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.
<Astron. J., 130, 1145-1170 (2005)>
=2005AJ....130.1145D 2005AJ....130.1145D
ADC_Keywords: YSOs ; Stars, pre-main sequence ; Infrared sources ;
Rotational velocities ; Effective temperatures
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∼18000), high signal-to-noise ratio,
2µm spectra of 52 IR-selected Class I and flat-spectrum young
stellar objects in the Taurus-Auriga, ρ 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 125 80 Journal of observations
table3.dat 82 41 Derived YSO properties
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 32 A32 --- Type Source type ("Class I and Flat-Spectrum Sample"
or "MK Standards")
34- 44 A11 --- Name Source name
49 A1 --- n_Name [b/c] Note on the observation (b or c) (1)
51- 53 A3 --- Cloud Source location (CrA, Oph, Per, Ser, Tau) (2)
55- 62 A8 --- SpT Spectral type
64- 65 I2 h RAh Hour of right ascension (J2000.0)
67- 68 I2 min RAm Minute of right ascension (J2000.0)
70- 74 F5.2 s RAs Second of right ascension (J2000.0)
76 A1 --- DE- Sign of the declination (J2000.0)
77- 78 I2 deg DEd Degree of declination (J2000.0)
80- 81 I2 arcmin DEm Arcminute of declination (J2000.0)
83- 86 F4.1 arcsec DEs Arcsecond of declination (J2000.0)
88-110 A23 --- Date UT date(s) of observation
112-116 F5.1 min Int Integration time
118-120 I3 --- S/N Signal to noise ratio
122-124 A3 --- Line Detection of photospheric lines (Yes or No)
125 A1 --- f_Line [a/d] Flag on Line (a or d) (3)
--------------------------------------------------------------------------------
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): Dark clouds:
CrA = Corona Australis,
Oph = Ophiuchus;
Per = Perseus;
Ser = Serpens;
Tau = Taurus.
Note (3): 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 2005A&A...429..543N) detect photospheric lines in this
source at higher S/N and measure heavy veiling, rK=6.0.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
13- 14 A2 --- l_Teff [≤] Upper limit flag on Teff
16- 19 I4 K Teff Effective temperature
21- 23 I3 K E_Teff Upper limit error on Teff
25- 27 I3 K e_Teff Lower limit error on Teff
29- 30 A2 --- l_logg [≤>] Limit flag on logg
32- 34 F3.1 [cm/s2] logg Log of the surface gravity
36- 39 F4.2 [cm/s2] E_logg Upper limit error on logg
41- 44 F4.2 [cm/s2] e_logg Lower limit error on logg
46- 47 I2 km/s vsini Rotational velocity
49- 51 F3.1 km/s E_vsini Upper limit error on vsini
53- 55 F3.1 km/s e_vsini Lower limit error on vsini
57- 59 F3.1 --- rK Amount of continuum veiling (1)
61- 65 F5.3 --- E_rK Upper limit error on rK
67- 71 F5.3 --- e_rK Lower limit error on rK
73- 77 F5.1 km/s VLSR Local Standard of Rest velocity (2)
79- 82 F4.1 Lsun Lum ? Luminosity (3)
--------------------------------------------------------------------------------
Note (1): The ratio of non stellar excess over the stellar flux at K
(rK=FK,ex/FK*).
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