Near- and far-infrared counterparts of millimeter dust cores in the Vela molecular ridge cloud D*,**

被引：0

作者：

De Luca, M. ^{[1
,2
]}

Giannini, T. ^{[1
]}

Lorenzetti, D. ^{[1
]}

Massi, F. ^{[3
]}

Elia, D. ^{[4
]}

Nisini, B. ^{[1
]}

机构：

[1] INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone (Roma), Italy

[2] Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy

[3] INAF - Osservatorio Astrofisico di Arcetri, Largo E.Fermi 5, 50125 Firenze, Italy

[4] Dipartimento di Fisica, Università di Lecce, CP 193, 73100 Lecce, Italy

来源：

Astronomy and Astrophysics | 2007年 / 474卷 / 03期

关键词：

Aims. Identify the young protostellar counterparts associated with dust millimeter cores of the Vela Molecular Ridge Cloud D through new IR observations (H2 narrow-band at 2.12 μm and N broad band at 10.4 μm) along with an investigation performed on the existing IR catalogues. Methods. The association of mm continuum emission with infrared sources from catalogues (IRAS; MSX; 2MASS); JHK data from the literature; and new observations; was established according to spatial coincidence; infrared colours and spectral energy distributions. Results. Only 7 out of 29 resolved mm cores (and 16 out of the 26 unresolved ones) do not exhibit signposts of star formation activity. The other ones are clearly associated with: far-IR sources; H2 jets pointing back to embedded objects not (yet) detected or near-IR objects showing a high intrinsic colour excess. The distribution of the spectral indices pertaining to the associated sources is peaked at values typical of Class I objects; while three objects are signalled as candidates Class 0 sources. Objects with far-IR colours similar to those of T-Tauri and Herbig Ae/Be stars seem to be very few. An additional population of young objects exists associated not with the mm-cores; but with both the diffuse warm dust emission and the gas filaments. We point out the high detection rate (30%) of H2 jets driven by sources located inside the mm-cores. They do not appear to be driven by the most luminous objects in the field; but rather by less luminous objects in young clusters; testifying the co-existence of both low- and intermediate-mass star formation. Conclusions. The presented results reliably describe the young population of VMR-D. However; the statistical evaluation of activity vs. inactivity of the investigated cores; even in good agreement with results found for other star forming regions; seems to reflect the limiting sensitivity of the available facilities rather than any property intrinsic to the mm-condensations. © ESO 2007;

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摘要：

Journal article (JA)

引用

页码：863 / 872

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