J/AJ/164/109 Gemini-LIGHTS protoplanetary disks (Rich+, 2022)
Gemini-LIGHTS: Herbig Ae/Be and massive T Tauri protoplanetary disks imaged
with Gemini Planet Imager.
Rich E.A., Monnier J.D., Aarnio A., Laws A.S.E., Setterholm B.R.,
Wilner D.J., Calvet N., Harries T., Miller C., Davies C.L., Adams F.C.,
Andrews S.M., Bae J., Espaillat C., Greenbaum A.Z., Hinkley S., Kraus S.,
Hartmann L., Isella A., McClure M., Oppenheimer R., Perez L.M., Zhu Z.
<Astron. J., 164, 109 (2022)>
=2022AJ....164..109R 2022AJ....164..109R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, emission ; Stars, pre-main sequence ;
Polarization ; Infrared
Keywords: Protoplanetary disks - Direct imaging - Exoplanets -
Herbig Ae/Be stars - Circumstellar dust
Abstract:
We present the complete sample of protoplanetary disks from the
Gemini- Large Imaging with the Gemini Planet Imager Herbig/T Tauri
Survey, which observed bright Herbig Ae/Be stars and T Tauri stars in
near-infrared polarized light to search for signatures of disk
evolution and ongoing planet formation. The 44 targets were chosen
based on their near- and mid-infrared colors, with roughly equal
numbers of transitional, pre-transitional, and full disks. Our
approach explicitly did not favor well-known, 'famous' disks or
those observed by the Atacama Large Millimeter/submillimeter Array,
resulting in a less-biased sample suitable to probe the major stages
of disk evolution during planet formation. Our optimized data
reduction allowed polarized flux as low as 0.002% of the stellar light
to be detected, and we report polarized scattered light around 80% of
our targets. We detected point-like companions for 47% of the targets,
including three brown dwarfs (two confirmed, one new), and a new
super-Jupiter-mass candidate around V1295 Aql. We searched for
correlations between the polarized flux and system parameters, finding
a few clear trends: the presence of a companion drastically reduces
the polarized flux levels, far-IR excess correlates with polarized
flux for nonbinary systems, and systems hosting disks with ring
structures have stellar masses <3M☉. Our sample also included
four hot, dusty "FS CMa" systems, and we detected large-scale
(>100au) scattered light around each, signs of extreme youth for these
enigmatic systems. Science-ready images are publicly available through
multiple distribution channels using a new FITS file standard that has
been jointly developed with members of the Very Large Telescope
Spectro-polarimetric High-contrast Exoplanet Research team.
Description:
We present the Gemini-LIGHTS survey, which observed 44 bright Herbig
Ae/Be stars and T Tauri stars with the GPI instrument at Gemini South.
We constructed our sample based on their near- and mid-infrared colors
selecting a number of transitional, pre-transitional, and full disks
in order to create an unbiased sample. Importantly, we did not select
against unequal mass binaries with moderate separations. Observations
of these 44 targets were taken in J and H bands utilizing
high-contrast polarized imagery. Our selection criteria facilitate an
unbiased approach to studying bright Herbig Ae/Be and T Tauri stars
that does not favor famous targets with large disks (>100au).
We define a standard FITS file for high-contrast polarization data.
This is motivated by large numbers of observations of protoplanetary
disks from multiple telescopes (e.g., GPI, SPHERE/IRDIS,
Subaru/HiCIAO, Subaru/CHARIS). A standard FITS file will allow for
better comparison of protoplanetary disk polarization imagery between
different studies and instruments. This FITS standard was created in
collaboration with Christian Ginski.
The data are held in a three-dimensional cube of 5*x*y, where x and y
are the pixel dimensions of the image, and 5 are the different image
types. The five different image types are I, Qphi, Uphi, Q, U, and
:LPI where I is the intensity image without stellar light
subtracted, Qphi, Uphi, Q, and U as defined above in Section 3,
and LPI, which is the linear polarized intensity or
(Q2+U2)1/2..
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table5.dat 51 71 Polarization flux and point-source detection
upper limits
table6.dat 93 34 Point sources detected in the Gemini-LIGHTS sample
list.dat 126 71 List of polarized light images
fits/* . 71 Individual polarized light images
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Target Primary central star name used in publication
13 A1 --- Band Band in either J or H band
15- 24 A10 "date" Epoch Date of observations (YYYYMMDD)
26 A1 --- l_Qphi/Fstar limit flag on Qphi/Fstar
27- 31 F5.2 --- Qphi/Fstar Ratio of summed Qphi divided by Flux
of the star
33- 36 F4.2 --- e_Qphi/Fstar ? Ratio of summed Qphi divided by Flux
of the star error
38- 45 E8.2 --- Pct5sig ? 5-sigma Contrast in which a point source
would have been detected
47- 51 F5.3 Msun MassPct5sig ? Lowest mass of a point source that would
have been detected at 5-sigma
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Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Target Primary central star name used in
publication
12 A1 --- Band Band in either J or H band
14- 23 A10 "date" Epoch Date of observations (YYYYMMDD)
25 I1 --- CompNumb Numbered point source in a given system
27- 31 F5.3 arcsec Sep Separation of point source and central star
33- 37 F5.3 arcsec e_Sep Separation uncertainty of point source and
central star
39- 45 F7.3 deg PA Position Angle of point source
47- 50 F4.2 deg e_PA Position Angle of point source uncertainty
52- 58 F7.3 --- Flux Estimated flux of point source
60- 65 F6.3 --- e_Flux Estimated flux uncertainty of point source
67- 71 A5 --- Sat [FALSE/TRUE ] if the point source is
saturated in images
73 A1 --- l_PMass Limit flag on PMass
74- 78 F5.3 Msun PMass Estimated Mass of point source
81- 85 F5.3 Msun e_PMass ? Estimated Mass lower uncertainty of point
source
88- 91 F4.2 Msun E_PMass ? Estimated Mass upper uncertainty of point
source
93 A1 --- f_PMass [*] * for any target with ages <0.5Myr that
are younger than the youngest model in
Baraffe et al. (2015A&A...577A..42B 2015A&A...577A..42B) or
Phillips et al. (2020A&A...637A..38P 2020A&A...637A..38P)
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Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28 I1 --- Nz Number of pixels along Z-axis
30- 39 A10 "date" Obs.date Observation date
41- 44 I4 Kibyte size Size of FITS file
46- 78 A33 --- FileName Name of FITS file, in subdirectory fits
80-126 A47 --- Title Title of the FITS file
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Acknowledgements:
Evan Rich, earich(at)umich.edu
(End) Patricia Vannier [CDS] 13-Dec-2022