J/AJ/140/1214 Near-IR spectroscopic survey of class I YSOs (Connelley+, 2010)
A near-infrared spectroscopic survey of class I protostars.
Connelley M.S., Greene T.P.
<Astron. J., 140, 1214-1240 (2010)>
=2010AJ....140.1214C 2010AJ....140.1214C
ADC_Keywords: YSOs ; Stars, pre-main sequence ; Infrared sources ;
Equivalent widths
Keywords: infrared: stars - stars: formation - stars: pre-main sequence -
surveys - techniques: spectroscopic
Abstract:
We present the results of a near-IR spectroscopic survey of 110 Class
I protostars observed from 0.80um to 2.43um at a spectroscopic
resolution of R=1200. This survey is unique in its selection of
targets from the whole sky, its sample size, wavelength coverage,
depth, and sample selection.
Description:
We observed a sample of Class I YSOs selected from the sample of
Connelley et al. (2008, Cat. J/AJ/135/2496). These objects were
selected from the whole sky and not limited to previously known
star-forming regions.
Our observations were conducted at the NASA Infrared Telescope
Facility (IRTF).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 90 110 Source characteristics
table2.dat 120 109 Spectral type and extinction estimates
table4.dat 113 110 Emission line equivalent widths
table6.dat 65 18 FU Ori and FU Ori-like objects, and objects
with excess CO absorption
table7.dat 38 10 Binary properties
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See also:
J/AJ/135/2496 : Near-IR survey of Class I protostars (Connelley+, 2008)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS name (HHMMm+DDMM, FHHMMm+DDMM)
12- 13 A2 --- m_IRAS Multiplicity index on IRAS
15 I1 --- SNo ? Source number on the findercharts in
Connelley et al. (2008, Cat. J/AJ/135/2496)
17- 18 I2 h RAh Right ascension (J2000) (1)
20- 21 I2 min RAm Right ascension (J2000) (1)
23- 27 F5.2 s RAs Right ascension (J2000) (1)
29 A1 --- DE- Declination sign (J2000) (1)
30- 31 I2 deg DEd Declination (J2000) (1)
33- 34 I2 arcmin DEm Declination (J2000) (1)
36- 39 F4.1 arcsec DEs Declination (J2000) (1)
41- 45 F5.2 mag Ksmag ?=- MKO/Ks magnitude (2)
47 A1 --- n_Ksmag [1] when Ksmag from 2MASS
49- 53 F5.2 --- alpha ?=- Spectral index of the source α (3)
55- 61 F7.1 Lsun Lbol ?=- Bolometric luminosity
63- 73 A11 "YYYY/MMM/DD" Date UT Date of observation
75- 78 I4 --- S/N Peak continuum K-band signal-to-noise ratio
80- 83 I4 s Time Total integration time on target
85- 90 A6 --- Flag Flags (4)
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Note (1): 2MASS coordinate for candidate YSO.
Note (2): K-band magnitudes from Table 4 of Connelley et al. (2008, Cat.
J/AJ/135/2496, 2008AJ....135.2526C 2008AJ....135.2526C), and are in the MKO photometric system
unless otherwise noted. Magnitudes noted with "1" in n_Ksmag are from 2MASS
and are in the 2MASS photometric system.
Note (3): Spectral index of the source (Lada, 1991, The Physics of Star
Formation and Early Stellar Evolution, ed. C. Lada & N. Kylafis (Dordrecht:
Kluwer), 343), calculated from the IRAS fluxes of the source.
Note (4): Flags as follows:
1 = no point source is seen at the K band. Flux likely dominated by scattered
light, which affects near-IR colors
2 = object associated with a reflection nebula, which may affect near-IR
colors
3 = light from both components of a known binary is in the spectrum
4 = spectrum has a triangular-shaped H-band continuum
5 = identified as a YSO in Table 12 of Evans et al. 2009, Cat J/ApJS/181/321
6 = well known as a T Tauri star
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS name (HHMMm+DDMM, FHHMMm+DDMM)
12- 13 A2 --- m_IRAS Multiplicity index on IRAS
15 I1 --- SNo ? Source number on the findercharts in
Connelley et al. (2008, Cat. J/AJ/135/2496)
17- 24 A8 --- SpT MK spectral type (with uncertainty) (1)
26 A1 --- l_AV Limit flag on AV
27- 31 F5.2 mag AV ? Extinction based on colors (2)
32- 35 F4.1 mag AVc ? Extinction based on continuum (3)
37- 40 F4.1 mag E_AVc ? Error on AVC (upper value)
42- 45 F4.1 mag e_AVc ? Error on AVC (lower value)
47- 50 F4.1 mag AVFe ? Extinction based on [Fe/H] (4)
52- 54 F3.1 mag e_AVFe ? rms uncertainty on AVFe
55 A1 --- n_AVFe [*] Note on AVFe (4)
57- 60 F4.1 mag AVP ? Extinction based on
Paschenβ / Brackettγ lines
62- 65 F4.2 mag e_AVP ? rms uncertainty on AVP
66- 70 F5.2 mag AVH ? Extinction based on H2Q(3)/S(1) line
72- 75 F4.2 mag E_AVH ? Error on AVH (upper value)
77- 80 F4.2 mag e_AVH ? Error on AVH (lower value)
82- 85 I4 K Tv ?=- Veiling temperature (3)
88- 91 I4 K E_Tv ? Veiling temperature (3)
94- 97 I4 K e_Tv ? Veiling temperature (3)
99-103 F5.2 --- rk ? Ratio of the veiling flux divided by the
continuum at the K band (5)
105-109 F5.2 --- E_rk ? Error on rk (upper value)
111-114 F4.2 --- e_rk ? Error on rk (lower value)
116-120 A5 --- n_rk Note on rk (6)
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Note (1): Based on matching photospheric absorption lines. Given as best-fit
spectral class, then the range of well-fit spectral classes as the
uncertainty range in the superscript and subscript. "FU Ori" designates
objects with a spectrum characteristic of FU Orionis-like objects and/or is
a known FU Orionis-like object.
Note (2): Based on dereddening the 2MASS colors to the T Tauri locus as defined
by Meyer et al. (1997AJ....114..288M 1997AJ....114..288M).
Note (3): Based on continuum fitting with the best-fit spectral type as the
input (when available, otherwise M2V was used). The maximum allowed veiling
temperature is 2000K, which often limits the upper error bar. A veiling
temperature is presented only if spectral fitting reasonably constrains the
veiling temperature.
Note (4): Based on the ratio of the [FeII] 1.257mum and 1.644mum lines.
The asterisk designates targets where the 1.644mum line is on the edge of a
comparatively strong absorption feature or is partially blended with the
Brackett 12 emission line.
Note (5): Based on either photospheric absorption lines or continuum fitting.
Note (6): "High" designated objects where we could not establish an upper limit
on rk because the veiling is too high.
The asterisk designates FU Orionis-like spectra where the veiling is much
higher than the result of the continuum fitting. The dearth of photospheric
lines shows that the actual extinction is likely to be much higher.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS name (HHMMm+DDMM, FHHMMm+DDMM)
12- 13 A2 --- m_IRAS Multiplicity index on IRAS
15 I1 --- SNo ? Source number on the findercharts in
Connelley et al. (2008, Cat. J/AJ/135/2496)
17- 22 F6.2 um W(Ca) ? CaII (0.866mum) equivalent width
24- 28 F5.2 um e_W(Ca) ? rms uncertainty on W(Ca)
30- 35 F6.2 um W(He) ? HeI (1.083mum) equivalent width (1)
37- 41 F5.2 um e_W(He) ? rms uncertainty on W(He)
42 A1 --- --- [,]
43- 47 F5.2 um W(He)2 ? Second value for HeI (1.083mum) equivalent
width (1)
49- 52 F4.2 um e_W(He)2 ? rms uncertainty on W(He)2
54- 60 F7.2 um W(Pa) ? Paβ (1.282mum) equivalent width
62- 65 F4.2 um e_W(Pa) ? rms uncertainty on W(Pa)
67- 72 F6.2 um W(Fe) ? [FeII] (1.644mum) equivalent width
74- 77 F4.2 um e_W(Fe) ? rms uncertainty on W(Fe)
79- 84 F6.2 um W(H2) ? H2 (2.122mum)equivalent width
86- 89 F4.2 um e_W(H2) ? rms uncertainty on W(H2)
91- 96 F6.2 um W(Br) ? Brγ (2.166mum) equivalent width
98-101 F4.2 um e_W(Br) ? rms uncertainty on W(Brg)
103-108 F6.2 um W(CO) ? CO (2.293mum) equivalent width
110-113 F4.2 um e_W(CO) ? rms uncertainty on W(CO)
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Note (1): The HeI line is often seen in emission and absorption simultaneously,
in which case positive and negative EW values are given for the absorption
and emission components.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS name, HHMMm+DDMM
12 A1 --- m_IRAS Multiplicity index on IRAS
14- 19 F6.2 0.1nm W(CO) ? CO equivalent width (Å)
21- 26 F6.2 Lsun Lbol ? Bolometric luminosity
28- 65 A38 --- Note Notes
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS name (HHMMm+DDMM or FHHMMm+DDMM)
14- 16 I3 pc Dist ? Distance
18- 22 F5.2 arcsec r ? Angular separation
24- 27 I4 AU rAU ? Projected separation on the sky
29- 32 F4.2 mag dK Difference in K magnitude between components
34- 38 A5 --- Veiling Veiling (excess continuum emission that
appears to weaken spectral lines)
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History:
* 30-Jun-2012: From electronic version of the journal
* 14-Aug-2012: several mismatches between the tables were fixed:
-- Tables 1 and 4:
IRAS 05384-0808 #1 transformed into 05384-0808 N
IRAS 05384-0808 #3 transformed into 05384-0808 S
IRAS 18270-0153 #1 transformed into 05384-0808 W
IRAS 18270-0153 #6 transformed into 05384-0808 E
-- Table 2:
IRAS 04286+1801 corrected into 04287+1801
IRAS 04073+3700 corrected into 04073+3800
IRAS 04181+2654 corrected into 04181+2655
IRAS 04369+4539 corrected into 04369+2539
IRAS F05384-0807 #1 corrected into 05384-0808 N
IRAS F05384-0807 #3 corrected into 05384-0808 S
IRAS F05391-0841 corrected into 05391-0841
IRAS 22324+4024 corrected into F22324+4024
-- Table 6:
IRAS 04287+1801 W corrected into 04287+1801 (=04286+1801 W)
-- Table 7:
IRAS F05391-0841 corrected into 05391-0841
(End) Francois Ochsenbein, Patricia Vannier [CDS] 30-Jun-2012