2018A&A...610A...9G


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.16CEST10:54:27

2018A&A...610A...9G - Astronomy and Astrophysics, volume 610A, 9-9 (2018/2-1)

The first frost in the Pipe Nebula.

GOTO M., BAILEY J.D., HOCUK S., CASELLI P., ESPLUGUES G.B., CAZAUX S. and SPAANS M.

Abstract (from CDS):

Context. Spectroscopic studies of ices in nearby star-forming regions indicate that ice mantles form on dust grains in two distinct steps, starting with polar ice formation (H2O rich) and switching to apolar ice (CO rich).
Aims. We test how well the picture applies to more diffuse and quiescent clouds where the formation of the first layers of ice mantles can be witnessed.
Methods. Medium-resolution near-infrared spectra are obtained toward background field stars behind the Pipe Nebula.
Results. The water ice absorption is positively detected at 3.0µm in seven lines of sight out of 21 sources for which observed spectra are successfully reduced. The peak optical depth of the water ice is significantly lower than those in Taurus with the same AV. The source with the highest water-ice optical depth shows CO ice absorption at 4.7µm as well. The fractional abundance of CO ice with respect to water ice is 16–6+7%, and about half as much as the values typically seen in low-mass star-forming regions.
Conclusions. A small fractional abundance of CO ice is consistent with some of the existing simulations. Observations of CO2 ice in the early diffuse phase of a cloud play a decisive role in understanding the switching mechanism between polar and apolar ice formation.

Abstract Copyright: © ESO, 2018

Journal keyword(s): astrochemistry - ISM: clouds - ISM: individual objects: the Pipe Nebula - ISM: molecules - infrared: ISM - solid state: volatile

VizieR on-line data: <Available at CDS (J/A+A/610/A9): list.dat pipe1.dat pipe2.dat pipe6.dat pipe7.dat pipe8.dat pipe14.dat pipe15.dat>

Simbad objects: 23

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Number of rows : 23

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3679 0
2 LDN 1595 DNe 05 27.7 +06 32           ~ 7 0
3 NAME Coalsack Nebula DNe 12 31 19 -63 44.6           ~ 246 0
4 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 702 1
5 NAME Lup Cloud SFR 16 03 -38.1           ~ 558 0
6 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1168 1
7 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3156 1
8 LDN 1746 DNe 17 11.3 -27 22           ~ 117 0
9 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 286 1
10 2MASS J17280535-2627053 * 17 28 05.3646269731 -26 27 05.310829526           M3III 1 0
11 2MASS J17281419-2620522 * 17 28 14.1983255639 -26 20 52.227506456           M5.5III 1 0
12 2MASS J17281466-2627361 * 17 28 14.6577127493 -26 27 36.258838880           M5.5III 1 0
13 2MASS J17282887-2617337 * 17 28 28.8802412119 -26 17 33.677625085           M6III 1 0
14 2MASS J17282929-2620358 * 17 28 29.3030619782 -26 20 35.938747803           M5.5III 1 0
15 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
16 2MASS J17312249-2629585 * 17 31 22.4955280289 -26 29 58.599241945           M6III 1 0
17 2MASS J17312818-2631268 * 17 31 28.1884664122 -26 31 26.867498024           M5.5III 1 0
18 NAME Galactic Center gam 17 45 39.60213 -29 00 22.0000           ~ 12108 0
19 LDN 429 DNe 18 16 44 -08 18.9           ~ 34 0
20 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 967 2
21 CK 2 Y*O 18 30 00.618 +01 15 20.12           K5-M0III 52 0
22 IC 5146 OpC 21 53 24 +47 16.0           ~ 400 2
23 NAME Galactic Bulge reg ~ ~           ~ 3564 0

    Equat.    Gal    SGal    Ecl

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2021.04.16-10:54:27

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