2013A&A...559A..77F


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:10:58

2013A&A...559A..77F - Astronomy and Astrophysics, volume 559A, 77-77 (2013/11-1)

DIGIT survey of far-infrared lines from protoplanetary disks. I. [OI], [CII], OH, H2O, and CH+.

FEDELE D., BRUDERER S., VAN DISHOECK E.F., CARR J., HERCZEG G.J., SALYK C., EVANS II N.J., BOUWMAN J., MEEUS G., HENNING T., GREEN J., NAJITA J.R. and GUEDEL M.

Abstract (from CDS):

We present far-infrared (50-200µm) spectroscopic observations of young pre-main-sequence stars taken with Herschel/PACS as part of the DIGIT key project. The sample includes 16 Herbig AeBe and 4 T Tauri sources observed in SED mode covering the entire spectral range. An additional 6 Herbig AeBe and 4 T Tauri systems have been observed in SED mode with a limited spectral coverage. Multiple atomic fine structure and molecular lines are detected at the source position: [OI], [CII], CO, OH, H2O, CH+. The most common feature is the [OI]63µm line detected in almost all of the sources, followed by OH. In contrast with CO, OH is detected toward both Herbig AeBe groups (flared and non-flared sources). An isothermal LTE slab model fit to the OH lines indicates column densities of 1013<NOH<1016cm–2, emitting radii 15<r<100AU and excitation temperatures 100<Tex<400K. We used the non-LTE code RADEX to verify the LTE assumption. High gas densities (n≥1010cm–3) are needed to reproduce the observations. The OH emission thus comes from a warm layer in the disk at intermediate stellar distances. Warm H2O emission is detected through multiple lines toward the T Tauri systems AS 205, DG Tau, S CrA and RNO 90 and three Herbig AeBe systems HD 104237, HD 142527, HD 163296 (through line stacking). Overall, Herbig AeBe sources have higher OH/H2O abundance ratios across the disk than do T Tauri disks, from near- to far-infrared wavelengths. Far-infrared CH+ emission is detected toward HD 100546 and HD 97048. The slab model suggests moderate excitation (Tex∼100K) and compact (r∼60AU) emission in the case of HD 100546. Off-source [OI] emission is detected toward DG Tau, whose origin is likely the outflow associated with this source. The [CII] emission is spatially extended in all sources where the line is detected. This suggests that not all [CII] emission is associated with the disk and that there is a substantial contribution from diffuse material around the young stars. The flux ratios of the atomic fine structure lines ([OI]63µm, [OI]145µm, [CII]) are analyzed with PDR models and require high gas density (n>105cm–3) and high UV fluxes (Go∼103-107), consistent with a disk origin for the oxygen lines for most of the sources.

Abstract Copyright:

Journal keyword(s): stars: variables: T Tauri, Herbig Ae/Be - astrochemistry - protoplanetary disks

Simbad objects: 31

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Number of rows : 31

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
2 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 932 2
3 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 95 0
4 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 358 0
5 HD 38120 Be* 05 43 11.8931815256 -04 59 49.881886291 9.08 9.10 9.1     B9Vnne 74 0
6 HD 50138 Ae* 06 51 33.3989891154 -06 57 59.445949919 6.28 6.68 6.67     A1Ib/II 198 0
7 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
8 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 458 0
9 HD 98922 Be* 11 22 31.6740564115 -53 22 11.456030308   6.80 6.76     B9Ve 114 1
10 HD 100453 Ae* 11 33 05.5765928993 -54 19 28.543792679   8.09 7.79     A9Ve 196 1
11 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
12 V* DX Cha Ae* 12 00 05.0870448691 -78 11 34.559255151   6.81 6.60     A0_sh 306 0
13 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 357 1
14 HD 139614 pr* 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 160 0
15 CD-33 10685 Or* 15 45 12.8670160092 -34 17 30.646921079 12.47 11.56 10.224 9.60 8.685 K3Ve 217 1
16 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 471 0
17 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 218 0
18 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 467 1
19 V* RU Lup Or* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 382 0
20 V* RY Lup Or* 15 59 28.3852522995 -40 21 51.255321659   12.62 9.90     G8/K1IV-V 167 0
21 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 211 1
22 V* V856 Sco Ae* 16 08 34.2868591379 -39 06 18.326059778 7.66 7.41 7.05 6.92   A7IIIne_sh 351 0
23 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 244 0
24 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 233 1
25 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 235 0
26 V* V1003 Oph Or* 16 34 09.1694383329 -15 48 16.776308800           G5 87 0
27 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 290 0
28 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 803 0
29 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 335 2
30 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 258 0
31 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 221 0

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2020.07.13-07:10:58

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