Parameter | Core 1 | Core 2 | Core 3 | Core 4 | Core 5 |
Galactic longitude (2000) | 123.388 | 123.511 | 123.559 | 123.687 | 123.690 |
Galactic latitude (2000) | +24.928 | +24.915 | +24.856 | +24.894 | +24.931 |
Right ascension (2000) | 01![]() ![]() ![]() |
01![]() ![]() ![]() |
01![]() ![]() ![]() |
01![]() ![]() ![]() |
02![]() ![]() ![]() |
Declination (2000) | +87![]() ![]() ![]() |
+87![]() ![]() ![]() |
+87![]() ![]() ![]() |
+87![]() ![]() ![]() |
+87![]() ![]() ![]() |
Distance (pc) | 150 | 150 | 150 | 150 | 150 |
Radius (pc) | 0.023 | 0.035 | 0.032 | 0.035 | 0.034 |
FWHM (pc) | 0.023 | 0.039 | 0.027 | 0.042 | 0.038 |
![]() |
<0.18 | <0.18 | <0.18 | <0.18 | <0.18 |
![]() |
4.26 ![]() |
10.19 ![]() |
7.56 ![]() |
7.63 ![]() |
5.44 ![]() |
![]() |
6.74 ![]() |
16.77 ![]() |
13.10 ![]() |
15.35 ![]() |
13.26 ![]() |
![]() |
3.61 ![]() |
8.98 ![]() |
7.27 ![]() |
9.05 ![]() |
8.50 ![]() |
![]() |
1.72 ![]() |
4.33 ![]() |
3.50 ![]() |
4.53 ![]() |
4.40 ![]() |
Temperature (K) | 12 ![]() |
12 ![]() |
12 ![]() |
11 ![]() |
10 ![]() |
N(H2)
![]() ![]() |
6 ![]() |
7 ![]() |
9 ![]() |
13 ![]() |
13 ![]() |
Mass (![]() |
0.1 | 0.3 | 0.3 | 0.4 | 0.5 |
n(H2)
![]() |
![]() ![]() |
![]() ![]() |
![]() ![]() |
![]() ![]() |
![]() ![]() |
![]() ![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
Notes. The Galactic latitude and longitude, as well as
right ascension and declination, are listed, along with the assumed
distance. The radius
of each core was measured by taking the column density map in Fig. 1 and
measuring the equivalent radius of the contour that encircled a column
density of
cm-2, and this radius is given in pc.
The full-width at half maximum (FWHM) is the geometric mean FWHM measured
on the peak of each source.
The integrated flux density within this contour at each of the Herschel
wavelengths is listed in Jy. The absolute uncertainty in the flux densities
is
15%. As described in the text, a temperature, peak column density
and mass were derived, and these are also listed. The uncertainty in the
masses could be as high as a factor of 2. A mean volume density is given,
assuming each core is spherical, within the given radius. Finally, a virial
mass for each core is estimated using CO and HCO+ linewidths.
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