DOI: 10.6084/m9.figshare.1230051
title: FITS spectra and CSV tables from “New low-mass members of the Octans stellar association..." (2015, MNRAS, 447, 1267)

description: The ZIP file contains reduced FITS spectra of 134 Octans association candidates and KM-type radial velocity standards observed in the paper (Murphy & Lawson, 2015, MNRAS, 447, 1267). The stars were observed between 2014 January and September with the Wide Field Spectrograph (WiFeS) on the Australian National University 2.3-m Telescope at Siding Spring Observatory. The spectra cover 5350-7100AA at a resolution of R~7000. They are not flux calibrated or telluric corrected. More information on the observing and reduction procedures used can be found in the FITS headers and the published journal article. <em>Notes for Table 1:</em> Results of the ANU 2.3-m/WiFeS spectroscopy for the 57 Octans candidates lying above the Pleiades isochrone in Fig.2. Candidates 5, 6, 7 and 10 were not observed. Ks magnitudes for all candidates are taken from 2MASS, with V magnitudes and proper motions from SPM4, except for candidates 3, 4, 12, 43AB, 47 (V from UCAC4), 61 (proper motion and V from UCAC4), 31 (proper motion from UCAC4), 25 and 42 (proper motions from Hipparcos). Candidates 18, 32 and 43 were marginally resolved as close doubles in the WiFeS field of view, but are unresolved in all-sky surveys. Spectroscopic binaries and the nine candidates with broader CCFs are indicated in the final column. <em>Notes for Table 2:</em> Octans members proposed in the literature. V magnitudes and proper motions are from SPM4, except for CD−30 3394AB (both from UCAC4), CD−72 248, (V from UCAC4), TYC 7066-1037-1 (V from UCAC4, proper motion from Tycho-2), TYC 9300-0529-1 and TYC 9300-0891-1 (proper motions from PPMXL). Membership and radial velocity references: T03: Torres et al. (2003b), T06: Torres et al. (2006), T08: Torres et al. (2008), M11: Moo ́r et al. (2011), M13: Murphy et al. (2013), E14: Elliott et al. (2014), CT: C. Torres (private communication). Li I 6708 equivalent widths are taken from Torres et al. (2006), except for RX J1123.2−7924 (M13) and BD−20 1111 (CT). The T08 members CD−72 248 and CD−66 395 are fast rotators (vsini = 190 km/s) with assumed large velocity errors. <em>Notes for Table 3:</em> Octans members selected by the kinematic analysis in Section 5.1. Kinematic distances (d_kin), heliocentric velocities (U, V, W) and positions (X, Y, Z) were computed from the mean space motion (−13.7, −4.8, −10.9 km/s) and the proper motions and radial velocities in Tables 1 and 2. Also listed are the space motion (Delta_v), radial velocity (Delta_RV) and total proper motion (Delta_mu) residuals. All stars selected as kinematic members satisfy Delta_v &lt; 5 km/s. <em>Notes for Table 4:</em> Possible Octans members not included in the final membership solution. The absolute magnitude given for the components of #32AB assumes an equal-mass system with combined brightness M_V = 5.77 mag. Notes for last column: (Delta_v): Rejected as kinematic member with Delta_v &gt; 5 km/s, (Halpha): Halpha in absorption but otherwise acceptable kinematic member, (Li): Lithium-rich star with EW_Li &gt; 100 mA. <em>Notes for Table 5:</em> Candidates with ROSAT counterparts lying on or above the RASS limit in Fig.10. Stars already identified with ROSAT sources in SACY (Torres et al. 2006, 2008; Elliott et al. 2014) or earlier works are not included. Stars #25/26 and #34/35 are matched to the same sources. The 0.1–2.4 keV X-ray luminosity (L_X) was derived from the kinematic distance, count rate and hardness ratio using the conversion factor given in Fleming et al. (1995), while fractional X-ray luminosities (log L_X/L_bol) were calculated from the V−Ks colour, V magnitude and the bolometric corrections tabled by Pecaut & Mamajek (2013).