A GMRT survey of regions towards the Taurus molecular cloud at 323 and 608 MHz

Ainsworth, Rachael; Coughlan, Colm P.; Green, David A.; Scaife, Anna M. M.; Ray, T. P.

doi:10.1093/mnras/stw1847

Cited by 5 publications

(5 citation statements)

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“…Based on its infrared properties, Gutermuth et al (2009) classified it as a Class II young stellar object. However, Dzib et al (2015) found no evidence of proper motions, a result that favors an extragalactic nature for the The data points at 323 and 608 MHz are from Ainsworth et al (2016),while the data points at 1.4, 4,5 and 9.9 GHz are from Condon et al (1998), Dzib et al (2015) and this paper, respectively. Blue and black dots correspond to the data compiled by Anglada (1995) and Furuya et al (2003), respectively, showing the relation for young stellar objects.…”

Section: Mhomentioning

confidence: 70%

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JVLA Observations of Young Brown Dwarfs

Rodríguez¹,

Zapata²,

Palau³

2017

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We present sensitive 3.0 cm JVLA radio continuum observations of six regions of low-mass star formation that include twelve young brown dwarfs and four young brown dwarf candidates. We detect a total of 49 compact radio sources in the fields observed, of which 24 have no reported counterparts and are considered new detections. Twelve of the radio sources show variability in timescales of weeks to months, suggesting gyrosynchrotron emission produced in active magnetospheres. Only one of the target brown dwarfs, FU Tau A, was detected. However, we detected radio emission associated with two of the brown dwarf candidates, WL 20S and CHLT 2. The radio flux densities of the sources associated with these brown dwarf candidates are more than an order of magnitude larger than expected for a brown dwarf and suggest a revision of their classification. In contrast, FU Tau A falls on the well-known correlation between radio luminosity and bolometric luminosity, suggesting that the emission comes from a thermal jet and that this brown dwarf seems to be forming as a scaled-down version of low-mass stars.

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Section: Mhomentioning

confidence: 70%

“…Fig. 2.-Radio spectrum of the source 2MASS J04322946+1814002, located in the MHO 5 region.The data points at 323 and 608 MHz are fromAinsworth et al (2016),while the data points at 1.4, 4,5 and 9.9 GHz are fromCondon et al (1998),Dzib et al (2015) and this paper, respectively.…”

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confidence: 99%

JVLA Observations of Young Brown Dwarfs

Rodríguez¹,

Zapata²,

Palau³

2017

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“…While Galactic cold cores are showing very low levels of AME that may be indicative of very small dust grains depletion, still nothing is known about the level of AME associated to YSOs. Radio observations obtained with the Giant Metre Radio Telescope (GMRT; Ainsworth et al 2016;Coughlan et al 2017) are probing the free-free emission associated with the outflow of T Tau. Any detection of AME associated with such objects in the frequency range 10-60 GHz would be indicative of dust grain evolution and possibly could be used as a star-formation evolution tracer.…”

Section: Future Directions For Galactic Ame Studiesmentioning

confidence: 99%

The State-of-Play of Anomalous Microwave Emission (AME) research

Dickinson

Ali-Haı̈moud

Barr

et al. 2018

New Astronomy Reviews

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Anomalous Microwave Emission (AME) is a component of diffuse Galactic radiation observed at frequencies in the range ≈ 10-60 GHz. AME was first detected in 1996 and recognised as an additional component of emission in 1997. Since then, AME has been observed by a range of experiments and in a variety of environments. AME is spatially correlated with far-IR thermal dust emission but cannot be explained by synchrotron or free-free emission mechanisms, and is far in excess of the emission contributed by thermal dust emission with the power-law opacity consistent with the observed emission at sub-mm wavelengths. Polarization observations have shown that AME is very weakly polarized ( 1 %). The most natural explanation for AME is rotational emission from ultra-small dust grains ("spinning dust"), first postulated in 1957.

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“…L1551-IRS 5 (Class 1). The close-by YSO L1551 is a Class 1 source with a core binary system in the Taurus molecular cloud complex (Osorio et al 2003;Lee et al 2014;Ainsworth et al 2016). Because of its proximity, luminosity, and accessibility for the IRAM 30m telescope, this source was considered to be a good candidate for our purposes.…”

Section: Astronomical Sourcesmentioning

confidence: 99%

Deep search for hydrogen peroxide toward pre- and protostellar objects

Fuchs

Witsch

Herberth

et al. 2020

A&A

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Context. In the laboratory, hydrogen peroxide (HOOH) was proven to be an intermediate product in the solid-state reaction scheme that leads to the formation of water on icy dust grains. When HOOH desorbs from the icy grains, it can be detected in the gas phase. In combination with water detections, it may provide additional information on the water reaction network. Hydrogen peroxide has previously been found toward ρ Oph A. However, further searches for this molecule in other sources failed. Hydrogen peroxide plays a fundamental role in the understanding of solid-state water formation and the overall water reservoir in young stellar objects (YSOs). Without further HOOH detections, it is difficult to assess and develop suitable chemical models that properly take into account the formation of water on icy surfaces. Aims. The objective of this work is to identify HOOH in YSOs and thereby constrain the grain surface water formation hypothesis. Methods. Using an astrochemical model based on previous work in combination with a physical model of YSOs, the sources R CrA-IRS 5A, NGCC1333-IRAS 2A, L1551-IRS 5, and L1544 were identified as suitable candidates for an HOOH detection. Long integration times on the APEX 12m and IRAM 30m telescopes were applied to search for HOOH signatures in these sources. Results. None of the four sources under investigation showed convincing spectral signatures of HOOH. The upper limit for HOOH abundance based on the noise level at the frequency positions of this molecule for the source R CrA-IRS 5A was close to the predicted value. For NGC1333-IRAS 2A, L1544, and L1551-IRS 5, the model overestimated the hydrogen peroxide abundances. Conclusions. HOOH remains an elusive molecule. With only one secure cosmic HOOH source detected so far, namely ρ Oph A, the chemical model parameters for this molecule cannot be sufficiently well determined or confirmed in existing models. Possible reasons for the nondetections of HOOH are discussed.

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A GMRT survey of regions towards the Taurus molecular cloud at 323 and 608 MHz

Cited by 5 publications

References 37 publications

JVLA Observations of Young Brown Dwarfs

JVLA Observations of Young Brown Dwarfs

The State-of-Play of Anomalous Microwave Emission (AME) research

Deep search for hydrogen peroxide toward pre- and protostellar objects

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