, warmer FIR/mm also: – More warm dust – comparable or larger IR/mm luminosities – large stellar masses
Modelling Extra-Planar HI in NGC 6503 K. Spekkens (RMC), E. W. Greisen (NRAO) VLA C configuration 14”, 5 km/s resolution NHI > 1. 8 x 1019 cm-2 1 kpc = 40” Intensity -> morphology Colour -> kinematics Greisen et al. 2009, AJ, submitted
Modelling Extra-Planar HI in NGC 6503 K. Spekkens (RMC), E. W. Greisen (NRAO) V, km/s Positionvelocity Dec 100 Channel map 4’ Ropt 0 0’ -100 R 3’ 6’ 1 - component models 9’ RA 0’ 4’ 8’ 2 - component models Thin disk Thin: thick ratio 4: 1 Thick disk Thin + truncated thick Greisen et al. 2009, AJ, submitted
Modelling Extra-Planar HI in NGC 6503 K. Spekkens (RMC), E. W. Greisen (NRAO) V, km/s Positionvelocity Dec 100 Channel map 4’ Ropt 0 0’ -100 R 3’ 6’ 9’ RA 0’ 4’ 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
HI Imaging of Void Galaxies K. Stanonik 1, E. Platen 2, M. A. Aragón-Calvo 3, J. van Gorkom 1, R. van de Weygaert 2, J. M. van der Hulst 2, K. Kovač4, C. -W. Yip 3, J. Peebles 5 (1) Columbia University, (2) Kapteyn Institute, (3) Johns Hopkins, (4) ETH Zurich, (5) Princeton
Local Analogs of the First AGNs: GH 10 SDSS VLA 8. 5 GHz FOV 5” = 7. 5 kpc 0. 4 m. Jy Black holes and galaxies co-evolve 5” 7. 5 kpc HST I First AGNs at z ~ 10 Black hole mass ~ 1 e 5 Msun Lbol / Ledd ~ 1 “Feedback luminosity” ~ 5 % Lbol GH 10 AGN at z ~ 0. 08 Black hole mass ~ 8 e 5 Msun Lbol / Ledd ~ 2 “Feedback luminosity” ~ 1 e 43 ergs/s ? Dwarf spheroidal-like host SFR 2 Msun/yr VLA imaging of GH 10 in 2007 Diameter 0. 15” = 220 pc Optically-thin synchrotron 1. 4 GHz power ~ 3 e 22 W/Hz Emission dominated by AGN GH 10 like Seyferts with AGN outflows Kinetic luminosities 1 e 43 ergs/s VLBA imaging of GH 10 in 2009 Resolution ~ 10 pc Outflow structure ? Outflow length scale ? 1. 4 GHz power 7 e 21 W/Hz Wrobel, Greene, Ho and Ulvestad 2008, Ap. J, 686, 838
VLA Spectra of a High Frequency Selected Sample of Radio Galaxies Bruce 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 AT 20 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 GB 6) – 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, ar. Xive: 0805. 1750) – Little correlation between low freq. and high freq. Spectra – Most spectra turn over > 22 GHz – Polarization low (all <4%0
From Lin et al.
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