Allen et al. (2005)Allen et al. (2005)

Johnstone et al. (2000)Johnstone et al. (2000)

Oph B2Oph B2

850 µm continuum (JCMT) NH3 (1,1) int. intensity (GBT)

NHNH33 emission shows excellent (but not perfect) emission shows excellent (but not perfect) correspondence with dust continuum emissioncorrespondence with dust continuum emission

Tracing Dense Core Structure with NHTracing Dense Core Structure with NH33

Oph B2Oph B2

850 µm continuum (JCMT) NH3 (1,1) int. intensity (GBT+ATCA)

NHNH33 emission shows excellent (but not perfect) emission shows excellent (but not perfect) correspondence with dust continuum emissioncorrespondence with dust continuum emission

Tracing Dense Core Structure with NHTracing Dense Core Structure with NH33

NHNH33 (1,1) in Oph B (1,1) in Oph B

Only 20/48 hr observed so far, rest scheduled for October+Only 20/48 hr observed so far, rest scheduled for October+

B1B1

B2B2

B3B3

Friesen et al. (2006, in preparation)

Tracing Dense Core Structure with NHTracing Dense Core Structure with NH33

NHNH33 in Oph B, C & F in Oph B, C & FOver next semester, will get more GBT and new VLA data:Over next semester, will get more GBT and new VLA data:

with (1,1) and (2,2) lines, will derive kinetic temperature with (1,1) and (2,2) lines, will derive kinetic temperature across several Oph coresacross several Oph cores

with opacity, column densities + NHwith opacity, column densities + NH33 abundances abundances

with line widths, probe velocities; with Twith line widths, probe velocities; with TKK, get thermal , get thermal and non-thermal motions simultaneously, dynamicsand non-thermal motions simultaneously, dynamics

Tracing Dense Core Structure with NHTracing Dense Core Structure with NH33

5 Rationales for a K-band FPA5 Rationales for a K-band FPA

increase NH3 observing speed by >1 order of magnitude, increase NH3 observing speed by >1 order of magnitude, map dense cores faster and with better samplingmap dense cores faster and with better sampling

allow for more serendipitous discovery (early cores?) with allow for more serendipitous discovery (early cores?) with wider areal coverage of mapswider areal coverage of maps

maximize usage of “precious” K-band conditions at GBmaximize usage of “precious” K-band conditions at GB

improve core statistics significantly with NHimprove core statistics significantly with NH33 follow-up of follow-up of new Galactic surveysnew Galactic surveys

will provide crucial single-dish data for K-band EVLA will provide crucial single-dish data for K-band EVLA projectsprojects

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Gould Belt consists of SF molecular clouds within 500 pc Gould Belt consists of SF molecular clouds within 500 pc including Orion, Taurus, Ophiuchus, Perseus, Serpens, etc.including Orion, Taurus, Ophiuchus, Perseus, Serpens, etc.

Grenier (2004)

Gould Belt: 3D schematic

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Orion

CepheusFlare

IC 5146

Pipe Nebula

Ophiuchus

Taurus

Lupus

Serpens

R CrA

~110 sq. deg. at~110 sq. deg. at AAvv ≥ 3 ≥ 3

~1000 sq. deg. at~1000 sq. deg. at AAvv ≥ 1 ≥ 1Nutter (2005), after Cambrésy (1999)Nutter (2005), after Cambrésy (1999)

New Local SF Surveys:New Local SF Surveys:

• JCMT Legacy SurveyJCMT Legacy Survey: using : using SCUBA-2/HARP to map Gould’s SCUBA-2/HARP to map Gould’s Belt clouds to ABelt clouds to Av v = 1-2 in 450/850 = 1-2 in 450/850 µµm + lines, polarization in sub-m + lines, polarization in sub-regions (2006+)regions (2006+)

• Herschel GT Key ProjectHerschel GT Key Project: using : using SPIRE/PACS to map entirety of SPIRE/PACS to map entirety of Gould’s Belt clouds to AGould’s Belt clouds to Av v > 3 at > 3 at 80/110, 170, 250, 360, 520 80/110, 170, 250, 360, 520 µµm m (2008+)(2008+)

• Spitzer c2d2 LegacySpitzer c2d2 Legacy: using : using IRAC+MIPS over GB clouds (2003-IRAC+MIPS over GB clouds (2003-2007)2007)

Herschel Space Observatory

SCUBA-2 HARP

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Spitzer Space Telescope

Infrared Dark Clouds:Infrared Dark Clouds:Extinction features in the mid-IRExtinction features in the mid-IR

~10,000 cold dust clouds seen in silhouette ~10,000 cold dust clouds seen in silhouette against warmer background dust.against warmer background dust.

MSX 8 µm continuum

from Jackson (2005)from Jackson (2005)

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

ll = 326-335 deg, | = 326-335 deg, |bb| < 1 | < 1 degdeg

New Galactic Plane Surveys:New Galactic Plane Surveys:

• JCMT Legacy SurveyJCMT Legacy Survey: (JPS) using : (JPS) using SCUBA-2 to map |SCUBA-2 to map |bb| < 1 (2006+)| < 1 (2006+)

• Herschel OT Key ProjectHerschel OT Key Project: (HiGal) : (HiGal) using SPIRE/PACS to map |using SPIRE/PACS to map |bb| < 1 | < 1 (2008+; not yet approved)(2008+; not yet approved)

• Spitzer LegacySpitzer Legacy: (GLIMPSE1, 2, & 3, : (GLIMPSE1, 2, & 3, MIPSGAL) (2003-2007), using MIPSGAL) (2003-2007), using IRAC and MIPS over various IRAC and MIPS over various ranges of ranges of ll

• HI SurveysHI Surveys: (IGPS, etc.), high-: (IGPS, etc.), high-resolution 21 cm mappingresolution 21 cm mapping

Herschel Space Observatory

SCUBA-2

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Spitzer Space Telescope

Summary: K-band FPASummary: K-band FPA

synergistic, unique data to other single-dish FPAssynergistic, unique data to other single-dish FPAs

allow large surveys of NHallow large surveys of NH33 emission, yielding kinetic emission, yielding kinetic temperatures, column densities, and insight into the temperatures, column densities, and insight into the dense core dynamics; improve core statisticsdense core dynamics; improve core statistics

maximize use of “precious” K-band conditions in maximize use of “precious” K-band conditions in Green BankGreen Bank

provide crucial single-dish data for K-band EVLA provide crucial single-dish data for K-band EVLA projects in NHprojects in NH33, CCS, HC, CCS, HC33N, RRLs, HN, RRLs, H22O masers, etc.O masers, etc.

a 10 x 10 array could yield 5’ x 5’ full-beam a 10 x 10 array could yield 5’ x 5’ full-beam coveragecoverage

Mr. KLEANMr. KLEAN

K-band Line Emission Array of NraoK-band Line Emission Array of Nrao