Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.atnf.csiro.au/research/hypercompact/talks/Titmarsh.pdf Äàòà èçìåíåíèÿ: Wed Sep 8 04:57:43 2010 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 15:51:04 2012 Êîäèðîâêà: koi8-r Ïîèñêîâûå ñëîâà: ï ï ï ï ï ï ï ï ï ï ï ï ï

First look with MALT90
Anita Titmarsh, Kate Brooks and the MALT90 team
University of Tasmania/CSIRO

8 Septemb er 2010


The MALT90 survey



3000 dense cores from ATLASGAL (870 µm) 3' â 3' maps of 90-GHz molecular lines with Mopra Cores divided into 4 categories based on mid-IR emission




Quiescent: cores without signs of star formation Protostellar: cores with an embedded protostar, typically seen at 24 µm HII region: HII regions, whether large or small PDR: these regions near HII regions and will show up as extended emission at 8 µm. Often the swept up dust here has little sign of star formation but is still not really quiescent


Selecting HCHII region candidates in MALT90

Started with sources from Andres Guzman


3 and 6 cm RMS flux densities give a p ositive sp ectral index MSX flux density for every source 50 out of 79 overlap b etween Guzman sources and MALT90 catalog majority of Guzman sources fall into 'HI I region' and 'Protostellar' categories




why not 100% overlap?




Guzman sources have MSX detections (8.28 µm - 21.3 µm) but not all have IRAS detections (12 µm - 100 µm), biased toward stronger mid-IR sources


biased toward hotter, more evolved YSOs



MALT90 catalog comes from ATLASGAL (survey at 870 µm), >50% of ATLASGAL sources discovered have no counterpart in IRAS and MSX


biased toward colder, younger YSOs


G302.486-00.030

MALT90 classifcation 8.6-GHz flux density 8.6-GHz size (p c) distance (kp c) luminosity (L ) 22-GHz water maser? 6.7-GHz methanol maser? EGO present?

HI I region 24.4 0.08567 3.83484 8447.35 yes -


¢¢¡¡ ¢¢¡¡ ¢ ¢ ¢¡ ¡ ¢¡ ¡
0.3
G302.486-00.030 c2h

0.3

G302.486-00.030

hcn

0.3

G302.486-00.030

hnc

0.2

0.2

0.2

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.1

0.1

Average Intensity (Jy/beam)

0.1

0.0

0.0

0.0

0.1

0.1

0.1

0.2120

100

80

60 Velocity (km/s)

40

20

0

0.2120

100

80

60 Velocity (km/s)

40

20

0

0.2120

100

80

60 Velocity (km/s)

40

20

0


G308.916+00.124

MALT90 classifcation 8.6-GHz flux density 8.6-GHz size (p c) distance (kp c) luminosity (L ) 22-GHz water maser? 6.7-GHz methanol maser? (107-GHz also) EGO present?

HI I region 374.1 0.16033 3.82749 133325 yes yes -


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0.6

G308.916+00.124

0.5

13c34s

0.5

G308.916+00.124

13cs

G308.916+00.124

c2h

0.4

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.3

Average Intensity (Jy/beam)

0.4

0.3

0.3

0.2

0.2

0.2

0.1

0.1

0.1

0.0

0.0

0.0

0.1

0.1

0.2

0.2

0.1

140

120

100

80 60 Velocity (km/s)

40

20

0

140

120

100

80 60 Velocity (km/s)

40

20

0

0.2140

120

100

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40

20

0

G308.916+00.124

hcn

1.0

G308.916+00.124

hcop

G308.916+00.124

hnc

0.6

0.8

0.6

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.4

0.6

Average Intensity (Jy/beam)

0.4

0.2

0.4

0.2

0.0

0.2

0.2

0.0

0.0

0.4140

120

100

80 60 Velocity (km/s)

40

20

0

0.2 140

0.2

120

100

80 60 Velocity (km/s)

40

20

0

140

120

100

80 60 Velocity (km/s)

40

20

0

0.5

G308.916+00.124

n2hp

0.4

Average Intensity (Jy/beam)

0.3

0.2

0.1

0.0

0.1

0.2

140

120

100

80 60 Velocity (km/s)

40

20

0


G338.927+00.632

MALT90 classifcation 8.6-GHz flux density 8.6-GHz size (p c) distance (kp c) luminosity (L ) 22-GHz water maser? 6.7-GHz methanol maser? EGO present?

Protostellar 166.5 0.07505 4.3 153331 -



0.6

G338.927+00.632

0.5

c2h

0.4

G338.927+00.632

h13cop

0.5

G338.927+00.632

hc3n

0.3

0.4

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.3

Average Intensity (Jy/beam)

0.4

0.2

0.3

0.2

0.1

0.2

0.1

0.0

0.1

0.0

0.0

0.1

0.1

0.1

0.2

0.2

0.2

140

120

100

80 60 Velocity (km/s)

40

20

0

140

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80 60 Velocity (km/s)

40

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0

140

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40

20

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G338.927+00.632

0.6

hcn

G338.927+00.632

hcop

0.5

G338.927+00.632

hn13c

0.6

0.4

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.4

0.4

Average Intensity (Jy/beam)

0.3

0.2

0.2

0.2

0.1

0.0

0.0

0.0

0.1

0.2

0.2

0.2

140

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20

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140

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20

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140

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40

20

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G338.927+00.632

0.8

n2hp

0.3

G338.927+00.632

sio

Average Intensity (Jy/beam)

0.4

Average Intensity (Jy/beam)

0.6

0.2

0.1

0.2

0.0

0.0

0.2

0.1

0.4140

120

100

80 60 Velocity (km/s)

40

20

0

0.2140

120

100

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40

20

0


G340.248-00.376

MALT90 classifcation 8.6-GHz flux density 8.6-GHz size (p c) distance (kp c) luminosity (L ) 22-GHz water maser? 6.7-GHz methanol maser? EGO present?

Protostellar 150.8 0.05969 3.8 51000 -


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0.5
G340.248-00.376 h13cop

0.5

G340.248-00.376

G340.248-00.376

hc3n

0.4

0.4

0.6

hcn

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.3

0.3

0.4

0.2

0.2

0.1

0.1

0.2

0.0

0.0

0.0

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0.1

0.2

0.2120

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0.2120

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1.0

G340.248-00.376

hcop

1.0

G340.248-00.376

hnc

0.5

G340.248-00.376

hnco404

0.8

0.8

0.4

Average Intensity (Jy/beam)

Average Intensity (Jy/beam)

0.6

0.6

Average Intensity (Jy/beam)

0.3

0.2

0.4

0.4

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0.2

0.2

0.0

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120

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G340.248-00.376

1.0

n2hp

0.5

G340.248-00.376

sio

0.8

0.4

Average Intensity (Jy/beam)

0.6

Average Intensity (Jy/beam)

0.3

0.4

0.2

0.2

0.1

0.0

0.0

0.2

0.1

120

100

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40

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0.2120

100

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40

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0


13c34s 13cs c2h ch3cn h13co+ h41a hc13ccn hc3n hcn hco+ hn13c hnc hnco404 hnco413 n2h+ si o

G302... offset y y -

G308... y y y y y y offset -

G338... y y y y y y y y y y

G340... y y y y y y y y

Optical depth Optical depth PDR Hot core Optical depth Ionized gas Hot core Hot core Density Density Optical depth Density Hot core Hot core Density Shock/outflow


Conclusions/future work



look for trends in all the Guzman sources in MALT90 2011 aim to observe promising candidates with the ATCA to model SEDs look for HCHI I region candidates not included in the source list from Guzman




MALT90 'Protostellar' bin may be the place to start generally more compact in their radio emission SiO and perhaps more hot core tracers