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GASPS—A Herschel Survey of Gas and Dust in Protoplanetary Disks: Summary and Initial Statistics

W. R. F. Dent, W. F. Thi, I. Kamp, J. P. Williams, F. Menard, S. Andrews, D. Ardila, G. Aresu, J.-C. Augereau, D. Barrado y Navascues, S. Brittain, A. Carmona, D. Ciardi, W. Danchi, J. Donaldson, G. Duchene, C. Eiroa, D. Fedele, C. Grady, I. de Gregorio-Molsalvo, C. Howard, N. Huélamo, A. Krivov, J. Lebreton, R. Liseau, C. Martin-Zaidi, G. Mathews, G. Meeus, I. Mendigutía, B. Montesinos, M. Morales-Calderon, A. Mora, H. Nomura, E. Pantin, I. Pascucci, N. Phillips, C. Pinte, L. Podio, S. K. Ramsay, B. Riaz, P. Riviere-Marichalar, A. Roberge, G. Sandell, E. Solano, I. Tilling, J. M. Torrelles, B. Vandenbusche, S. Vicente, G. J. White and P. Woitke
Publications of the Astronomical Society of the Pacific
Vol. 125, No. 927 (May 2013), pp. 477-505
DOI: 10.1086/670826
Stable URL: http://www.jstor.org/stable/10.1086/670826
Page Count: 29
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GASPS—A Herschel Survey of Gas and Dust in Protoplanetary Disks: Summary and Initial Statistics
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Abstract

ABSTRACT.We describe a large-scale far-infrared line and continuum survey of protoplanetary disk through to young debris disk systems carried out using the ACS instrument on the Herschel Space Observatory. This Open Time Key program, known as GASPS (Gas Survey of Protoplanetary Systems), targeted ∼250∼250 young stars in narrow wavelength regions covering the [OI] fine structure line at 63 μmμm the brightest far-infrared line in such objects. A subset of the brightest targets were also surveyed in [OI]145 μμm, [CII] at 157 μμm, as well as several transitions of H2OH2O and high-excitation CO lines at selected wavelengths between 78 and 180 μμm. Additionally, GASPS included continuum photometry at 70, 100 and 160 μμm, around the peak of the dust emission. The targets were SED Class II–III T Tauri stars and debris disks from seven nearby young associations, along with a comparable sample of isolated Herbig AeBe stars. The aim was to study the global gas and dust content in a wide sample of circumstellar disks, combining the results with models in a systematic way. In this overview paper we review the scientific aims, target selection and observing strategy of the program. We summarise some of the initial results, showing line identifications, listing the detections, and giving a first statistical study of line detectability. The [OI] line at 63 μμm was the brightest line seen in almost all objects, by a factor of ∼10∼10. Overall [OI]63 μμm detection rates were 49%, with 100% of HAeBe stars and 43% of T Tauri stars detected. A comparison with published disk dust masses (derived mainly from sub-mm continuum, assuming standard values of the mm mass opacity) shows a dust mass threshold for [OI]63 μμm detection of ∼10-5 M⊙∼10-5  M⊙. Normalising to a distance of 140 pc, 84% of objects with dust masses ≥10-5 M⊙≥10-5  M⊙ can be detected in this line in the present survey; 32% of those of mass 10-6–10-5 M⊙10-6–10-5  M⊙, and only a very small number of unusual objects with lower masses can be detected. This is consistent with models with a moderate UV excess and disk flaring. For a given disk mass, [OI] detectability is lower for MM stars compared with earlier spectral types. Both the continuum and line emission was, in most systems, spatially and spectrally unresolved and centred on the star, suggesting that emission in most cases was from the disk. Approximately 10 objects showed resolved emission, most likely from outflows. In the GASPS sample, [OI] detection rates in T Tauri associations in the 0.3–4 Myr age range were ∼50%∼50%. For each association in the 5–20 Myr age range, ∼2∼2 stars remain detectable in [OI]63 μμm, and no systems were detected in associations with age >20 Myr>20  Myr. Comparing with the total number of young stars in each association, and assuming a ISM-like gas/dust ratio, this indicates that ∼18%∼18% of stars retain a gas-rich disk of total mass ∼1 MJupiter∼1  MJupiter for 1–4 Myr, 1–7% keep such disks for 5–10 Myr, but none are detected beyond 10–20 Myr. The brightest [OI] objects from GASPS were also observed in [OI]145 μμm, [CII]157 μμm and CO J = 18 - 17J=18-17, with detection rates of 20–40%. Detection of the [CII] line was not correlated with disk mass, suggesting it arises more commonly from a compact remnant envelope.

Notes and References

This item contains 174 references.

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