J/A+A/594/A59 Far-IR lines in YSOs Herschel-PACS (Riviere-Marichalar+, 2016)
Herschel-PACS observations of far-IR lines in YSOs.
I: [OI] and H2O at 63 microns.
Riviere-Marichalar P., Merin B., Kamp I., Eiroa C., Montesinos B.
<Astron. Astrophys. 594, A59 (2016)>
=2016A&A...594A..59R 2016A&A...594A..59R (SIMBAD/NED BibCode)
ADC_Keywords: Infrared sources ; YSOs
Keywords: astrochemistry - circumstellar matter - stars: evolution -
stars: protostars
Abstract:
Gas plays a major role in the dynamical evolution of young stellar
objects (YSOs). Its interaction with the dust is the key to our
understanding planet formation later on in the protoplanetary disc
stage. Studying the gas content is therefore a crucial step towards
understanding YSO and planet formation. Such a study can be made
through spectroscopic observations of emission lines in the
far-infrared, where some of the most important gas coolants emit, such
as the [OI] 3P1-3P2 transition at 63.18 microns. We provide a
compilation of observations of far-IR lines in 362 young stellar
objects covering all evolutionary stages, from Class 0 to Class III
with debris discs. In the present paper we focus on [OI] and o-H2O
emission at 63 microns. We have retrieved all the available
Herschel-PACS spectroscopic observations at 63 microns that used the
dominant observing mode, the chop-nod technique. We provide
measurements of line fluxes for the [OI] 3P1-3P2 and o-H2O
808-717 transitions at 63 microns computed using different
methods. Taking advantage of the PACS IFU, we check for spatially
extended emission and further study the presence of multiple dynamical
components in line emission. The final compilation consists of line
and continuum fluxes at 63 microns for a total of 362 young stellar
objects (YSOs). We detected [OI] line emission at 63 microns in 194
sources out of 362, and line absorption in another five sources.
o-H2O was detected in 42 sources. We find evidence of extended [OI]
emission in 77 sources, and detect 3sigma residual emission in 71 of
them. The number of sources showing extended emission decays from
Class 0 to Class II. We also looked for different components
contributing to the line emission, and found evidence for multiple
components in 30 sources. We explored correlations between line
emission and continuum emission and find a clear correlation between
WISE fluxes from 4.6 to 22 microns and [OI] line emission. We conclude
that the observed emission is typically a combination of disc/envelope
and jet emission.
Description:
Continuum and line fluxes for a sample of 362 young stellar objects.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 75 362 Sample description, including name, position,
spectral type, source class and cluster
tableb2.dat 101 432 Line and continuum fluxes from central spaxel
tableb3.dat 80 230 [OI] line flux from central spaxel,
central 3x3 spaxel and integrated IFU
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 26 A26 --- Name Source name (G2)
28- 38 F11.7 deg RAdeg Source right ascension (J2000.0)
40- 50 F11.7 deg DEdeg Source declination (J2000.0)
51- 52 A2 --- SpType Source spectral type
54- 60 A7 --- DiscType Source classification
62- 75 A14 --- Assoc Source association, if any
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Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 26 A26 --- Name Source name (G2)
28- 38 F11.7 deg RAdeg Source right ascension (J2000.0) (G2)
39- 49 F11.7 deg DEdeg Source declination (J2000.0) (G2)
50- 59 I10 --- OBSID Herschel OBSID for this observation
61- 66 I6 10-18W/m2 FOI OI line flux at 63.185 microns
68- 71 I4 10-18W/m2 e_FOI ?=0 OI line flux error at 63.185 microns
(an error of 0.0 is given for upper limits)
73 A1 --- l_FOI [0/1] Limit flag on OI line flux (G1)
75- 78 I4 10-18W/m2 FH2O o-H2O line flux at 63.323 microns
80- 82 I3 10-18W/m2 e_FH2O ?=0 o-H2O line flux error at 63.323 microns
(an error of 0.0 is given for upper limits)
84 A1 --- l_FH2O [0/1] Limit flag on o-H2O line flux (G1)
86- 93 F8.3 Jy F63 Continuum flux at 63 microns
95- 99 F5.2 Jy e_F63 ?=0 Error in continuum flux at 63 microns
(an error of 0.0 is given for upper limits)
101 A1 --- l_F63 [0/1] Limit flag on continuum at 63 microns
flux (G1)
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 26 A26 --- Name Source name
27- 36 I10 --- OBSID Herschel OBSID for this observation
38- 42 I5 10-18W/m2 FOI OI line flux at 63.185 microns
44- 47 I4 10-18W/m2 e_FOI ?=0 OI line flux error at 63.185 microns
(an error of 0.0 is given for upper limits)
49 A1 --- l_FOI [0/1] Limit flag on OI line flux (G1)
51- 56 I6 10-18W/m2 FOI3x3 OI line flux at 63.185 microns from
co-adding the central 3x3 spaxel
58- 62 I5 10-18W/m2 e_FOI3x3 ?=0 OI line flux error at 63.185 microns
from co-adding the central 3x3 spaxel
(an error of 0.0 is given for upper limits)
64 A1 --- l_FOI3x3 [0/1] Limit flag on OI line flux from
central 3x3 spaxel (G1)
66- 72 I7 10-18W/m2 FOI5x5 OI line flux at 63.185 microns from
co-adding 5x5 spaxel in the IFU
74- 78 I5 10-18W/m2 e_FOI5x5 ?=0 OI line flux error at 63.185 microns
from co-adding 5x5 spaxel in the IFU
(an error of 0.0 is given for upper limits)
80 A1 --- l_FOI5x5 [0/1] Limit flag on OI line flux from
co-adding 5x5 spaxel in the IFU (G1)
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Global notes:
Note (G1): Flag as follows:
0 = upper limit
1 = detection
Note (G2): In tables, B1 and B2, V833 Ori was very likely a misprint
for V883 Ori; corrected by CDS.
In tables, B1 and B2, Oph 01 is SSTc2d J162659.1-243503; addendum
from the author; ambiguous ID changed by CDS.
In table B2, coordinates of HD 9672, tau Ceti, HD 38206,
HR 1998, PDS 27, AS 205, HIP 79439 and RNO 90 have been corrected
to match those of table B1.
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History:
13-Oct-2016: Insert into VizieR
06-Jul-2018: Tables B1 and B2 corrected for the misprints in Name and
coordinates (see Note (G2)).
17-Jul-2018: Table B1 and B2 corrected: Oph 01 is SSTc2d J162659.1-243503,
in SIMBAD. Many thanks to Pablo Riviere-Marichalar for the update.
Acknowledgements:
Pablo Riviere-Marichalar, pablo.riviere (at) csic.es
(but soon Spanish National Astronomical Observatory).
(End) Patricia Vannier [CDS] 04-Aug-2016