Double Trouble: ASKAP Early Science using Radio Galaxies

Lawrence Rudnick, University of Minnesota

Deep+wideband+polarization~30mJy,800sq deg 700-1800

More science using subsamples

This is single project from large surveyFeasible with JVLA only: NVSS

level investment

102.X – 3 hrNo

Use of all bands

HOT! HOTOutcomes: low risk

1. CR origins in radio galaxies: in the AGN? or in situ ? (a vs. z)

2. RG environments + small scale Galactic structure

1. Cosmic Ray origins

Why a vs. z* ? Intrinsic (AGN) vs. Environment

BUT, environments messy, so look at a1 vs. a2

*Not

a K

-cor

recti

on (K

amer

++)

Ly a

DeBrueck + 2000

RG local Intervening Galactic

2. RG environments (Faraday) + Galactic small scale structure

L. Rudnick, Shea Brown, Caitlin Johnson (still! In prep)Using NVSS, Taylor, Stil, Sundstrom

Defining a sample of double radio galaxies (DRGs)

and Random Pairs(RPs)

RPDRG

Two lobes do “know” about each other (somewhat)

ROTATION MEASUREFRACTIONAL POLARIZATION

RM1

RM2 ± 100 rad/m2

± 10

0 ra

d/m

2

Foreground st

retching

Some numbers … (tentative!!)• To determine a (< ± 0.1), need ~ 1.2 mJy• ~ 140/sq. deg (< 1’-0.5’ pairs, ~ 7-14 / sq. deg) 7-14,000 sources in 1000 sq. deg survey

• For RM, need ~0.3 mJy (P) 3.5 mJy I (@8.4%)

• ~ 30/sq deg. (< 1’-0.5’ pairs, ~ 1.5-3 / sq. deg) 1500-3000 sources in 1000 sq. deg survey

Deep+wideband+polarization~30mJy,800sq deg 700-1800

More science using subsamples

This is single project from large surveyFeasible with JVLA only: NVSS

level investment

102.X – 3 hrNo

Use of all bands

Outcomes: low risk

HOT! HOT! HOT!