J/A+A/617/A27 Kinematics of dense gas in L1495 filament (Punanova+, 2018)
Kinematics of dense gas in the L1495 filament.
Punanova A., Caselli P., Pineda J. E., Pon A., Tafalla M., Hacar A.,
Bizzocchi L.
<Astron. Astrophys. 617, A27 (2018)>
=2018A&A...617A..27P 2018A&A...617A..27P (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Molecular clouds ;
Spectra, millimetric/submm
Keywords: stars: formation - ISM: kinematics and dynamics - ISM: clouds -
ISM: molecules - ISM: individual objects: L1495 - radio lines: ISM
Abstract:
Nitrogen bearing species, such as NH3, N2H+, and their
deuterated isotopolo- gues show enhanced abundances in CO-depleted
gas, and thus are perfect tracers of dense and cold gas in
star-forming regions. The Taurus molecular cloud contains the long
L1495 filament providing an excellent opportunity to study the process
of star formation in filamentary environments.
We study the kinematics of the dense gas of starless and protostellar
cores traced by the N2D+(2-1), N2H+(1-0), DCO+(2-1), and
H13CO+(1-0) transitions along the L1495 filament and the kinematic
links between the cores and surrounding molecular cloud.
We measured velocity dispersions, local and total velocity gradients,
and estimate the specific angular momenta of 13 dense cores in the
four transitions using on-the-fly observations with the IRAM 30-m
antenna. To study a possible connection to the filament gas, we used
the C18O(1-0) observations.
Description:
We present here the hyperfine structure fit results (see Section 3 of
the paper for details) of the N2D+(2-1), N2H+(1-0),
DCO+(2-1), and H13CO+(1-0) lines mapped across 13 dense cores in
L1495 with the IRAM 30 m antenna. They are maps of integrated
intensity, velocity dispersion, central velocity and opacity. For the
velocity dispersion and central velocity there are also uncertainty
maps; for the integrated intensity one can calculate the uncertainty
from the rms given in Tables A3 and A4 of the paper. There are two
sets of the maps: convoled to the natural beam size (all parameters)
and those convolved to the largest beam (integrated intensity and
central velocities). The dense cores are named by numbers following
Hacar et al. (2013A&A...554A..55H 2013A&A...554A..55H, Cat. J/A+A/554/A55).
Due to the limit of 8 characters on the file names we code the file
names as follows:
NAAMM_PP.fit where N stands for native resolution (or S for smoothed)
AA for the object name (e.g. 02 or 16i, [HTK2013] NN in Simbad)
MM is a code for the line:
ND = N2D+(2-1)
NH = N2H+(1-0);
DC = DCO+(2-1)
HC = H13CO+(1-0).
_ splits the two parts of the name
PP stands for the parameter:
II = integrated intensity;
D_ = velocity dispersion;
V_ = central velocity;
T_ = opacity;
'e' instead of '_' is for the uncertainty maps.
Example: N02NH_Te.fit - is the native resolution Core 2 N2H+(1-0)
opacity uncertainty map.
Objects:
-----------------------------------------
RA (2000) DE Designation(s)
-----------------------------------------
04 18.1 +27 37 L1495 = LDN 1495
-----------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 128 433 List of fits maps
fits/* . 433 Individual fits maps
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See also:
J/A+A/554/A55 : C18O(1-0) and N2H+(1-0) in L1495/B213 (Hacar+, 2013)
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 21 I2 --- Nx Number of pixels along X-axis
23- 24 I2 --- Ny Number of pixels along Y-axis
26- 27 I2 Kibyte size Size of FITS file
29- 40 A12 --- FileName Name of FITS file, in subdirectory fits
42-128 A87 --- Title Title of the FITS file
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Acknowledgements:
Anna Punanova, punanovaanna(at)gmail.com
(End) Patricia Vannier [CDS] 20-Aug-2018