VLA cm-wave survey of young stellar objects in the Oph A cluster: constraining extreme UV- and X-ray-driven disk photoevaporation: A pathfinder for Square Kilometre Array studies
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VLA cm-wave survey of young stellar objects in the Oph A cluster : constraining extreme UV- and X-ray-driven disk photoevaporation: A pathfinder for Square Kilometre Array studies. / Coutens, A.; Liu, H. B.; Jiménez-Serra, I.; Bourke, T. L.; Forbrich, J.; Hoare, M.; Loinard, L.; Testi, L.; Audard, M.; Caselli, P.; Chacón-Tanarro, A.; Codella, C.; Di Francesco, J.; Fontani, F.; Hogerheijde, M.; Johansen, A.; Johnstone, D.; Maddison, S.; Panić, O.; Pérez, L. M.; Podio, L.; Punanova, A.; Rawlings, J. M.C.; Semenov, D.; Tazzari, M.; Tobin, J. J.; van der Wiel, M. H. D.; Van Langevelde, H. J.; Vlemmings, W.; Walsh, C.; Wilner, D.
In: Astronomy and Astrophysics, Vol. 631, A58, 2019.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - VLA cm-wave survey of young stellar objects in the Oph A cluster
T2 - constraining extreme UV- and X-ray-driven disk photoevaporation: A pathfinder for Square Kilometre Array studies
AU - Coutens, A.
AU - Liu, H. B.
AU - Jiménez-Serra, I.
AU - Bourke, T. L.
AU - Forbrich, J.
AU - Hoare, M.
AU - Loinard, L.
AU - Testi, L.
AU - Audard, M.
AU - Caselli, P.
AU - Chacón-Tanarro, A.
AU - Codella, C.
AU - Di Francesco, J.
AU - Fontani, F.
AU - Hogerheijde, M.
AU - Johansen, A.
AU - Johnstone, D.
AU - Maddison, S.
AU - Panić, O.
AU - Pérez, L. M.
AU - Podio, L.
AU - Punanova, A.
AU - Rawlings, J. M.C.
AU - Semenov, D.
AU - Tazzari, M.
AU - Tobin, J. J.
AU - van der Wiel, M. H. D.
AU - Van Langevelde, H. J.
AU - Vlemmings, W.
AU - Walsh, C.
AU - Wilner, D.
N1 - Publisher Copyright: © A. Coutens et al..
PY - 2019
Y1 - 2019
N2 - Observations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ∼ 0.′′4 × 0.′′2. We achieved a 5 μJy beam-1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free-free emission from thermal jets, free-free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation.
AB - Observations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ∼ 0.′′4 × 0.′′2. We achieved a 5 μJy beam-1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free-free emission from thermal jets, free-free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation.
KW - Protoplanetary disks
KW - Radio continuum: stars
KW - Stars: activity
KW - Stars: formation
U2 - 10.1051/0004-6361/201935340
DO - 10.1051/0004-6361/201935340
M3 - Journal article
AN - SCOPUS:85074453310
VL - 631
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - A58
ER -
ID: 327055078