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A&A 635, L1 (2020) https: //doi. org /10. 1051 /0004-6361 /201937309 c⃝ESO 2020Astronomy&Astrophysics LETTER TO THE EDITOR 2MASS J15491331-3539118: a new low-mass wide companion of the GQ Lup system⋆ J. M. Alcalá1, F. Z. Majidi2,3, S. Desidera3, A. Frasca4, C. F. Manara5, E. Rigliaco3, R. Gratton3, M. Bonnefoy6, E. Cov... |
A&A 635, L1 (2020) SHINE SPHERE-GTO targets (Chauvin et al. 2017) in the Gaia DR2, finding several tens of candidates. We focused on a few objects around stars of high specific interest due to the presence of planetary or BD companions and spatially resolved circum-stellar discs. GQ Lup, a ∼1M⊙(Alcalá et al. 2017; Mac Gr... |
J. M. Alcalá et al. : New companion to GQ Lup Table 1. Physical stellar parameters of 2MASS J15491331. Sp T AV Teff L⋆ R⋆ M⋆ (mag) (K) ( L⊙) ( R⊙) ( M⊙) M4±0. 5 1. 0±0. 5 3190±100 0. 004±0. 001 0. 21±0. 06 0. 15±0. 05 Table 2. Parameters derived from ROTFIT. Teff logg R⋆(†)L⋆(†)RVvsini (K) ( R⊙) ( L⊙) (km s-1) (km s-1) 3... |
A&A 635, L1 (2020) very small, and can be ruled out based on the statistical grounds presented in Appendix E. The inclination i=60. 2°of the circumprimary disc (Mac Gregor et al. 2017; Ansdell et al. 2018) and the edge-on geometry of the 2MASS J15491331 disc might in principle be an indication that the angular momentum... |
J. M. Alcalá et al. : New companion to GQ Lup Appendix A: Observational strategy and data processing The X-shooter science exposure of GQ Lup consisted in a two-cycle (A-B-B-A) nodding mode observation for a total on-source exposure of 1. 2 h using the 1′′. 0 slits; as part of the same observ-ing block, an additional s... |
A&A 635, L1 (2020) Fig. C. 1. Portion of the X-shooter spectrum of 2MASS J15491331 around the H αline. The He iλ6678 Å and the forbidden lines of [N ii] and [S ii] and the Li iλ6708 Å are labelled. wavelength [nm]2MASS J15491331 Fig. C. 2. Ultraviolet spectrum of 2MASS J15491331 in the region of the Balmer jump (red li... |
J. M. Alcalá et al. : New companion to GQ Lup dimension of the region emitting the observed [O i]. We find L∼0. 15 AU, and assuming a peak velocity of ∼1 km s-1, this translates into a typical timescale of τ∼0. 8 yr. The mass loss rate we obtain is therefore Mloss∼7. 0×10-12M⊙yr-1(at 152 pc, or Mloss∼8. 9×10-12M⊙yr-1at ... |
A&A 635, L1 (2020) candidates are expected to be Sco-Cen members or objects unre-lated to Lupus I. In fact, some of the selected candidates appear rather scattered on the µαcosδversusµδscatter plot in compar-ison with the previously known YSOs (see Fig. E. 2). It is also worth noting that the typical linear density of ... |
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