2015A&A...573A..82C


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.19CEST04:15:40

2015A&A...573A..82C - Astronomy and Astrophysics, volume 573A, 82-82 (2015/1-1)

A near-infrared spectroscopic survey of massive jets towards extended green objects.

CARATTI O GARATTI A., STECKLUM B., LINZ H., GARCIA LOPEZ R. and SANNA A.

Abstract (from CDS):

Protostellar jets and outflows are the main outcome of the star formation process, and their analysis can provide us with major clues about the ejection and accretion history of young stellar objects (YSOs). We aim at deriving the main physical properties of massive jets from near-infrared (NIR) observations, comparing them to those of a large sample of jets from low-mass YSOs, and relating them to the main features of their driving sources. We present a NIR imaging (H2 and Ks) and low-resolution spectroscopic (0.95-2.50µm) survey of 18 massive jets towards GLIMPSE extended green objects (EGOs), driven by intermediate- and high-mass YSOs, which have bolometric luminosities (Lbol) between 4x102 and 1.3x105L. As in low-mass jets, H2 is the primary NIR coolant, detected in all the analysed flows, whereas the most important ionic tracer is [FeII], detected in half of the sampled jets. Our analysis indicates that the emission lines originate from shocks at high temperatures and densities. No fluorescent emission is detected along the flows, regardless of the source bolometric luminosity. On average, the physical parameters of these massive jets (i.e. visual extinction, temperature, column density, mass, and luminosity) have higher values than those measured in their low-mass counterparts. The morphology of the H2 flows is varied, mostly depending on the complex, dynamic, and inhomogeneous environment in which these massive jets form and propagate. All flows and jets in our sample are collimated, showing large precession angles. Additionally, the presence of both knots and jets suggests that the ejection process is continuous with burst episodes, as in low-mass YSOs. We compare the flow H2 luminosity with the source bolometric luminosity confirming the tight correlation between these two quantities. Five sources, however, display a lower LH2/Lbol efficiency, which might be related to YSO evolution. Most important, the inferred LH2 vs. Lbol relationship agrees well with the correlation between the momentum flux of the CO outflows and the bolometric luminosities of high-mass YSOs indicating that outflows from high-mass YSOs are momentum driven, as are their low-mass counterparts. We also derive a less stringent correlation between the inferred mass of the H2 flows and Lbol of the YSOs, indicating that the mass of the flow depends on the driving source mass. By comparing the physical properties of jets in the NIR, a continuity from low- to high-mass jets is identified. Massive jets appear as a scaled-up version of their low-mass counterparts in terms of their physical parameters and origin. Nevertheless, there are consistent differences such as a more variegated morphology and, on average, stronger shock conditions, which are likely due to the different environment in which high-mass stars form.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: protostars - stars: massive - circumstellar matter - ISM: jets and outflows - infrared: ISM

CDS comments: MHO 1900-1902 not in SIMBAD.

Simbad objects: 44

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Number of rows : 44

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HH 34 HH 05 35 31.30 -06 28 43.0     16     ~ 469 2
2 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 283 1
3 HH 111 HH 05 51 44.2 +02 48 34           ~ 386 0
4 [HSL2000] IRS 2 IR 12 11 45.72 -61 46 19.8           ~ 3 0
5 IRAS 12091-6129 of? 12 11 47.67600 -61 46 20.5464           ~ 23 0
6 IRAS 12405-6219 PN? 12 43 31.1 -62 36 13           ~ 12 0
7 MSX6C G302.0213+00.2542 IR 12 43 31.3 -62 36 13           ~ 3 0
8 2MASS J12433151-6236135 IR 12 43 31.516 -62 36 13.55           ~ 3 0
9 IRAS 13481-6124 Y*O 13 51 37.85568 -61 39 07.5168           ~ 39 0
10 IRAS 13484-6100 cor 13 51 58.43 -61 15 41.3           ~ 26 0
11 EGO G310.15+0.76 of? 13 51 59.2 -61 15 37           ~ 4 0
12 2MASS J14245547-6145227 Y*? 14 24 55.47504 -61 45 22.7268           ~ 2 0
13 AKARI-IRC-V1 J1424563-614450 * 14 24 56.31744 -61 44 47.2956           ~ 1 0
14 2MASS J14250114-6144576 IR 14 25 01.146 -61 44 57.68           ~ 1 0
15 EGO G313.76-0.86 of? 14 25 01.3 -61 44 57           ~ 4 0
16 IRAS 14212-6131 HII 14 25 01.51896 -61 44 57.5916           ~ 16 0
17 GAL 316.72+00.07 DNe 14 44.4 -59 45           ~ 1 0
18 OH 316.76 -0.01 Mas 14 44 56.18 -59 48 12.3           ~ 11 0
19 2MASS J14445623-5947593 IR 14 44 56.2319682957 -59 47 59.315435951           ~ 2 0
20 IRAS 14416-5937 HII 14 45 28.6 -59 49 59           ~ 23 1
21 OH 322.16 +0.63 Mas 15 18 34.64 -56 38 25.3           ~ 31 0
22 MSX5C G322.1587+00.6262 IR 15 18 37.1 -56 38 55           ~ 2 0
23 EGO G326.48+0.70 of? 15 43 17.5 -54 07 11           ~ 3 0
24 2MASS J15431897-5407356 Y*O 15 43 18.97 -54 07 35.6           ~ 7 0
25 IRAS 15394-5358 HII 15 43 20.69 -54 07 35.7           ~ 23 0
26 IRAS 15450-5431 Y*? 15 48 55.232 -54 40 37.59           ~ 6 0
27 EGO G332.33-0.12 of? 16 16 03.3 -50 55 34           ~ 4 0
28 IRAS 16122-5047 IR 16 16 05.2 -50 54 36           ~ 4 0
29 SSTGLMC G332.3526-00.1154 IR 16 16 06.878 -50 54 27.06           ~ 1 0
30 2MASS J16160689-5054274 IR 16 16 06.897 -50 54 27.40           ~ 1 0
31 EGO G332.35-0.12 of? 16 16 07.0 -50 54 30           ~ 3 0
32 EGO G343.12-0.06 of? 16 58 16.6 -42 52 04           ~ 3 0
33 IRAS 16547-4247 Y*O 16 58 17.21 -42 52 08.9           ~ 113 0
34 [PCB2009] F39 Y*? 18 21 12.088 -16 30 04.56           ~ 3 0
35 [WWS2012] G014.86-00.99 cor 18 21 12.4936 -16 30 17.536           ~ 12 1
36 SDC G35.041-0.471 DNe 18 56 58.04 +01 39 44.5           ~ 4 0
37 MHO 2429 EmO 18 56 58.1 +01 39 37           ~ 3 0
38 EGO G035.04-0.47 of? 18 56 58.1 +01 39 37           ~ 10 0
39 SSTGLMC G035.0393-00.4735 IR 18 56 58.1 +01 39 34           ~ 1 0
40 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 91 0
41 [TRP85] G35.2N IRS 1 Y*O 18 58 13.106 +01 40 39.90           ~ 15 0
42 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 133 0
43 [MSM95] G35.20 FIR 1 FIR 18 58 13.2 +01 40 26           ~ 8 0
44 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 398 0

    Equat.    Gal    SGal    Ecl

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2020.09.19-04:15:40

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