Obscured AGNs and Deep Radio SurveysD.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 DOGsShane Bussmann, Univ. of Arizona

Poster #22

• 350m and 1mm imaging

• Td > 50-60 K

• VLA 1.4 GHz imaging Dec. 15th and 18th

R R

24m 24m

NGC 2403 Group

M81/M82 Group

Do Galaxy Interactions Generate High Velocity Clouds?

Katie Mae Chynoweth, Vanderbilt & NRAO, Poster #3

NGC 2403M81/M821

23

4 5

50 kpc 50 kpc

Mapping the Recent Star Formation History of the Disk of M51Katie Kaleida, Paul Scowen Arizona State University

This work was supported by NASA/STScI Grant HST-AR 1068401A to Arizona State University.

M51 / NGC 5195 –Hubble WFC/ACS Optical: B, V, and I broadband and Hα

1.7 Myr

0.84 Myr

0.71 Myr

< 0.5 Myr

Unknown

10 pc50 pc100 pc

•MS Turnoff Age-dating is only effective for a small minority of clusters at this distance and resolution

900+ Potential Stellar Associations

N

E

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 269-049. Padua isochrones for these filters and for a metallicity of Z=0.0004 are overlaid.

Fig. 3 - H image in the ACS/HRC F658N filterFig. 4 - HI emission map and velocity field with the GMRT 28x24-arcsec2 resolution (Begum et al. 2006)

Extragalactic Ammonia (NHExtragalactic Ammonia (NH33))

With the EVLA:With the EVLA:

(1)(1) Molecular kineticMolecular kinetic temperature maps of temperature maps of entire galaxies.entire galaxies.

(2)(2) Measurements of the Measurements of the proton-to-electronproton-to-electron mass ratio as a function of mass ratio as a function of

redshift, location or densityredshift, location or density

Talk by Karl MentenTalk by Karl Menten

10 K 10 K T Tkinkin1200 K1200 K

(C. Henkel/MPIfR)(C. Henkel/MPIfR)

Paper:Kimball & Ivezić AJ, 2008, 136, 684

faint galaxies quasars

Com

pact

Res

olve

dC

ompl

ex bright

faint

flatspec.

steepspec. Results from cross-

correlating large sky surveys

Webpage:www.astro.washington.edu/users/akimball/radiocat

Amy KimballUniv. Washington

The nature of the radio sources in the FORS Deep FieldJ. 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 galaxies340 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 KothesDRAO, Herzberg Institute of Astrophysics

Tyler FosterDept. of Physics & Astronomy

Brandon U.

1.2mm Observations of z~2 SWIRE ULIRGs, Carol Lonsdale, NRAO

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

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

Modelling Extra-Planar HI in NGC 6503

K. Spekkens (RMC), E. W. Greisen (NRAO)

Greisen et al. 2009, AJ, submitted

1 kpc = 40”

Intensity -> morphologyColour -> kinematics

VLA C configuration14”, 5 km/s resolution

NHI > 1.8x1019 cm-2

Greisen et al. 2009, AJ, submitted

Modelling Extra-Planar HI in NGC 6503

K. Spekkens (RMC), E. W. Greisen (NRAO)

Position-velocity

Channelmap

100

V, km/s

-100R 3’ 6’ 9’

0 Ropt

RA

1 - component models 2 - component models

0’

4’

Dec

0’ 4’ 8’

Thin + truncated thick

Thin disk Thin:thick ratio 4:1

Thick disk

Modelling Extra-Planar HI in NGC 6503

K. Spekkens (RMC), E. W. Greisen (NRAO)

Position-velocity

Channelmap

100

V, km/s

-100R 3’ 6’ 9’

0 Ropt

RA

2 - component models

0’

4’

Dec

0’ 4’ 8’

Thin + truncated thick

Thin:thick ratio 4:1Thick HI disk extent is correlated with optical disk: feedback at work!

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

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

VLA imaging of GH 10 in 2007Diameter 0.15” = 220 pcOptically-thin synchrotron1.4 GHz power ~ 3e22 W/HzEmission dominated by AGN

GH 10 like Seyferts with AGN outflowsKinetic luminosities 1e43 ergs/s

VLBA imaging of GH 10 in 2009Resolution ~ 10 pcOutflow structure ? Outflow length scale ?

VLA 8.5 GHzFOV 5” = 7.5 kpc

0.4 mJy

SDSS

5”7.5 kpcHST I

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.