J/MNRAS/395/855 Spectroscopy (310-1040nm) of HH 202 (Mesa-Delgado+, 2009)
Properties of the ionized gas in HH 202.
II. Results from echelle spectrophotometry with ultraviolet visual echelle
spectrograph.
Mesa-Delgado A., Esteban C., Garcia-Rojas J., Luridiana V., Bautista M.,
Rodriguez M., Lopez-Martin L., Peimbert M.
<Mon. Not. R. Astron. Soc., 395, 855-876 (2009)>
=2009MNRAS.395..855M 2009MNRAS.395..855M
ADC_Keywords: Molecular clouds ; Ultraviolet ; Spectroscopy
Keywords: ISM: abundances - dust, extinction - ISM: Herbig-Haro objects -
ISM: individual: Orion Nebula - ISM: individual: HH 202
Abstract:
We present results of deep echelle spectrophotometry of the brightest
knot of the Herbig-Haro object HH 202 in the Orion Nebula - HH 202-S -
using the Ultraviolet Visual Echelle Spectrograph in the spectral
range from 3100 to 10400Å The high spectral resolution of the
observations has permitted to separate the component associated with
the ambient gas from that associated with the gas flow. We derive
electron densities and temperatures from different diagnostics for
both components, as well as the chemical abundances of several ions
and elements from collisionally excited lines, including the first
determinations of Ca+ and Cr+ abundances in the Orion Nebula. We
also calculate the He+, C2+, O+ and O2+ abundances from
recombination lines.
Description:
HH 202 was observed on 2003 March 30 at Cerro Paranal Observatory,
Chile, using the UT2 (Kueyen) of the Very Large Telescope (VLT) with
the Ultraviolet Visual Echelle Spectrograph (UVES).
Objects:
-------------------------------------------
RA (2000) DE Designation(s)
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05 35 11.5 -05 22 46 HH 202 = HH 202
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 75 382 Identifications, reddening-corrected line ratios
[I(Hbeta)=100] for an area of 1.5x2.5arcsec2
and heliocentric velocities for the nebular and
shock components
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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- 8 F8.2 0.1nm lambda0 [3187/10371] Laboratory wavelength
10- 17 A8 --- Ion Ion (1)
19- 25 A7 --- Mult Multiplet
27- 32 F6.3 --- f(lambda) ? Value of the extinction curve adopted
(Blagrave et al., 2007ApJ...655..299B 2007ApJ...655..299B)
34- 35 I2 km/s HVn ? Nebular component heliocentric velocity (2)
37- 43 F7.3 --- In ? Nebular component dereddened flux line
ratio (Hβ=100)
44 A1 --- u_In Uncertainty flag on In (Error larger than 40%)
46- 47 I2 % e_In ? Error on In
49- 51 I3 km/s HVs ? Shock component heliocentric velocity (2)
53- 59 F7.3 --- Is ? Shock component dereddened flux line
ratio (Hβ=100)
60 A1 --- u_Is Uncertainty flag on Is (Error larger than 40%)
62- 63 I2 % e_Is ? Error on Is
65- 70 F6.3 --- Is/In ? Shock to nebular flux ratio
72- 75 A4 --- Notes Notes about individual lines (4)
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Note (1): Dubious identifications are marked with "?".
Note (2): The typical error is 1-2km/s.
Note (4): Notes as follows:
g = Line blended with another line and deblended via Gaussian fitting
h = Contaminated by 'ghost'
i = Contaminated by telluric emissions and not deblended
j = Deblended from telluric emissions
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History:
From electronic version of the journal
References:
Mesa-Delgado et al., Paper I 2009MNRAS.394..693M 2009MNRAS.394..693M
(End) Patricia Vannier [CDS] 29-Sep-2009