2025A&A...701A..51P


Query : 2025A&A...701A..51P

2025A&A...701A..51P - Astronomy and Astrophysics, volume 701A51 (2025/9-1)

The planetary-mass-limit VLT/SINFONI library Spectral extraction and atmospheric characterization via forward modeling.

PALMA-BIFANI P., BONNEFOY M., CHAUVIN G., ROJO P., BAUDOZ P., CHARNAY B., DENIS A., HOCH K., PETRUS S., RAVET M., SIMONNIN A. and VIGAN A.

Abstract (from CDS):

Context. Access to medium-resolution spectra (Rλ ∼ 1000 - 10 000) at near-infrared wavelengths of young M-L objects allows us to study their atmospheric properties. Specifically, this approach can unveil a rich set of molecular features related to the atmospheric chemistry and physics.
Aims. We aim to deepen our understanding of the M-L transition on planetary-mass companions and isolated brown dwarfs, while searching for evidence of possible differences between these two populations of objects. To this end, we present a set of 21 VLT/SINFONI K-band (1.95-2.45 µm) observations from five archival programs at Rλ ∼ 4000. We aim to measure the atmospheric properties, such as Teff, log (ɡ), [M/H], and C/O, and to understand the similarities and differences between objects ranging in spectral type from M5 to L5.
Methods. We extracted the spectra of these targets with the TExTRIS code. We modeled them using ForMoSA, a Bayesian forward modeling tool for spectral analysis, and we explored four families of self-consistent atmospheric models: ATMO, BT-Settl, Exo-REM, and Sonora Diamondback.
Results. Here, we present the spectra of our targets and the derived parameters from the atmospheric modeling process. We confirm a drop in Teff as a function of the spectral type of more than 500 K at the M/L transition. In addition, we report C/O measurements for three companions, 2M 0103 AB b, AB Pic b, and CD-35 2722 b, thereby adding to the growing list of exoplanets with measured C/O ratios.
Conclusions. The VLT/SINFONI Library highlights two key points. First, there is a critical need to further investigate the discrepancies among grids of spectra generated by self-consistent models, as these models yield varying results and do not uniformly explore the parameter space. Second, we do not observe any obvious discrepancies in the K-band spectra between companions and isolated brown dwarfs, which suggests that these super-Jupiter objects might have formed through a similar process; however, this possibility warrants further investigation.

Abstract Copyright: © The Authors 2025

Journal keyword(s): planets and satellites: atmospheres - planets and satellites: composition - planets and satellites: formation - planets and satellites: gaseous planets - planets and satellites: general

VizieR on-line data: <Available at CDS (J/A+A/701/A51): list.dat fits/*>

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NAME THA MGr 00 00 -62.0           ~ 540 0
2 SCR J0103-5515C LM* 01 03 35.58 -55 15 54.6           ~ 64 0
3 SCR J0103-5515 SB* 01 03 35.655120 -55 15 56.24316   16.99 15.40 14.96 12.09 M4.5Ve 54 0
4 [BLH2002] KPNO-Tau 1 LM* 04 15 14.7215444352 +28 00 09.383811048     24.063     M8.5Ve 44 0
5 V* FU Tau B BD* 04 23 35.7463331664 +25 02 59.644831416       22.16 19.11 L0.3 49 0
6 [BLH2002] KPNO-Tau 4 BD* 04 27 27.9991044840 +26 12 05.085665388     24.722 20.54 18.75 L0 73 0
7 V* DH Tau Or* 04 29 41.5525353432 +26 32 58.126559604 15.14 14.62 13.10 13.01   M1Ve 323 0
8 V* DH Tau B LM* 04 29 41.66 +26 32 56.5           M9.25 105 1
9 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1453 0
10 [BLH2002] KPNO-Tau 6 LM* 04 30 07.2454086048 +26 08 20.709374568     22.292 20.56 17.90 M8.5Ve 65 0
11 [QGH2010] CAHA Tau 1 BD* 04 36 09.00 +24 08 21.2       22.89 20.00 L2 3 0
12 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
13 NAME AF Lep b Pl 05 27 04.7633281608 -11 54 03.466002240           ~ 75 0
14 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 627 1
15 CD-35 2722B BD* 06 09 19.2082646634 -35 49 31.062882043           L0-1 71 0
16 HD 44627 Er* 06 19 12.9130449912 -58 03 15.527294208   10.01 9.205   8.185 K1V(e) 207 1
17 NAME AB Dor Moving Group MGr 06 38 53.4 -42 50 04           ~ 540 0
18 TWA 27B BD* 12 07 33.50 -39 32 54.4           L3 321 0
19 SIPS J1256-1257B BD* 12 56 01.83264 -12 57 27.6912           L7 154 0
20 NAME TYC 8998-760-1 c Pl 13 25 12.1262905080 -64 56 20.688979668           ~ 30 0
21 NAME TYC 8998-760-1B LM* 13 25 12.33 -64 56 19.7           ~ 71 0
22 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 894 0
23 HD 143567B LM* 16 01 55.65696 -21 58 53.0076           M8 43 0
24 UScoCTIO 108 LM* 16 05 54.0734809368 -18 18 44.376318180           M7 51 0
25 2MASS J16060374-2219298 LM* 16 06 03.7646429328 -22 19 29.956749564           M12.00 23 0
26 2MASS J16060629-2335133 BD* 16 06 06.29400 -23 35 13.3656           L0 25 0
27 UScoCTIO 134 LM* 16 06 48.1814420832 -22 30 40.025477124           M8.00 20 0
28 2MASS J16072782-2239040 BD* 16 07 27.82416 -22 39 04.0644           L1 21 0
29 2MASS J16081843-2232248 BD* 16 08 18.43608 -22 32 24.8280           L0 25 0
30 2MASS J16083048-2335109 LM* 16 08 30.4965232728 -23 35 10.989080232           M9.00 31 0
31 2MASS J16104714-2239492 LM* 16 10 47.1390030984 -22 39 49.326872040           M9.00 28 0
32 NAME Upper Sco Association As* 16 12 -23.4           ~ 1586 1
33 2MASS J16122764-2156407 BD* 16 12 27.64512 -21 56 40.7148           L0 13 0
34 2MASS J16130232-2124283 BD* 16 13 02.32224 -21 24 28.3788           L0 19 0
35 * eta Tel B LM* 19 22 51.3580284238 -54 25 31.569876496           M7.5V 78 0
36 HD 218396e Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 255 1
37 HD 218396b Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 323 1
38 HD 218396d Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 286 1
39 HD 218396c Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 312 1
40 NAME Carina Moving Group MGr ~ ~           ~ 66 0

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