J/AJ/130/1145 YSO near-infrared properties (Doppmann+, 2005) ================================================================================ The physical natures of class I and flat-spectrum protostellar photospheres: a near-infrared spectroscopic study. Doppmann G.W., Greene T.P., Covey K.R., Lada C.J. =2005AJ....130.1145D (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: YSOs ; Stars, pre-main sequence ; Infrared sources ; Rotational velocities Keywords: stars - stars: formation - stars: fundamental parameters - stars: late-type - stars: low-mass, brown dwarfs - stars: pre-main-sequence -stars: rotation - techniques: spectroscopic Abstract: We present high-resolution (R~18,000), high signal-to-noise ratio, 2{mu}m spectra of 52 IR-selected Class I and flat-spectrum young stellar objects in the Taurus-Auriga, {rho} Ophiuchi, Serpens, Perseus, and Corona Australis dark clouds. We detect key absorption lines in 41 objects and fit synthetic spectra generated from pre-main-sequence models to deduce the effective temperatures, surface gravities, near-IR veilings, rotation velocities, and radial velocities of each of these 41 sources. Description: Near-IR spectra of the protostellar sample and MK spectral standards were acquired on 2000 May 29-30, 2001 July 7-10, 2001 November 4-6, and 2003 June 19-21 UT. All data were acquired with the 10m Keck II telescope on Mauna Kea, Hawaii, using the NIRSPEC multiorder cryogenic echelle facility spectrograph. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 121 80 Journal of observations table3.dat 85 41 Derived YSO properties -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 32 A32 --- Type Source type 34- 44 A11 --- Name Source name 49 A1 --- n_Name [b/c] Note on the observation (1) 51- 58 A8 --- Loc Source location 60- 61 I2 h RAh Hour of right ascension (J2000.0) 63- 64 I2 min RAm Minute of right ascension (J2000.0) 66- 70 F5.2 s RAs Second of right ascension (J2000.0) 72 A1 --- DE- Sign of the declination (J2000.0) 73- 74 I2 deg DEd Degree of declination (J2000.0) 76- 77 I2 arcmin DEm Arcminute of declination (J2000.0) 79- 82 F4.1 arcsec DEs Arcsecond of declination (J2000.0) 84-106 A23 --- ObsDate Date(s) of observation 108-112 F5.1 min IntTime Integration time 114-116 I3 --- S/N Signal to noise ratio 118-120 A3 --- Line [Yes/No ] Detection of photospheric lines 121 A1 --- f_Line [a/d] Flag on Line (2) -------------------------------------------------------------------------------- Note (1): Note on the observation, defined as follows: b = Source was observed on multiple nights. The final spectrum is the noise-weighted sum of spectra obtained on each individual night. No shifting of the spectra was required, as radial velocity differences were less than 1 pixel (~4.5km/s). c = The final spectrum is the noise-weighted sum of spectra obtained on both nights. The July 8 observation exhibits slightly broader and asymmetric lines, suggesting the presence of a cooler (<3900K) binary companion with a marginal velocity separation (<=2 resolution elements). Note (2): Flag on Line, defined as follows: a = CO and Na line absorption is marginally detected in this source, but at too low S/N for us to apply our standard fitting technique. d = Nisini et al. (2005A&A...429..543N) detect photospheric lines in this source at higher S/N and measure heavy veiling, r_K_=6.0. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 A11 --- Name Source name 13- 16 A4 --- f_Teff Limit flag on Teff 17- 20 I4 K Teff Effective temperature 22- 24 I3 K E_Teff Upper limit error on Teff 26- 28 I3 K e_Teff Lower limit error on Teff 30- 33 A4 --- f_log(g) Limit flag on log(g) 34- 36 F3.1 [cm/s2] log(g) Log of the surface gravity 38- 41 F4.2 [cm/s2] E_log(g) Upper limit error on log(g) 43- 46 F4.2 [cm/s2] e_log(g) Lower limit error on log(g) 48- 49 I2 km/s vsini Rotational velocity 51- 53 F3.1 km/s E_vsini Upper limit error on vsini 55- 57 F3.1 km/s e_vsini Lower limit error on vsini 59- 61 F3.1 --- rK Amount of continuum veiling (1) 63- 67 F5.3 --- E_rK Upper limit error on rK 69- 73 F5.3 --- e_rK Lower limit error on rK 75- 79 F5.1 km/s VLSR Local Standard of Rest velocity (2) 81- 84 F4.1 solLum Lum ? Luminosity (3) -------------------------------------------------------------------------------- Note (1): The ratio of non stellar excess over the stellar flux at K. Note (2): A systematic shift of +1.8km/s has been applied to these values, consistent with our radial velocity measurements measured in MK standards with published values (Fig. 13). Note (3): Stellar luminosities are based on derived K-band extinctions which have been elevated by 0.88 magnitudes to account for the effects of scattered light (see Section 3.8). -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Greg Schwarz [AAS], Marianne Brouty [CDS] 16-Nov-2005