Dissection of the protostellar envelope  surrounding IRAS 05173-0555 in L1634

Beltrán, M. T.; Wiseman, Jennifer; Ho, Paul T. P.; Estalella, R.; Fuller, G. A.; Wootten, Alwyn

doi:10.1051/0004-6361:20079224

Cited by 4 publications

(5 citation statements)

References 28 publications

(69 reference statements)

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“…A similar outline of the eastern outflow cavity walls is also visible, but cannot be traced all the way to the unresolved source, due to absorption from the nearly edge-on disk surrounding the driving source. The point source, presumably at or very near the driving protostellar source of the outflow, is located at α(2000) = 05:19:48.37, δ(2000) = -05:52:03.9, consistent with the positions given by Beltrán et al (2002) for the sub-mm source, and by Beltrán et al (2008) for the peak of the NH 3 position in VLA measurements.…”

Section: Shock Front Proper Motionssupporting

confidence: 72%

“…′′ 3 from that source. The mid-point between these innermost shock fronts -located at α(2000) = 05:19:48.74 -does not show any detectable K-band continuum source, is not morphologically consistent with the apex of the cavity outline, and does not coincide with any significant feature in the maps of Beltrán et al (2002) and Beltrán et al (2008).…”

Section: Shock Front Proper Motionsmentioning

confidence: 89%

“…More detailed sub-mm maps were published by Chini et al (1997) and Beltrán et al (2002), clearly showing some sub-mm emission from the IRS 7 source. While Beltrán et al (2008) have mapped the outflow cavity of the main (IRAS 05173-0555) flow, no NH 3 (1,1) emission was detected at the position of IRS 7. Bally et al (2009) identify a third outflow, labeled L1634N, which is located at the northern edge of the L1634 cloud.…”

Section: Introductionmentioning

confidence: 98%

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Periodic Accretion Instabilities in the Protostar L1634 Irs 7

Hodapp

Chini

2015

ApJ

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The small molecular cloud Lynds 1634 contains at least three outflow sources. We found one of these, IRS 7, to be variable with a period of 37.14 ± 0.04 days and an amplitude of approximately 2 mag in the K s band. The light curve consists of a quiescent phase with little or no variation, and a rapid outburst phase. During the outburst phase, the rapid brightness variation generates light echoes that propagate into the surrounding molecular cloud, allowing a measurement of the distance to IRS 7 of 404 pc ± 35 pc. We observed only a marginally significant change in the H − K color during the outburst phase. The K-band spectrum of IRS 7 shows CO bandhead emission but its equivalent width does not change significantly with the phase of the light curve. The H 2 1-0 S(1) line emission does not follow the variability of the continuum flux. We also used the imaging data for a proper motion study of the outflows originating from the IRS 7 and the FIR source IRAS 05173-0555, and confirm that these are indeed distinct outflows.

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Section: Shock Front Proper Motionssupporting

confidence: 72%

Section: Shock Front Proper Motionsmentioning

confidence: 89%

Section: Introductionmentioning

confidence: 98%

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Periodic Accretion Instabilities in the Protostar L1634 Irs 7

Hodapp

Chini

2015

ApJ

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“… a Outflow activity previously detected by [1]Fukui et al (1993), Lefloch, Lazareff & Castets (1997), Wu et al (2004); [2]Wu et al (2004); [3]Fukui et al (1993), De Vries et al (2002), Wu et al (2004), Beltrán et al (2008); [4]De Vries et al (2002), Wu et al (2004); [5]De Vries et al (2002). …”

Section: Resultsmentioning

confidence: 99%

CO observations towards bright-rimmed clouds

Morgan

Urquhart

2009

Monthly Notices of the Royal Astronomical Society

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Original article can be found at : http://www3.interscience.wiley.com/ Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]Bright-rimmed clouds (BRCs) appear to be sites of triggered star formation induced through the propagation of shocks initiated by the expansion of nearby H ii regions. Our main aim is to establish support for observations of star-forming activity within a sample of BRCs. A secondary aim is to establish a plausible link between such star formation and observed external influences. We have conducted CO (J = 2???1) observations using the James Clerk Maxwell Telescope to probe the environments of a sample of star-forming BRCs associated with embedded protostellar cores. Local thermodynamic equilibrium analysis allows the determination of the physical properties of these protostars and investigation of the structure and kinematic motions within the molecular gas. Using a combination of archival radio and mid-infrared data, and submillimeter observations, we have refined the Sugitani, Fukui and Ogura (SFO) catalogue, excluding 18 BRCs that do not show any evidence of photoionization induced collapse. Of the remaining 26 clouds that are being photoionized, we find 20 that are associated with embedded protostars. These 20 clouds are excellent candidates with which to further investigate the radiatively driven implosion mode of triggered star formation. Comparing the physical parameters of the triggered and untriggered samples, we find that the surface temperatures of the potentially triggered clouds are significantly higher (by ???10 K) than those in which triggering is considered unlikely. The higher surface temperatures found towards the sample of potentially triggered clouds are consistent with the hypothesis that these clouds are being externally heated through their exposure to the H ii region

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“…Ammonia has been previously observed to probe cavity walls around evolved molecular outflows (Anglada et al 1995;Beltrán et al 2008), and to take part in collimated high-velocity outflows (Bachiller et al 1993;Tafalla & Bachiller 1995;Curiel et al 1996). In the latter case, the gas properties (line shapes, kinetic temperatures, enhanced ammonia abundances) show clear evidence for shocks.…”

Section: Core Kinematicsmentioning

confidence: 98%

High-resolution ammonia mapping of the very young protostellar core Chamaeleon-MMS1

Väisälä

Harju

Mantere

et al. 2014

A&A

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Aims. The aim of this study is to investigate the structure and kinematics of the nearby candidate first hydrostatic core Cha-MMS1. Methods. Cha-MMS1 was mapped in the NH 3 (1, 1) line and the 1.2 cm continuum using the Australia Telescope Compact Array (ATCA). The angular resolution of the ATCA observations is 7 (∼1000 AU), and the velocity resolution is 50 m s −1 . The core was also mapped with the 64 m Parkes Telescope in the NH 3 (1, 1) and (2, 2) lines. Observations from Herschel Space Observatory and Spitzer Space Telescope were used to help interpretation. The ammonia spectra were analysed using Gaussian fits to the hyperfine structure. A two-layer model was applied in the central parts of the core where the ATCA spectra show signs of self-absorption. Results. A compact high column density core with a steep velocity gradient (∼20 km s −1 pc −1 ) is detected in ammonia. We derive a high gas density (∼10 6 cm −3 ) in this region, and a fractional ammonia abundance compatible with determinations towards other dense cores (∼10 −8 ). This suggests that the age of the high density core is comparable to the freeze-out timescale of ammonia in these conditions, on the order of 10 4 years. The direction of the velocity gradient agrees with previous single-dish observations, and the overall velocity distribution can be interpreted as rotation. The rotation axis goes through the position of a compact far-infrared source detected by Spitzer and Herschel. The specific angular momentum of the core, ∼10 −3 km s −1 pc, is typical for protostellar envelopes. A string of 1.2 cm continuum sources is tentatively detected near the rotation axis. The ammonia spectra suggest the presence of warm embedded gas in its vicinity. An hourglass-shaped structure is seen in ammonia at the cloud's average LSR velocity, also aligned with the rotation axis. Although this structure resembles a pair of outflow lobes the ammonia spectra show no indications of shocked gas. Conclusions. The observed ammonia structure mainly delineates the inner envelope around the central source. The velocity gradient is likely to originate in the angular momentum of the contracting core, although influence of the outflow from the neighbouring young star IRS4 is possibly visible on one side of the core. The tentative continuum detection and the indications of a warm background component near the rotation axis suggest that the core contains a deeply embedded outflow which may have been missed in previous single-dish CO surveys owing to beam dilution.

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Dissection of the protostellar envelope surrounding IRAS 05173-0555 in L1634

Cited by 4 publications

References 28 publications

Periodic Accretion Instabilities in the Protostar L1634 Irs 7

Periodic Accretion Instabilities in the Protostar L1634 Irs 7

CO observations towards bright-rimmed clouds

High-resolution ammonia mapping of the very young protostellar core Chamaeleon-MMS1

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