the local universe a ccat perspective christine wilson mcmaster university, canada 7 january...

The Local Universe

A CCAT perspective

Christine WilsonMcMaster University, Canada

7 January 2013 1AAS 221 – Long Beach, CA

27 January 2013 AAS 221 – Long Beach, CA

Science in the local universe

CCAT can help us understand how star formation is regulated in galaxies how the interstellar medium in galaxies

varies with environment how energetic processes such as AGN and

starbursts impact the ISM in galaxies

Resolving power of Herschel

Resolving power of CCAT


The high impact of CCAT

Three case studies from the nearby universe: Star formation in the Magellanic Clouds Dust and gas on the scale of molecular

clouds in M83 A spectroscopic survey of AGNs to z=0.2


(1) Star formation in the Magellanic Clouds

QuickTime™ and a decompressor

are needed to see this picture.

(Herschel image: ESA/NASA/ JPL-Caltech/ STScI)

LMC star forming regions imaged with CCAT

W43 (d=6 kpc) with Herschel at 500 microns (Nguyen Luong et al. 2013, in prep.)

CCAT at 350 microns will be able to image similar filaments in the LMC with the same spatial resolution as in this image.


CCAT’s sensitivity and resolution will allow us to identify and study individual young stellar objects in the Magellanic Clouds

A 5 sigma sensitivity of 3.6 mJy at 350 microns is roughly 1-3 Mo of gas+dust at 50 kpc distance

3.5” resolution is about 1 pc CCAT can map all of the star forming regions in

LMC/SMC to this sensitivity in a few 100 hours Complete census of YSOs to near a solar mass!

Star formation in the Magellanic Clouds


(2) Dust and gas in M83

• Herschel images at 500 and 70 microns (Foyle et al. 2012, MNRAS)

• Uniform gas-to-dust ratio• Local temperature variations


CCAT’s view of M83


M83 is a gas-rich galaxy with a nuclear starburst at a distance of 3.5 Mpc in the southern sky

3.5” resolution is 60 pc, so we can study dust on scale of individual giant molecular clouds

use dust instead of CO to find and study clouds (0.9 mJy at 350 microns is 1000 Mo at 3.5 Mpc)

Regulation of star formation: in starburst, spiral arms, interarm regions

Use [CI] lines as tracer for CO-dark molecular gas

Dust and gas in M83


(3) Active galaxies to z=0.2Arp 220, Rangwala et al. 2012, ApJ

Characterizing the ISM of galaxies

CO SLED constrains molecular gas reservoir, sources of gas heating(PDR, XDR, cosmic rays, microturbulent shocks)

Arp 220 molecular gas parameters from Herschel (Rangwala et al. 2011)


Wide-band spectroscopy of active galaxies with CCATBridge the gap between the Milky Way and high-

redshift studies: BAT hard Xray selected AGN flux limited sample of ULIRGs excitation source (PDRs, XDRs, shocks,

mechanical heating all seen with Herschel) astrochemistry


The promise of CCAT spectroscopy: XSPEC Band 3

Arp 220, Rangwala et al. 2012, ApJ


The promise of CCAT spectroscopy: XSPEC Band 3

Arp 220 as seen at z=0.2


The Local Universe with CCAT

CCAT will provide: a complete census of solar-type YSOs in the

Magellanic Clouds the ability to study dust and gas on GMC scales in

nearby galaxies like M83 measurement of gas reservoir and dominant heat

source in many AGNs and starbursts to z=0.2

And many more observations of the diverse local universe!


The CCAT Local Universe

CCAT will help us understand how star formation is regulated in galaxies how the interstellar medium in galaxies

varies with environment how energetic processes such as AGN and

starbursts impact the ISM in galaxies

the local universe a ccat perspective christine wilson mcmaster university, canada 7 january...

Documents

ca slide

power of ccat slide

long beach

apj slide

power of herschel slide

lmc star

ca m83

ca ccats view of m83