SiO
                    <i>J</i>
                    = 5-4 in the HH 211 Protostellar Jet Imaged with the Submillimeter Array

Hirano, Naomi; Liu, Sheng-Yuan; Shang, Hsien; Ho, P. T. P.; Huang, Hui‐Chun; Kuan, Yi‐Jehng; McCaughrean, M. J.; Zhang, Qizhou

doi:10.1086/500201

Cited by 98 publications

(141 citation statements)

References 14 publications

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“…Interestingly, the highest T MB suggests high excitation conditions with T kin ≥ 100 K and n H 2 ≥ 10 5 cm −3 , in agreement with the estimates found for SiO clumps associated with other protostellar outflows (e.g. Hirano et al 2006;Nisini et al 2007;Cabrit et al 2007), confirming the association of SiO with shocked material. If we model the T MB ∼ 30 K of the high-velocity SO(6 5 -5 4 ) emission observed towards clump C using RADEX coupled with the collision rates provided by Green (1994), we find N SO ∼ 10 16 -10 17 cm −2 and n H 2 ≥ 10 5 cm −3 , supporting, as for SiO, shocked (compressed) gas.…”

Section: High Brightness Temperatures and Excitation Conditionssupporting

confidence: 88%

First results from the CALYPSO IRAM-PdBI survey

Codella

Maury

Gueth

et al. 2014

A&A

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Context. The earliest evolutionary stages of low-mass protostars are characterised by hot and fast jets which remove angular momentum from the circumstellar disk, thus allowing mass accretion onto the central object. However, the launch mechanism is still being debated. Aims. We would like to exploit high-angular (∼0. 8) resolution and high-sensitivity images to investigate the origin of protostellar jets using typical molecular tracers of shocked regions, such as SiO and SO. Methods. We mapped the inner 22 of the NGC 1333-IRAS2A protostar in SiO(5-4), SO(6 5 -5 4 ), and the continuum emission at 1.4 mm using the IRAM Plateau de Bure Interferometer in the framework of the CALYPSO IRAM large program. Results. For the first time, we disentangle the NGC 1333-IRAS2A Class 0 object into a proto-binary system revealing two protostars (MM1, MM2) separated by ∼560 AU, each of them driving their own jet, while past work considered a single protostar with a quadrupolar outflow. We reveal (i) a clumpy, fast (up to |V − V LSR | ≥ 50 km s −1 ), and blueshifted jet emerging from the brightest MM1 source; and (ii) a slower redshifted jet, driven by MM2. Silicon monoxide emission is a powerful tracer of high-excitation (T kin ≥ 100 K; n H 2 ≥ 10 5 cm −3 ) jets close to the launching region. At the highest velocities, SO appears to mimic SiO tracing the jets, whereas at velocities close to the systemic one, SO is dominated by extended emission, tracing the cavity opened by the jet. Conclusions. Both jets are intrinsically monopolar, and intermittent in time. The dynamical time of the SiO clumps is ≤30-90 yr, indicating that one-sided ejections from protostars can take place on these timescales.

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Section: High Brightness Temperatures and Excitation Conditionssupporting

confidence: 88%

First results from the CALYPSO IRAM-PdBI survey

Codella

Maury

Gueth

et al. 2014

A&A

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“…In some cases it seems to be associated with the most excited parts of the flows (136-356 and 137-408 outflows, this paper; HH 211, Hirano et al 2006 ;Palau et al 2006) while in other cases it is associated with internal shocks in the outflows, ( L1157, Gueth et al 1998;L1448, Dutrey et al 1997136-359 CO outflow, this paper). One possibility for unifying these two mechanisms would be if the SiO molecule is formed / excited in shocks that are propagating down the jet (''internal working surfaces''), as proposed by Arce et al (2006).…”

Section: Discussionmentioning

confidence: 75%

“…The CO emission is possibly tracing low-density entrained gas with a less broad range of velocities, as has been observed by Palau et al (2006) in the HH 211 flow. Following this premise, in these SiO observations we have imaged unresolved emission from the jet itself, as observed by Hirano et al (2006) and Palau et al (2006). However, for this mechanism to work, we need strong chemical mechanisms that would strongly favor the detection of each molecule in the two components of different density.…”

Section: Discussionmentioning

confidence: 94%

Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC 1 South Region

Zapata

Rodrı́guez

et al. 2006

ApJ

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We present high angular resolution (2B8 ; 1B7) SiO J ¼ 5 ! 4, v ¼ 0 line observations of the OMC 1S region in the Orion Nebula made using the Submillimeter Array (SMA). We detect for the first time a cluster of four compact bipolar and monopolar outflows that show high-, moderate-, and low-velocity gas and appear to be energized by millimeter and infrared sources associated with this region. The SiO molecular outflows are compact (<3500 AU ), and in most of the cases, they are located very close to their exciting sources. We thus propose that the SiO thermal emission is tracing the youngest and most highly excited parts of the outflows that cannot be detected by other molecules. Moreover, since the ambient cloud is weak in the SiO line emission, these observations can reveal flows that in other molecular transitions will be confused with the ambient velocity cloud emission.

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“…The highvelocity jet-like structure is also traced by SiO emission (e.g. Hirano et al 2006). The total extent of the outflow is ∼1.2 , with a terminal radial velocity of 25 km s −1 on the blue lobe and 35 km s −1 on the red lobe (with respect to the cloud V LSR of +9.2 km s −1 Palau et al 2006).…”

Section: Hh211-mmmentioning

confidence: 97%

Warm gas in protostellar outflows

Gómez-Ruiz

Wyrowski

Leurini

et al. 2013

A&A

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Context. Observations of CO rotational transitions in the 0.3−0.4 millimeter range, now possible from exceptional sites on the ground, provide the opportunity of studying the warm component of molecular outflows in star-forming regions. Aims. This study aims to characterize the role of the warm gas in high-velocity and collimated outflows from Class 0 low-mass protostars. Methods. We used the CHAMP + heterodyne array on the APEX telescope to map the CO (6-5) and CO (7-6) emission in the wellknown Class 0 outflows L1448-mm and HH211-mm. We complement these data with 13 CO (6-5) observations and also with previous low-J CO observations. Results. The CO (6-5) and (7-6) emission was detected to be tracing the outflow lobes. In L1448, extremely high-velocity (EHV) emission was detected in both transitions. In HH211, high-velocity CO (6-5) emission was detected to be tracing the regions close to the central object, but it was also found close to the bow-shock regions seen in the mid-IR. A large velocity gradient code applied to these and the complementary low-J CO data revealed the high-velocity components to be dense (>10 5 cm −3 ) and warm (T > 200 K) gas, in agreement with previous observations of shock tracers such as SiO. Conclusions. The high-velocity emission of these mid-J CO transitions are very good tracers of the inner highly excited part of outflows, which possibly is molecular material related to the underlying jet. In addition, these transitions are also strong at the bowshock positions, which make them a good tool for probing these environments.

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SiO J = 5-4 in the HH 211 Protostellar Jet Imaged with the Submillimeter Array

Cited by 98 publications

References 14 publications

First results from the CALYPSO IRAM-PdBI survey

First results from the CALYPSO IRAM-PdBI survey

Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC 1 South Region

Warm gas in protostellar outflows

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