J/ApJ/707/103 Observation of Ser FIRS 1 at 230GHz (Enoch+, 2009)
Disk and envelope structure in class 0 protostars.
I. The resolved massive disk in Serpens FIRS 1.
Enoch M.L., Corder S., Dunham M.M., Duchene G.
<Astrophys. J., 707, 103-113 (2009)>
=2009ApJ...707..103E 2009ApJ...707..103E
ADC_Keywords: Radio continuum ; Interferometry ; Molecular clouds ; YSOs ;
Infrared sources ; Interstellar medium ; Millimetric/submm sources
Keywords: infrared: ISM - ISM: individual (Serpens) - stars: formation -
submillimeter
Abstract:
We present the first results of a program to characterize the disk and
envelope structure of typical Class 0 protostars in nearby low-mass
star-forming regions. We use Spitzer Infrared Spectrograph (IRS)
mid-infrared spectra, high-resolution Combined Array for Research in
Millimeter-wave Astronomy (CARMA) 230GHz continuum imaging, and
two-dimensional radiative transfer models to constrain the envelope
structure, as well as the size and mass of the circumprotostellar disk
in Serpens FIRS 1. The primary envelope parameters (centrifugal
radius, outer radius, outflow opening angle, and inclination) are well
constrained by the spectral energy distribution (SED), including
Spitzer IRAC and MIPS photometry, IRS spectra, and 1.1mm Bolocam
photometry. These together with the excellent uv-coverage
(4.5-500kλ) of multiple antenna configurations with CARMA allow
for a robust separation of the envelope and a resolved disk. The SED
of Serpens FIRS 1 is best fit by an envelope with the density profile
of a rotating, collapsing spheroid with an inner (centrifugal) radius
of approximately 600AU, and the millimeter data by a large resolved
disk with Mdisk∼1.0M☉ and Rdisk∼300AU.
Description:
Mid-infrared spectra were obtained with the IRS on the Spitzer Space
Telescope during 2007 October 5 with the Low Res 7.4-14.5um (SL1;
R∼100), Hi Res 9.9-19.6um (SH; R∼600), and Hi Res 18.7-37.2um (LH;
R∼600) modules. See Figure 2.
Continuum observations at ν=230GHz (λ=1.3mm) were completed
with the CARMA, a 15 element interferometer consisting of nine 6.1m
and six 10.4m antennas. Data were obtained in the B array (100-1000m
baselines), C array (30-350m), D array (11-150m), and E array (8-66m)
configurations between 2007 October 24 and 2008 December 31. These
data were combined to provide uv-coverage from 4.5 to 500kλ.
Objects:
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RA (2000) DE Designation(s)
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18 29 49.6 +01 15 22 NAME SER FIRS 1 = NAME SERPENS SMM 1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 17 99 CARMA 230GHz visibilities
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See also:
J/ApJ/692/973 : Protostars in Perseus, Serpens and Ophiuchus (Enoch+, 2009)
J/ApJ/691/672 : Spectrocopy of YSOs in Serpens molecular cloud (Oliveira+
2009)
J/ApJ/684/1240 : Prestellar cores in Perseus, Serpens and Ophiuchus (Enoch+,
2008)
J/ApJ/663/1149 : Spitzer survey of Serpens YSO population (Harvey+, 2007)
J/ApJ/669/493 : Spitzer/Chandra YSOs in Serpens cloud core (Winston+, 2007)
J/A+A/463/275 : Chandra obs. of Serpens star-forming region (Giardino+, 2007)
J/A+A/421/623 : ISOCAM survey of YSOs in Serpens Cloud Core (Kaas+, 2004)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 --- uv-dist The uv-distance in units of kλ; 1.3m
8- 12 F5.3 Jy Flux The 230GHz flux density (1)
14- 17 F4.2 Jy e_Flux Uncertainty in Flux
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Note (1): The amplitude bias, or expected value for zero signal, has been
subtracted from the data.
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History:
From electronic version of the journal
References:
Enoch et al. Paper II. 2011ApJS..195...21E 2011ApJS..195...21E
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 29-Dec-2011