J/ApJ/638/293 1.1mm sources in the Perseus Molecular Cloud (Enoch+, 2006)
Bolocam survey for 1.1mm dust continuum emission in the c2d Legacy clouds.
I. Perseus.
Enoch M.L., Young K.E., Glenn J., Evans Ii N.J., Golwala S., Sargent A.I.,
Harvey P., Aguirre J., Goldin A., Haig D., Huard T.L., Lange A.,
Laurent G., Maloney P., Mauskopf P., Rossinot P., Sayers J.
<Astrophys. J., 638, 293-313 (2006)>
=2006ApJ...638..293E 2006ApJ...638..293E
ADC_Keywords: Millimetric/submm sources ; Molecular clouds ; Interstellar medium
Keywords: ISM: clouds - ISM: individual (Perseus) - stars: formation
Abstract:
We have completed a 1.1mm continuum survey of 7.5°2 of the
Perseus Molecular Cloud using Bolocam at the Caltech Submillimeter
Observatory. This represents the largest millimeter or submillimeter
continuum map of Perseus to date. Our map covers more than 30,000 31"
(FWHM) resolution elements to a 1σ rms of 15mJy/beam. We detect
a total of 122 cores above a 5σ point-source mass detection
limit of 0.18M☉, assuming a dust temperature of TD=10K, 60 of
which are new millimeter or submillimeter detections.
Description:
Continuum observations at 1.1mm were made with Bolocam7 at CSO on
Mauna Kea, Hawaii during 2003 January 28-February 15. All observations
of Perseus were completed in the 1.1mm mode, which has a bandwidth of
45GHz and band center at 268GHz.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 122 Source IDs, positions, and peak flux density
table2.dat 122 122 Source photometry, masses, column density,
sizes, and morphology
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See also:
J/A+A/440/151 : Observations at 850um in Perseus clusters (Hatchell+, 2005)
J/BaltA/12/301 : Vilnius photometry in Barnard 1 (Cernis+, 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [Bolo]
6- 8 I3 --- [EYG2006] Source identification
10- 11 I2 h RAh Hour of Right Ascension (J2000)
13- 14 I2 min RAm Minute of Right Ascension (J2000)
16- 19 F4.1 s RAs Second of Right Ascension (J2000)
21 A1 --- DE- Sign of the Declination (J2000)
22- 23 I2 deg DEd Degree of Declination (J2000)
25- 26 I2 arcmin DEm Arcminute of Declination (J2000)
28- 31 F4.1 arcsec DEs Arcsecond of Declination (J2000)
33- 36 I4 mJy Fp 1.1mm peak flux density in units of mJy/beam
38- 39 I2 mJy e_Fp The 1σ uncertainty in Peak (1)
41- 45 F5.1 --- S/N Signal-to-Noise
47- 81 A35 --- OName Other name(s) (2)
83- 93 A11 --- MIPS MIPS 24µm source? (3)
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Note (1): Does not include an additional systematic uncertainty of 15%
in the peak flux density.
Note (2): Other names listed are the most common identifications from the
literature, and are not meant to be a complete list. References
are given in parentheses:
1 = O'Linger et al. (1999ApJ...515..696O 1999ApJ...515..696O);
2 = Barsony et al. (1998ApJ...509..733B 1998ApJ...509..733B);
3 = Hatchell et al. (2005, Cat. J/A+A/440/151);
4 = Froebrich et al. (2003MNRAS.346..163F 2003MNRAS.346..163F);
5 = Juan et al. (1993A&A...270..432J 1993A&A...270..432J);
6 = Jennings et al. (1987MNRAS.226..461J 1987MNRAS.226..461J);
7 = Sandell & Knee (2001ApJ...546L..49S 2001ApJ...546L..49S);
8 = Ladd et al. (1994ApJ...433..117L 1994ApJ...433..117L);
9 = Lefloch et al. (1998A&A...334..269L 1998A&A...334..269L);
10 = Sandell et al. (1991ApJ...376L..17S 1991ApJ...376L..17S);
11 = Bachiller et al. (1991A&A...251..639B 1991A&A...251..639B);
12 = Mathews & Wilson (2002ApJ...574..822M 2002ApJ...574..822M);
13 = McGaughrean et al. (1994ApJ...436L.189M 1994ApJ...436L.189M);
14 = Eisloeffel et al. (2003ApJ...595..259E 2003ApJ...595..259E);
15 = Motte & Andre (2001A&A...365..440M 2001A&A...365..440M).
Note (3): Presence of MIPS source is from the c2d database (Stapelfeldt
et al. 2005, in preparation), as follows:
Y = present;
N = not present;
N/A = regions of Perseus not yet available, an IRAS source (within 1')
is indicated if appropriate.
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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- 4 A4 --- --- [Bolo]
6- 8 I3 --- [EYG2006] Source identification
10- 13 F4.2 Jy F40 ? 40" diameter aperture flux density (1)
15- 18 F4.2 Jy e_F40 ? The 1σ uncertainty in F40
20- 23 F4.2 Jy F80 ? 80" diameter aperture flux density (1)
25- 28 F4.2 Jy e_F80 ? The 1σ uncertainty in F80
30- 33 F4.2 Jy F120 ? 120" diameter aperture flux density (1)
35- 38 F4.2 Jy e_F120 ? The 1σ uncertainty in F120
40- 45 F6.3 Jy Ftot Total integrated flux density (1)
47- 51 F5.3 Jy e_Ftot The 1σ uncertainty in Ftot
53- 57 F5.2 solMass Mass Total mass (2)
59- 62 F4.2 solMass e_Mass The 1σ uncertainty Mass (3)
64- 66 I3 mag AV Peak V band extinction (4)
68- 70 I3 arcsec MinAxis Minor axis FWHM of Gaussian fit
72- 74 F3.1 arcsec e_MinAxis The 1σ uncertainty in MinAxis (5)
76- 78 I3 arcsec MajAxis Major axis FWHM of Gaussian fit
80- 82 F3.1 arcsec e_MajAxis The 1σ uncertainty in MajAxis (5)
84- 86 I3 deg PA [-90,+90] Position angle of Gaussian fit (6)
88- 89 I2 deg e_PA Uncertainty in PA (5)
91- 93 E3.1 cm-3 ? Mean particle density (7)
95-122 A28 --- Morph Morphology description (8)
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Note (1): Integrated flux densities are measured assuming a sky value of zero,
and corrected for the gaussian beam so that a point source has the
same integrated flux density in all apertures with diameter greater
than the beam. No integrated flux density is given if the distance
to the nearest neighboring source is smaller than the aperture
diameter.
Note (2): Masses are calculated according to
M=[d2Sν]/[Bν(TD)κν] from the total flux
density assuming a single dust temperature of TD=10K and a dust
opacity at 1.1mm of κ1.1mm=0.0114cm2/g.
Note (3): Uncertainties for masses are from photometry only, and do not include
uncertainties from κ, T_D, or d, which can be up to a factor of
a few or more.
Note (4): Calculated from the peak flux density as in Section 4.2.
Note (5): Uncertainties for the FWHM and PA are formal fitting errors from the
elliptical gaussian fit; additional uncertainties of 10-15% apply to
the FWHM, and ∼5 degrees to the PA (determined from simulations).
Note (6): Measured east of north of the major axis.
Note (7): As calculated from the total mass and the deconvolved
average FWHM size.
Note (8): The morphology keyword(s) given indicates whether the source is
multiple (within 3' of another source), extended (major axis FW
at 2σ>1'), elongated (axis ratio at 4σ>1.2), round
(axis ratio at 4σ<1.2), or weak (peak flux densities less
than 5 times the RMS/pixel in the unfiltered map).
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History:
From electronic version of the journal
References:
Young et al. Paper II. 2006ApJ...644..326Y 2006ApJ...644..326Y
Enoch et al. Paper III. 2007ApJ...666..982E 2007ApJ...666..982E
Enoch et al. Paper IV. 2009ApJ...692..973E 2009ApJ...692..973E Cat. J/ApJ/692/973
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 27-Feb-2007