An ALMA Survey of Faint Disks in the Chamaeleon I Star-forming Region: Why Are 
Some Class II Disks so Faint?

Long, Feng; Herczeg, Gregory J.; Pascucci, Ilaria; Apai, Dániel; Henning, Thomas; Manara, Carlo F.; Mulders, Gijs D.; Szűcs, László.; Hendler, Nathanial P.

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Journal Article

An ALMA Survey of Faint Disks in the Chamaeleon I Star-forming Region: Why Are Some Class II Disks so Faint?

MPS-Authors

Long, Feng
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Herczeg, Gregory J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pascucci, Ilaria
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Apai, Dániel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Henning, Thomas
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Manara, Carlo F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mulders, Gijs D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Szűcs, László.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hendler, Nathanial P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2018ApJ...863...61L
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Citation

Long, F., Herczeg, G. J., Pascucci, I., Apai, D., Henning, T., Manara, C. F., et al. (2018). An ALMA Survey of Faint Disks in the Chamaeleon I Star-forming Region: Why Are Some Class II Disks so Faint? The Astrophysical Journal, 863.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CC76-1

Abstract

ALMA surveys of nearby star-forming regions have shown that the dust mass in the disk is correlated with the stellar mass, but with a large scatter. This scatter could indicate either different evolutionary paths of disks or different initial conditions within a single cluster. We present ALMA Cycle 3 follow-up observations for 14 Class II disks that were low signal-to-noise (S/N) detections or non-detections in our Cycle 2 survey of the ̃2 Myr old Chamaeleon I star-forming region. With five times better sensitivity, we detect millimeter dust continuum emission from six more sources and increase the detection rate to 94% (51/54) for Chamaeleon I disks around stars earlier than M3. The stellar-disk mass scaling relation reported in Pascucci et al. is confirmed with these updated measurements. Faint outliers in the F _mm-M _* plane include three non-detections (CHXR71, CHXR30A, and T54) with dust mass upper limits of 0.2 M _⊕ and three very faint disks (CHXR20, ISO91, and T51) with dust masses ̃0.5 M _⊕. By investigating the SED morphology, accretion property and stellar multiplicity, we suggest for the three millimeter non- detections that tidal interaction by a close companion (≲100 au) and internal photoevaporation may play a role in hastening the overall disk evolution. The presence of a disk around only the secondary star in a binary system may explain the observed stellar SEDs and low disk masses for some systems.