Photometry of DQ Tau requested in support of multiwavelength observations
Abstract:
Update: The last set of JWST observations were scheduled for March 2, 2025. Please continue observations at the cadence of multiple observations per night through March. Original request: Dr. Agnes Kospal (Konkoly Observatory) writes: DQ Tau is being observed with the VLBA in the radio, JWST in the infrared, and Chandra in the X-ray. Four sets of observations are planned between now and March 4, 2025. We request optical photometric observations to monitor the brightness of DQ Tau in order to know its exact state of accretion during the VLBA, JWST, and Chandra observations.
Justification:
DQ Tau is a young binary system consisting of two equal-mass T Tauri stars surrounded by a circumbinary protoplanetary disk. The two stars orbit each other on an eccentric orbit with a period of 15.8 days. During periastron, the mass accretion from the disk onto the stars have a peak, causing the brightening of the system. Although the brightenings are periodic with P=15.8 days, not all events have the same light curve shape: the strength and duration of the brightenings change from orbit to orbit, thus the need for contemporaneous monitoring. DQ Tau with its periodically changing accretion rate offers a unique opportunity to study how the disks react to variable irradiation, such as changes in its physical (temperature, emitting area) and chemical (molecular abundances) properties. The results of this research project will have important implications on disk evolution and planet formation, as the disk provides the material necessary to form the solid cores of planets and their atmospheres as well.
Requested Data Types:
Photometry
Targets
| Name | Magnitude | Variability Type | Photometry Notes | Spectroscopy Notes |
|---|---|---|---|---|
| DQ Tau | 12.40 | CTTS/ROT+* |
Cadence: Custom Precision: 100 |
Not Requested |
Spectroscopy Lines:
No spectroscopy lines provided
Photometry Filters:
No photometry filters provided
Comparison Stars:
Finder charts with comparison stars may be created using the AAVSO Variable Star Plotter (https://apps.aavso.org/vsp).
Co-Authorship
Observers are eligible for co-authorship.
Additional Observer Input:
CCD photometry is requested. BVRI is preferred, with V given highest priority. Multiple observations per night would be good, ideally with a cadence of 5 minutes during .
Additional Submission Location:
Not provided
Notes:
No public notes