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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. <Astron. J., 132, 2135-2155 (2006)> =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 Hα 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 Hα 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 Hα, in Å 38 A1 --- u_EWHa1 Uncertainty flag in EW-hi 40- 43 I4 0.1nm EWHa2 ? Low-res equivalent width of Hα, in Å 45- 47 F3.1 0.1nm EWLi ? Equivalent width of Li (6707), in Å 48 A1 --- u_EWLi Uncertainty flag in EW-Li 50- 54 A5 --- Type Halpha type (2) 56- 58 I3 km/s FWHa ? Hα 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): Hα 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 Hα 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 Hα 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 10-8M/yr (see text). We do not provide an accretion value for stars not observed in U band and broad or probably broad Hα profiles. For the exceptional star 13-277, whose spectral type is uncertain due to veiling, we provide an approximate accretion rate from the Hα 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 Hα 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. J/AJ/128/805 Sicilia-Aguilar et al., Paper II 2005AJ....130..188S, Cat. J/AJ/130/188 Sicilia-Aguilar et al., Paper III 2006ApJ...638..897S, Cat. J/ApJ/638/897
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 24-Jul-2008
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