J/ApJ/684/1240 Prestellar cores in Perseus, Serpens and Ophiuchus (Enoch+, 2008)
The mass distribution and lifetime of prestellar cores in Perseus, Serpens, and
Ophiuchus.
Enoch M.L., Evans II N.J., Sargent A.I., Glenn J., Rosolowsky E., Myers P.
<Astrophys. J., 684, 1240-1259 (2008)>
=2008ApJ...684.1240E 2008ApJ...684.1240E
ADC_Keywords: Molecular clouds ; Interstellar medium ; Millimetric/submm sources
Keywords: infrared: ISM - ISM: clouds - ISM: individual (Ophiuchus, Perseus,
Serpens) - stars: formation - submillimeter
Abstract:
We present an unbiased census of starless cores in Perseus, Serpens,
and Ophiuchus, assembled by comparing large-scale Bolocam 1.1mm
continuum emission maps with Spitzer c2d surveys. We use the c2d
catalogs to separate 108 starless from 92 protostellar cores in the
1.1mm core samples from Enoch and Young and their coworkers. A
comparison of these populations reveals the initial conditions of the
starless cores.
Description:
Utilizing large-scale 1.1mm surveys (Paper I-III: Enoch et al. 2006,
Cat. J/ApJ/638/293; Young et al. 2006ApJ...644..326Y 2006ApJ...644..326Y; Enoch et al.
2007ApJ...666..982E 2007ApJ...666..982E) together with Spitzer IRAC and MIPS maps from the
c2d Legacy program (Evans et al. 2003PASP..115..965E 2003PASP..115..965E), we have carried
out an unbiased census of prestellar and protostellar cores in the
Perseus, Serpens, and Ophiuchus molecular clouds.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 71 108 Starless cores in Perseus, Serpens, and Ophiuchus
table2.dat 71 92 Protostellar cores in Perseus, Serpens, and Ophiuchus
table4.dat 35 70 Dynamical properties of Perseus cores
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See also:
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/A+A/487/993 : MAMBO Mapping of c2d Clouds and Cores (Kauffmann+, 2008)
J/ApJS/175/509 : Ammonia spectral atlas in Perseus (Rosolowsky+, 2008)
J/ApJ/663/1149 : Spitzer survey of Serpens YSO population (Harvey+, 2007)
J/ApJ/668/1042 : Dense cores in Perseus molecular cloud (Kirk+, 2007)
J/ApJ/669/493 : Spitzer/Chandra YSOs in Serpens cloud core (Winston+, 2007)
J/ApJ/638/293 : 1.1mm sources in the Perseus Molecular Cloud (Enoch+, 2006)
Byte-by-byte Description of file: table[12].dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Cloud Molecular cloud name
11- 13 A3 --- Cld Cloud (constellation) name: Per, Ser or Oph
14- 18 A5 --- --- [Bolo-]
20- 22 I3 --- ID Bolocam identification number in Cld (G1) (1)
24- 25 I2 h RAh Hour of Right Ascension (J2000)
27- 28 I2 min RAm Minute of Right Ascension (J2000)
30- 33 F4.1 s RAs Second of Right Ascension (J2000)
35 A1 --- DE- Sign of the Declination (J2000)
36- 37 I2 deg DEd Degree of Declination (J2000)
39- 40 I2 arcmin DEm Arcminute of Declination (J2000)
42- 43 I2 arcsec DEs Arcsecond of Declination (J2000)
45- 48 I4 mJy Sp Peak flux at 1.1mm in units of mJy/beam
50- 54 F5.2 solMass TMass Total mass (2)
56- 60 F5.1 arcsec theta ? Deconvolved angular FWHM size (3)
62- 64 F3.1 --- a/b [1,3] Core axis ratio (3)
66- 71 E6.2 cm-3 Mean density (4)
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Note (1): Note that the Ophiuchus identifications are different than Tables
1 and 2 of Paper II (Young et al. 2006ApJ...644..326Y 2006ApJ...644..326Y, <[YEE2006] NN>
in Simbad) for Oph-Bolo 35 and above due to an adjustment of the
source list, resulting in 43 rather than 44 sources (IDs are shifted
by -1 for Oph-Bolo 35 and up). The peak flux, total mass, sizes, etc.
for Oph-Bolo 35 and Oph-Bolo 36 are also different than in Paper II.
Note (2): Calculated from the total flux at 1.1mm, assuming TD=10K.
Note (3): Derived from an elliptical gaussian fit, deconvolved by the 31"
beam.
Note (4): Calculated in a fixed linear aperture of diameter 1E4 AU for each
source.
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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- 8 A8 --- --- [Per-Bolo]
10- 12 I3 --- ID Bolocam identification from Papers I-III (G1)
14- 17 F4.1 K Temp Kinetic temperature (2)
19- 22 F4.1 10+3.AU Rad Effective radius
24- 27 F4.2 km/s sigH2 Linewidth (1)
29- 31 F3.1 solMass Mdust Dust mass (2)
33- 35 F3.1 solMass Mvir Virial mass of the core (3)
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Note (1): Derived from the NH3 observations of Perseus cores completed by
Rosolowsky et al. (2008, Cat. J/ApJS/175/509; <[RPF2008] NH3SRC NNN>
in Simbad).
Note (2): Calculated from the total 1.1mm flux (Tables 1 and 2).
Note (3): Calculated according to Eq. 5:
Mvir=(5σ2H2R)/aG, where a accounts for the central
concentration of the core, R is the radius of the core, and
σH2 is the line width of the molecular gas inferred from
the ammonia line width. The effective radius is estimated as the
deconvolved HWHM of the 1.1mm identified core.
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Global Notes:
Note (G1): Identifications as follows:
Per-Bolo = <[EYG2006] Bolo NNN> in Simbad (Enoch et al. 2006,
Cat. J/ApJ/638/293, Paper I),
Oph-Bolo = <[YEE2006] Bolo NN> in Simbad (Young et al., 2006ApJ...644..326Y 2006ApJ...644..326Y,
Paper II); NN+1 for 35 and up (see Note (1) of tables 1 and 2).
Ser-Bolo = <[EGE2007] Bolo NN> in Simbad (Enoch et al., 2007ApJ...666..982E 2007ApJ...666..982E,
Paper III),
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 10-Dec-2010