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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 (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:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: tableb1.dat
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
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)
Byte-by-byte Description of file: tableb3.dat
Bytes Format Units Label Explanations
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)
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 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.
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)). Acknowledgements: Pablo Riviere-Marichalar, priviere(at)sciops.esa.int
(End) Patricia Vannier [CDS] 04-Aug-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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