J/A+A/689/A185 JWST/MIRI HR 2562 B images (Godoy+, 2024)
A new atmospheric characterization of the sub-stellar companion HR 2562 B with
JWST/MIRI observations.
Godoy N., Choquet E., Serabyn E., Danielski C., Stolker T., Charnay B.,
Hinkley S., Lagage P.O., Ressler M.E., Tremblin P., Vigan A.
<Astron. Astrophys. 689, A185 (2024)>
=2024A&A...689A.185G 2024A&A...689A.185G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Photometry, infrared
Keywords: instrumentation: high angular resolution - methods: data analysis -
techniques: image processing - planets and satellites: atmospheres -
infrared: planetary systems
Abstract:
HR 2562 B is a planetary-mass companion at an angular separation of
0.56arcsec (19au) from the host star, which is also a member of a
select number of L/T transitional objects orbiting a young star. This
companion gives us a great opportunity to contextualize and understand
the evolution of young objects in the L/T transition. However, the
main physical properties (e.g., Teff and mass) of this companion have
not been well constrained (34% uncertainties on Teff , 22% uncertainty
for log(g)) using only near-infrared (NIR) observations.
We aim to narrow down some of its physical parameters uncertainties
(e.g., Teff : 1200K-1700K, log(g): 4-5) incorporating new observations
in the Rayleigh-Jeans tail with the JWST/MIRI filters at 10.65, 11.40,
and 15.50um, as well as to understand its context in terms of the
L/T transition and chemical composition.
We processed the MIRI observations with reference star differential
imaging (RDI) and detect the companion at high S/N (around 16) in the
three filters, allowing us to measure its flux and astrometry. We used
two atmospheric models, ATMO and Exo-REM, to fit the spectral energy
distribution using different combinations of mid-IR and near-IR
datasets. We also studied the color-magnitude diagram using the F1065C
and F1140C filters combined with field brown dwarfs to investigate the
chemical composition in the atmosphere of HR 2562 B, as well as a
qualitative comparison with the younger L/T transitional companion VHS
1256 b.
We improved the precision on the temperature of HR 2562 B (Teff=1255K)
by a factor of 6x compared to previous estimates (±15K vs ±100K)
using ATMO. The precision of its luminosity was also narrowed down to
∼4.69±0.01dex. The surface gravity still presents a wider range of
values (4.4 to 4.8dex). While its mass was not narrowed down, we find
the most probable values between 8MJup (3σ lower limit from
our atmospheric modeling) and 18.5MJup (from the upper limit provided
by astrometric studies). We report a sensitivity to objects of mass
ranging between 2-5MJup at 100au, reaching the lower limit at
F1550C. We also implemented a few improvements in the pipeline related
to the background subtraction and stages 1 and 2.
HR 2562 B has a mostly (or near) cloud-free atmosphere, with the ATMO
model demonstrating a better fit to the observations. From the
color-magnitude diagram, the most probable chemical species at MIR
wavelengths are silicates (but with a weak absorption feature);
however, follow-up spectroscopic observations are necessary to either
confirm or reject this finding. The mass of HR 2562 B could be better
constrained with new observations at 3-4um. Although HR 2562 B
and VHS 1256 b have very similar physical properties, both are in
different evolutionary states in the L/T transition, which makes HR
2562 B an excellent candidate to complement our knowledge of young
objects in this transition. Considering the actual range of possible
masses, HR 2562 B could be considered as a planetary-mass companion;
hence, its name then ought to be rephrased as HR 2562 b.
Description:
These data corresponds to several datasets used in some figures of the
paper.
I) The magnitudes of the Ultracool dwarfs observed with the Spitzer
infrared spectrograph (Suarez and Metchev, 2022MNRAS.513.5701S 2022MNRAS.513.5701S, Cat.
J/MNRAS/513/5701).
II) The magnitudes for HR2562b and VHS1256b in MIRI/coro filters. The
VHS1256b magnitudes were calculated from the MIRI/MRS spectrum (Miles
et al. 2023ApJ...946L...6M 2023ApJ...946L...6M).
III) Contrast curves of HR2562 observations in F1065C, F1140C, and
F1550C.
IV) FITS files with the post- processed observations.
Objects:
----------------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------------
06 50 01.01 -60 14 56.9 HR2562 = HD 50571
12 56 01.83 -12 57 27.6 VHS1256 = NAME VHS J1256-1257B
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
cmd.dat 424 113 Color-magnitude diagram data
table.dat 324 2 HR2562b and VHS1256b data
cf1065c.dat 128 477 HR2562 contrast - F1065C
cf1140c.dat 128 457 HR2562 contrast - F1140C
cf1550c.dat 128 457 HR2562 contrast - F1550C
list.dat 145 3 List of fits datacubes
fits/* . 3 Individual fits datacubes
--------------------------------------------------------------------------------
See also:
J/MNRAS/513/5701 : Silicate clouds in ultracool dwarfs (Suarez+, 2022)
Byte-by-byte Description of file: cmd.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Target name
25- 33 A9 --- OName ID from Suarez and Metchev,
2022MNRAS.513.5701S 2022MNRAS.513.5701S, Cat. J/MNRAS/513/5701
35- 42 F8.4 deg RAdeg Right Ascension (J2000)
44- 51 F8.4 deg DEdeg Declination (J2000)
53- 73 F21.16 pc Dist ?=-100.0 Target distance
75- 98 F24.19 pc e_Dist ?=-100.0 Target distance uncertainty
100-106 A7 --- SpType1 ? Spectral type (1)
108-114 A7 --- SpType2 ? Secondary Spectral type classification (1)
116-120 F5.2 --- Water ? Water spectral index (1)
122-126 F5.2 --- e_Water ? Wather spectral index uncertainty
128-131 F4.2 --- Methane Methane spectral index (1)
133-136 F4.2 --- e_Methane Methane spectral index uncertainty
138-141 F4.2 --- Ammonia Ammonia spectral index (1)
143-146 F4.2 --- e_Ammonia Ammonia spectral index uncertainty
148-152 F5.2 --- Silicates ? Silicates spectral index (1)
154-158 F5.2 --- e_Silicates ? Silicates spectral index uncertainty
160-177 F18.15 mag F1065Cmag MIRI.F1065C (10.65um) apparent magnitude (2)
179-199 F21.19 mag e_F1065Cmag MIRI.F1065C apparent magnitude uncertainty (2)
201-219 F19.16 mag F1140Cmag MIRI.F1140C (11.40um) apparent magnitude (2)
221-241 F21.19 mag e_F1140Cmag MIRI.F1140C apparent magnitude uncertainty (2)
243-262 F20.16 mag F1550Cmag ? MIRI.F1550C (15.50um) apparent magnitude (2)
264-284 F21.18 mag e_F1550Cmag ? MIRI.F1550C apparent magnitude
uncertainty (2)
286-305 F20.16 mag F1065CMAG ? MIRI.F1065C (10.65um) absolute magnitude (2)
307-327 F21.19 mag e_F1065CMAG MIRI.F1065C absolute magnitude uncertainty (2)
329-347 F19.15 mag F1140CMAG ? MIRI.F1140C (11.40um) absolute magnitude (2)
349-369 F21.19 mag e_F1140CMAG MIRI.F1140C absolute magnitude uncertainty (2)
371-389 F19.15 mag F1550CMAG ? MIRI.F1550C (15.50um) absolute magnitude (2)
391-411 F21.18 mag e_F1550CMAG ? MIRI.F1550C absolute magnitude
uncertainty (2)
413 A1 --- SpType Spectral type adopted in this study
415-424 A10 --- Color Color used to plot Fig. 14 and E.1 -
sub-class color markers (3)
--------------------------------------------------------------------------------
Note (1): from Suarez and Metchev, 2022MNRAS.513.5701S 2022MNRAS.513.5701S, Cat. J/MNRAS/513/5701
Note (2): calculated from Spizer spectrum (Suarez and Metchev,
2022MNRAS.513.5701S 2022MNRAS.513.5701S, Cat. J/MNRAS/513/5701.
Note (3): Code as follows:
orange = M0-M4
red = M5-M9
lime = L0-L4
lightcoral = L5-L9
green = T0-T4
moccasin = T5-T9
black = unclassified
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Target name
10- 26 F17.13 deg RAdeg Right Ascension (J2000)
28- 44 F17.13 deg DEdeg Declination (J2000)
46- 63 F18.15 pc Dist Target distance
65- 82 F18.16 pc e_Dist Target distance uncertainty
84-101 F18.15 mag F1065Cmag MIRI.F1065C (10.65um) apparent magnitude
103-121 F19.17 mag e_F1065Cmag MIRI.F1065C apparent magnitude uncertainty
123-139 F17.14 mag F1140Cmag MIRI.F1140C (11.40um) apparent magnitude
141-160 F20.18 mag e_F1140Cmag MIRI.F1140C apparent magnitude uncertainty
162-182 E21.16 mag F1550Cmag MIRI.F1550C (15.50um) apparent magnitude
184-205 E22.17 mag e_F1550Cmag MIRI.F1550C apparent magnitude uncertainty
207-224 F18.15 mag F1065CMAG MIRI.F1065C (10.65um) absolute magnitude
226-244 F19.17 mag e_F1065CMAG MIRI.F1065C absolute magnitude uncertainty
246-263 F18.15 mag F1140CMAG MIRI.F1140C (11.40um) absolute magnitude
265-283 F19.17 mag e_F1140CMAG MIRI.F1140C absolute magnitude uncertainty
285-304 F20.16 mag F1550CMAG MIRI.F1550C (15.50um) absolute magnitude
306-324 F19.17 mag e_F1550CMAG MIRI.F1550C absolute magnitude uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: cf1065c.dat cf1140c.dat cf1550c.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 F20.17 pix Sep-pix Angular separation in pixels
22- 41 F20.18 arcsec Sep-arcsec Angular separation in arcsec
using 0.11arcsec/pixel
43- 64 E22.17 --- contrast 5-sigma contrast computed using
spaceKLIP
66- 86 F21.18 mag contrast-mag 5-sigma contrast in magnitude
88-109 E22.17 --- smoothed-contrast De-noised contrast curve
111-128 F18.15 mag smoothed-contrast-mag De-noised contrast curve
in magnitude
--------------------------------------------------------------------------------
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- 29 I2 --- Nz Number of pixels along Z-axis
31- 34 I4 Kibyte size Size of FITS file
36-111 A76 --- FileName Name of FITS file, in subdirectory fits
113-145 A33 --- Title Title of the FITS file
--------------------------------------------------------------------------------
History:
From Nicolas Godoy, nicolas.godoy(at)lam.fr `
Acknowledgements:
We thank B. Miles et al. for providing the VHS 1256 b spectrum and B.
Miles for the discussions about chemistry on VHS 1256 b relative to HR
2562 B. We thank A. Carter and Y. Zhou for providing the photometric
data of the population of low-mass stars, brown dwarfs, and direct
imaged planets/planetary-mass companions. We thank the authors
Konopacky et al., Mesa et al., and Sutlieff et al. for providing
and/or publishing the observational data used in this study. This
project is funded/Co-funded by the European Union (ERC, ESCAPE,
project No 101044152). Views and opinions expressed are however those
of the author(s) only and do not necessarily reflect those of the
European Union or the European Research Council Executive Agency.
Neither the European Union nor the granting authority can be held
responsible for them. Part of this work was carried out at the Jet
Propulsion Laboratory, California Insitute of Technology, under
contract with NASA (80NM00018D0004). C.D. acknowledges financial
support from the INAF initiative 'IAF Astronomy Fellowships in
Italy', grant name GExoLife. This work is based on observations made
with the NASA/ESA/CSA James Webb Space Telescope. The data were
obtained from the Mikulski Archive for Space Telescopes at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-03127 for JWST. These observations are associated with program
#1241. This work has made use of data from the European Space Agency
(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the
Gaia Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the
DPAC has been provided by national institutions, in particular, the
institutions participating in the Gaia Multilateral Agreement. This
research has made use of the Spanish Virtual Observatory
(https://svo.cab.inta-csic.es) project funded by
MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00.
This publication makes use of VOSA, developed under the Spanish
Virtual Observatory (https://svo.cab.inta-csic.es) project funded by
MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00.
VOSA has been partially updated by using funding from the European
Union's Horizon 2020 Research and Innovation Programme, under Grant
Agreement no 776403 (EXOPLANETS-A). This publication makes use of data
products from the Two Micron All Sky Survey, which is a joint project
of the University of Massachusetts and the Infrared Processing and
Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation. This publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aero-nautics and Space Administration. This work has made use of data
from the European Space Agency (ESA) mission Gaia
(https://www.cosmos.esa.int/gaia), processed by the Gaia Data
Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the
DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement. This
work has benefitted from The UltracoolSheet, maintained by Will Best,
Trent Dupuy, Michael Liu, Rob Siverd, and Zhoujian Zhang, and
developed from compilations by Dupuy & Liu (2012, ApJS, 201, 19),
Dupuy & Kraus (2013, Science, 341, 1492), Liu et al. (2016, ApJ, 833,
96), Best et al. (2018, ApJS, 234, 1), and Best et al. (2020b, AJ, in
press). This research has made use of the Washington Double Star
Catalog maintained at the U.S. Naval Observatory.
(End) Patricia Vannier [CDS] 28-Oct-2024