J/A+A/631/A30 Emission line flux densities for 12 YSOs (Postel+, 2019)
Infrared and sub-mm observations of outbursting young stars with Herschel
and Spitzer.
Postel A., Audard M., Vorobyov E., Dionatos O., Rab C., Guedel M.
<Astron. Astrophys. 631, A30 (2019)>
=2019A&A...631A..30P 2019A&A...631A..30P (SIMBAD/NED BibCode)
ADC_Keywords: Spectroscopy ; Millimetric/submm sources ; Protostars ;
Stars, pre-main sequence ; YSOs
Keywords: stars: formation - stars: protostars - stars: pre-main sequence -
protoplanetary disks - accretion, accretion disks - infrared: stars
Abstract:
Episodic accretion plays an important role in the evolution of young
stars. Although it has been under investigation for a long time, the
origin of such episodic accretion events is not yet understood. We
investigate the dust and gas emission of a sample of young outbursting
sources in the infrared to get a better understanding of their
properties and circumstellar material, and we use the results in a
further work to model the objects. We used Herschel data, from our PI
program of 12 objects and complemented with archival observations to
obtain the spectral energy distributions (SEDs) and spectra of our
targets. We report here the main characteristics of our sample,
focussing on the SED properties and on the gas emission lines detected
in the PACS and SPIRE spectra. The SEDs of our sample show the
diversity of the outbursting sources, with several targets showing
strong emission in the far-infrared from the embedded objects. Most of
our targets reside in a complex environment, which we discuss in
detail. We detected several atomic and molecular lines, in particular
rotational CO emission from several transitions from J=38-37 to J=4-3.
We constructed rotational diagrams for the CO lines, and derived in
three domains of assumed local thermodynamic equilibrium (LTE)
temperatures and column densities, ranging mainly between 0-100K
and 400-500K. We confirm correlation in our sample between intense
CO J=16-15 emission and the column density of the warm domain of CO,
N(warm). We notice a strong increase in luminosity of HH 381 IRS and a
weaker increase for PP 13 S, which shows the beginning of an outburst.
Description:
Emission line flux densities of Herschel data for 12 YSOs. Spectra of
the following objects have been analyzed:
Haro 5a IRS, HH 354 IRS, HH 381 IRS, Parsamian 21, PP 13 S, Re 50 N
IRS (=HBC 494), V346 Nor, V733 Cep, V883 Ori, EX Lup, and V1647 Ori We
provide errors for the flux densities and upper limits for most lines.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 56 12 List of studied stars
fluxes.dat 282 97 Line fluxes for the YSOs
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Star name
15- 16 I2 h RAh Simbad Right ascension (J2000)
18- 19 I2 min RAm Simbad Right ascension (J2000)
21- 25 F5.2 s RAs Simbad Right ascension (J2000)
27 A1 --- DE- Declination sign (J2000)
28- 29 I2 deg DEd Declination (J2000)
31- 32 I2 arcmin DEm Declination (J2000)
34- 37 F4.1 arcsec DEs Declination (J2000)
39- 43 A5 --- Label Label used in table1
45- 56 A12 --- SName Simbad name
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Byte-by-byte Description of file: fluxes.dat
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Bytes Format Units Label Explanations
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1- 13 F13.9 um lambda Wavelength of the observed line
15- 20 A6 --- Mol/Ato Molecule or Atom
22- 46 A25 --- Trans Energy transition of the line
48 A1 --- l_BRAN Limit flag on BRAN
49- 56 E8.3 W/m2 BRAN ?=- Bran 76 flux density of line or
upper limit
57 A1 --- n_BRAN [*] Note on BRAN (1)
59- 65 E7.2 W/m2 e_BRAN ?=- Error on BRAN
67 A1 --- l_EXLup Limit flag on EXLup
68- 75 E8.3 W/m2 EXLup ?=- EX Lup flux density of line or upper limit
76 A1 --- n_EXLup [*] Note on EXLup (1)
78- 84 E7.2 W/m2 e_EXLup ?=- Error on EXLup
86 A1 --- l_Haro Limit flag on Haro
87- 95 E9.3 W/m2 Haro ?=- Haro 5a IRS flux density of line or
upper limit
96 A1 --- n_Haro [*] Note on Haro (1)
97-103 E7.2 W/m2 e_Haro ?=- Error on Haro
105 A1 --- l_HH354 Limit flag on HH354
106-114 E9.3 W/m2 HH354 ?=- HH354 IRS flux density of line or
upper limit
115 A1 --- n_HH354 [*] Note on HH354 (1)
117-123 E7.2 W/m2 e_HH354 ?=- Error on HH354
125 A1 --- l_HH381 Limit flag on HH381
126-134 E9.3 W/m2 HH381 ?=- HH381 IRS flux density of line or
upper limit
135 A1 --- n_HH381 [*] Note on HH381 (1)
137-143 E7.2 W/m2 e_HH381 ?=- Error on HH381
145 A1 --- l_Pars Limit flag on Pars
146-153 E8.3 W/m2 Pars ?=- Parsamian 21 flux density of line or
upper limit
154 A1 --- n_Pars [*] Note on Pars (1)
156-162 E7.2 W/m2 e_Pars ?=- Error on Pars
164 A1 --- l_PP13 Limit flag on PP13
165-173 E9.3 W/m2 PP13 ?=- PP 13 S flux density of line or
upper limit
174 A1 --- n_PP13 [*] Note on PP13 (1)
176-182 E7.2 W/m2 e_PP13 ?=- Error on PP13
184 A1 --- l_Re50 Limit flag on Re50
185-193 E9.4 W/m2 Re50 ?=- Re 50 N IRS (HBC 494) flux density of line
or upper limit
194 A1 --- n_Re50 [*] Note on Re50 (1)
196-202 E7.2 W/m2 e_Re50 ?=- Error on Re50
204 A1 --- l_V346 Limit flag on V346
205-213 E9.3 W/m2 V346 ?=- V346 Nor flux density of line or
upper limit
214 A1 --- n_V346 [*] Note on V346 (1)
216-222 E7.2 W/m2 e_V346 ?=- Error on V346
224 A1 --- l_V733 Limit flag on V733
225-233 E9.3 W/m2 V733 ?=- V733 Cep flux density of line or
upper limit
234 A1 --- n_V733 [*] Note on V733 (1)
236-243 E8.3 W/m2 e_V733 ?=- Error on V733
244 A1 --- l_V883 Limit flag on V883
245-253 E9.3 W/m2 V883 ?=- V883 Ori flux density of line or
upper limit
254 A1 --- n_V883 [*] Note on V883 (1)
256-262 E7.2 W/m2 e_V883 ?=- Error on V883
264 A1 --- l_V1647 Limit flag on V1647
265-273 E9.3 W/m2 V1647 ?=- V1647 Ori flux density of line or
upper limit
274 A1 --- n_V1647 [*] Note on V1647 (1)
276-282 E7.2 W/m2 e_V1647 ?=- Error on V1647
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Note (1): * for detection below 3σ.
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Acknowledgements:
Andreas Postel, andreas.postel(at)unige.ch
(End) Patricia Vannier [CDS] 19-Sep-2019