J/A+A/658/A63 DR Tau VLT/SPHERE and LBTI/LMIRCam maps (Mesa+, 2022)
Signs of late infall and possible planet formation around DR Tau using
VLT/SPHERE and LBTI/LMIRCam.
Mesa D., Ginski C., Gratton R., Ertel S., Wagner K., Bonavita M., Fedele D.,
Meyer M., Henning T., Langlois M., Garufi A., Antoniucci S., Claudi R.,
Defrere D., Desidera S., Janson M., Pawellek N., Rigliaco E.,
Squicciarini V., Zurlo A., Boccaletti A., Bonnefoy M., Cantalloube F.,
Chauvin G., Feldt M., Hagelberg J., Hugot E., Lagrange A.-M., Lazzoni C.,
Maurel D., Perrot C., Petit C., Rouan D., Vigan A.
<Astron. Astrophys. 658, A63 (2022)>
=2022A&A...658A..63M 2022A&A...658A..63M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, variable ; Polarization ;
Infrared sources
Keywords: instrumentation: adaptive optics - methods: data analysis -
techniques: imaging spectroscopy - planetary systems -
stars: individual: DR Tau
Abstract:
Protoplanetary disks around young stars often contain substructures
like rings, gaps, and spirals that could be caused by interactions
between the disk and forming planets.
We aim to study the young (1-3Myr) star DR Tau in the near-infrared
and characterize its disk, which was previously resolved through
sub-millimeter interferometry with ALMA, and to search for possible
sub-stellar companions embedded into it.
We observed DR Tau with VLT/SPHERE both in polarized light (H broad
band) and total intensity (in Y, J, H, and K spectral bands). We also
performed L' band observations with LBTI/LMIRCam on the Large
Binocular Telescope (LBT). We applied differential imaging techniques
to analyze the polarized data, using dual beam polarization imaging
(DPI), and total intensity data, using both angular and spectral
differential imaging (ADI, SDI).
We found two previously undetected spirals extending north-east and
south of the star, respectively. We further detected an arc-like
structure north of the star. Finally a bright, compact and elongated
structure was detected at separation of 303±10 mas and position
angle 21.2±3.7 degrees, just at the root of the north-east spiral
arm. Since this feature is visible both in polarized light and in
total intensity and has a flat spectrum it is likely caused by stellar
light scattered by dust.
The two spiral arms are at different separation from the star, have
very different pitch angles, and are separated by an apparent
discontinuity, suggesting they might have a different origin. The very
open southern spiral arm might be caused by infalling material from
late encounters with cloudlets into the formation environment of the
star itself. The compact feature could be caused by interaction with a
planet in formation still embedded in its dust envelope and it could
be responsible for launching the north-east spiral. We estimate a mass
of the putative embedded object of the order of few M Jup .
Description:
In the first epoch, during the night of 26 November 2018, SPHERE was
operating in dual beam polarization imaging (DPI) using the IRDIS
infrared camera in the broad-band H filter (λ=1.625um,
{DELTA}λ=0.29um).
VDRTau2018-11-26Q_phi.fits : Fits file with IRDIS polarized data
from 2018-11-26 (used for Fig. 1, 4 and 5 in the paper)
The second epoch observation of DR Tau with SPHERE was performed on
the night of 28 November 2019 in the context of the SHINE (SpHere
INfrared survey for Exoplanets) survey. The observation was performed
using the IRDIFS_EXT observing mode with the integral field
spectrograph (IFS) operating in Y, J, and H spectral bands (between
0.95 and 1.65um) and with IRDIS using the K band with the K12 filter
pair (wavelength K1=2.110um; wavelength K2=2.251um).
DRTausnrmapmodi10allevol.fits : Fits file with IFS total intensity
data from 2019-11-28 (used for Fig. 2 in the paper)
DRTausnrmapmodi2_all.fits : Fits file with IRDIS total intensity
data from 2019-11-28 (used for Fig. 2 in the paper)
We also observed DR Tau in the L' band with LBTI/LMIRCam using the
instrument's non-interferometric, individual-aperture,
adaptive-optics imaging mode (Ertel et al. 2020). These observations
were executed on the night of 3 March 2020 using only the left side of
the LBTI and the Annular Groove Phase Mask (AGPM) coronagraph.
DRTausnrmapmodi10all.fits : Fits file with LBTI/LMIRCam data from
2020-02-03 (used for Fig. 3 in the paper)
Objects:
-------------------------------------------------------
RA (2000) DE Designation(s)
-------------------------------------------------------
04 47 06.22 +16 58 42.8 DR Tau = TYC 1271-1233-1
-------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 148 4 List of fits files
fits/* . 4 Individual fits files
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Simbad right ascension (J2000)
4- 5 I2 min RAm Simbad right ascension (J2000)
7- 11 F5.2 s RAs Simbad right ascension (J2000)
12 A1 --- DE- Simbad declination sign (J2000)
13- 14 I2 deg DEd Simbad declination (J2000)
16- 17 I2 arcmin DEm Simbad declination (J2000)
19- 22 F4.1 arcsec DEs Simbad declination (J2000)
24- 27 I4 --- Nx Number of pixels along X-axis
29- 32 I4 --- Ny Number of pixels along Y-axis
34- 37 I4 Kibyte size Size of FITS file
39- 71 A33 --- FileName Name of FITS file, in subdirectory fits
73-148 A76 --- Title Title of the FITS file
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Acknowledgements:
Dino Mesa, dino.mesa(at)inaf.it
(End) Patricia Vannier [CDS] 13-Nov-2021