Science with ALMA: a new era for Astrophysics 13 - 17 November 2006 Madrid, Spain. Fig.1. Fig.2. 24 m m 70 m m. Fig.3. 24 m m 70 m m. 70 m m 24 m m. Fig.5. Fig.4. 70 m m 24 m m. 70 m m 24 m m. Resolving the dust emission in the Vela Molecular Ridge
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13 - 17 November 2006
Resolving the dust emission in the Vela
M. De Luca(1,2),T. Giannini(2), D. Lorenzetti(2), D. Elia(3), G. Fazio(4),
M. Marengo(4), F. Massi(5), B. Nisini(2), H. A. Smith(4)
(1)Dipart. di Fisica - Università di Roma "Tor Vergata", (2)INAF - Oss. Astronomico di Roma, (3) Dipart. di Fisica - Università di Lecce, (4)Harvard Smithsonian Center for Astrophysics - MA (USA), (5)INAF - Oss. Astrofisico di Arcetri
The Vela Molecular Cloud - D, located in the Vela Molecular Ridge (VMR-D, at 700 pc), is a region characterized by high efficiency in producing both young embedded clusters and
Figures: 24(blue) and 70(red)mmimages of some unresolved dust peaks with overlaid contours of 1.2 mm emission (in green, from 3sin steps of 3s). The positions of IRAS and MSX point sources (cyan 3suncertainty ellipses) and a new 10.4 mm detection (magenta diamond in Fig.3, Timmi2-ESO) are shown as well.
and isolated stars and constitutes one of the best southern hemisphere sites to investigate low- to intermediate-mass star formation.
Our observations of the dust continuum emission (1.2 mm) of about 1 square degree with the SIMBA (SEST) bolometer array (24" HPBW), reveals a clumpy structure with 29 resolved (q > 24") and 26 unresolved (q < 24") peaks . The majority of these latter (hereafter: umms), present clear signs of star formation activity, such as association with: (i) far infrared point sources (IRAS  -MSX ); (ii) near infrared sources with intrinsic excess evidenced by two colour diagrams; (iii) jet-like H2 emission (this topic is
is discussed in Giannini et al., this conference).
Therefore such peaks might represent real detections of faint compact mm emission and, hence, suitable candidates of low-mass star forming sites. As such, they deserve further investigation.
To better improve both sensitivity and resolution in the mid- far-infrared and to reconstruct the spectral energy distributions,
distributions, we observed these unresolved dust peaks with Spitzer-MIPS: here we present some interesting cases where point-like far infrared counterparts have been revealed.
Association of unresolved dust peaks with far infrared point sources
(IRAS, MSX point source catalogs and MIPS images).
of 12" from the dust peak (SIMBA HPBW)
of 24" from the dust peak (2 x SIMBA HPBW)
 Liseau R., Lorenzetti D., Nisini B. et al. 1992 A&A 265, 577
 Massi F., De Luca M., Elia D. et al. 2006 A&A, submitted 399,14
C.A. Beichman et al. 1988, Infrared Astronomical Satellite (IRAS)
Catalogs and Atlases, vol. 1, Explanatory Supplement
 Price, S.D.et al. 2001 AJ 121, 2819