J/A+A/565/A64 Molecular ions in L1157-B1 (Podio+, 2014)
Molecular ions in the protostellar shock L1157-B1.
Podio L., Lefloch B., Ceccarelli C., Codella C., Bachiller R.
<Astron. Astrophys. 565, A64 (2014)>
=2014A&A...565A..64P 2014A&A...565A..64P
ADC_Keywords: Molecular clouds ; Interstellar medium ; Spectroscopy
Keywords: stars: formation - ISM: jets and outflows - ISM: molecules -
ISM: abundances - astrochemistry
Abstract:
In this work, we perform a complete census of molecular ions with an
abundance larger than ∼10-10 in the protostellar shock L1157-B1.
This allows us to study the ionization structure and chemistry of the
shock.
An unbiased high-sensitivity survey of L1157-B1 performed with the
IRAM-30m and Herschel/HIFI as part of the CHESS and ASAI large
programs allows searching for molecular ions emission. Then, by means
of a radiative transfer code in the Large Velocity Gradient
approximation, the gas physical conditions and fractional abundances
of molecular ions are derived. The latter are compared with estimates
of steady-state abundances in the cloud and their evolution in the
shock calculated with the chemical model Astrochem.
Description:
The ascii files contain the line spectra shown in Figure 2 of the paper.
The spectra are obtained with the IRAM-30m and Herschel/HIFI.
The IRAM-30m data are part of the ASAI Large Programme.
The Herschel/HIFI data are from the Guaranteed Time Key Project CHESS.
Objects:
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RA (2000) DE Designation(s)
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20 39 10.2 +68 01 10.5 L1157-B1 = [DE95] LDN 1157 B1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 117 26 *Properties of the detected lines from molecular ions
sp/* . 17 Individual line spectra shown in Figure 2
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Note on table1.dat: For each species we report a 3σ upper limit for the
first non-detected transition covered by our observations
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Mol Molecule: HCO+, HCS+, HOCO+,
H13CO+, N2H+, or SO+
11 A1 --- n_Mol [bcd] Note on the molecule (1)
13- 39 A27 --- Trans Transition
41- 42 A2 --- n_Trans [ng *] Note on Trans (2)
44- 52 F9.2 MHz nu0 [85347/713343] Frequency of the transition (3)
54- 56 I3 K E1 [4/154] Upper energy level
58- 59 I2 arcsec HPBW [7/40] Telescope Half Power Beam Width
61- 62 I2 mK rms [1/35] rms noise
64- 67 F4.1 km/s Vpeak ?=- Peak velocity
69- 71 F3.1 km/s e_Vpeak [0.1/1.5]? rms uncertainty on Vpeak
73- 75 F3.1 km/s FWHM [1.8/6.9]?=- Full width at half maximum
77- 79 F3.1 km/s e_FWHM [0.2/2]?=- rms uncertainty on FWHM
81- 84 I4 mK Tpeak [8/1095]?=- Peak temperature
(in main-beam temperature unit)
86- 87 I2 mK e_Tpeak [1/14]? rms uncertainty on Tpeak
89- 90 A2 --- l_TmbdV [≤ ] Limit flag on TmbdV
91- 94 F4.2 K.km/s TmbdV [0.03/7.4] Integrated intensity
96- 99 F4.2 K.km/s e_TmbdV ? rms uncertainty on TmbdV
101-117 A17 --- FileName Name of the spectrum file in subdirectory sp
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Note (1): Note on Species as follows:
b = the line properties quoted for the N2H+ 1-0 and 3-2 transitions
refer to the brightest of their 15 and 45 hyperfine components, i.e.
the F1, F=2,3-1,2 and the F1, F=4,5-3,4 components, respectively.
The line intensity is integrated over all the components.
c = the transitions of HOCO+ are characterized by the quantum numbers J,
which is the total angular momentum, and K-1, K1, which are the angular
momenta around the molecule's symmetry axis.
d = SO+ is a reactive radical with 2Π_1/2 ground state, whose
spin-doubled rotational transitions, characterized by the quantum
number J, are further split by {LAMBDA}-type doubling.
Note (2): Notes as follows:
* = All transitions are observed with IRAM-30m/FTS, except those indicated
by the * which are observed with Herschel/HIFI.
ng = A gaussian fit is applied to estimate the line properties for most of
the transitions. When the line profile is non-gaussian (ng) the line
intensity is obtained by integrating the area below the profile.
Note (3): Frequencies are from the JPL molecular database (Pickett et al.,
1998, J. Quant. Spec. Radiat. Transf., 60, 883), and from the CDMS database
(Muller et al., 2001A&A...370L..49M 2001A&A...370L..49M) for N2H+.
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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3- 18 F16.12 km/s Vlsr [-53/53] LSR velocity
19- 29 E11.5 K Ta Line intensity in antenna temperature
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Acknowledgements:
Linda Podio, lpodio(at)arcetri.astro.it
(End) Patricia Vannier [CDS] 04-Mar-2014