12/30/2023 0 Comments Spectra twoUsing the parallax and proper motion determined in Kirkpatrick et al. Additionally, the spectrum exhibits the characteristic triangular shape in the H-band often seen in VL-G dwarfs, further confirming the classification of W0755−3259 as L7 VL-G. Another gravity index is the K-band H 2( K) index described in Canty et al. The H-cont index for W0755−3259 is 1.00 ± 0.04, a value expected for VL-G dwarfs with H-cont ≈ 1. For L7 and later, one of the few accurate methods is measuring the H-cont index of the blue side of the H-band, as discussed in Allers & Liu ( 2013). 2016) (see Figure 1), so we assign a classification of L7 VL-G even though the K-band of W0755−3259 is still redder.ĭetermining the gravity type of these objects through non-visual means is challenging, as many methods of gravity classification are designed for dwarfs with spectral types earlier than L7 (e.g., Allers & Liu 2013 Cruz et al. When comparing to INT-G and VL-G dwarf spectra in the SPLAT library (Burgasser & the SPLAT Development Team 2017), a close visual correlation was found between the J- band and H-band of W0755−3259 and the L7 VL-G dwarf WISEA J114724.10-204021.3 (Schneider et al. All spectra are normalized between 1.27 and 1.29 μm.(The data used to create this figure are available.) Bottom panel: The full resolution near-infrared spectrum of W1659−3511 (gray) and smoothed (black) compared to the L7 near-infrared spectral standard 2MASSI J0825196+211552 (Kirkpatrick et al. 3. Analysis of W0755-3259 Spectrumįigure 1. Top panel: The full resolution near-infrared spectrum of W0755−3259 (gray) and smoothed (black) compared to the L5 near-infrared spectral standard SDSS J083506.16+195304.4 (Chiu et al. W0755−3259 is a previously known source discovered in Scholz & Bell ( 2018), but its spectrum has not yet been analyzed and the parallax for this source has not yet been used to investigate moving group membership. 2004) using A0 stars taken just after the target. Spectral extractions and telluric corrections were performed with a modified version of the SpeXtool package (Vacca et al. 180 s exposures were taken at different nod positions, with 16 nods obtained for W0755−3259 and 20 nods obtained for W1659−3511. ![]() Using a slit width of 1 1, Triplespec4 returns simultaneous spectra across six cross-dispersed orders covering the 0.8–2.4 μm range with a resolving power of ∼3500. Observations were taken in queue mode on 2023 April 17 (UT) and 2023 April 29 (UT), respectively. 2020) located at the 4.1 m Southern Astrophysical Research (SOAR) telescope. Near-infrared spectra of W0755−3259 and W1659−3511 were obtained using the TripleSpec4 near-infrared spectrograph (Schlawin et al. School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK Planétarium Rio Tinto Alcan, 4801 Pierre-de Coubertin Ave, Montreal, Quebec H1V 3V4, Canada California Blvd., Pasadena, CA 91125, USAĭepartment of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, NY 10024, USAĬenter for Astrophysics and Space Science, University of California San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USAĮxoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA IPAC, Mail Code 100-22, California Institute of Technology, 1200 E. United States Naval Observatory, Flagstaff Station, 10391 West Naval Observatory Rd., Flagstaff, AZ 86005, USA ![]() NSF's National Optical-Infrared Astronomy Research Laboratory, 950 N. Department of Astronomy, University of Florida, 201 Criser Hall, Gainesville, FL 32611, USA
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