Radio continuum, CO, and Radio continuum, CO, and thermal infrared emission in thermal infrared emission in nearby star-forming galaxiesnearby star-forming galaxies

Tony WongTony WongCSIRO Australia Telescope & University of New South

Wales

SMA meeting, 13 Jun 2005QuickTime™ and a

TIFF (Uncompressed) decompressorare needed to see this picture.

WithWith A. Hughes A. Hughes22, R. Ekers, R. Ekers11, R. Paladino, R. Paladino33, M. Murgia, M. Murgia3,43,4, ,

L. BlitzL. Blitz55, T. Helfer, T. Helfer55, L. Moscadelli, L. Moscadelli33, L. Gregorini, L. Gregorini44, L. , L.

Staveley-SmithStaveley-Smith11, M. Filipovic, M. Filipovic66, Y. Sofue, Y. Sofue77, N. Mizuno, N. Mizuno77

1ATNF, 2Swinburne U., 3INAF-Cagliari, 4CNR Italy, 5UC Berkeley, 6U. Western Sydney, 7Nagoya U.

The Radio/FIR Correlation• Amazingly tight correlation

(factor of 2 scatter over >4 orders of magnitude)

• Correlation persists even when normalizing by mass (Xu et al. 1994).

• Correlation of radio with FIR better than with other SF tracers (e.g. UV, H).

• Has been used as redshift indicator (Carilli & Yun 1999) and to identify high-redshift submm galaxies.

Yu

n, R

ed

dy,

& C

on

do

n 2

00

1

LMC

Why It’s Surprising

Courtesy Ron Ekers

High Correlation!

MagneticField

Molecular clouds UV

Grain props

FIR

Hot stars

Heating

WarmDust

Stars form

SN

SNR

ISMShocks Cosmic Ray

Acceleration

Synchrotron

Radio

LMC images

• IRAS 60µm image processed via HIRES algorithm (courtesy J. Surace, IPAC)

• ATCA + Parkes 1.4 GHz continuum image (courtesy M. Wolleben & L. Staveley-Smith)

• ATCA + Parkes 21cm HI image (Kim et al. 2003)

• NANTEN CO image (courtesy Fukui et al., Nagoya U.)

• SHASSA H image (Gaustad et al. 2001)

To examine correlations as a function of size scale, we compared several images, all at ~1’-2’ resolution:

1.4 GHz Continuum and HI

FIR and CO

Wavelet filtered images

The Pet Hat Wavelet

The “Pet Hat” wavelet is essentially an annulus in the Fourier plane that picks out structure on a certain scale.

5 k 20”

Frick et al. (2001)

An Example

30º

0º

LMC SubregionEach image 2° square

LMC SubregionEach image 2° square

Correlations Compared

Best correlations among 60 µm, H, and 1.4 GHz.

Correlations with gas tracers (CO, HI) degrade below ~200 pc (12.5 arcmin).

Correlations Compared

Best correlations among 60 µm, H, and 1.4 GHz.

Results even more pronounced for galaxy as a whole.

Correlations with gas tracers degrade below ~1 kpc.

LMC ResultsWe have examined the correlations between FIR, 1.4

GHz radio, CO, H, and HI emission in the LMC from scales of 2’ (40 pc) to 4° (4 kpc).

• Best correlations are between the “star formation

tracers” FIR, 1.4 GHz, and H, beginning to break down only scales of <0.1 kpc.

• Correlation of FIR and 1.4 GHz with cold gas tracers (e.g., HI) relatively poor on sub-kpc scales. Problem for B-gas coupling?

• Caveat is larger fraction of thermal emission in the LMC (~50% at 1.4 GHz, Haynes et al. 1991).

The CO/RC Correlation CO/RC ratio map RC vs. CO fluxes

Murgia et al. (2005)

Spiral GalaxiesN

GC

473

6N

GC

733

1

RC vs. mid-IR

Although correlation between 24 µm and 1.4 GHz emission is good on a pixel-by-pixel basis, a drop in scale-dependent correlation is often seen on scales of < 2 kpc.

RC vs. CO

The correlation between CO and 1.4 GHz emission is better in some galaxies and worse in others, but also shows breakdown in the 1-2 kpc range.

mid-IR vs. CO

The best correlation is probably between 24 µm and CO emission, although still breaking down on sub-kpc scales.

Caveats1. 24 µm emission dominated by dust heated by SF; may

exclude diffuse emission from cooler dust that contributes to overall FIR flux.

2. Sensitivity of RC images to bright point sources (e.g. nuclear or background AGN), which contribute power on all scales.

3. Possibility of missing interferometer spacings (e.g. combining VLA B- and D-arrays)

4. Signal-to-noise differs between images, producing an artificial decorrelation in wavelet analysis.

Conclusions1.4 GHz radio emission in LMC: mostly thermal?

• Similarity of FIR, RC, H suggest they all trace recent SF.

• Overall synchrotron weak (<~50%) and may be dominated by compact SNRs (Klein et al. 1989).

• Lack of synchrotron (compared to massive gals) could be due to greater ease of cosmic ray escape (e.g. Chi & Wolfendale 1990).

In nearby spirals, correlations of radio continuum with mid-IR and CO break down at 1-2 kpc scales.

• Non-thermal emission neither correlating with recent star formation nor tightly coupled to molecular clouds.

• Need better radio images & thermal/non-thermal separation.

Role of Sub-mm ObservationsDoes non-thermal RC trace the interface between strong CR

flux and strong B field?

• Can compare with classic “PDR” tracers such as CI and CII.

• CI: 3P13P0 transition (492 GHz): ncr~103 cm-3, ∆E~24 K, ~0.1-1.

• In well-shielded regions, CI abundance may be enhanced due to cosmic ray heating (e.g. Flower et al. 1994).

Importance of cold (T < 20 K) dust

• Coldest dust dominates at sub-mm wavelengths and correlates with HI+H2: how well does it correlate with radio continuum?

• Examine low Lfir/Lopt regions at >100µm to assess importance of

dust heating by old stars & its effect on correlation.