VizieR Online Data Catalog: Solar neighborhood. XXXIII. 45 M dwarfs (Riedel+, 2014)

The sample of 45 star systems in this paper was drawn from the hundreds of targets in the Cerro Tololo Inter-American Observatory Parallax Investigation (CTIOPI) target list. This is the 13th paper publishing parallax results from the ongoing CTIOPI program (Jao et al., 2003AJ....125..332J; Jao et al., 2005AJ....129.1954J; Costa et al., 2005AJ....130..337C; Costa et al, 2006AJ....132.1234C; Henry et al., 2006AJ....132.2360H; Subasavage et al., 2009AJ....137.4547S; Riedel et al., 2010AJ....140..897R; Jao et al., 2011AJ....141..117J; Boyd et al. 2001, cat. J/AJ/142/10) at the CTIO 0.9m telescope. The targets in this paper are all nearby bright M dwarfs Among the 45 systems considered here, we have individual photometry and astrometry of 51 components, because six of our star systems contain binaries with separations more than 1''.

All CTIOPI photometry is conducted with the CTIO 0.9m telescope, initially (1999-2003) under the NOAO Survey Programs grant; later (2003-present) via the SMARTS Consortium. Photometry is conducted in three filters (Tektronix 2 VRI), utilizing only the central quarter (6.8*6.8' FOV, 401mas/pixel) of the Tektronics 2046*2046 CCD. These values are then transformed to standard Johnson/Kron-Cousins V_JR_KCI_KC (the central wavelengths for V_J, R_KC, and I_KC are 5475, 6425, and 8075Å, respectively) photometry. The resulting photometry can be found in Table 2. Further details of the observation and reduction procedures can be found in Jao et al. (2005AJ....129.1954J) and Winters et al. 2011 (cat. J/AJ/141/21).

CTIOPI astrometry is carried out using the same telescope and camera configuration as that used for photometry but uses only one filter for each object. Between 2005 March and 2009 September, a different V-band filter was used for astrometric and photometric observations. Additional details of CTIOPI observing procedures can be found in Jao et al. (2005AJ....129.1954J; Paper XIII), Henry et al. (2006AJ....132.2360H; Paper XVII), and other papers in this series.

Four of the objects in this paper (BD-21°1074BC, SCR 0613-2742AB, L 449-1AB, and SCR 2010-2801AB) were selected for their X-ray brightness and observed with the Hubble Space Telescope's (HST's) Fine Guidance Sensors (FGSs) in Cycle 16B, in proposal 11943/11944 ("Binaries at the Extremes of the H-R Diagram") using the F583W filter (the bandpass of the F583W filter is shown here: http://www.stsci.edu/hst/fgs/design/filters, checked 2013 June 4) with no pupil.

Spectroscopic observations of all the resolved objects in this paper (except SCR 0613-2742AB) were carried out between 2003-2006 and 2009-2011 using the CTIO 1.5m telescope under the aegis of the SMARTS Consortium. The CTIO 1.5m Richey-Chretien Spectrograph (RCSpec) was used with the 32/I grating setting, covering 6000-9600Å at a resolution of 8Å.

We obtained spectra of SCR 0613-2742AB with the CTIO 4.0m telescope's RCSpec on 2008 September 18 and 2008 September 19 using the KPGLF-1 (632g/mm) grating, which covers 4900-8050Å at a resolution of 1.9Å/pixel.

One spectrum of SCR 0613-2742AB was taken with the FEROS spectrograph on the MPG 2.2m telescope at La Silla Observatory on 2013 February 18 as part of ESO program 090.C-0200(A). FEROS is an echelle spectrograph fed by two 2.0'' fibers and provides R~48000 spectra over a wavelength range of 3500-9200Å.

SCR 1425-4113AB was observed on the Canada-France-Hawaii Telescope (CFHT) with the ESPaDOnS. ESPaDONs was used in the "star+sky" mode, to get a resolving power of R=68000 covering 3700-10500Å over 40 grating orders.

(11 data files).