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


Query : 2013A&A...559A..77F

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 - 2023
#notes
1 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 1000 1
2 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1012 2
3 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 102 0
4 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 428 0
5 HD 38120 Be* 05 43 11.8932782280 -04 59 49.889995692 9.08 9.10 9.1     B9Vnne 83 0
6 HD 50138 Ae* 06 51 33.3989823840 -06 57 59.450772852 6.28 6.68 6.67     A1Ib/II 214 0
7 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1787 1
8 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 515 0
9 HD 98922 Be* 11 22 31.6743077592 -53 22 11.457008148   6.80 6.76     B9Ve 126 1
10 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 253 1
11 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 744 1
12 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 330 0
13 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 424 1
14 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 193 0
15 CD-33 10685 Or* 15 45 12.8678037432 -34 17 30.644403036 12.47 11.56 10.224 9.60 8.685 K3Ve 253 1
16 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 510 0
17 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 246 0
18 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 582 1
19 V* RU Lup TT* 15 56 42.3108692112 -37 49 15.473946900 9.27 10.07 9.60     K7/M0e 432 0
20 V* RY Lup Or* 15 59 28.3864710696 -40 21 51.249496176   12.62 9.90     G8/K1IV-V 204 0
21 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 230 1
22 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 374 0
23 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 269 0
24 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 262 1
25 IRAS 16245-2423 TT* 16 27 37.1906433768 -24 30 35.025246828       16.66 14.67 B5-F2 274 0
26 V* V1003 Oph TT* 16 34 09.1696133088 -15 48 16.776092124     13.44     G5 94 0
27 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 307 0
28 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 1002 0
29 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 408 2
30 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 271 0
31 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 241 0

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2023.01.30-22:02:02

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