JVLA Observations of Young Brown Dwarfs

Rodríguez, Luis F.; Zapata, Luis A.; Palau, Aina

doi:10.3847/1538-3881/aa6681

Cited by 18 publications

(15 citation statements)

References 77 publications

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“…The proper motion direction is consistent with the orientation of the outburst nebula, the 12 CO blueshifted outflow (Feddersen et al 2020), and the position angle of the binary radio counterpart of HOPS 383 at 4 cm (Galván-Madrid et al 2015). We note that the unresolved 3 cm counterpart (Rodríguez et al 2017) corresponds to the faint northwest component at 4 cm, JVLA-NW, which suggests that JVLA-NW would be the base of the radio thermal jet launched by HOPS 383, whereas the brighter southeast component at 4 cm, JVLA-SE, would be an emission knot along this thermal jet (Fig. 1c).…”

Section: Near-infrared Resultssupporting

confidence: 88%

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Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

Grosso

Hamaguchi

Principe

et al. 2020

A&A

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Context. Class 0 protostars represent the earliest evolutionary stage of solar-type stars, during which the majority of the system mass resides in an infalling envelope of gas and dust and is not yet in the central, nascent star. Although X-rays are a key signature of magnetic activity in more evolved protostars and young stars, whether such magnetic activity is present at the Class 0 stage is still debated. Aims. We aim to detect a bona fide Class 0 protostar in X-rays. Methods. We observed HOPS 383 in 2017 December in X-rays with the Chandra X-ray Observatory (∼84 ks) and in near-infrared imaging with the Southern Astrophysical Research telescope. Results. HOPS 383 was detected in X-rays during a powerful flare. This hard (E > 2 keV) X-ray counterpart was spatially coincident with the northwest 4 cm component of HOPS 383, which would be the base of the radio thermal jet launched by HOPS 383. The flare duration was ∼3.3 h; at the peak, the X-ray luminosity reached ∼4 × 1031 erg s−1 in the 2−8 keV energy band, a level at least an order of magnitude larger than that of the undetected quiescent emission from HOPS 383. The X-ray flare spectrum is highly absorbed (NH ∼ 7 × 1023 cm−2), and it displays a 6.4 keV emission line with an equivalent width of ∼1.1 keV, arising from neutral or low-ionization iron. Conclusions. The detection of a powerful X-ray flare from HOPS 383 constitutes direct proof that magnetic activity can be present at the earliest formative stages of solar-type stars.

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Section: Near-infrared Resultssupporting

confidence: 88%

“…The blue pluses are radio sources (Galván-Madrid et al 2015;Rodríguez et al 2017). The blue and green arrows show the direction of the thermaljet candidate and the proper motion of the H 2 emission knot SMZ 1-2B, respectively.…”

Section: Observationsmentioning

confidence: 99%

Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

Grosso

Hamaguchi

Principe

et al. 2020

A&A

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“…The primary FU Tau A could be a low-mass star or a high-mass brown dwarf as its mass was estimated as ∼80 M Jup (Stelzer et al 2013). Multi-wavelength tracers ranging from X-ray, optical spectroscopy, to 3 cm free-free emission have indicated that FU Tau A is actively accreting and may also have outflows (Stelzer et al 2010(Stelzer et al , 2013Rodríguez et al 2017). The companion FU Tau b, 5.…”

Section: Targetsmentioning

confidence: 99%

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Bowler

Sheehan

et al. 2020

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Characterizing the physical properties and compositions of circumplanetary disks can provide important insights into the formation of giant planets and satellites. We report ALMA 0.88 mm (Band 7) continuum observations of six planetary-mass (10-20 M Jup ) companions: CT Cha b, 1RXS 1609 b, ROXs 12 b, ROXs 42B b, DH Tau b, and FU Tau b. No continuum sources are detected at the locations of the companions down to 3σ limits of 120-210 µJy. Given these non-detections, it is not clear whether disks around planetary-mass companions indeed follow the disk flux-host mass trend in the stellar regime. The faint radio brightness of these companion disks may result from a combination of fast radial drift and a lack of dust traps. Alternatively, as disks in binary systems are known to have significantly lower millimeter fluxes due to tidal interactions, these companion disks may instead follow the relationship of moderate-separation binary stars. This scenario can be tested with sensitive continuum imaging at rms levels of 10 µJy.

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“…The white contours show the 12 CO blueshifted outflow of HOPS 383 (Feddersen et al 2020). The blue pluses are radio sources (Galván-Madrid et al 2015;Rodríguez et al 2017). The blue and green arrows show the direction of the thermal-jet candidate and the proper motion of the H 2 emission knot SMZ 1-2B, respectively.…”

Section: Observationsmentioning

confidence: 99%

Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

Grosso,

Hamaguchi,

Principe

et al. 2020

Preprint

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Context. Class 0 protostars represent the earliest evolutionary stage of solar-type stars, during which the majority of the system mass resides in an infalling envelope of gas and dust and is not yet in the central, nascent star. Although X-rays are a key signature of magnetic activity in more evolved protostars and young stars, whether such magnetic activity is present at the Class 0 stage is still debated. Aims. We aim to detect a bona fide Class 0 protostar in X-rays. Methods. We observed HOPS 383 in 2017 December in X-rays with the Chandra X-ray Observatory (∼84 ks) and in near-infrared imaging with the Southern Astrophysical Research telescope. Results. HOPS 383 was detected in X-rays during a powerful flare. This hard (E > 2 keV) X-ray counterpart was spatially coincident with the northwest 4 cm component of HOPS 383, which would be the base of the radio thermal jet launched by HOPS 383. The flare duration was ∼3.3 h; at the peak, the X-ray luminosity reached ∼4 × 10 31 erg s −1 in the 2-8 keV energy band, a level at least an order of magnitude larger than that of the undetected quiescent emission from HOPS 383. The X-ray flare spectrum is highly absorbed (N H ∼ 7 × 10 23 cm −2 ), and it displays a 6.4 keV emission line with an equivalent width of ∼1.1 keV, arising from neutral or low-ionization iron. Conclusions. The detection of a powerful X-ray flare from HOPS 383 constitutes direct proof that magnetic activity can be present at the earliest formative stages of solar-type stars.

show abstract

JVLA Observations of Young Brown Dwarfs

Cited by 18 publications

References 77 publications

Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

ALMA 0.88 mm Survey of Disks around Planetary-mass Companions

Evidence for magnetic activity at starbirth: a powerful X-ray flare from the Class 0 protostar HOPS 383

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