J/AJ/147/85 Solar neighborhood. XXXIII. 45 M dwarfs (Riedel+, 2014) ================================================================================ The solar neighborhood. XXXIII. Parallax results from the CTIOPI 0.9 m program: trigonometric parallaxes of nearby low-mass active and young systems. Riedel A.R., Finch C.T., Henry T.J., Subasavage J.P., Jao W.-C., Malo L., Rodriguez D.R., White R.J., Gies D.R., Dieterich S.B., Winters J.G., Davison C.L., Nelan E.P., Blunt S.C., Cruz K.L., Rice E.L., Ianna P.A. =2014AJ....147...85R ================================================================================ ADC_Keywords: Associations, stellar ; Stars, dwarfs ; Stars, M-type ; Stars, nearby ; Photometry, VRI ; Spectral types ; Parallaxes, trigonometric ; Proper motions ; Radial velocities ; Stars, distances ; Positional data ; Velocity dispersion ; Space velocities ; Equivalent widths ; Stars, ages Keywords: open clusters and associations: general - parallaxes - solar neighborhood - stars: low-mass - stars: pre-main sequence Abstract: We present basic observational data and association membership analysis for 45 young and active low-mass stellar systems from the ongoing Research Consortium On Nearby Stars photometry and astrometry program at the Cerro Tololo Inter-American Observatory. Most of these systems have saturated X-ray emission (log(L_X_/L_bol_)>-3.5) based on X-ray fluxes from the ROSAT All-Sky Survey, and many are significantly more luminous than main-sequence stars of comparable color. We present parallaxes and proper motions, Johnson-Kron-Cousins VRI photometry, and multiplicity observations from the CTIOPI program on the CTIO 0.9m telescope. To this we add low-resolution optical spectroscopy and line measurements from the CTIO 1.5m telescope, and interferometric binary measurements from the Hubble Space Telescope Fine Guidance Sensors. We also incorporate data from published sources: JHK_S_ photometry from the Two Micron All Sky Survey point source catalog, X-ray data from the ROSAT All-Sky Survey, and radial velocities from literature sources. Within the sample of 45 systems, we identify 21 candidate low-mass pre-main-sequence members of nearby associations, including members of {beta} Pictoris, TW Hydrae, Argus, AB Doradus, two ambiguous {approx}30Myr old systems, and one object that may be a member of the Ursa Major moving group. Of the 21 candidate young systems, 14 are newly identified as a result of this work, and six of those are within 25pc of the Sun. Description: 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_J_R_KC_I_KC_ (the central wavelengths for V_J_, R_KC_, and I_KC_ are 5475, 6425, and 8075{AA}, 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{deg}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 6000-9600{AA} at a resolution of 8{AA}. 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 4900-8050{AA} at a resolution of 1.9{AA}/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 3500-9200{AA}. 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 3700-10500{AA} over 40 grating orders. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 147 51 Photometric results table3.dat 147 51 Astrometric results table4.dat 118 52 Data used to calculate UVWXYZ table5.dat 59 72 Deblended magnitudes for isochrones table6.dat 67 50 Photometric and spectroscopic properties table7.dat 134 45 Young star results table8.dat 96 13 Nearby young associations (NYA) table9.dat 94 54 UVWXYZ kinematics table10.dat 100 28 Multiple star parameters refs.dat 72 34 References notes.dat 2486 24 Notes -------------------------------------------------------------------------------- See also: II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) IX/29 : ROSAT All-Sky Survey Faint Source Catalog (Voges+ 2000) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999) III/198 : Palomar/MSU nearby star spectroscopic survey (Hawley+ 1997) I/238 : Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995) J/AJ/147/94 : Solar neighborhood. XXXII. L and M dwarfs (Dieterich+, 2014) J/ApJ/762/88 : Young stellar kinematic group candidate members (Malo+, 2013) J/AJ/144/64 : Solar neighborhood. XXVIII. Substellar companions (Dieterich+, 2012) J/AJ/143/134 : Candidate members of B Pic /AB Dor groups (McCarthy+, 2012) J/AJ/143/80 : Low-mass member candidates of B Pic & AB Dor (Schlieder+, 2012) J/ApJ/758/56 : Young M dwarfs within 25pc. II. Kinematics (Shkolnik+, 2012) J/AJ/142/92 : New proper motion stars with pm>=0.18''/yr (Boyd+, 2011) J/A+A/531/A92 : Deep all-sky census of the Hyades (Roeser+, 2011) J/AJ/142/10 : New proper motion stars 0.40''/yr>pm>=0.18''/yr (Boyd+, 2011) J/AJ/141/21 : CCD distance estimates of SCR targets (Winters+, 2011) J/AJ/140/119 : BPic and AB Dor moving groups members (Schlieder+, 2010) J/A+A/499/129 : Old MS stars in young moving groups (Lopez-Santiago+, 2009) J/ApJ/699/649 : Young M dwarfs within 25pc. I. (Shkolnik+, 2009) J/AJ/134/252 : New nearby white dwarf systems (Subasavage+, 2007) J/AJ/133/2898 : New proper-motion stars (-90] Limit flag on Age 89- 91 F3.1 Gyr Age [1/7.5]? H{alpha} age 93- 95 A3 --- f_Age [N/A] Not analysed 97 A1 --- u_NYA [?] Uncertainty flag on NYA 98-110 A13 --- NYA Name of the Nearby Young Association (Unknown=Unknown association) (3) 112-116 A5 --- Ref References; in refs.dat file 118-134 A17 --- n_Ref Name of the association find in reference -------------------------------------------------------------------------------- Note (1): We take a value of {gamma} less than 4 as a potentially significant match for the kinematic association (only the {gamma} value for the most consistent association is given here). See Section 4.1.2 and Equation (1) for further details. Note (2): BANYAN (Malo et al. 2013, cat. J/ApJ/762/88) is an independent Bayesian methodology for finding young stars. BANYAN uses IJ photometry, Baraffe et al. (1998, cat. J/A+A/337/403; 2002A&A...382..563B) model isochrones, and a slightly different set of UVWXYZ values for the known associations. It searches for members of the known nearby associations {beta} Pictoris, TW Hydra, Tucana-Horologium, Columba, Carina, Argus, and AB Doradus, with "Field" as the default hypothesis. Note (3): In addition, there is one system (L 449-1 AB) kinematically consistent with the Ursa Majoris moving group. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table8.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 17 A17 --- Name Name of the nearby association (1) 19 A1 --- f_Name Reference for the data (2) 21- 26 F6.2 km/s Uvel U space velocity component 28- 31 F4.2 km/s sUvel Velocity dispersion on Uvel {sigma}_U_ (3) 33- 38 F6.2 km/s Vvel V space velocity component 40- 43 F4.2 km/s sVvel Velocity dispersion on Vvel {sigma}_V_ (3) 45- 50 F6.2 km/s Wvel W space velocity component 52- 55 F4.2 km/s sWvel Velocity dispersion on Wvel {sigma}_W_ (3) 57- 60 I4 pc Xpos ? Minimum X space position 62- 65 I4 pc XPos ? Maximum X space position 67- 72 F6.1 pc Ypos ? Minimum Y space position 74- 78 F5.1 pc YPos ? Maximum Y space position 80- 84 F5.1 pc Zpos ? Minimum Z space position 86- 90 F5.1 pc ZPos ? Maximum Z space position 92- 94 I3 Myr Age Age 96 A1 --- n_Age [ab] Origin of Age (4) -------------------------------------------------------------------------------- Note (1): All data in this table (unless otherwise specified) from Torres et al. (2008hsf2.book..757T). Note (2): Reference defined as follows: c = Dimensions Soderblom et al. (2005AJ....129.1616S), 13pc tidal radius Adams et al. (2001AJ....121.2053A); d = Barrado y Navascues (1998A&A...339..831B); e = King et al. (2003AJ....125.1980K); f = Roser et al. 2011 (cat. J/A+A/531/A92). Note (3): In the case of the association, the dispersion represent the intrinsic dispersion of real members. Note (4): Flag defined as follows: a = Only these ages are known with any degree of certainty or corroboration; b = Age from Luhman et al. (2005ApJ...628L..69L). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table9.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 15 A15 --- Name Name of the star system 17- 19 A3 --- m_Name Component identification 21- 26 F6.2 km/s Uvel ? U space velocity component (1) 28- 32 F5.2 km/s e_Uvel ? Error in Uvel 34- 39 F6.2 km/s Vvel ? V space velocity component (1) 41- 45 F5.2 km/s e_Vvel ? Error in Vvel 47- 52 F6.2 km/s Wvel ? W space velocity component (1) 54- 58 F5.2 km/s e_Wvel ? Error in Wvel 60- 65 F6.2 pc Xpos X space position (1) 67- 70 F4.2 pc e_Xpos Error in Xpos 72- 77 F6.2 pc Ypos Y space position (1) 79- 82 F4.2 pc e_Ypos Error in Ypos 84- 89 F6.2 pc Zpos Z space position (1) 91- 94 F4.2 pc e_Zpos Error in Zpos -------------------------------------------------------------------------------- Note (1): These UVWXYZ coordinates are right-handed Cartesian Galactic coordinates aligned so that the U/X axis is toward the galactic center, the V/Y axis is in the direction of galactic rotation, and the W/Z axis is toward the north Galactic pole. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table10.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- Name Name of the star system 15- 16 A2 --- m_Name Primary component identification 18- 30 A13 --- SName Name of the star system 32- 33 A2 --- m_SName Secondary component identification 35- 42 F8.3 arcsec Sep ? Separation 44- 48 F5.1 deg PA ? Position angle 50 A1 --- f_PA [b] Indicates ambiguous sign on X-axis of solution 52- 53 I2 --- r_PA ? Reference for Sep and PA; in refs.dat file 55 A1 --- F1 [ac] Sep and PA estimated (1) 57- 60 F4.2 mag Dmag ? Delta magnitude {Delta}mag 62- 68 A7 --- Phot Photometric system 70- 74 A5 --- Flt Name of filter in the system 76- 77 I2 --- r_Flt ? Reference for magnitude; in refs.dat file 79 A1 --- F2 [ac] Joined of estimated magnitude (1) 81 A1 --- l_Per [~<>] Limit or approximation flag on Per 82- 85 F4.1 --- Per ? Period 87 A1 --- f_Per Unit of the period (y=year, d=day) 89- 90 I2 --- r_Per ? Reference for period; in refs.dat file 92-100 A9 --- Obs Resolving observation (2) -------------------------------------------------------------------------------- Note (1): Flag on reference defined as follows: a = Relative to unresolved components; c = estimate from PSF peaks. Note (2): Resolving observations are defined as follows: VB = Visual binary; SB = Spectroscopic binary; PB = Astrometric binary with perturbation in data from Cerro Tololo Inter-American Observatory Parallax Investigation (CTIOPI); AO = Resolved by AO; LI = Resolved by Lucky Imaging; SP = Resolved by Speckle Interferometry; FGS = Resolved by Fine Guidance Sensor (FGS; on Hubble Space Telescope) interferometry. -------------------------------------------------------------------------------- Byte-by-byte Description of file: refs.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Ref Reference identifier 4- 22 A19 --- BibCode Bibliographic code 24- 49 A26 --- Aut Author's name 51- 72 A22 --- Com Comments -------------------------------------------------------------------------------- Byte-by-byte Description of file: notes.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- Name Name of the star system 15- 17 A3 --- m_Name Component identification 19-2486 A2468 --- Note Notes about the star -------------------------------------------------------------------------------- Global notes: Note (G1): In Cerro Tololo Inter-American Observatory Parallax Investigation (CTIOPI; 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). Note (G2): The notes are defined as follows: b = Astrometric results and relative photometry include new V filter data. Between 2005 March and 2009 September, a different V-band filter was used for astrometric and photometric observations. While photometrically identical to the original V filter, it exhibited slightly inferior astrometric performance (Paper XXII, Riedel et al., 2010AJ....140..897R); c = No independent photometry; d = Not using independent astrometry (see Section 5); e = Astrometric perturbation was incorporated into the final astrometric fit; f = Reference field was reddened, and a generic correction to absolute parallax was adopted. -------------------------------------------------------------------------------- History: From electronic version of the journal References: Henry et al., Paper I 1994AJ....108.1437H Kirkpatrick et al., Paper II 1995AJ....109..797K Simons et al., Paper III 1996AJ....112.2238S Henry et al., Paper IV 1997AJ....114..388H Patterson et al., Paper V 1998AJ....115.1648P Henry et al., Paper VI 2002AJ....123.2002H Jao et al., Paper VII 2003AJ....125..332J Hambly et al., Paper VIII 2004AJ....128..437H Golimowski et al., Paper IX 2004AJ....128.1733G Henry et al., Paper X 2004AJ....128.2460H Deacon et al., Paper XI 2005AJ....129..409D Subasavage et al., Paper XII 2005AJ....129..413S, Cat. J/AJ/129/413 Jao et al., Paper XIII 2005AJ....129.1954J Costa et al., Paper XIV 2005AJ....130..337C Subasavage et al., Paper XV 2005AJ....130.1658S, Cat. J/AJ/130/1658 Costa et al., Paper XVI 2006AJ....132.1234C Henry et al., Paper XVII 2006AJ....132.2360H Finch et al., Paper XVIII 2007AJ....133.2898F, Cat. J/AJ/133/2898 Subasavage et al., Paper XIX 2007AJ....134..252S, Cat. J/AJ/134/252 Subasavage et al., Paper XX 2008AJ....136..899S Subasavage et al., Paper XXI 2009AJ....137.4547S Riedel et al., Paper XXII 2010AJ....140..897R Winters et al., Paper XXIII 2011AJ....141...21W, Cat. J/AJ/141/21 Jao et al., Paper XXIV 2011AJ....141..117J Boyd et al., Paper XXV 2011AJ....142...10B, Cat. J/AJ/142/10 Riedel et al., Paper XXVI 2011AJ....142..104R Boyd et al., Paper XXVII 2011AJ....142...92B, Cat. J/AJ/142/92 Dieterich et al., Paper XXVIII 2012AJ....144...64D, Cat. J/AJ/144/64 Cantrell et al., Paper XXIX 2013AJ....146...99C Mamajek et al., Paper XXX 2013AJ....146..154M Jao et al., Paper XXXI 2014AJ....147...21J Dieterich et al., Paper XXXII 2014AJ....147...94D, Cat. J/AJ/147/94 Lurie et al., Paper XXXIV 2014AJ....148...91L Winters et al., Paper XXXV 2015AJ....149....5W, Cat. J/AJ/149/5 Hosey et al., Paper XXXVI 2015AJ....150....6H, Cat. J/AJ/150/6 Winters et al., Paper XXXVIII 2017AJ....153...14W, Cat. J/AJ/153/14 Subasavage et al., Paper XXXIX 2017AJ....154...32S, Cat. J/AJ/154/32 Bartlett et al., Paper XXXX 2017AJ....154..151B, Cat. J/AJ/154/151 Clements et al., Paper XLI 2017AJ....154..124C, Cat. J/AJ/154/124 Jao et al., Paper XLII 2017AJ....154..191J Jao et al., Paper XLII 2017AJ....154..191J, Cat. J/AJ/154/191 Riedel et al., Paper XLIII 2018AJ....156...49R, Cat. J/AJ/156/49 Henry et al., Paper XLIV 2018AJ....155..265H, Cat. J/AJ/155/265 Winters et al., Paper XLV 2019AJ....157..216W ================================================================================ (End) Sylvain Guehenneux [CDS] 22-Jan-2015