Obscured AGNs and Deep Radio Surveys
D.R. Ballantyne
Center for Relativistic Astrophysics, School of Physics, Georgia Tech
AGN dN/dS predicted from a synthesis
model of the X-ray background. Includes
Compton-thick AGN.
AGN dN/dS 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 1mm imaging
• Td > 50-60 K
• VLA 1.4 GHz imaging
Dec. 15th and 18th
24m
R
24m
R
Do Galaxy Interactions Generate High Velocity Clouds?
M81/M82
NGC 2403
1
M81/M82 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 M51
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
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
Resolved Stellar Populations in the Extremely Metal-poor Galaxy
CGCG 269-049
Hwihyun Kim
(ASU)
Fig. 1 - HST ACS/HRC color composite
of F330W, F550M and F814W 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 F658N filter
Fig. 4 - HI emission map and velocity field with the GMRT
28x24-arcsec2 resolution (Begum et al. 2006)
Extragalactic Ammonia (NH3)
(C. Henkel/MPIfR)
With the EVLA:
(1) Molecular kinetic
temperature maps of
entire galaxies.
(2) Measurements of the
proton-to-electron
mass ratio as a function of
redshift, location or density
 Talk by Karl Menten
10 K  Tkin1200 K
steep
spec.
flat
spec.
Complex
faint
galaxies
quasars
Results from crosscorrelating large
sky surveys
bright
Amy Kimball
Univ. Washington
Paper:
Kimball & Ivezić
AJ, 2008, 136, 684
Compact
Resolved
faint
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 = 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!!!
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
Brandon U.
Tyler Foster
Dept. of Physics
& Astronomy
1.2mm Observations of z~2 SWIRE ULIRGs,
Carol Lonsdale, NRAO
SUMMARY
• Spitzer 24um-selected starburst vs AGN-dominated ULIRGs
can be of
IRS Observations
32 4.5µm peakers,
reliably separated by IRAC-24um SEDs
Farrah et al 2008
• IRS spectra confirm this
• The band 2 peakers (z~1.7) have very similar SED IRS spectra, which
1.2mm observations
resemble the mean localMAMBO
starburst
of Brandl et al (2006) more than
of 61 Spitzer 5.8µm peakers.
local compact ULIRGs: extended SF?
They have lower 1.2mm/24µm
ratioslower
than “SMGs”
and
• Band 3 peakers (z~2) have
1.2mm/24um
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 > 1.8x1019 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. 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
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
5”
7.5 kpc
HST I
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
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 ?
1.4 GHz power  7e21 W/Hz
Wrobel, Greene, Ho and Ulvestad
2008, ApJ, 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 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
From Lin et al.