Survey of intermediate/high mass star-forming regions at centimeter and millimeter wavelengths

Sánchez-Monge, Á.; Palau, Aina; Estalella, R.; Beltrán, M. T.; Girart, J. M.

doi:10.1051/0004-6361:20078406

Cited by 37 publications

(71 citation statements)

References 72 publications

(130 reference statements)

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“…These observations reveal two sources in the field: an eastern source coincident with the UCH ii region, and a second and fainter source located ∼15 to the west. Figure 1b shows the resulting image after combining the new VLA C-configuration observations with previous VLA Dconfiguration observations (Sánchez-Monge et al 2008). Since the combined dataset has a better uv-coverage, we recovered faint structure to the south of the UCH ii region similar to the double-source structure detected at 1.3 cm by Sánchez-Monge et al (2008).…”

Section: Centimeter Continuum Emissionmentioning

confidence: 74%

“…c) VLA-D 1.3 cm continuum emission. Levels are −3, 3, and 6 times 0.07 mJy beam −1 (Sánchez-Monge et al 2008). d) VLA-D 0.7 cm continuum emission.…”

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

“…Levels are −3, and 3 to 21 in steps of 3, times 0.19 mJy beam −1 . Grey contours: IRAM 30 m continuum emission tracing the "dusty cloud", from Sánchez-Monge et al (2008). Levels are 4,6,8,10, and 12 times the rms of the map, 8 mJy beam −1 .…”

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

“…Note that the coordinates of MM1 correspond to the coordinates of MM1-main, listed in Table 3. (c) Data from Sánchez-Monge et al (2008). Deconvolved size and PA correspond to the component VLA 3 from Sánchez-Monge et al (2008), which is the component associated with the easternmost 2MASS source shown in Fig.…”

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

“…(a) Data from the VLA archive. The low sensitivity of the archival dataset does not allow to obtain better maps (when we combined the C and D configuration data) than previous VLA-D data maps (Sánchez-Monge et al 2008). conditions of the cloud in the cluster formation process and ultimately in the formation of intermediate/high-mass stars.…”

Section: Introductionmentioning

confidence: 96%

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Three intermediate-mass young stellar objects with different properties emerging from the same natal cloud in IRAS 00117+6412

Palau¹,

Sánchez-Monge

Busquet

et al. 2010

A&A

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Aims. Our main aim is to study the influence of the initial conditions of a cloud in the intermediate/high-mass star formation process. Methods. We observed with the VLA, PdBI, and SMA the centimeter and millimeter continuum, N 2 H + (1-0), and CO (2-1) emission associated with a dusty cloud harboring a nascent cluster with intermediate-mass protostars.Results. At centimeter wavelengths we found a strong source, tracing a UCH ii region, at the eastern edge of the dusty cloud, with a shell-like structure, and with the near-infrared counterpart falling in the center of the shell. This is presumably the most massive source of the forming cluster. About 15 to the west of the UCH ii region and well embedded in the dusty cloud, we detected a strong millimeter source, MM1, associated with centimeter and near-infrared emission. MM1 seems to be driving a prominent high-velocity CO bipolar outflow elongated in the northeast-southwest direction, and is embedded in a ridge of dense gas traced by N 2 H + , elongated roughly in the same direction as the outflow. We estimated that MM1 is an intermediate-mass source in the Class 0/I phase. About 15 to the south of MM1, and still more deeply embedded in the dusty cloud, we detected a compact millimeter source, MM2, with neither centimeter nor near-infrared emission, but with water maser emission. MM2 is associated with a clump of N 2 H + , whose kinematics reveal a clear velocity gradient and additionally we found signposts of infall motions. MM2, being deeply embedded within the dusty cloud, with an associated water maser but no hints of CO outflow emission, is an intriguing object, presumably of intermediate mass.Conclusions. The UCH ii region is found at the border of a dusty cloud which is currently undergoing active star formation. Two intermediate-mass protostars in the dusty cloud seem to have formed after the UCH ii region and have different properties related to the outflow phenomenon. Thus, a single cloud with similar dust emission and similar dense gas column densities seems to be forming objects with different properties, suggesting that the initial conditions in the cloud are not determining all the star formation process.

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Section: Centimeter Continuum Emissionmentioning

confidence: 74%

“…c) VLA-D 1.3 cm continuum emission. Levels are −3, 3, and 6 times 0.07 mJy beam −1 (Sánchez-Monge et al 2008). d) VLA-D 0.7 cm continuum emission.…”

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

Section: Plateau De Bure Interferometer Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

See 3 more Smart Citations

Three intermediate-mass young stellar objects with different properties emerging from the same natal cloud in IRAS 00117+6412

Palau¹,

Sánchez-Monge

Busquet

et al. 2010

A&A

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Accretion disks in luminous young stellar objects

Beltrán

Wit

2016

Astron Astrophys Rev

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193

189

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An observational review is provided of the properties of accretion disks around young stars. It concerns the primordial disks of intermediate-and high-mass young stellar objects in embedded and optically revealed phases. The properties were derived from spatially resolved observations and therefore predominantly obtained with interferometric means, either in the radio/(sub)millimeter or in the optical/infrared wavelength regions. We make summaries and comparisons of the physical properties, kinematics, and dynamics of these circumstellar structures and delineate trends where possible. Amongst others, we report on a quadratic trend of mass accretion rates with mass from T Tauri stars to the highest mass young stellar objects and on the systematic difference in mass infall and accretion rates.

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Radio jets from young stellar objects

Anglada

Rodrı́guez²,

Carrasco-González³

2018

Astron Astrophys Rev

137

151

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Jets and outflows are ubiquitous in the process of formation of stars since outflow is intimately associated with accretion. Free-free (thermal) radio continuum emission in the centimeter domain is associated with these jets. The emission is relatively weak and compact, and sensitive radio interferometers of high angular resolution are required to detect and study it. One of the key problems in the study of outflows is to determine how they are accelerated and collimated. Observations in the cm range are most useful to trace the base of the ionized jets, close to the young central object and the inner parts of its accretion disk, where optical or near-IR imaging is made difficult by the high extinction present. Radio recombination lines in jets (in combination with proper motions) should provide their 3D kinematics at very small scale (near their origin). Future instruments such as the Square Kilometre Array (SKA) and the Next Generation Very Large Array (ngVLA) will be crucial to perform this kind of sensitive observations. Thermal jets are associated with both high and low mass protostars and possibly even with objects in the substellar domain. The ionizing mechanism of these radio jets appears to be related to shocks in the associated outflows, as suggested by the observed correlation between the centimeter luminosity and the outflow momentum rate. From this correlation and that of the centimeter luminosity with the bolometric luminosity of the system it will be possible to discriminate between unresolved HII regions and jets, and to infer additional physical properties of the embedded objects. Some jets associated with young stellar objects (YSOs) show indications of nonthermal emission (negative spectral indices) in part of their lobes. Linearly polarized synchrotron emission has been found in the jet of HH 80-81, allowing one to measure the direction and intensity of the jet magnetic field, a key ingredient to determine the collimation and ejection mechanisms. As only a fraction of the emission is polarized, very sensitive observations such as those that will be feasible with the interferometers previously mentioned are required to perform studies in a large sample of sources. Jets are present in many kinds of astrophysical scenarios. Characterizing radio jets in YSOs, where thermal emission allows one to determine their physical conditions in a reliable way, would also be useful in understanding acceleration and collimation mechanisms in all kinds of astrophysical jets, such as those associated with stellar and supermassive black holes and planetary nebulae.

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Survey of intermediate/high mass star-forming regions at centimeter and millimeter wavelengths

Cited by 37 publications

References 72 publications

Three intermediate-mass young stellar objects with different properties emerging from the same natal cloud in IRAS 00117+6412

Three intermediate-mass young stellar objects with different properties emerging from the same natal cloud in IRAS 00117+6412

Accretion disks in luminous young stellar objects

Radio jets from young stellar objects

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