J/AJ/132/2135 High-resolution spectroscopy in Tr 37 (Sicilia-Aguilar+, 2006) ================================================================================ High-resolution spectroscopy in Tr 37: gas accretion evolution in evolved dusty disks. Sicilia-Aguilar A., Hartmann L.W., Furesz G., Henning T., Dullemond C., Brandner W. =2006AJ....132.2135S ================================================================================ ADC_Keywords: Associations, stellar ; Equivalent widths ; Rotational velocities Keywords: accretion, accretion disks - line: profiles - planetary systems: protoplanetary disks - stars: pre-main sequence - stars: rotation Abstract: Using the Hectochelle multifiber spectrograph, we have obtained high-resolution (R~34000) spectra in the H{alpha} region for a large number of stars in the 4Myr old cluster Tr 37, containing 146 previously known members and 26 newly identified ones. We present the H{alpha} line profiles of all members, compare them to our IR observations of dusty disks (Two Micron All Sky Survey JHK + IRAC + MIPS 24um), use the radial velocities as a membership criterion, and calculate the rotational velocities. Description: Hectochelle is the high-resolution, multifiber echelle spectrograph, which operates at the wide-field mode of the Cassegrain 6.5m MMT telescope in Mount Hopkins, Arizona. We observed two fields in Tr 37 during two engineering runs on 2004 December 1 and 2. A total of 231 and 233 objects, respectively, were observed in the configurations. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 103 183 Spectral Information table2.dat 85 170 Summary of disk and stellar properties of members and probable members -------------------------------------------------------------------------------- See also: J/AJ/128/805 : Low-mass stars in Cepheus OB2 region (Sicilia-Aguilar+, 2004) J/AJ/130/188 : Young stars in Tr 37 and NGC 7160 (Sicilia-Aguilar+, 2005) J/ApJ/638/897 : IR photometry in Tr 37 and NGC 7160 (Sicilia-Aguilar+, 2006) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- [SHB2004] Identification (NN-NNNN), if exist (G1) 9- 24 A16 --- 2MASS The 2MASS identification (HHMMSSss+DDMMSSs) 26- 33 A8 --- SpType MK spectral type 35- 37 I3 0.1nm EWHa1 ? Hi-res equivalent width of H{alpha}, in {AA} 38 A1 --- u_EWHa1 Uncertainty flag in EW-hi 40- 43 I4 0.1nm EWHa2 ? Low-res equivalent width of H{alpha}, in {AA} 45- 47 F3.1 0.1nm EWLi ? Equivalent width of Li (6707), in {AA} 48 A1 --- u_EWLi Uncertainty flag in EW-Li 50- 54 A5 --- Type H{alpha} type (2) 56- 58 I3 km/s FWHa ? H{alpha} full width measured at 10% intensity 60- 63 F4.1 --- R ? Goodness of the cross-correlation 64 A1 --- u_R Uncertainty flag in R 66- 71 F6.1 km/s cz ? Radial velocity 73- 75 F3.1 km/s e_cz ? Uncertainty in cz 76 A1 --- u_cz Uncertainty flag in cz 78- 81 F4.1 km/s vsini ? Rotational velocity (vsin(i)) (3) 82 A1 --- u_vsini Uncertainty in Vsini 84-103 A20 --- Com Comment(s) (4) -------------------------------------------------------------------------------- Note (2): H{alpha} type is a combination of c, c: (c), w, w: and (w) meaning: c = (standing for CTTS) if broad emission with extended velocity wings was detected w = (standing for WTTS) otherwise Note (3): The error in the rotational velocity is proportional to the rotational velocity times 1/(1+R). Note (4): Membership is stated with the abbreviations: Y = sure member P = probable member PN = probable non-member N = non-member (e) = membership was obtained from the presence of H{alpha} strong emission and/or Li absorption lines (r) = membership was obtained via the radial velocity (r) * = new members conf = denotes previous possible members (from low-resolution spectroscopy) that are confirmed as members based on the radial velocities rej = denotes previous possible members that are most likely non-members according to radial velocities. Finally, a comment on binarity (SB2 or SB1) is added in this field. TOn = nonaccreting transition object TOa = accreting transition object -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- [SHB2004] Identification (NN-NNNN), if exist (G1) (1) 9- 24 A16 --- 2MASS 2MASS identification (HHMMSSss+DDMMSSs) 26- 34 A9 --- SpType MK spectral type 36- 45 F10.1 Myr Age ? Age (2) 47- 49 F3.1 solMass Mass ? Stellar mass (2) 51- 54 F4.1 km/s vsini ? Rotational velocity (vsin(i)) 56- 58 F3.1 km/s e_vsini ? Uncertainty in vsini (3) 59 A1 --- u_vsini Uncertainty flag in vsini 61- 70 A10 10-8solMass/yr dM/dt ? Accretion rate (4) 72- 85 A14 --- Com Class and comments (5) -------------------------------------------------------------------------------- Note (1): Summary of the properties of the stars in Tr 37. Only the star being sure or probable members are displayed here. Note (2): Ages and masses are derived from the V vs. V-I diagram, using the isochrones by Siess et al. 2000A&A...358..593S (see Paper I, Paper II (2004AJ....128..805S, 2005AJ....130..188S) for a detailed description of spectral typing and age/mass calculation). Note (3): Errors in the vsini are derived as vsini/(1+R) (see Tonry & Davis 1979AJ.....84.1511T; Hartmann et al., 1986ApJ...309..275H). Note (4): The best estimate of the accretion rate is selected for this summary. Whenever accretion rates derived from U band photometry were available (Paper II), we included them. Since some stars had been observed in U band in two campaigns, we include both values. As in the text, we denote with dM/dt=0 those stars with no U excess and H{alpha} profiles consistent with diskless WTTS or Class III objects. For stars with no detectable U excess but broad profiles, we give an upper limit to accretion of <0.1 10^-8^M_{sun}_/yr (see text). We do not provide an accretion value for stars not observed in U band and broad or probably broad H{alpha} profiles. For the exceptional star 13-277, whose spectral type is uncertain due to veiling, we provide an approximate accretion rate from the H{alpha} width at 10% maximum (see text). Most of these stars without a value for accretion are likely to be accreting (showing broad profiles, see figures). Note (5): The comments include the class (I, II, III or Transition object), the binarity as: SB1 = single-lined spectroscopic binary; SB2 = double-lined spectroscopic binary and the details on the H{alpha} profile: Ba = blue-shifted absorption; Ra= red-shifted absorption; Za = absorption with approximately zero velocity shift; B = blue-shifted emission; R=red-shifted emission; IPC = inverse P-Cygni profile. Uncertain values are denoted by " : " . -------------------------------------------------------------------------------- Global notes: Note (G1): [SHB2004] Trumpler 37 NN-NNNN in Simbad -------------------------------------------------------------------------------- History: From electronic version of the journal References: Sicilia-Aguilar et al., Paper I 2004AJ....128..805S, Cat. Sicilia-Aguilar et al., Paper II 2005AJ....130..188S, Cat. Sicilia-Aguilar et al., Paper III 2006ApJ...638..897S, Cat. ================================================================================ (End) Greg Schwarz [AAS], Patricia Vannier [CDS] 24-Jul-2008